Chandra proposals are divided into the following categories:
***********************************************************************************
SOLAR SYSTEM
--------------------------------------------------
===================================================================================
Proposal Number: 03100101
Proposal Title: SEARCH FOR X-RAYS FROM URANUS ALTERNATE TARGET
PI: GORDON GARMIRE
Subject Category: SOLAR SYSTEM
Abstract: The detection of X-rays from Uranus would help constrain the mechanism
for generating X-rays in planetary magnetospheres. X-rays have been detected from
Jupiter and are likely from saturn. IUE and Voyager 2 found evidence for auroral
acitvity from Uranus, particularly from the south pole. A 30 ks observation by
Chandra should either support (if X-rays are detected) or refute the analog with
Jupiter.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
21:59:07.16 -13:08:15.30 URANUS ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03100308
Proposal Title: X-RAY OBSERVATIONS OF JUPITER
PI: J WAITE
Subject Category: SOLAR SYSTEM
Abstract: Jupiter is an interesting source of x-rays within the solar system.
ACIS and HRI observations are being analyzed at this time that will redefine the
Jovian x-ray source. Spectral observations appear to verify the charge exchange
source of energetic ions, but HRC observations indicate a source location and
oscillatory light curve that are totally unexpected. Many new questions arise. We
propose to use a combination of HRC, ACIS, and HST-STIS to investigate these
exciting new possibilities.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
08:51:29.61 +18:32:18.71 JUPITER HRC-I NONE 72.00
===================================================================================
Proposal Number: 03100792
Proposal Title: ACIS-S LOW ENERGY SPECTROSCOPY AND PHOTOMETRIC IMAGING OF CHARGE
EXCHANGE X-RAY EMISSION FROM COMET C/LINEAR WM1 (2000)
PI: CAREY LISSE
Subject Category: SOLAR SYSTEM
Abstract: Using ACIS-S observations of comet C/LINEAR 1999 S4 with Chandra in
Cycle 1, we conclusively demonstrated the presence of x-ray line emission driven
by charge exchange between highly ionized solar wind minor ions and gases emitted
from the cometary nucleus. A number of important uncertainties remain, however,
that can be answered with ACIS-S observations of the brighter, closer comet
C/LINEAR WM1 (2000) in December 2001: How many CXE lines are ultimately
detectable with Chandra in the 250 - 900 eV energy range? Can we detect spatial
hardness variations due to progressive solar wind charging from the cometary
neutrals? What is the temporal history of the emission? We request a small amount
of ACIS-S time, 35 ksec in Cycle 3, to answer these important questions.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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22:13:00.91 -51:55:03.14 C/LINEAR WM1 (2000) ACIS-S LETG 8.75
22:13:32.79 -51:51:41.80 C/LINEAR WM1 (2000) ACIS-S LETG 8.75
22:14:04.18 -51:48:16.45 C/LINEAR WM1 (2000) ACIS-S LETG 8.75
22:14:37.02 -51:44:33.07 C/LINEAR WM1 (2000) ACIS-S LETG 8.75
===================================================================================
Proposal Number: 03108065
Proposal Title: X-RAY OBSERVATIONS OF THE FIRST COUNTERPART TO A FAST X-RAY
TRANSIENT, XRF010930
PI: FIONA HARRISON
Subject Category: SOLAR SYSTEM
Abstract: Thanks to BeppoSAX we are now aware of a new type of transient -- X-ray
flashes (XRFs, also called Fast X-ray Transients). About one third of the events
seen by the WFC are XRFs. Until today, NOT A SINGLE member of this class has been
localized to arcsecond accuracy. Only gradually has the community come to
appreciate that XRFs have a rate comparable to GRBs. There are two possibilities:
1. XRFs are highly redshifted GRBs (e.g. Heise, Lloyd) 2) XRFs are explosive
events producing Lorentz factors intermediate between GRBs and SNe and thus peak
in the X-ray. On 30.25 October 2001 (UT) the BeppoSAX Wide Field Camera (WFC)
detected a XRF, hereafter XRF011030, unaccompanied by any increased rate in the
Gamma Ray Burst Monitor (GRBM) on SAX, HETE-2 or Ulysses.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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20:43:32.30 +77:17:18.90 FXRT011030 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03108067
Proposal Title: X-RAY OBSERVATIONS OF THE FIRST COUNTERPART TO A FAST X-RAY
TRANSIENT, XRF010930
PI: FIONA HARRISON
Subject Category: SOLAR SYSTEM
Abstract: Thanks to BeppoSAX we are now aware of a new type of transient -- X-ray
flashes (XRFs, also called Fast X-ray Transients). About one third of the events
seen by the WFC are XRFs. Until today, NOT A SINGLE member of this class has been
localized to arcsecond accuracy. Only gradually has the community come to
appreciate that XRFs have a rate comparable to GRBs. There are two possibilities:
1. XRFs are highly redshifted GRBs (e.g. Heise, Lloyd) 2) XRFs are explosive
events producing Lorentz factors intermediate between GRBs and SNe and thus peak
in the X-ray. On 30.25 October 2001 (UT) the BeppoSAX Wide Field Camera (WFC)
detected a XRF, XRF011030, and a Chandra DDF has found an X-ray source coincident
with a radio transient (see below).
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
20:43:32.30 +77:17:18.90 FXRT011030 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03108076
Proposal Title: SPECTROSCOPIC IMAGING OF CHARGE EXCHANGE X-RAY EMISSION FROM
COMET C/2002 C1
PI: KONRAD DENNERL
Subject Category: SOLAR SYSTEM
Abstract: Comet C/2002 C1, discovered on February 1, 2002, is predicted to be as
bright as 4 - 5 mag when it will become observable with Chandra from April 10,
2002. We propose to utilize this opportunity for direct spectroscopic imaging
with ACIS-S. This has never been done for such a bright comet. Thanks to a
favorable observing geometry, we can apply a novel observing technique: as the
comet will slowly move along the comet-Sun line, an automatic scan of the x-ray
emission properties will be provided along this direction, where the charge
exchange model predicts a characteristic spectral evolution, which could,
however, not be tested so far. While previous Chandra images and spectra of
comets suffer from low photon statistics, we expect to get about 40 times more
photons than from C/LINEAR S4. This will allow us to utilize the full spectral
and spatial resolution of Chandra. A detailed Scientific Justification is
provided in the attached Postscript file.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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C/2002 C1 ACIS-S NONE 8.00
23:20:00.22 +55:46:43.93 C/2002 C1 ACIS-S NONE 12.00
23:30:26.68 +54:54:45.40 C/2002 C1 ACIS-S NONE 12.00
===================================================================================
Proposal Number: 03108123
Proposal Title: A SEARCH FOR SOFT X-RAY AURORAS ON EARTH
PI: G. GLADSTONE
Subject Category: SOLAR SYSTEM
Abstract: Chandra HRC-I observations of Jupiter made in Dec. 2000 in support of
the Cassini flyby have revealed the surprising result that jovian auroral x-ray
emissions are concentrated in a small `hot spot' which pulsates with a ~45-m
period. The location of the hot spot near the magnetic pole implies a particle
source region near Jupiter's magnetopause, and high-latitude reconnection of
heavy solar wind ions is now a viable explanation for these soft x-ray emissions.
The identical process should operate at Earth as well. Hard x-ray emissions from
electron bremsstrahlung are well known in the terrestrial aurora. Surprisingly,
however, there have been no searches of Earth's aurora for emissions at <2keV. We
propose here a simple slew observation by HRC-I across the auroral region to look
for Earth's soft x-ray aurora. The detection of a Jupiter-like hot spot at Earth
would imply that heavy ion solar wind charge exchange is important for producing
x-rays at planets as well as comets.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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05:26:24.00 -32:51:00.00 EARTH HRC-I NONE 1.00
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NORMAL STARS AND WD
--------------------------------------------------
===================================================================================
Proposal Number: 03200012
Proposal Title: A YSO-LIKE PULSED ASTROPHYSICAL JET AND BIPOLAR NEBULA IN A
DYING STAR: WFPC2/STIS STUDY OF HE2-90
PI: RAGHVENDRA SAHAI
Subject Category: NORMAL STARS AND WD
Abstract: We have discovered an extended, highly-collimated, bipolar jet in
He2-90, an object long classified as a planetary nebula (PN). The discovery
images (obtained with WFPC2/HST) show that the morphology of He2-90 does not look
like that of any known PN, but resembles that of a classical young stellar object
(YSO). This appears to be a unique object. We propose to map the jet near the
central source using the long-slit, medium resolution mode of STIS. We also
propose Chandra X-ray observations (with ACIS-I) to check the association of an
EGRET >~mma-ray source which lies in the direction of He2-90.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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13:09:36.40 -61:19:36.30 HEN2-90 ACIS-S NONE 10.00
===================================================================================
Proposal Number: 03200024
Proposal Title: ORIGIN OF THE X-RAY EMISSION OF THE PREMAIN SEQUENCE STAR V 410
TAU
PI: PETER PREDEHL
Subject Category: NORMAL STARS AND WD
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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04:18:31.10 +28:27:16.00 V 410 TAU ACIS-S NONE 11.20
04:18:31.10 +28:27:16.00 V 410 TAU ACIS-S NONE 15.00
04:18:31.10 +28:27:16.00 V 410 TAU ACIS-S NONE 18.80
===================================================================================
Proposal Number: 03200038
Proposal Title: PROBING THE GAS IN THE V471 TAU SYSTEM WITH ABSORPTION
SPECTROSCOPY
PI: FREDERICK WALTER
Subject Category: NORMAL STARS AND WD
Abstract: The eclipsing dA+K2V binary V471 Tau affords an opportunity to use
X-ray absorption to probe the spatial extent of the chromosphere/corona of an
active dwarf star. HST observations have shown chromospheric and transition
region species (O I through N V) in absorption at radial extents of up to 2 K
star radii on one side of the star, but not on the other. X-ray observations have
revealed large absorption dips, primarily but not exclusively from gas near the
inner Lagrangian points of the system. CHANDRA can probe the neutral gas, by
observing the time-variability of the neutral Hydrogen absorption column, and by
oberving the variations of the depths of absorption edges. The white dwarf
photosphere provides a bright, soft continuous spectrum against which to observe
these changes.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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03:50:25.00 +17:14:47.40 V471 TAU HRC-S LETG 90.00
===================================================================================
Proposal Number: 03200050
Proposal Title: VIOLENT MASSIVE STAR FORMATION IN THE GALAXY: W51 ALTERNATE
TARGET
PI: GORDON GARMIRE
Subject Category: NORMAL STARS AND WD
Abstract: The proposed observation of W51 will provide a valuable springboard to
understanding starbursts in galaxies other than our own.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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19:23:40.00 +14:31:06.00 W51 ACIS-I NONE 21.00
19:23:40.00 +14:31:06.00 W51 ACIS-I NONE 59.00
===================================================================================
Proposal Number: 03200056
Proposal Title: HIGH RESOLUTION SPECTROSCOPY OF THE YOUNG STELLAR CLUSTER NGC
2362
PI: CLAUDE CANIZARES
Subject Category: NORMAL STARS AND WD
Abstract: We propose a deep HETGS observation of the young stellar cluster NGC
2362. Only 5-7 Myrs old, NGC 2362 is one of the youngest clusters in our Galaxy.
Unlike in most other star forming regions, this cluster is almost completely
devoid of residual gas and it is somewhat deficient in low-mass stars. It main
star, tau CMa, is actaully at least a double star with quite equal massive
constituents and is believed that it already eveloved away from the zero-age main
sequence (ZAMS). As part of our program to perform high resolution spectroscopy
on very young early type O stars we observe tau CMa for 95 ks in order to search
for X-ray emission from dense and hot plasmas. This cluster also enables us to
study high resolution X-ray spectra of ZAMS B-type stars. stars and will provide
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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07:18:43.00 -24:56:59.90 NGC2362 ACIS-S HETG 47.00
07:18:43.00 -24:56:59.90 NGC2362 ACIS-S HETG 48.00
===================================================================================
Proposal Number: 03200079
Proposal Title: HETGS SPECTROSCOPY OF THE LONG-PERIOD ACTIVE BINARY, IM PEGASI.
PI: DAVID HUENEMOERDER
Subject Category: NORMAL STARS AND WD
Abstract: RS CVn binary systems are well known for their activity, interpreted as
large-scale versions of Solar phenomena: spots, prominences, coronae, all with
dynamic behavior. Stellar X-ray luminosity is well known to correlate with
rotation and RS CVn stars are among the most luminous of late-type sources; they
are prime candidates for X-ray spectroscopy. IM Peg is a long-period system
(25d), and relatively X-ray luminous. We propose to obtain 8 HETGS spectra
sampled several times during 2-3 rotations. Each exposure will well expose strong
lines and also provide an integrated flux. Summed spectra will be used for
deriviation of emission measure and abundances. Both long and short-term
variability will be examined and correlated with activity diagnostics.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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22:53:02.30 +16:50:28.30 IM PEG ACIS-S HETG 25.00
22:53:02.30 +16:50:28.30 IM PEG ACIS-S HETG 25.00
22:53:02.30 +16:50:28.30 IM PEG ACIS-S HETG 25.00
22:53:02.30 +16:50:28.30 IM PEG ACIS-S HETG 25.00
22:53:02.30 +16:50:28.30 IM PEG ACIS-S HETG 25.00
22:53:02.30 +16:50:28.30 IM PEG ACIS-S HETG 25.00
22:53:02.30 +16:50:28.30 IM PEG ACIS-S HETG 25.00
22:53:02.30 +16:50:28.30 IM PEG ACIS-S HETG 25.00
===================================================================================
Proposal Number: 03200093
Proposal Title: X-RAYS FROM STARS AT THE FAR END OF THE MAIN SEQUENCE
PI: GORDON GARMIRE
Subject Category: NORMAL STARS AND WD
Abstract: ACIS observations and detection of HH2 has shown that these outflows
can generate X-rays when they strike the ISM. To increase the sample, we propose
to search for HH80/81 which should be more luminous but farther away..
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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18:19:06.06 -20:51:55.22 HH80/81 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03200086
Proposal Title: HIGH-RESOLUTION SPECTRA OF T TAURI STARS
PI: STEPHEN MURRAY
Subject Category: NORMAL STARS AND WD
Abstract: We request a 35 (to 100) ksec observation (depending upon actual target
approved) with the HETGS to characterize the corona of a young pre-main sequence
star by measuring density sensitive x-ray lines and estimating the mean coronal
density of the (presumed) emitting loop structures. In the cases of the fast
rotator targets (Speedy Mic or HD 283572), we also expect to be able to estimate
the radial extent of the coronal structure by the detecting possible broadening
of the emitted lines. (Our simulation for HD 283572 suggests we may see this
effect for it and, even more likely, for Speedy Mic). By combining density and
the radial extent estimates, we can gain a better picture of the corona of young
fast rotator stars. GTO Priority "B"
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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20:47:45.00 -36:35:40.80 SPEEDY MIC ACIS-S HETG 35.00
20:47:45.00 -36:35:40.80 SPEEDY MIC ACIS-S HETG 35.00
===================================================================================
Proposal Number: 03200049
Proposal Title: AN X-RAY STUDY OF X-RAYS FROM THE BETA PIC SYSTEM
PI: GORDON GARMIRE
Subject Category: NORMAL STARS AND WD
Abstract: Search for X-rays from possible planets around Beta Pic displaced from
Beta Pic itself.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:47:17.00 -51:03:59.40 BETA PIC ACIS-S NONE 10.00
===================================================================================
Proposal Number: 03200161
Proposal Title: A HIGH-RESOLUTION STUDY OF THE ACTIVE BINARY SYSTEM V824 ARA
PI: STEPHEN DRAKE
Subject Category: NORMAL STARS AND WD
Abstract: We propose to observe the active G5+K0 dwarf binary system V824 Ara (HD
155555), a very young (zero-age main-sequence or pre-main sequence) system with a
1.68 day orbital period, using the Chandra ACIS-S/HETG instrument. V824 Ara is a
synchronized binary similar in age to the prototype young single K dwarf AB Dor.
We will study the X-ray spectrum, both integrated over the whole exposure and as
a function of orbital/rotational phase and overall emission level. We will use
these spectra to infer the coronal temperature structure or DEM, and elemental
abundances. We will compare these coronal properties to those of evolved active
binaries (e.g., AR Lac), and also to those of AB Dor and similar young stars, to
see if there are discernible differences due to binarity and evolutionary stage.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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17:17:25.50 -66:57:03.00 V824 ARA ACIS-S HETG 100.00
===================================================================================
Proposal Number: 03200170
Proposal Title: HARD X-RAY EMISSION FROM THE CLASS I AND CLASS 0 OUTFLOW SOURCES
IN L1630
PI: THEODORE SIMON
Subject Category: NORMAL STARS AND WD
Abstract: The L1630 dark cloud contains three very rare Class 0 and at least six
Class I protostars. Several of them are tightly clustered around HH 24-26, a site
of molecular jets and a luminous but unresolved ASCA X-ray source. We propose to
image this region for 70 ks with the ACIS-S in order to (a) search for the onset
of X-ray emission in the Class 0 stars, (b) perform precise astrometry of the
X-ray emission of the Class I stars, and (c) from spectrometry of the Class I
sources, derive spectral parameters of their associated X-ray sources. Our goal
is to establish an evolutionary progression in X-ray properties within a single
cloud and thus explore the relationship between protostellar X rays, accretion
disks, magnetically collimated jets, and large-scale molecular outflows.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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05:46:08.40 -00:11:52.00 HH 24-26 ACIS-S NONE 70.00
===================================================================================
Proposal Number: 03200178
Proposal Title: THE LOW-MASS POPULATION OF NGC2264 AND ITS CORONAL PROPERTIES.
PI: SALVATORE SCIORTINO
Subject Category: NORMAL STARS AND WD
Abstract: We propose to perform a Chandra ACIS-I 100 ks observation of the star
forming region NGC 2264 (in Monoceros), achieving an unprecedent sensitivity of
fx ~ 5e-16 erg cm-2 s-1 (0.1-4 kev), or Lx ~ 4e28 erg s-1 (for the commonly
assumed distance of 760 pc). This will allow us to detect more than 85% of NGC
2264 low-mass members at least down to 0.1 Msun and a sizable fraction of even
lower mass members making possible: 1) to derive a reliable Initial Mass Function
(IMF) at the very low-mass end, 2) to investigate the role of magnetic fields in
the formation process and resulting IMF, 3) to test the coronal emission level of
young brown dwarfs, 4) to study the relation between coronal emission level and
PMS evolution during the first 3-10 millon year of stellar lifetime.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
06:40:58.10 +09:34:00.40 NGC 2264 ACIS-I NONE 100.00
===================================================================================
Proposal Number: 03200188
Proposal Title: ON THE ORIGIN OF THE X-RAY EMISSION IN LATE B-TYPE STARS
PI: NURIA HUELAMO
Subject Category: NORMAL STARS AND WD
Abstract: We propose for Chandra observations of X-ray emitting late B-type
stars. Because they are (theoretically) not expected to emit X-rays, their X-ray
detections have been attributed to unresolved late-type, magnetically active
stars. The aim of this study is to resolve close binary systems comprised of late
B-type stars and visual late-type companions, in order to identify the X-ray
emitter. The binary separations are between (1-8)'', i.e. well resolvable by
Chandra but not with previous instruments. If we found that X-rays are always
emitted by the late-type companions, it can be taken as evidence against
intrinsic X-ray emission from late B-type stars. If not, it would indicate that
these stars could be intrinsic X-ray emitters and stellar theories may have to be
revised.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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00:20:39.00 -69:37:29.70 HD1685 ACIS-I NONE 2.40
14:08:51.90 -43:28:14.80 HD123445 ACIS-I NONE 2.30
15:08:12.10 -40:35:02.10 HD133880 ACIS-I NONE 2.40
18:31:22.40 -62:16:41.90 HD169978 ACIS-I NONE 2.40
===================================================================================
Proposal Number: 03200237
Proposal Title: UNDERSTANDING THE ENGINE OF GROWTH IN PLANETARY NEBULAE
PI: JOEL KASTNER
Subject Category: NORMAL STARS AND WD
Abstract: We propose a survey of X-ray emission from planetary nebulae (PNs) that
builds on our previous Chandra discoveries of extended X-ray emission from PNs.
The proposed program, consisting of Chandra/ACIS observations of a sample of
well-studied, representative objects, has the potential to firmly establish
extended X-ray emission as a defining characteristic of the class of young,
molecule-rich PNs. By enabling the investigation of the morphology and evolution
of X-ray emission in PNs and the determination of physical conditions that are
otherwise inaccessible to study in these nebulae, these observations will provide
stringent tests of contemporary theories of PN formation and evolution.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
07:37:18.60 -09:38:48.00 M 1-16 ACIS-S NONE 50.00
16:17:12.60 -51:59:08.00 MZ 3 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03200240
Proposal Title: CORONAL EVOLUTION IN SINGLE GIANTS WITH CHANDRA LETGS X-RAY
SPECTROSCOPY
PI: JURGEN SCHMITT
Subject Category: NORMAL STARS AND WD
Abstract: We propose to obtain high resolution Chandra LETGS spectra of the three
single giants 24 UMa, $\beta$ Cet and 39 Cet. These stars are located at
strategic places in the HR-diagram covering the mass range between 1.6 - 3 solar
masses. The data will be sensitive enough to carry out detailed plasma
diagnostics of the coronae of evolved stars. Density diagnostics, differential
emission measure construction and abundance analysis will be carried out. A
comparison to photospheric abundances will be performed since $beta$ Cet has
solar abundances, while the other target stars do not. The three target stars are
the only single giants within practical reach of the Chandra LETGS and will allow
us to study the influence of stellar mass on activity among giant stars.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:43:35.30 -17:59:12.00 BETA CETI HRC-S LETG 110.00
===================================================================================
Proposal Number: 03200289
Proposal Title: THE AGE-ROTATION-ACTIVITY RELATION IN LATE-TYPE STARS BETWEEN
~1-10 MYR
PI: JOHN STAUFFER
Subject Category: NORMAL STARS AND WD
Abstract: We propose to conduct a fundamental census of X-ray emission from stars
in Orion and NGC 2264 for which we have a wealth of supporting multi-wavelength
data. This will allow us to investigate a wide variety of scientific questions.
The most important scientific goal of this study is investigating the
relationship between age, rotation, and X-ray activity for late-type stars
ranging in age from ~1-10 Myr. Understanding the X-ray environment of young stars
and how rotation is related to X-ray flux has direct implications for the
chemical and dynamical evolution of protoplanetary disks, and, consequently, for
planet formation.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:35:05.60 -05:41:04.70 ONC FLANKING FIELD S ACIS-I NONE 50.00
05:35:19.10 -04:48:31.40 ONC FLANKING FIELD N ACIS-I NONE 50.00
06:40:48.00 +09:50:60.00 NGC 2264 ACIS-I NONE 50.00
===================================================================================
Proposal Number: 03200359
Proposal Title: STELLAR CORONAE AT THE BOTTOM OF THE MAIN SEQUENCE: A
MULTI-WAVELENGTH STUDY
PI: ROBERT RUTLEDGE
Subject Category: NORMAL STARS AND WD
Abstract: It is well established that coronal activity dramatically decreases at
the bottom of the main sequence. This was expected: the transition near type M2.5
to fully convective interiors gave impetus for the search for a decline in
coronal activity. However, most of the decline occurs later than this transition.
Even there, X-ray, H-alpha, and radio flaring continues to at least as late as
the brown dwarf LP 944-20 (M9.5), and perhaps is the only means of releasing
magnetic energy from an apparently still active dynamo. This leaves us with the
question: what is supressing the persistent coronal emission, even as the
magnetic flares continue? We will address this question by observing low-mass
stars from M6 to L6 in X-ray, H-alpha, and radio wavelengths.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:36:16.00 +18:21:10.00 2MASSW0036+18 ACIS-S NONE 22.00
15:07:48.00 -16:27:38.00 2MASSW1507-16 ACIS-S NONE 28.00
===================================================================================
Proposal Number: 03200381
Proposal Title: STAR FORMATION IN QUIESCENT GIANT MOLECULAR CLOUDS
PI: ERIC FEIGELSON
Subject Category: NORMAL STARS AND WD
Abstract: Most stars are formed in rich stellar clusters within giant molecular
clouds (GMCs). A wide range in GMC star formation efficiencies exists -- half of
GMCs do not have even a single O star. The reason for GMC quiescence is poorly
understood. We propose a Chandra ACIS observation of the prototype quiescent GMC,
G 216-2.5 or Maddalena's Cloud, which will have extraordinary sensitivity to its
present and past star formation rate. This is achieved because pre-main sequence
stars of all masses and a wide range of ages have greatly enhanced X-ray
emission. Possible outcomes are a episodic star formation, a truncated IMF, or
true quiescence. Any of these results will have significant implications for star
formation in the Galaxy.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
06:49:05.50 -04:33:50.00 MADDALENA'S CLOUD ACIS-I NONE 30.00
===================================================================================
Proposal Number: 03200497
Proposal Title: BURIED ALIVE IN THE CORONAL GRAVEYARD?!
PI: THOMAS AYRES
Subject Category: NORMAL STARS AND WD
Abstract: We propose 20 ks pointings with Chandra HRC-I to obtain detections of 3
red giants in the depths of the "coronal graveyard." Stellar coronal activity is
important to the Sun-Earth connection, to the fate of primitive planetary
atmospheres, and to a broad reaching set of magnetic phenomena in many cosmic
environments. Understanding the activity, and its evolution, therefore is a key
objective in astrophysics. The birth of magnetic activity in young stars is
well-studied; the death of coronae in highly evolved stars is not. Our program
ultimately will test the hypothesis that significant coronal activity persists on
the red giants, but smothered beneath a "cool absorber" in the chromospheric
envelope. Such activity might be the long-sought initiator of red giant winds.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
04:35:55.20 +16:30:33.00 ALPHA TAURI HRC-I NONE 20.00
14:15:39.60 +19:10:57.00 ALPHA BOOTIS HRC-I NONE 20.00
===================================================================================
Proposal Number: 03200546
Proposal Title: HIGH ENERGY EMISSION FROM THE YOUNG MASSIVE CLUSTER RCW 38
PI: SCOTT WOLK
Subject Category: NORMAL STARS AND WD
Abstract: Taking advantage of Chandra's unique capabilities, we propose to study
the youngest, most embedded, massive cluster studied to date in X-rays - RCW 38.
The immediate goals of this project are the identification of the embedded PMS
stellar population, the investigation of the X-ray properties of the individual
class 0-III sources (~10 class 0 & I protostars) and the derivation of a XLF for
an extremely young (~0.5 Myr) massive cluster. We will derive the gas-to-dust
ratio and its variations towards hundreds of lines of sight across the cluster.
Complementary NIR data already taken with the VLT, which probe approximately the
same cloud depths, allow an unique multi-wavelength description of a massive star
formation episode and its consequences to the surrounding interstellar medium.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
08:59:19.20 -47:30:22.00 RCW 38 ACIS-I NONE 100.00
===================================================================================
Proposal Number: 03200558
Proposal Title: DENSITY STRATIFICATION OF THE VERY HOT CORONA OF YY MENSAE
PI: MANUEL GUEDEL
Subject Category: NORMAL STARS AND WD
Abstract: Chandra HETGS observations give access to a number of He-like line
triplets that are sensitive to the density of hot coronal plasma. The present
proposal requests observing time on an outstanding single star that has revealed
an extremely hot and luminous corona. We aim at measuring the density structure
of its corona together with its anomalous abundances. The target, YY Mensae,
reveals a corona in which 90 percent of the emission measure resides at 30-40 MK.
It has been suggested that such coronae are heated by statistical flares. A
thorough spectroscopic study of this object could decide on whether its corona is
indeed composed of numerous high-density compact flaring loops. The emission
measure distribution will be studied to investigate whether it is generated by
frequent flaring.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
04:58:17.90 -75:16:38.00 YY MEN, HD 32918 ACIS-S HETG 90.00
===================================================================================
Proposal Number: 03200561
Proposal Title: HEAVY ION TRANSPORT: MULTI-TEMPERATURE ABUNDANCE STUDIES OF THE
ACTIVE RS CVN LAMBDA AND
PI: NANCY BRICKHOUSE
Subject Category: NORMAL STARS AND WD
Abstract: We propose a 100 ks observation with Chandra LETG to conduct a
comprehensive study of the coronal abundances of the active binary Lambda And.
Chandra HETG observations of Lambda And indicate that the Ne/Fe abundance at high
temperature (10 million K) is about four times larger than the abundance at lower
coronal temperature (1 million) K. LETG offers unique coverage of intermediate
ionization states of many elements, as well as high resolution to isolate weaker
lines from ions previously unresolved by EUVE. Determining the abundance patterns
under different physical conditions in the same system will constrain models of
acceleration, heating, diffusion, and gravitational settling. We will measure
abundances for C, N, O, Ne, Mg, Si, S, and Fe across a broad temperature range.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
23:37:33.80 +46:27:29.30 LAMBDA AND HRC-S LETG 50.00
23:37:33.80 +46:27:29.30 LAMBDA AND HRC-S LETG 50.00
===================================================================================
Proposal Number: 03200569
Proposal Title: X-RAY DOPPLER IMAGING OF CONTACT BINARIES: THE PARTIALLY
ECLIPSING VW CEP
PI: NANCY BRICKHOUSE
Subject Category: NORMAL STARS AND WD
Abstract: Chandra LETG observations of the X-ray bright contact binary VW Cep
will provide diagnostics of coronal structures under the extreme conditions of
rapid rotation. Optical Doppler images of VW Cep have recently provided the first
evidence for large polar spots on a contact binary, similar to polar spots
observed on the less rapidly rotating RS CVn systems. We propose to exploit the
unique spectral resolution of the LETG at long wavelengths to search for Doppler
line shifts from the orbiting poles. Phase-resolved emission line intensity
diagnostics for temperature, density, and abundances will complement the velocity
measurements. This test for localized activity could definitively establish a new
coronal phenomenon in fast rotators.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
20:37:21.50 +75:36:01.50 VW CEP HRC-S LETG 100.00
===================================================================================
Proposal Number: 03200598
Proposal Title: X-RAYS FROM BROWN DWARFS IN THE SIGMA ORIONIS CLUSTER
PI: SCOTT WOLK
Subject Category: NORMAL STARS AND WD
Abstract: We propose a deep HRC-I observation of the young star forming region
around Sigma Orionis to detect X--ray emission from young brown dwarfs (BDs)
which have been discovered there. We will also measure of the X--ray luminosity
of a well understood sample of hundreds of PMS stars. Detections of BDs by
Chandra have been sparse, this is, in part, because the detector of choice for
clusters, ACIS-I, has very low effective area where BDs are bright, below 400 eV.
The Sigma Ori cluster is uniquely suited to this study; it spans different
stellar interior conditions, almost 3 orders of magnitude in mass, it is
relatively close, almost dust free (5% of the ONC), the proper age to have a good
mix of stars with and without disks and we have measured its mass function well
below the BD limit.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:38:44.80 -02:36:00.20 SIGMA ORIONIS HRC-I NONE 100.00
===================================================================================
Proposal Number: 03200602
Proposal Title: STELLAR WINDS FROM DME STARS
PI: BRADFORD WARGELIN
Subject Category: NORMAL STARS AND WD
Abstract: Despite the fact that the most stars have low mass and lie on the main
sequence, we know virtually nothing about their stellar winds. Existing
measurements of stellar winds extend down only to a few times 1e-10 M_solar/yr
and only apply to high-mass stars and red giants and supergiants. With Chandra's
unparalleled imaging resolution, high sensitivity, and energy resolution, winds
from nearby dwarf stars are now detectable via their X-ray emission from the
charge exchange of stellar wind ions with neutral gas in the ISM. Our proposed
observations of dwarf M flare stars will be capable of imaging stellar winds
comparable to those of the Sun (mass loss rate 2e-14 M_solar/yr), and will
provide information on wind and magnetosphere geometry, ion composition, and mass
loss rates.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:49:49.49 -23:50:11.00 ROSS 154 ACIS-S NONE 60.00
===================================================================================
Proposal Number: 03200661
Proposal Title: X-RAY EVOLUTION OF ACCRETING PROTOSTARS
PI: PHILIPPE ANDRE'
Subject Category: NORMAL STARS AND WD
Abstract: Recent developments have shown that the environment of protostars plays
an important role for their structure and evolution: in dense clusters like
Ophiuchus they have relatively compact envelopes and a rapidly decreasing
accretion rate; in dispersed regions like Taurus they have the extended envelopes
and constant accretion rates considered by the standard model of star formation.
We want to investigate for the first time the corresponding evolution of the
X-ray emission (over time scales ~10^4-10^5 yrs) in Taurus, and search whether
protostellar structure, evolution, and X-ray emission are related. Such a
relation could be the result of feedback effects of X-rays on accretion and
outflow acceleration.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
04:21:56.90 +15:29:46.00 IRAM04191 ACIS-I NONE 20.00
04:39:53.90 +26:03:10.00 L1527 ACIS-I NONE 13.00
04:39:53.90 +26:03:10.00 L1527 ACIS-I NONE 20.00
===================================================================================
Proposal Number: 03200663
Proposal Title: A TALE OF TWO G STARS
PI: THOMAS AYRES
Subject Category: NORMAL STARS AND WD
Abstract: High-quality HETGS exposures of key coronal stars are presenting a
unique, novel view of some of the most ubiquitous high-energy phenomena in the
galaxy; and taking crucial steps toward making X-ray spectroscopy an
indispensable remote-sensing tool for Astronomy. We will focus on the influence
of stellar surface gravity by adding to our ongoing program the active G dwarf
Chi1 Orionis (G0V) and the active G giant 24 Ursae Majoris (G4III). Chandra
transmission grating spectroscopy offers a new way to determine temperatures and
densities in the hot outer atmospheres of cool stars, probe chemical
fractionation processes, and explore plasma dynamics. Our program will add to the
Chandra Emission Line Project and help interpret lower-res XMM-Newton/RGS spectra
of fainter stars.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
09:34:28.80 +69:49:49.00 24 URSAE MAJORIS ACIS-S HETG 33.52
09:34:28.80 +69:49:49.00 24 URSAE MAJORIS ACIS-S HETG 50.00
09:34:28.80 +69:49:49.00 24 URSAE MAJORIS ACIS-S HETG 50.00
===================================================================================
Proposal Number: 03200659
Proposal Title: A CHANDRA STUDY OF THE PLANETARY NEBULA NGC 246
PI: ANDREW SZENTGYORGYI
Subject Category: NORMAL STARS AND WD
Abstract: We propose ACIS observations of the planetary nebula NCG 246 to search
for nebular emission from thermal gas at temperatures between 300,000 and 1
million K. In models of wind-blown bubbles, the fast wind from the central star
(3500 km/s for NGC 246) shocks when it encounters the high pressure imposed by
the external shell. New images of NGC 246 in [Ne V] show an exceptionally bright
structure surrounding a faint central region, possibly a tracer of the boundary
of the wind-blown bubble. Since the central star has Wolf-Rayet abundances, the
CNO-processed gas is expected to have an enormous cooling rate. ACIS images and
spectra will constrain the temperature, composition, and density of the X-ray
emitting gas inside [Ne V] boundary.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:47:03.00 -11:52:20.00 NGC 246 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03200672
Proposal Title: STAR FORMATION AND MYSTERIOUS HARD X-RAY EMISSION IN THE VERY
YOUNG HII REGION, TRIFID NEBULA
PI: JEONGHEE RHO
Subject Category: NORMAL STARS AND WD
Abstract: The Trifid Nebula (M~20) is one of the best-known HII regions, ionized
by a single O7.5 star, HD 164492. The Trifid was rediscovered as a dynamic,
"pre-Orion" star forming region containing young stars undergoing violent mass
ejections. The ROSAT image revealed strong emission from HD 164492 and a dozen
X-ray sources. ASCA spectra of the O star show an unexpectedly hot (3 keV)
component in addition to a cooler component from the O star atmosphere. We
propose an ACIS-S observation of the Trifid Nebula for 60 ks. The sub arcsec
image will resolve the O star from its immediate environment, and likely detect
hundreds of low mass objects. We will examine the high-energy interaction between
the wind from the O star and the dense ISM.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:02:30.31 -23:01:29.40 TRIFID NEBULA ACIS-I NONE 60.00
===================================================================================
Proposal Number: 03200677
Proposal Title: PHASE-RESOLVED SPECTROSCOPY OF THETA-1 ORIONIS C (O7 V)
PI: MARC GAGNE
Subject Category: NORMAL STARS AND WD
Abstract: We propose to obtain phase-constrained HETG spectra of the candidate
magnetic O star theta-1 Orionis C, the ionizing source of the Orion Nebula.
theta-1 Ori C exhibits remarkable 15.4-day periodic X-ray, UV and optical line
variations thought to arise from the interaction of a radiatively driven O-star
wind with a magnetosphere. New MHD calculations predict that strong X-ray shocks
and rotational modulation occur if the magnetic poles are inclined with respect
to the rotation axis. HEG and MEG spectra obtained at X-ray min (phase 0.5) and
max (phase 0.0) along with archival spectra obtained at phases 0.82 and 0.37 will
be used to measure line ratios, line profiles and phase-dependent temperatures,
abundances, and absorption to test magnetic wind shock emission models.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:35:16.50 -05:23:23.10 HD 37022 ACIS-S HETG 50.00
05:35:16.50 -05:23:23.10 HD 37022 ACIS-S HETG 50.00
===================================================================================
Proposal Number: 03200678
Proposal Title: RESOLVING THE MASSIVE OB CORE OF THE YOUNG CLUSTER NGC 6193
PI: STEPHEN SKINNER
Subject Category: NORMAL STARS AND WD
Abstract: Located at the center of the young open cluster NGC 6193 are two nearly
identical O stars HD 150135 (O6V) and HD 150136 (O5 III-V), separated by only 10
arc-secs. This pair was detected as a bright variable X-ray source by ROSAT, but
was not resolved. We propose to use ACIS-S/HETG to resolve the pair and determine
the origin of the X-ray emission. The HETG spectrum will allow us to discriminate
between X-rays from radiative shocks in the winds of one or both O stars and
colliding wind shock emission in HD 150136, which is known to be a O + O
spectroscopic binary. The sensitive ACIS-S image will provide the first accurate
X-ray census of the massive OB concentration at the center of NGC 6193.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:41:20.40 -48:45:46.60 HD 150136 ACIS-S HETG 95.00
===================================================================================
Proposal Number: 03200698
Proposal Title: CORONAL DYNAMICS AND THE COMPLETE FLARE ENERGY BUDGET FOR THE M
DWARF FLARE STAR AD LEO
PI: ALEXANDER BROWN
Subject Category: NORMAL STARS AND WD
Abstract: We propose coordinated Chandra-HETGS (110 ksec), HST-STIS (6 orbits),
and FUSE (50 ksec) observations of the the dMe flare star AD Leo to accurately
measure for the first time the complete energy budget for coronal flares. FUV
observations of the Fe XVIII 975 A and Fe XXI 1354 A coronal forbidden lines are
needed from FUSE and STIS to determine the dynamical energy losses of the flares.
HETGS spectra will be used to measure the temporal changes in the coronal
emission measure, temperature, density, and elemental abundances. AD Leo is one
of the brightest dMe stars in X-rays and flaring rate data suggests that we
should see about 10 moderate (factor of a few) and one large (factor of 10-20
enhancement) flares in a 30 hour observation.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
10:19:36.22 +19:52:11.60 AD_LEO ACIS-S HETG 50.00
===================================================================================
Proposal Number: 03200704
Proposal Title: CHANDRA HETGS OBSERVATIONS OF THE RAPIDLY ROTATING OE STAR ZETA
OPH
PI: WAYNE WALDRON
Subject Category: NORMAL STARS AND WD
Abstract: We propose a 92 ks Chandra HETG observation of the O 9.5V(e) star Zeta
Oph. Several very interesting results have emerged from HETG observations of O
stars, e.g., not only are the X-rays distributed throughout the stellar wind, we
also find X-ray emission from high ion stages (S XV and Si XIII) at the base of
the wind. These results were determined from O stars with moderately thick winds.
To probe near surface X-ray emission characteristics we need high resolution
spectra of an O star in an optically thin environment. Zeta Oph is the ideal
target. It is a well know X-ray source, relatively bright in X-rays, has an
optically thin windto all HETG X-rays, and is one of the most rapidly rotating O
stars, showing Be characteristics, which by itself makes it a very interesting
target.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:37:09.40 -10:34:02.00 ZETA OPH ACIS-S HETG 40.00
16:37:09.40 -10:34:02.00 ZETA OPH ACIS-S HETG 52.00
===================================================================================
Proposal Number: 03200743
Proposal Title: OBSERVING FAST AND MASSIVE HOT STAR WINDS IN THE CYG OB2
ASSOCIATION
PI: JOSEPH CASSINELLI
Subject Category: NORMAL STARS AND WD
Abstract: We will use HETG spectra of the very luminous star Cyg OB2 8a to
investigate the effects of higher speeds and denser winds on resolved X-ray line
profiles. Higher ion stages and a greater attenuation of line emission from the
far side of the star are expected. These observations could explain the anomalous
broadening of X-ray emission lines in Chandra spectra of other O-stars. We can
simultaneously obtain another HETG spectrum and several ACIS spectra of other
early-type stars in the association.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
20:33:15.10 +41:18:50.50 CYG OB2 8A ACIS-S HETG 70.00
===================================================================================
Proposal Number: 03200765
Proposal Title: TRACING THE CHRONICLE OF MASSIVE YOUNG STARS IN A GIANT
MOLECULAR CLOUD NGC 6334
PI: YU-ICHIRO EZOE
Subject Category: NORMAL STARS AND WD
Abstract: We propose 40 ksec X 2 pointing observations of NGC 6334 with the
Chandra ACIS-I. It is one of the most luminous giant molecular clouds in infrared
and X-rays, and contains many active massive star-forming regions at different
stages of stellar evolution. With ASCA, we found luminous high-temperature X-ray
emission from these regions. With Chandra, we can resolve young stellar objects
at various evolution stages simultaneously, and study the X-ray properties of
young stellar objects as a function of the evolutionary stage.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:20:01.00 -35:56:07.00 NGC 6334 REGION 2 ACIS-I NONE 40.00
17:20:54.00 -35:47:04.00 NGC 6334 REGION 1 ACIS-I NONE 40.00
===================================================================================
Proposal Number: 03200773
Proposal Title: HIGH-RESOLUTION X-RAY SPECTROSCOPY OF BETA CRUCIS: A NEARBY HOT
STAR WITH A HIGH X-RAY COUNT RATE
PI: DAVID COHEN
Subject Category: NORMAL STARS AND WD
Abstract: We propose to use HETG spectroscopy to diagnose the bulk motions and
the temperature and density distributions in the hot plasma on the nearby
early-type star beta Cru. We will use these data to constrain our models of
hot-star X-ray production: the intrinsic wind shock (IWS) model as well as the
magnetically confined wind shock (MCWS) model. Beta Cru is the brightest normal
hot star not already observed with Chandra, and will provide a high
signal-to-noise HETG spectrum. We will make detailed comparisons with the HETG
data from the several other hot stars observed with this instrument. Comparisons
with the anomalous star, tau Sco, which is of a very similar spectral type to
beta Cru will be especially illuminating.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:47:43.30 -59:41:19.50 BETA CRU ACIS-S HETG 90.00
===================================================================================
Proposal Number: 03200776
Proposal Title: INVESTIGATING COLLIDING WINDS AND MAGNETISED STARS IN YOUNG
PLANETARY NEBULAE IMAGED WITH HST
PI: RAGHVENDRA SAHAI
Subject Category: NORMAL STARS AND WD
Abstract: The biggest stumbling blocks to progress in our understanding of the
death of intermediate-mass stars and the accompanying formation of planetary
nebulae (PNs), are the complex stellar-wind episodes and the interactions between
them which occur during the post-AGB phase. We propose ACIS-S observations of 5
young PNs with very fast outflows for which HST emission-line images are
available, in order to directly probe the very hot (10$^{7-8}$K) shocked gas
resulting from the most recent wind-wind interactions in these objects, as well
as compact X-ray emission from the (possibly) magnetised central stars. A
comparative analysis of the CXO and HST data on these PNs, supplemented by
detailed modelling, will be invaluable in solving the mystery of how PNs are
formed and shaped.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
13:39:34.70 -67:22:51.00 MYCN 18 ACIS-S NONE 40.00
14:11:52.20 -51:26:24.00 HEN2-104 ACIS-S NONE 20.00
17:05:37.70 -10:08:32.50 M 2-9 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03200352
Proposal Title: STUDY OF THE X-RAY EMISSION MECHANISM AND ITS EVOLUTION OF BROWN
DWARFS
PI: KATSUJI KOYAMA
Subject Category: NORMAL STARS AND WD
Abstract: We propose ACIS-S observations on two intermediate-age (10-600 Myr)
brown dwarfs, PC 0025+0447 and 296A. We will establish a unified picture of
X-rays from brown dwarfs, together with the recent discoveries of X-rays from
young (~1 Myr) and old (~1 Gyr) brown dwarfs. The scientific objectives of our
Chandra observations are (1) to search for any correlations of X-rays to other
physical parameters; age, H alpha intensity, bolometric luminosity, and
circumstellar disk, and (2) to extend the X-ray detection toward a lower mass
star (M9.5), which is one step to a big challenge of searching for young Jupiter
type planets using X-rays.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:27:42.00 +05:03:41.00 PC 0025+0447 ACIS-S NONE 70.00
===================================================================================
Proposal Number: 03200753
Proposal Title: PROBING WIND-WIND INTERACTIONS AND STELLAR MAGNETIC FIELDS IN
PRE-PLANETARY NEBULAE
PI: RAGHVENDRA SAHAI
Subject Category: NORMAL STARS AND WD
Abstract: Preplanetary nebulae (PPNs) - the progenitors of planetary nebulae
(PNs) - hold the key to our understanding of the very late stages of stellar
evolution. Recent HST studies show that the fast wind-slow wind interaction
process believed to produce diffuse X-ray emission from PNs, must already be
active in PPNs. Sensitive observations for X-ray emission in PPNs, however, do
not exist. We propose ACIS-S observations of 4 well-studied PPNs with very fast
outflows in order to directly probe (a) the very hot (10$^{7-8}$K) shocked gas
which must result from the interaction, and (b) the presence of strong stellar
magnetic fields which may be responsible for collimating the fast outflows. These
data will be invaluable in testing theoretical models of X-ray emission in PPNs
and PNs.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:45:14.20 -17:56:47.00 HEN3-1475 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03200591
Proposal Title: X-RAY INDUCED CHEMISTRY IN PROTOSTARS
PI: THIERRY MONTMERLE
Subject Category: NORMAL STARS AND WD
Abstract: The envelopes of protostars are the subject of intense research in the
mm domain because of their cold temperatures (T ~ 10-30 K). However, for some
moderately luminous protostars (Lbol ~ 10 Lsun) there is evidence for enhanced
heating and ionization in their interiors (T ~ 300 K), from CO+, SO+ and FIR
high-J CO studies. We have developed a model to explain these enhancements in
terms of internal irradiation by a central luminous X-ray source (Lx ~ 10^31 erg
s-1, Tx ~ 3 keV), quite comparable with existing X-ray detections of protostars.
We propose for the first time a "live" study of the chemical interactions between
X-rays and circumstellar envelopes, by searching for X-ray emission from three
"chemically active" young protostars.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:32:22.70 -24:28:32.00 IRAS16293 ACIS-I NONE 30.00
===================================================================================
Proposal Number: 04200312
Proposal Title: UNVEILING ETA CAR: CHANDRA OBSERVATIONS DURING THE 2003.5 EVENT
PI: MICHAEL CORCORAN
Subject Category: NORMAL STARS AND WD
Abstract: Understanding the supermassive star Eta Car is important for a variety
of topics: the formation and evolution of extremely massive stars and their
influence on their environments. Eta Car has been a mystery since its giant
eruption in the 1840s. A possible key to the puzzle is the identification of
periodic changes in some near IR emission lines, and the discovery of repeatable
X-ray eclipses. The next X-ray eclipse will occur during AO4, and we propose to
use HETG to observe the variations in the spectral and spatial distribution of
the emission during this event. In conjunction with scheduled HST/STIS, INTEGRAL,
IR and optical spectroscopy, and radio observations, these HETG observation
provide key information which may finally help us solve the riddle of this star.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
10:45:03.60 -59:41:04.30 ETA CARINAE ACIS-S HETG 100.00
10:45:03.60 -59:41:04.30 ETA CARINAE ACIS-S HETG 100.00
10:45:03.60 -59:41:04.30 ETA CARINAE ACIS-S HETG 100.00
10:45:03.60 -59:41:04.30 ETA CARINAE ACIS-S HETG 100.00
10:45:03.60 -59:41:04.30 ETA CARINAE ACIS-S HETG 100.00
***********************************************************************************
WD BINARIES AND CV
--------------------------------------------------
===================================================================================
Proposal Number: 03300018
Proposal Title: FLARES, MAGNETIC RECONNECTIONS AND ACCRETION DISK VISCOSITY
PI: WILLIAM WELSH
Subject Category: WD BINARIES AND CV
Abstract: Accretion disks are invoked to explain a host of astrophysical
phenomena, from protostellar objects to AGN. Yet the mechanism allowing accretion
disks to operate are completely unknown. This proposal seeks to observe the
``smoking gun'' signature of magnetically-driven viscosity in accretion disks.
Magnetically-induced viscosity is a plausible and generally accepted hypothesis,
but it is completely untested. These data will establish the importance of
magnetic fields in accretion disks. Because of its known flaring properites, we
will observe the accretion disk in EM Cyg simulataneously with STIS/FUV-MAMA and
CHANDRA. The simultaneous X-rays are absolutely necessary for the unambiguous
detection of accretion disk magnetic reconnection flares.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:38:40.10 +30:30:28.00 EM CYG ACIS-S NONE 25.00
19:38:40.10 +30:30:28.00 EM CYG ACIS-S NONE 25.00
===================================================================================
Proposal Number: 03300064
Proposal Title: RESOLVING THE COMPACT BINARIES IN NGC 6397
PI: STEPHEN MURRAY
Subject Category: WD BINARIES AND CV
Abstract: We propose to obtain two moderately deep ACIS-S observations (25ksec
each) of the globular cluster NGC 6397 in order to resolve and identify the
population of compact binaries we have discovered in our cycle 1 ACIS-I
observation. Each exposure will approximately match the counts obtained for each
of the 14 sources found within 10arcsec of the cluster center, allowing the
spectral variability to be measured for the bright sources (>500 cts) and total
flux variability for the faintest (3ct) sources. This will enable the population
of millisecond pulsars (MSPs) to be distinguished from the cataclysmic variables
(CVs) and quiescent low mass x-ray binaries (qLMXBs), and will also enable a deep
search for flaring main sequence binaries. GTO Priority "A"
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:40:42.00 -53:40:27.90 NGC6397 ACIS-S NONE 30.00
17:40:42.00 -53:40:27.90 NGC6397 ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03300181
Proposal Title: BOUNDARY LAYERS AND HOT FLOWS IN QUIESCENT DWARF NOVAE
PI: JOHN RAYMOND
Subject Category: WD BINARIES AND CV
Abstract: The X-ray emitting boundary layers of quiescent dwarf novae offer a
rare opportunity to probe the thermal and dynamical structure of the flow in the
vicinity of the white dwarf via detailed spectroscopic diagnostics. Using an
extension of the Raymond-Smith code able to compute the detailed continuum and
line emission spectrum expected from a hot flow with arbitrary temperature and
density profiles, we are in a position to carry out such diagnostics. We propose
to observe the promising candidate WX Hyi with the Chandra X-ray Observatory and
test the various theoretical models of boundary layers and hot accretion flows
developed in this context.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
02:09:50.80 -63:18:40.30 WX HYI ACIS-S HETG 50.00
02:09:50.80 -63:18:40.30 WX HYI ACIS-S HETG 50.00
===================================================================================
Proposal Number: 03300197
Proposal Title: ACCRETION IN HIGH DENSITY AND TEMPERATURE CONDITIONS (V426 OPH)
PI: PAULA SZKODY
Subject Category: WD BINARIES AND CV
Abstract: We will use HETG to observe the 0.4-10 keV spectrum of the bright, high
mass transfer rate, disk accreting cataclysmic variable V426 Oph, which is known
from Ginga, ASCA data to have a strong Fe complex as well as other emission lines
in the 0.5-2 keV region. These lines provide information on the correct T and
density, the photoionization/collisional processes and the abundances of the
plasma as it undergoes the transition from a 14-19 keV low density regime to the
atmosphere of an accreting 30,000K white dwarf. The velocity broadening of the
lines will provide insights into the rotation and location of the gas as it
follows its accretion path from the Keplerian disk to the slower rotating white
dwarf, possibly along magnetic field lines.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:07:51.70 +05:51:48.50 V426 OPH ACIS-S HETG 50.00
===================================================================================
Proposal Number: 03300263
Proposal Title: MULTIWAVELENGTH TARGET OF OPPORTUNITY OBSERVATIONS OF A BRIGHT
NOVA IN OUTBURST
PI: SUMNER STARRFIELD
Subject Category: WD BINARIES AND CV
Abstract: We propose to obtain spectrophotometry with CHANDRA, plus ground based
optical and IR spectra of one bright nova in outburst. Our X-ray studies have
shown that X-rays are the best tool for studying the hot phase of the outburst.
In Cycle 1 we obtained spectra of V382 Vel and V1494 Aql. V382 Vel showed only an
emission line spectrum in our data while V1494 Aql evolved from an emission line
spectrum to that of a Super Soft Source (SSS). Observations of these phases
provided an opportunity to study the composition of the underlying white dwarf,
the lifetime of the TNR phase of the outburst, and the energy budget of the
explosion. More data on new novae is needed because the behavior of these two
novae was very different, which is expected from theory.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
IM Nor HRC-S LETG 25.00
IM Nor HRC-S LETG 25.00
15:39:26.50 -52:19:18.20 IM Nor ACIS-S NONE 5.00
===================================================================================
Proposal Number: 03300412
Proposal Title: THE HIGH RESOLUTION X-RAY SPECTRUM OF AM HERCULIS: PROBING THE
ACCRETION PROCESS
PI: ANDREW BEARDMORE
Subject Category: WD BINARIES AND CV
Abstract: We propose a 100ks Chandra HETG observation of the polar AM Herculis.
To ensure data is obtained when the source is in a high state we request a TOO
(or even an `anti-TOO') observation. With the good quality, high energy
resolution data this will provide, we be able to use the HEG to: (i) examine the
nature of the 6.4 keV fluorescence line in order to see if it has its origin in
reflection from the white dwarf surface or absorption in the pre-shock flow. (ii)
Measure the widths of the thermal Fe Kalpha lines in order to constrain the
importance of Compton broadening in this star. Also, using the MEG we will be
able to (iii) measure the line strengths of the lighter elements and estimate the
physical conditions in the post-shock region.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:16:13.33 +49:52:04.20 AM HERCULIS ACIS-S HETG 100.00
===================================================================================
Proposal Number: 03300437
Proposal Title: A UNIFORM STUDY OF GLOBULAR CLUSTER X--RAY SOURCES: THE KEYS TO
CLUSTER DYNAMICAL EVOLUTION
PI: WALTER LEWIN
Subject Category: WD BINARIES AND CV
Abstract: We propose to extend our ongoing studies of the dynamical evolution of
globular clusters by observing their populations of low-luminosity X-ray sources.
Many of these sources are binary systems (or have evolved from them) and hold the
key to the cluster's dynamical evolution. We propose observations of a variety of
clusters with widely different physical properties such as central concentration,
cluster size and mass, which are all key ingredients in the formation and
evolution of binaries. To make this study as uniform as possible, the clusters
will be observed to the same limiting luminosity. Numerical simulations with the
world's fastest computer will assist in the interpretation of our observational
data.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
15:18:33.80 +02:04:57.70 NGC 5904 ACIS-S NONE 45.00
17:01:12.60 -30:06:44.50 NGC 6266 ACIS-S NONE 63.00
17:27:44.30 -05:04:35.90 NGC 6366 ACIS-S NONE 24.00
===================================================================================
Proposal Number: 03300823
Proposal Title: RESOLVING THE COMPACT BINARY DISTRIBUTION IN THE CENTRAL HALF
ARCMIN OF THE COLLAPSED-CORE GLOBULAR CLUSTER M30
PI: HALDAN COHN
Subject Category: WD BINARIES AND CV
Abstract: The collapsed-core globular cluster M30 is a prime target for the study
of the formation and evolution of compact binaries in one of the densest
environments found in the Galaxy. ROSAT observations have detected X-ray emission
from the vicinity of the cluster core, that probably arises from a population of
low-Lx, compact binaries, including cataclysmic variables. Only Chandra can
resolve this emission into individual sources to study their properties and
spatial distribution. Grindlay et al (2001) have detected over 100 faint Chandra
sources in the dense cluster 47 Tuc. We propose a deep ACIS-S exposure, to be
used with our deep HST imaging of M30, to investigate the expected population of
compact binaries in the central half arcmin.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
21:40:22.00 -23:10:45.00 NGC 7099 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03300829
Proposal Title: CHANDRA GRATING SPECTROSCOPY OF DWARF NOVAE
PI: PETER WHEATLEY
Subject Category: WD BINARIES AND CV
Abstract: Dwarf novae are spectacular examples of accreting systems that have
formed the basis of much of our understanding of accretion disks, from AGN to
YSOs. Chandra grating observations have the power to resolve the temperature
structure of the X-ray bright boundary layer for the first time, both in the
optically-thin quiescent state and optically-thick outburst state, however only
two systems have been observed to date. Here we propose to observe SU~UMa and
VW~Hyi, the 2nd and 3rd brightest dwarf novae.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
08:12:28.20 +62:36:23.00 SU UMA ACIS-S HETG 25.00
08:12:28.20 +62:36:23.00 SU UMA ACIS-S HETG 50.00
===================================================================================
Proposal Number: 03300850
Proposal Title: MULTIWAVELENGTH OBSERVATIONS OF V1494 AQL IN OUTBURST
PI: SUMNER STARRFIELD
Subject Category: WD BINARIES AND CV
Abstract: We propose 2 HRC-S+LETG followup observations of V1494 Aql which we
observed with CHANDRA as a TOO in Cycle 1. Our grating data show that it has
become a Super Soft Source (SSS) and an analysis of the light curve shows a 2500s
period. More grating data is necessary both to determine its evolution during the
SSS phase and to measure any changes in period. We also observed a factor of 6
rise in counts during the observation and further data could help to determine if
this were a common phenomenon. It is evolving slowly in the optical and should
still be bright in X-rays in Cycle 3. Analysis of the grating data will allow us
to study the composition of the ejecta, the lifetime of the TNR phase of the
outburst, and the energy budget of the explosion.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:23:05.30 +04:57:21.60 V1494 AQL HRC-S LETG 25.00
19:23:05.30 +04:57:21.60 V1494 AQL HRC-S LETG 25.00
===================================================================================
Proposal Number: 03300300
Proposal Title: MULTIWAVELENGTH STUDY OF THE GLOBULAR CLUSTER M28 (NGC~6626)
PI: WERNER BECKER
Subject Category: WD BINARIES AND CV
Abstract: We propose a 60 ks, ACIS-S observation of the globular cluster M28.
This medium deep exposure will clarify the nature of the apparently extended
X-ray emission at its core and establish the X-ray luminosity function of M28's
constituents down to 10^31 erg/s. In addition, the exposure will provide an
accurate, confusion-free spectrum of the millisecond pulsar PSR B1821-24 near the
center of M28, and spectra of various other X-ray sources in the globular cluster
we will detect. Furthermore, by referencing the Chandra-determined positions to
the very accurate radio position of PSR B1821-24 and the X-ray bright star HD
315622, we shall determine the absolute positions of identified sources to better
than 0.25\arcsec, greatly facilitating identifications studies in the optical and
radio band.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:24:32.00 -24:52:10.70 M28 ACIS-S NONE 13.33
18:24:32.00 -24:52:10.70 M28 ACIS-S NONE 13.33
18:24:32.00 -24:52:10.70 M28 ACIS-S NONE 13.33
===================================================================================
Proposal Number: 03308072
Proposal Title: TOO OBSERVATIONS OF THE RECURRENT NOVA IM NORMAE IN OUTBURST
PI: SUMNER STARRFIELD
Subject Category: WD BINARIES AND CV
Abstract: IM Nor is a Recurrent Nova (RN) discovered in outburst on 10 Jan 02. It
rose to V~7.7 on 16 Jan suggesting that it was caught at the beginning of its
outburst. Based on its first outburst in 1920 (near maximum for ~ 100 days), it
is one of only two SLOW RN. While CHANDRA observed another RN with ACIS-S (CI Aql
in 2000), the resulting spectrum was weak. However, CI Aql was fainter at maximum
and the spectrum was taken after it had returned to quiescence. RN may be
progenitors of SN Ia suggesting that we need to obtain as much information as we
can about their properties. We, therefore, propose a 5 ksec ACIS-S observation to
see if it is bright in X-rays followed by a 25 kse c HRC-S+LETG spectrum to study
the ejecta. The ACIS-S spectrum will show either emission lines from a hot gas
(seen in V382 Vul) or a hot continuum from a white dwarf atmosphere (V1494 Aql).
Neither of these resemble the spectrum of a dwarf nova (WZ Sge).
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
15:39:26.50 -52:19:18.20 IM NORMAE ACIS-S NONE 5.00
15:39:26.50 -52:19:18.20 IM NORMAE ACIS-S NONE 25.00
===================================================================================
Proposal Number: 03308083
Proposal Title: CHANDRA HETG SPECTROSCOPY OF GK PER IN OUTBURST
PI: CHRISTOPHER MAUCHE
Subject Category: WD BINARIES AND CV
Abstract: GK Persei is an extraordinary object: the first nova of the last
century, it contains a magnetic white dwarf, an evolved secondary, and a large
truncated accretion disk. ASCA demonstrated that in outburst the X-ray spectrum
of GK Per contains strong Fe K emission lines and a strong low-energy (0.5-3 keV)
excess. The nature of the low-energy excess is not known, but it is expected to
consist of a mixture of thermal emission lines from the accretion column and
fluorescent emission lines from the white dwarf surface and accretion disk. We
propose to obtain two Chandra HETG observations of GK Per in outburst to
determine the nature of the low-energy emission, measure the Fe K emission line
strengths, and search for other emission lines, thereby constraining the
accretion geometry and the plasma conditions (range of temperatures, abundances,
and density) of the X-ray--emitting plasma.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
03:31:11.80 +43:54:16.80 GK PER ACIS-S HETG 35.00
03:31:11.80 +43:54:16.80 GK PER ACIS-S HETG 35.00
***********************************************************************************
BH AND NS BINARIES
--------------------------------------------------
===================================================================================
Proposal Number: 03400017
Proposal Title: ULTRALUMINOUS X-RAY SOURCES AND INTERMEDIATE MASS BLACK HOLES
PI: JOEL BREGMAN
Subject Category: BH AND NS BINARIES
Abstract: Ultraluminous X-ray sources (ULX) are second only to AGNs in
point-source luminosity yet they have no known optical counterparts. These
extraordinary X-ray objects, which radiate at the Eddington luminosity of a
30-100 Mo object, are non-nuclear sources in normal disk galaxies. One
explanation is that they are binary systems where the accreting black hole has a
mass of 30-100 Mo. Another possibility is that ULXs are intermediate mass black
holes (1E3-1E4 Mo), acting as micro-quasars in galaxy disks and representing the
link between stellar black holes (4-10 Mo) and supermassive black holes (1E6-1E10
Mo). We can distinguish between the models by identifying the optical
counterparts of ULXs and measuring their colors.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:35:50.60 +27:54:47.00 NGC 4559 ACIS-S NONE 3.00
===================================================================================
Proposal Number: 03400284
Proposal Title: UNTWISTING THE TORNADO
PI: BRYAN GAENSLER
Subject Category: BH AND NS BINARIES
Abstract: G357.7-0.1 ("the Tornado") is an unusual radio source whose morphology
defies classification. We have discovered an X-ray source coincident with the
Tornado, which we argue represents either a central pulsar or an exotic accreting
system, both of which could power the surrounding radio emission. High-resolution
X-ray imaging, followed by a search for an infrared counterpart, can distinguish
between these possibilities. We thus propose ACIS observations with which we can
establish the properties of the central source in the Tornado, and so finally
determine the nature of this enigmatic object.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:40:11.70 -30:58:38.20 TORNADO ACIS-I NONE 21.00
===================================================================================
Proposal Number: 03400295
Proposal Title: CHANDRA OBSERVATIONS OF LONG-DURATION TRANSIENTS AND PERSISTENT
LOW-MASS X-RAY BINARIES IN QUIESCENCE
PI: RUDY WIJNANDS
Subject Category: BH AND NS BINARIES
Abstract: We propose to observe a long-duration transient or a persistent
low-mass X-ray binary when it turns-off and transits in to quiescence. This will
give an excellent opportunity to study the effects of prolonged accretion on the
quiescent properties of low-mass X-ray binaries. A follow-up observation taken
about half a year later will provide important information about the time
evolution of the quiescent properties, i.e., the neutron-star cooling time.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:02:06.30 -29:56:45.00 MXB 1659-298 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03400303
Proposal Title: OBSERVATIONS OF THE TRANSIENT X-RAY PULSAR 2S 1845-024
PI: MARK FINGER
Subject Category: BH AND NS BINARIES
Abstract: 2S 1845-024 is a 94 second transient X-ray pulsar which outbursts near
the periastron passage of its highly eccentric, 242 day binary orbit. Its yet
unidentified companion is likely a Be star. The source's outbursts have occurred
regularly each orbit for at least the last 10 years. The source is unique in
showing both evidence for its companion's equator being inclined with respect to
the orbital plane, and in showing evidence for accretion disk formation during
recurrent outbursts. Our proposal is to make Chandra ACIS-S/HETG observations
during the outburst expected in September 2002 to study the spectral evolution
associated with the disk formation. A secondary objective of our proposal is to
obtain an accurate source position so that the optical companion may be
identified.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:48:18.00 -02:25:12.00 2S 1845-024 ACIS-S NONE 5.00
18:48:18.00 -02:25:12.00 2S 1845-024 ACIS-S HETG 15.00
18:48:18.00 -02:25:12.00 2S 1845-024 ACIS-S HETG 15.00
18:48:18.00 -02:25:12.00 2S 1845-024 ACIS-S HETG 15.00
===================================================================================
Proposal Number: 03400316
Proposal Title: LOCATING THE ELUSIVE COUNTERPART OF THE UNUSUAL X-RAY DIPPER
X1624-490
PI: STEFANIE WACHTER
Subject Category: BH AND NS BINARIES
Abstract: X-ray dippers are high inclination low mass X-ray binary systems in
which the central X-ray source is periodically occulted by a thickened region of
the accretion disk rim. X1624-490 is one of the most unusual members of this
class; its persistent X-ray emission is the brightest, its dip profiles the most
erratic, and its 20.9-hour orbital period is the longest. Despite a wealth of
X-ray observations, the optical counterpart of X1624-490 has not yet been
identified. With its high spatial resolution, the Chandra HRC-I is the perfect
instrument for, and the only one capable of, directly pinpointing the optical/IR
counterpart of X1624-490. This project can be achieved with a minimal amount of
observing time (1 ksec) and the result can be applied immediately to already
existing IR data.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:28:03.30 -49:11:30.30 X1624-490 HRC-I NONE 1.00
===================================================================================
Proposal Number: 03400384
Proposal Title: THE FAINTEST 'FIELD' LOW-MASS X-RAY BINARIES
PI: MICHIEL VAN DER KLIS
Subject Category: BH AND NS BINARIES
Abstract: We propose to continue our survey, begun in Cycle 1, of the group of
persistently faint galactic X-ray sources outside globular clusters which are
thought to be LMXBs, but about which very little was known before Chandra. Our
exploratory Cycle 1 work confirmed the low Lx of these objects, and produced some
intriguing new results. Given theoretical as well as empirical arguments for the
detection of spectral lines, in Cycle 3 we propose HETG follow-up observations
for 4 sources, and further exploratory ACIS pointings for 4 others. Our aim is to
extend knowledge about compact-object accretion physics towards lower accretion
levels than previously accessible and to provide a sample against which to
compare the faint globular-cluster LMXBs.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:05:45.80 +25:51:45.00 1603.6+2600 ACIS-S NONE 8.00
17:14:19.20 -34:02:57.60 1711-339 ACIS-S NONE 5.00
17:42:44.00 -30:30:51.50 1739-304 ACIS-S NONE 1.00
17:42:44.00 -30:30:51.50 1739-304 ACIS-S NONE 3.00
17:50:03.90 -32:25:51.00 1746.7-3224 ACIS-S NONE 8.00
===================================================================================
Proposal Number: 03400337
Proposal Title: RESOLVING GALACTIC BLACK HOLE ACCRETION GEOMETRY WITH CHANDRA
PI: WALTER LEWIN
Subject Category: BH AND NS BINARIES
Abstract: Recent results have shown that the X-ray states observed in all black
hole X-ray binary systems cannot be driven solely by the mass accretion rate, but
depend on the accretion flow geometry in a complicated way. Our own results from
AO-1 and AO-2 may reveal a previously unseen geometry. Additionally, correlations
between discrete radio ejections, radio jets, and the X-ray state, have been
noted recently. We propose to probe the accretion flow geometry in a black hole
system in outburst with the HETGS to diagnose the geometry in different X-ray
states; by doing so we will constrain what mechanisms act with the mass accretion
rate to drive the state transitions. Ours is a global, simultaneous,
multi-wavelength effort, which spans the radio, IR, optical, X-ray and gamma-ray
bands.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:50:01.00 -49:57:45.00 BHC TRANSIENT ACIS-S HETG 15.00
16:50:01.00 -49:57:45.00 XTE J1650-500 ACIS-S HETG 30.00
16:50:01.00 -49:57:45.00 XTE J1650-500 ACIS-S HETG 30.00
===================================================================================
Proposal Number: 03400454
Proposal Title: HIGH RESOLUTION SPECTROSCOPY OF HERCULES X-1
PI: DANIEL SCOTT
Subject Category: BH AND NS BINARIES
Abstract: We propose a set of high resolution spectral observations of the
accreting pulsar X-ray binary Her X-1/HZ Her. A strong, pulsed, blackbody
spectral component has been detected with a temperature of about 0.1 keV probably
originating from X-ray reprocessing by the inner edge of the precessing accretion
disk. Chandra LETGS observations can determine if emission lines from this
component are present and if so use them to probe the physical conditions there.
Observations with the HETGS will resolve the strong Fe K line and determine
whether a mysterious large unresolved bump in the spectrum between 0.8 and 1.4
keV is due to a multi-temperature Fe L emission complex or involves other lines.
The Main High state peak and flux decline and a Short High state will be
surveyed.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:57:49.80 +35:20:32.90 HER X-1 SHORT HI ACIS-S HETG 20.00
16:57:49.80 +35:20:32.90 HER X-1 SHORT HI ACIS-S HETG 20.00
16:57:49.80 +35:20:32.90 HER X-1 MAIN HI PEAK HRC-S LETG 10.00
16:57:49.80 +35:20:32.90 HER X-1 MAIN HI LATE ACIS-S HETG 20.00
16:57:49.80 +35:20:32.90 HER X-1 MAIN HI PEAK ACIS-S HETG 10.00
===================================================================================
Proposal Number: 03400510
Proposal Title: AN ULTRALUMINOUS BINARY IN A HORSESHOE NEBULA?
PI: PATRICK SLANE
Subject Category: BH AND NS BINARIES
Abstract: We propose a Chandra observation of 1E0953.8+6918 to assess its
relationship to the very strange horseshoe-shaped nebulosity seen in the
direction of the galaxy Ho IX. The position and morphology of the X-ray emission
is currently not well known, and this is crucial for our understanding of the
nebula. If located in Ho IX, Lx is very high, possibly indicating a 100 solar
mass BH binary, and the size of the nebula implies a huge shock-heated structure,
which is difficult to understand. However, a Galactic interpretation is no less
puzzling. The proposed observation will provide an improvement in the source
location, permit a search for multiple emission components, and allow us to
search pulsations from any compact emission region identified in the high
resolution Chandra image.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
09:57:53.00 +69:03:51.00 1E0953.8+6918 HRC-I NONE 7.00
===================================================================================
Proposal Number: 03400562
Proposal Title: THE EXTRAORDINARY GLOBULAR CLUSTER SYSTEM OF M87: THE VIEW FROM
CHANDRA
PI: PATRICK COTE
Subject Category: BH AND NS BINARIES
Abstract: With the launch of Chandra, a new era in the study of globular cluster
(GC) X-ray sources has arrived. It is at last possible to identify bright X-ray
sources belonging to the GCs of giant elliptical galaxies: the natural targets
for such studies by virtue of their rich GC systems. We propose to exploit the
exceptional spatial resolution and sensitivity of Chandra to carry out the
definitive study of LMXBs in GC environments. Our target is M87, the cD galaxy in
the nearby Virgo cluster. Its GC system (the most populous of any galaxy within
20 Mpc) is the focus of a comprehensive optical study we are conducting with HST
and ground-based telescopes. This program will reveal hundreds of LMXBs
associated with M87 GCs, and provide a definitive test of models for their
origin.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:30:49.40 +12:23:28.00 NGC4486 ACIS-S NONE 23.00
12:30:49.40 +12:23:28.00 NGC4486 ACIS-S NONE 105.00
===================================================================================
Proposal Number: 03400564
Proposal Title: RESOLVING IRON K-ABSORPTION LINE FEATURES IN THE X-RAY SPECTRA
OF THE LOW MASS X-RAY BINARY GX 13+1
PI: YOSHIHIRO UEDA
Subject Category: BH AND NS BINARIES
Abstract: We propose to observe the Low Mass X-ray Binary GX 13+1 with Chandra
HETGS, which is the unique neutron-star binary that exhibits iron-K absorption
lines revealed from previous ASCA observations. Moreover, since GX 13+1 is a
relatively bright and persistent radio source, it is of great interest to study
the relation to the transient superluminal sources GRO J1655-40 and GRS 1915+105,
which have shown similar spectral features in the X-ray spectra. The high
resolution spectroscopy of GX 13+1 in the iron-K band will give important clues
for understanding common physics of an accretion disk in neutron star and black
hole binaries.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:14:31.00 -17:09:26.00 GX 13+1 ACIS-S HETG 30.00
===================================================================================
Proposal Number: 03400614
Proposal Title: THE HIGH LATITUDE NEUTRON STAR X-RAY TRANSIENT XTE J2123-058
PI: JOHN TOMSICK
Subject Category: BH AND NS BINARIES
Abstract: XTE J2123-058 is a high Galactic latitude neutron star transient. The
high latitude of the source provides the observational advantage of low
extinction, which is critical for soft X-ray and optical observations. From
optical spectroscopy, we find that the source distance is near 8.9 kpc, making it
unusually far from the Galactic plane for an LMXB. We previously obtained an
X-ray luminosity upper limit of 3.6E33 erg/s for this source with BeppoSAX, and
more sensitive observations are required. I propose to observe XTE J2123-058 with
Chandra to measure its luminosity. Although a detection is likely, a
non-detection will provide a luminosity upper limit of 3E31 erg/s, which has
implications for the question of whether quiescent black hole systems are dimmer
than neutron star systems.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
21:23:14.50 -05:47:52.90 XTE J2123-058 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03400623
Proposal Title: OUTFLOWS FROM X-RAY PULSARS IN THE PROPELLER STATE
PI: WEI CUI
Subject Category: BH AND NS BINARIES
Abstract: As an accreting X-ray pulsar enters the propeller state, the accreted
matter encounters a centrifugal barrier and thus cannot follow the field lines to
reach the magnetic poles. Consequently, the X-ray pulsation ceases. It is thought
that in this state the accreted material is actually ejected and thus forms an
outflow. Indirect evidence for such an outflow exists for GX 1+4, based on the
non-thermal nature of its observed X-ray spectrum in the propeller state. Now the
powerful combination of the HETG and ACIS allows, for the first time, an attempt
to studying gas dynamics in X-ray pulsars during this poorly understood state, by
measuring Doppler-shifted iron fluorescent lines. We propose a joint Chandra and
RXTE ToO campaign to observe GX 1+4 in the propeller state.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:32:03.00 -24:44:44.30 GX 1+4 ACIS-S HETG 60.00
===================================================================================
Proposal Number: 03400626
Proposal Title: ACIS-HETG OBSERVATIONS OF MICROQUASAR XTE J1748-288
PI: JULIA LEE
Subject Category: BH AND NS BINARIES
Abstract: The recently discovered microquasar XTE J1748-288 show spectral
differences between the very high, high, and low state. ASCA and RXTE
observations show prominent iron line(s). We propose to observe with HETG for a
140ks total exposure over these 3 phases in order to characterize the X-ray
spectral features and resolve presently unknown lines for these states. We will
also look for emission lines from any X-ray jet, and P-Cygni profiles indicative
of a disk-wind. This will be compared to previous Chandra observations of similar
energetic systems. We were awarded time in the last Chandra cycle for this
proposal but did not trigger on the TOO. The source has remained off.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:48:08.00 -28:28:48.00 XTE J1748-288 ACIS-S HETG 30.00
17:48:08.00 -28:28:48.00 XTE J1748-288 ACIS-S HETG 55.00
17:48:08.00 -28:28:48.00 XTE J1748-288 ACIS-S HETG 55.00
===================================================================================
Proposal Number: 03400636
Proposal Title: MONITORING THE MORPHOLOGY OF THE MICRO-QUASARS GRS 1758-258 AND
1E 1740.7-2942
PI: WILLIAM HEINDL
Subject Category: BH AND NS BINARIES
Abstract: We propose to monitor the "micro-quasars" GRS 1758-258 and 1E
1740.7-2942 in order to search for changes in the morphology of their arcsecond
scale extended X-ray emission. In GRS 1758-258, this extended structure changed
shape (as seen by the Chandra/HRC-I) in about a month, indicating a possible
near-luminal outflow. In this investigation, we will use the HRC-I in concert
with our approved RXTE/Proportional Counter Array and VLA monitoring programs to
track changes in the extended X-ray morphology of GRS 1758-258 and see if similar
changes occur in 1E 1740.7-2942. We will correlate these variations with the
radio flux and hard X-ray (3-60 keV) spectral behavior which will allow us to
study the role of the disk/corona with the ejection of material from the binary
system.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:43:54.80 -29:44:42.80 1E 1740.7-2942 HRC-I NONE 7.50
17:43:54.80 -29:44:42.80 1E 1740.7-2942 HRC-I NONE 7.50
17:43:54.80 -29:44:42.80 1E 1740.7-2942 HRC-I NONE 7.50
17:43:54.80 -29:44:42.80 1E 1740.7-2942 HRC-I NONE 30.00
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 3.33
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 3.33
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 3.33
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 3.33
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 3.33
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 3.33
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 3.33
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 3.33
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 10.00
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 10.00
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 10.00
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 10.00
===================================================================================
Proposal Number: 03400642
Proposal Title: A CHANDRA STUDY OF NEARBY PERSISTENT MICROQUASAR LS 5039
PI: WALTER LEWIN
Subject Category: BH AND NS BINARIES
Abstract: LS 5039 is a persistent microquasar with many striking similarities to
SS 433. Located only 3 kpc away and suffering minimal extinction, the X-ray
structure of the jets and inner accretion region may be revealed simultaneously
with Chandra. We propose an HETGS observation of this source to resolve the jet
structure and energetics, to constrain the accretion flow geometry in this
system, to place LS 5039 in the context of other microquasars such as SS 433, 1E
1740.7-2942, and GRS 1915+105.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:26:14.90 -14:50:51.00 LS 5039 ACIS-S HETG 10.00
===================================================================================
Proposal Number: 03400646
Proposal Title: BLACK HOLE X-RAY TRANSIENTS DURING OUTBURST DECAY
PI: JOHN TOMSICK
Subject Category: BH AND NS BINARIES
Abstract: Most observations of black hole candidate (BHC) X-ray transients have
been made when the sources are at very high luminosity (>1E36 erg/s) or very low
luminosity (<1E32 erg/s), and not much observing time has been devoted to
intermediate luminosities. Observations in this intermediate regime are critical
since the competing theoretical models predict different emission properties
here. We propose to use Chandra to observe a BHC X-ray transient in this
luminosity regime during outburst decay. These observations will provide
constraints on accretion geometries and emission mechanisms and will provide
definitive tests of existing theoretical models. We have an active RXTE program
for observing these systems during decay, and will use our RXTE observations to
trigger this TOO.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:50:01.00 -49:57:45.00 XTE J1650-500 ACIS-S HETG 10.00
16:50:01.00 -49:57:45.00 XTE J1650-500 ACIS-S HETG 10.00
16:50:01.00 -49:57:45.00 XTE J1650-500 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03400757
Proposal Title: LOCALIZING THE HIGH LATITUDE X-RAY TRANSIENT 4U 0042+32
PI: JOHN TOMSICK
Subject Category: BH AND NS BINARIES
Abstract: 4U 0042+32 is a very interesting and unusual high Galactic latitude
X-ray transient. This source was detected in X-rays several times during the
1970s, and is probably a black hole X-ray transient, but has not been observed in
outburst for over 20 years. Due to its high latitude, the level of extinction is
low, but 4U 0042+32 has not been optically identified. We propose to use
Chandra's sensitivity and positioning capabilities to localize 4U 0042+32 in
quiescence to facilitate its optical identification. We have already obtained a
deep optical image so that a Chandra detection is likely to lead to a rapid
identification. Follow-up optical observations could then be performed to
determine the source distance, the binary orbital parameters and possibly the
mass of the compact object.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:44:50.30 +33:01:17.00 4U 0042+32 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03400827
Proposal Title: PROBING THE CIRCUMSTELLAR MATERIAL IN GX 301-2
PI: MASAO SAKO
Subject Category: BH AND NS BINARIES
Abstract: We propose to obtain high-resolution spectroscopic data of the
high-mass X-ray binary GX 301-2/Wray977 to study the geometry of circumstellar
material in the system. The observation consists of two exposures --
pre-periastron (PP) and near-apastron (NA) flares -- during which the source
brightens by as much an order of magnitude compared to the normal quiescent
state. The emission line spectrum, especially in the iron K region, changes
dramatically during these flares, and a detailed spectral analysis will allow us
to probe the distribution of material in the system, as well as the dynamical
properties of the stellar wind. Measurements of the Fe K fluorescent line profile
will also unambiguously distinguish the broadening mechanism, which has been
difficult with low-resolution spectra.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:26:37.60 -62:46:13.00 GX 301-2 ACIS-S HETG 40.00
12:26:37.60 -62:46:13.00 GX 301-2 ACIS-S HETG 60.00
12:26:37.60 -62:46:13.00 GX 301-2 ACIS-S HETG 60.00
===================================================================================
Proposal Number: 03400837
Proposal Title: COMPLETE COMPACT OBJECT AND BINARY SURVEY OF 47TUC
PI: JONATHAN GRINDLAY
Subject Category: BH AND NS BINARIES
Abstract: Our cycle 1 observation of 47Tuc has shown its promise as the ultimate
laboratory for study of the production and evolution of compact binaries and
compact objects in globular clusters. We propose a deep (4 x 75ksec) ACIS-S
observation to measure the complete populations of millisecond pulsars (MSPs) and
cataclysmic variables (CVs) by their variability and spectra and to constrain the
main sequence binary population. Coordinated HST (ACS) data would provide unique
identifications of CVs and many MSPs and allow the full population of quiescent
low mass x-ray binaries to be distinguished from CVs. This dataset would provide
fundamental constraints for the origins of neutron stars, millisecond pulsars,
magnetic white dwarfs and compact binaries in globular clusters.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:24:05.80 -72:04:51.20 47 TUCANAE ACIS-S NONE 5.00
00:24:05.80 -72:04:51.20 47 TUCANAE ACIS-S NONE 5.00
00:24:05.80 -72:04:51.20 47 TUCANAE ACIS-S NONE 5.00
00:24:05.80 -72:04:51.20 47 TUCANAE ACIS-S NONE 5.00
00:24:05.80 -72:04:51.20 47 TUCANAE ACIS-S NONE 69.00
00:24:05.80 -72:04:51.20 47 TUCANAE ACIS-S NONE 69.00
00:24:05.80 -72:04:51.20 47 TUCANAE ACIS-S NONE 69.00
00:24:05.80 -72:04:51.20 47 TUCANAE ACIS-S NONE 69.00
===================================================================================
Proposal Number: 03400840
Proposal Title: MEASURING THE ABSOLUTE DISTANCE TO THE BURSTER GS 1826-238
PI: RICHARD ROTHSCHILD
Subject Category: BH AND NS BINARIES
Abstract: We propose to measure the distance to the clocked x-ray burster GS
1826-238 by measuring the burst-induced temporal variability of the x-ray
scattering halo. When combined with the bolometric flux measured simultaneously
with Chandra and RXTE, this will yield the absolute bolometric luminosity from
this object for both the persistent and burst emission. This novel and very
powerful technique for absolute distance determination will provide a measurement
of the neutron star radius as well as the fraction of the neutron star surface
involved in the persistent, steady state hydrogen burning. It is important to
establish this method of distance determination since it could have wide
applications for variable sources.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:29:28.20 -23:47:49.12 GS 1826-238 ACIS-S HETG 70.00
===================================================================================
Proposal Number: 03400841
Proposal Title: PHASE RESOLVED HIGH ENERGY RESOLUTION SPECTROSCOPY OF THE BLACK
HOLE X-RAY BAINARY CYGNUS X-1
PI: SHUANG ZHANG
Subject Category: BH AND NS BINARIES
Abstract: We propose to carry out phase resolved high resolution spectroscopy of
the black hole X-ray binary Cygnus X-1 with ACIS-S HETG. Our observations consist
of four snap-shots of 5-ks each at orbital phases 0.0, 0.25, 0.5 and 0.75. Our
observational goals are to determine the Oxygen abundance, column density and the
continuum spectrum independent of each other. Our scientific objectives include
the study of the properties of the corona and accretion disk around the black
hole and disk formation in wind accretion system. Our feasibility study
demonstrates that our proposed observations serve our objectives well.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:58:21.70 +35:12:05.80 CYG X-1 ACIS-S HETG 5.00
19:58:21.70 +35:12:05.80 CYG X-1 ACIS-S HETG 5.00
19:58:21.70 +35:12:05.80 CYG X-1 ACIS-S HETG 5.00
19:58:21.70 +35:12:05.80 CYG X-1 ACIS-S HETG 5.00
===================================================================================
Proposal Number: 03400937
Proposal Title: WIND ACCRETION IN LOW-MASS X-RAY BINARIES
PI: DUNCAN GALLOWAY
Subject Category: BH AND NS BINARIES
Abstract: We have identified a group of neutron-star low-mass X-ray binaries
which are likely accreting from the stellar wind of their companion rather than
via the usual Roche-lobe overflow. If confirmed,this would be a previously
unrecognized mode of mass transfer in LMXBs with significant implications for our
understanding of their evolution and population, since these binaries could be
X-ray active without being in contact. We will test for wind accretion by using
the HETGS to search for fluorescent lines from stellar wind nebulae in these
sources.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:32:02.20 -24:44:43.60 GX 1+4 ACIS-S HETG 20.00
17:47:56.00 -26:33:48.60 GX 3+1 ACIS-S HETG 10.00
===================================================================================
Proposal Number: 03400979
Proposal Title: RESOLVING THE SOFT EXCESS IN 4U 1850-087
PI: DEEPTO CHAKRABARTY
Subject Category: BH AND NS BINARIES
Abstract: A soft excess near 0.7 keV, consistent with unresolved emission lines,
has been previously reported in several LMXBs. Our recent reanalysis of archival
ASCA and BeppoSAX data shows that this excess can also be explained by
photoelectric absorption by material with non-solar abundance, or by a failure to
account for the thermodynamically required turnover of the power law continuum at
low energies. We propose an ACIS-S/LETGS observation of the soft excess source 4U
1850-087 in order to discriminate between these alternatives.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:53:04.80 -08:42:19.80 4U 1850-087 ACIS-S LETG 5.00
18:53:04.80 -08:42:19.80 4U 1850-087 ACIS-S LETG 55.00
===================================================================================
Proposal Number: 03400860
Proposal Title: STUDY OF THE IRON LINE AND LOW ENERGY FEATURES IN 4U 1728-34
WITH CHANDRA/HETGS
PI: TIZIANA DI SALVO
Subject Category: BH AND NS BINARIES
Abstract: We propose a 30 ks Chandra/HETGS observation of 4U 1728-34 to perform a
detailed study of the iron Kalpha line and other low energy features. This source
shows a broad (1 keV FWHM) iron Kalpha line: several hypotheses can be proposed
to explain the width (e.g. relativistic and Doppler effects in an accretion disk,
Compton scattering, line-blending), and we expect that the high energy resolution
of Chandra HETGS will be able to resolve the complex line shape and to constrain
the various models proposed. These kind of sources are also expected to be rich
sources of discrete features at low energy (0.3-3 keV), because of the presence
of a photoionized corona (ADC). These low energy features are an important
diagnostic tool for the physical conditions of the emitting regions.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:31:57.40 -33:50:05.00 4U 1728-34 ACIS-S HETG 30.00
===================================================================================
Proposal Number: 03400921
Proposal Title: SPECTRAL SIGNATURES OF A PRECESSING ACCRETION DISK IN HER X-1
PI: CHARLES HAILEY
Subject Category: BH AND NS BINARIES
Abstract: Observations of Her X-1 with the XMM-Newton RGS show the most prominent
line emission in the low-state of its 35-day flux cycle. Chandra HETG can detect
a dozen H-like and He-like ion lines and test our photoionized disk atmosphere
model, which has been successful in predicting the lines of EXO 0748-67 and
4U1822-37. The precessing disk hypothesis for Her X-1 can be tested by observing
changes in velocity dispersion with the 35-day cycle, as the inner disk comes in
and out of view. Her X-1 is one of the brightest low-mass X-ray binaries (LMXB)
at high inclination, making it a prime target to observe line emission.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:57:49.80 +35:20:32.60 HER X-1 ACIS-S HETG 50.00
===================================================================================
Proposal Number: 03400987
Proposal Title: A SEARCH FO EMISSION LINES IN THE MICRO-QUASAR GRS 1758-258
PI: WILLIAM HEINDL
Subject Category: BH AND NS BINARIES
Abstract: We propose to obtain a high significance, high resolution spectrum of
the micro-quasar GRS 1758-258 in order to search for emission lines from possible
X-ray jets. As revealed in Chandra/HRC observations, GRS 1758-258 has arcsecond
scale extended X-ray emission associated with a core point source. This extended
structure changed shape in about a month, evidence for a near-light-speed
outflow. In this investigation, we will use the ACIS-S/HETG, supported by
concurrent Rossi X-ray Timing Explorer and VLA observations, to search for red-
and blue-shifted emission lines. If found, these lines will confirm the presence
of relativistic flows in this system and should allow us to constrain the
geometry of the system.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:01:12.40 -25:44:35.90 GRS 1758-258 ACIS-S HETG 30.00
===================================================================================
Proposal Number: 03401009
Proposal Title: MULTIWAVELENGTH OBSERVATIONS OF THE BLACK HOLE XTE J1118+480 IN
QUIESCENCE
PI: STEPHEN MURRAY
Subject Category: BH AND NS BINARIES
Abstract: The X-ray nova XTE J1118+480 has minimal interstellar extinction and
therefore represents an outstanding opportunity for multiwavelength studies. In
outburst we conducted a comprehensive study of this object that was extremely
rewarding. Now we propose an analogous campaign to observe the quiescent state
using Chandra, HST and the MMT. Our objectives are to (1) assemble the best
possible optical to X-ray spectrum of a quiescent black hole, (2) constrain the
radius of the inner edge of the accretion disk, (3) determine if the UV/optical
emission is due to the accretion disk or to an advection-dominated flow, (4)
acquire key data on the extreme faintness of black holes relative to neutron
stars, and (5) test models proposed to explain the faintness of quiescent black
holes.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:18:10.80 +48:02:12.30 XTE J1118+480 ACIS-S NONE 10.00
11:18:10.80 +48:02:12.30 XTE J1118+480 ACIS-S NONE 42.00
===================================================================================
Proposal Number: 03400483
Proposal Title: ``QPO-FOLDED'' SPECTROSCOPIC STUDY OF 3 LOW-MASS X-RAY BINARIES
AND DIPPING SOURCES
PI: MARIANO MENDEZ
Subject Category: BH AND NS BINARIES
Abstract: We will use Chandra's ACIS-S detector in combination with HETG and LETG
to do phase-resolved spectroscopy of the three low-mass X-ray binaries and
dippers 4U 1746-37, 4U 1323-62, and EXO 0748-676. Using the 1 Hz QPO that we
recently discovered in these sources we will construct ``QPO-folded'' light
curves to study separately spectra from different QPO-phase intervals. We will
correlate the presence/absence of emission and absorption features in the energy
spectrum of Chandra (and XMM-Newton) with timing properties measured both by
Chandra, and simultaneous RXTE observations. This should help us determine how
timing properties depend on mass accretion rate, and whether mass flows onto the
central object through different channels of accretion.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:50:12.70 -37:03:08.00 4U 1746-37 ACIS-S HETG 40.00
===================================================================================
Proposal Number: 03408078
Proposal Title: IMAGING THE JET/ISM INTERACTIONS AROUND THE BLACK HOLE
XTEJ1550-564
PI: STEPHANE CORBEL
Subject Category: BH AND NS BINARIES
Abstract: We discovered a new radio source, 22" West of the black hole
XTEJ1550-564 (IAUC 7795; 2002 Jan 19). Subsequent observations show it has a
variable spectrum, is extended toward XTEJ1550 and is located along the axis of
the VLBI jets observed during the Sept 1998 radio flare. Our Chandra images from
Aug-Sept 2000 show an extended X-ray source also along the VLBI jet axis, but
directly opposite the radio source (23" to the East), and with similar flux
during the two Chandra observations (21 days apart). We found a transient radio
source in archival data at this position in Feb 2001, indicating a lifetime of a
few months. It is likely that both components represent superluminal plasmons
ejected during the Sept 1998 major radio flare and interacting with the ISM. The
proposed Chandra observation will allow us to study the physics of jet/ISM
interactions and the total power of relativistic jets, with implications for our
understanding of relativistic jets from AGN.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
15:50:58.70 -56:28:35.60 XTE J1550-564 ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03408085
Proposal Title: A FAINT NEUTRON STAR SOFT X-RAY TRANSIENT RETURNING TO
QUIESCENCE
PI: PETER JONKER
Subject Category: BH AND NS BINARIES
Abstract: Approx 10 SXTs like SAXJ1808.4-3658 form a class of faint SXTs,
calculations show that the NS magnetic field will not be buried in these systems.
We propose to obtain three observations of a faint SXT as it returns to
quiescence. Monitoring observations will allow us to observe the transition from
a spectrally hard state in outburst to a soft spectral state in quiescence. To
find out which emission mechanism is responsible for the low-level X-ray
emission, it is crucial to get good 0.1-8 keV spectra and to identify at which
luminosity the transition from hard to soft takes place. For this study the low
N_H of this source is vital. Given a neutron star magnetic field strength, for
lower mass accretion rates (unaccessible for RXTE) the magnetosphere will be
larger and the polar caps onto which magnetically channelled matter accretes
smaller, resulting in larger pulsed fractions. Observations with ACIS-S in CC
mode will allow us to search for pulsations at frequencies less than 166 Hz.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:09:30.20 -26:39:27.00 RX J170930.2-263927 ACIS-S NONE 5.00
17:09:30.20 -26:39:27.00 RX J170930.2-263927 ACIS-S NONE 5.00
17:09:30.20 -26:39:27.00 RX J170930.2-263927 ACIS-S NONE 5.00
17:09:30.20 -26:39:27.00 RX J170930.2-263927 ACIS-S NONE 5.00
17:09:30.20 -26:39:27.00 RX J170930.2-263927 ACIS-S NONE 5.00
17:09:30.20 -26:39:27.00 RX J170930.2-263927 ACIS-S NONE 8.48
17:09:30.20 -26:39:27.00 RX J170930.2-263927 ACIS-S NONE 10.00
17:09:30.20 -26:39:27.00 RX J170930.2-263927 ACIS-S NONE 10.00
17:09:30.20 -26:39:27.00 RX J170930.2-263927 ACIS-S NONE 10.00
17:09:30.20 -26:39:27.00 RX J170930.2-263927 ACIS-S NONE 15.00
17:09:30.20 -26:39:24.00 RX J170930.2-263927 ACIS-S NONE 5.00
17:09:30.20 -26:39:24.00 RX J170930.2-263927 ACIS-S NONE 5.00
===================================================================================
Proposal Number: 04400362
Proposal Title: MONITORING TWO QUASI-PERSISTENT X-RAY BINARIES IN QUIESCENCE
PI: RUDY WIJNANDS
Subject Category: BH AND NS BINARIES
Abstract: We propose to observe the quasi-persistent neutron-star low-mass X-ray
binaries KS 1731-260 and MXB 1659-298 twice in their quiescent state during cycle
4 of Chandra. These observations will strongly constrain the time evolution
behavior of the quiescent properties of those systems. In the context of the
cooling neutron star model for the quiescent emission in neutron star X-ray
transients, our proposed observations will follow the cooling time of the crust
and core of the neutron stars in those systems. Our previous Chandra and
XMM-Newton observations of KS 1731-260 have already shown that the neutron star
crust in KS 1731-260 cooled down rapidly, setting stringent constraints on the
structure of the neutron star in this system.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:02:06.40 -29:56:44.30 MXB 1659-298 ACIS-S NONE 30.00
17:02:06.40 -29:56:44.30 MXB 1659-298 ACIS-S NONE 30.00
17:34:13.50 -26:05:18.80 KS 1731-260 ACIS-S NONE 30.00
17:34:13.50 -26:05:18.80 KS 1731-260 ACIS-S NONE 30.00
===================================================================================
Proposal Number: 04400385
Proposal Title: A SEARCH FOR X-RAY JETS IN QUIESCENT MICROQUASARS
PI: JOHN TOMSICK
Subject Category: BH AND NS BINARIES
Abstract: Although relativistic jets are present in AGN, Galactic compact objects
(called microquasars) and probably gamma-ray bursts, their production and basic
properties are not well-understood. Using Chandra, we have discovered extended
X-ray jet emission from the black hole X-ray transient and microquasar XTE
J1550-564. Based on the behavior of XTE J1550-564, we believe it is likely that
X-ray jets are present for other transient microquasars in quiescence, and we
propose to observe V4641 Sgr, XTE J1859+226 and CI Cam for 25 ks each with the
goal of detecting X-ray jets.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:19:21.60 -25:24:25.60 V4641 SGR ACIS-S NONE 25.00
18:58:41.60 +22:39:29.40 XTE J1859+226 ACIS-S NONE 25.00
===================================================================================
Proposal Number: 04400460
Proposal Title: JET INTERACTIONS AROUND THE BLACK HOLE XTE J1550-564
PI: STEPHANE CORBEL
Subject Category: BH AND NS BINARIES
Abstract: We have discovered X-ray emission from the superluminal jet of the
Galactic black hole XTE J1550-564. The emission is due to either internal shocks
in the relativistic plasmons or interaction of the jet with the interstellar
medium. We propose to use Chandra to study in detail the dynamical evolution of
the jet, something impractical for AGN jets due to the time scales involved.
These observations, together with contemporaneously radio and optical
observations, may help us understand the physics of jet/ISM interactions, the
total power of relativistic jets, and the broadband emission mechanisms of
superluminal jets. This will have implications not only for the study of jets
from galactic X-ray binaries, but also for our understanding of relativistic jets
from AGN and gamma ray bursts.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
15:50:58.70 -56:28:35.60 XTE J1550-564 (JET) ACIS-S NONE 25.00
15:50:58.70 -56:28:35.60 XTE J1550-564 (JET) ACIS-S NONE 25.00
===================================================================================
Proposal Number: 03408089
Proposal Title: AN ACCURATE POSITION FOR THE BLACK HOLE CANDIDATE XTE J1908+094
PI: MICHAEL RUPEN
Subject Category: BH AND NS BINARIES
Abstract: We request a 1 ksec ACIS-S scan of the new transient J1908+094, to
obtain an accurate position to pin down a possible IR/radio counterpart, as well
as a quick X-ray spectrum. The source was detected by chance during PCA
observations of SGR 1900+014 on 21 Feb 2002; a scan on 18 Mar gave a 2' error box
~24' from the SGR, and showed it had risen from 26 to 64 mCrab (IAUC 7856). The
timing characteristics (IAUC 7856) and a strong hard tail (IAUC 7861) make this a
strong black hole candidate. The field is quite confused in the near IR, and
although our INT I image (19 Mar) suggests a possible faint counterpart, our VLA
data (21-22 Mar) show no radio source at that position, though there is another
(~1 mJy) source within the RXTE error box. We need a Chandra position to either
confirm the IR or radio counterpart, or to allow much deeper limits based on more
accurate astrometry. There are other possibilities; the I band image for instance
does not rule out a blue counterpart as in J1655-40.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:08:52.54 +09:23:02.50 XTE J1908+094 ACIS-S NONE 1.00
===================================================================================
Proposal Number: 03408090
Proposal Title: VARIABLE THERMAL EMISSION AND FEATURE FROM AQL X-1 IN QUIESCENCE
PI: ROBERT RUTLEDGE
Subject Category: BH AND NS BINARIES
Abstract: Aql X-1 went into outburst Feb 15 (ATEL 83) and was below 3 sigma
detection in the 1-day ASM countrate on Mar 25. On Apr 1, it has been undetected
with ASM for 7 days, which indicates it has returned to quiescence. We request
observations to monitor the quiescent spectrum and intensity over 140 days, for 2
goals: (1) Long-term time-variability was observed between our 4 AO1 observations
of Aql X-1. The variability may be secular, due to slow atmospheric-related
processes, as opposed to stochastic processes like accretion-power. (2) Two
important phenomena related to accretion were observed during only one (of the
four) observations: short time-scale variability (32+8-6% rms, 1-10000 sec
timescale) and a (time-variable) deficit of counts in the 0.45-0.6 keV band,
where the first absorption feature due to metals in a NS atmosphere should occur.
Multiple observations with the previous sensitivity can again detect variability
and the deficit of counts in >1 observation.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:11:16.00 +00:35:06.00 AQL X-1 ACIS-S NONE 7.00
19:11:16.00 +00:35:06.00 AQL X-1 ACIS-S NONE 7.00
19:11:16.00 +00:35:06.00 AQL X-1 ACIS-S NONE 7.00
19:11:16.00 +00:35:06.00 AQL X-1 ACIS-S NONE 7.00
19:11:16.00 +00:35:06.00 AQL X-1 ACIS-S NONE 7.00
19:11:16.00 +00:35:06.00 AQL X-1 ACIS-S NONE 7.00
19:11:16.00 +00:35:06.00 AQL X-1 ACIS-S NONE 7.00
===================================================================================
Proposal Number: 03408093
Proposal Title: OBSERVATIONS OF THE NEWLY DISCOVERED MILLISECOND ACCRETING
PULSAR XTE J1751-305
PI: CRAIG MARKWARDT
Subject Category: BH AND NS BINARIES
Abstract: Millisecond pulsars are probably the endpoint of evolution of low mass
X-ray binaries (LMXBs). However, the actual detection of neutron star spin
frequencies in LMXBs has been problematic, with SAX J1808.4-3658 being the only
known millisecond accreting pulsar. The newly discovered source (03 Apr 2002) XTE
J1751-305 was detected by RXTE PCA as a 435 Hz pulsar. Ultimately we hope to
measure the orbital period and determine mass constraints for the primary and
secondary stars. This will lead to constraints on population evolution of LMXBs.
A position determined from the BeppoSAX WFC (by J. in 't Zand) refines the
position to within 1.2 arcmin. Because this region is near the galactic center, a
rapid and accurate X-ray position determination is important. This will enable
prompt follow-up observations in the IR and radio bands. We request Chandra HRC-S
observations in "Imaging Mode" primarily to determine the position, and also to
improve the timing solution.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:51:16.00 -30:37:30.00 XTE J1751-305 HRC-S NONE 3.00
===================================================================================
Proposal Number: 03408100
Proposal Title: SPECTROSCOPY OF THE HIGH-LATITUDE ACCRETING MILLISECOND PULSAR
XTE J0929-314
PI: DEEPTO CHAKRABARTY
Subject Category: BH AND NS BINARIES
Abstract: The 3rd msec X-ray pulsar, XTE J0929-314 (Pspin=5.4 ms, Porb=43 min)
was just discovered (IAUC 7893). Along with the other two (SAX J1808.4-3658,
Pspin=2.5 ms, Porb=2 hr; XTE J1751-305, Pspin=2.3 ms, Porb=42 min), this
establishes a pattern of msec pulsars being found in very close binaries. The
donors in ultracompact binaries (Porb < 80 min) are H-poor and likely degenerate.
As seen in CXO observations of the ultracompact 4U 1626-67 (Schulz et al. 2001,
ApJ), this exotic composition can be traced through X-ray spectroscopy. The
source (like 1626) is high-latitude (14 deg) and low-column (Nh<1e21), making it
an ideal target. (J1751 was at Galactic ctr!) From orbital size, a C-O or O-Ne-Mg
donor is likely. We request LETG/ACIS spectra to search for emission lines and
absorption edges. (ACIS for larger area <50 A.) We also hope to compare the edges
with HST UV Ly-alpha measurement of Nh (HST DDT prop submitted) to explore local
composition (cf. 1626 paper).
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
09:29:20.20 -31:23:02.70 XTE J0929-314 ACIS-S LETG 20.00
===================================================================================
Proposal Number: 03408104
Proposal Title: THE LOW/SOFT STATE IN THE MICROQUASAR 1E1740.7-2942
PI: WILLIAM HEINDL
Subject Category: BH AND NS BINARIES
Abstract: Based on RXTE monitoring, the microquasar 1E1740.7-2942 has faded and
softened dramatically, entering a "low/soft" state seen only in its twin
microquasar, GRS1758-258. It is unlikely that this state will occur again for a
decade. The usual black hole "high/soft" state appears at high luminosity, but
this low/soft state appears while the source is dim/fading. We speculate that
this is caused by the shutoff of accretion to two simultaneous flows: a thin disk
and a hot, radial coronal flow. The transition occurs because the hot flow
accretes away rapidly (free-fall timescale) while the disk is consumed on the
viscous timescale (weeks). GRS1758-258 showed an exponential flux decay with a
timescale of about a month after the transition. We expect similar behavior in
1E1740.7-2942. Chandra will confirm the presence of a simple disk spectrum seen
now without a corona. If the corona has been ejected, it may detect jets via
extended morphology or Doppler shifted emission lines.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:43:54.80 -29:44:42.80 1E 1740.7-2942 ACIS-S NONE 5.00
17:43:54.80 -29:44:42.80 1E 1740.7-2942 ACIS-S HETG 10.00
===================================================================================
Proposal Number: 03408105
Proposal Title: FURTHER IMAGING OF THE JETS OF THE BLACK HOLE XTEJ1550-564
PI: STEPHANE CORBEL
Subject Category: BH AND NS BINARIES
Abstract: Following our discovery of a radio jet from the black hole candidate
XTEJ1550-564 (IAUC 7795), we detected X-rays from both the western and eastern
jets. The western jet has a sharp peak along its leading edge (away from the BHC)
and is extended along the trailing edge. The spectrum is a power law with a
photon index near 1.7. The eastern jet gives the first detection of proper motion
in X-rays for a jet from a black hole and proves that the jets move with
relativistic speeds on large scales as hypothesized for AGN jets. The proposed
observation will allow us to study the dynamics of jet/ISM interactions on time
scales inaccessible for AGN jets by determining the evolution of the flux,
morphology, and spectrum of the jets. We will measure the proper motion of the
western jet to an accuracy of 3 mas/day which will show whether it is still
travelling at relativistic speeds (the average proper motion up to March was 18
mas/day) or has reached a termination shock.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
15:50:58.70 -56:28:35.60 XTE J1550-564 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03408111
Proposal Title: AN ACIS LOOK AT MACHO-99-BLG-22:AN INTERMEDIATE MASS BLACK HOLE
ON OUR DOORSTEP?
PI: CHRISTOPHER REYNOLDS
Subject Category: BH AND NS BINARIES
Abstract: We request a 20ks ACIS-S observation at the position of the longest
ever detected microlensing event, MACHO-99-BLG-22. A likelyhood analysis of the
lensing event shows that the lens is either a stellar mass black hole (BH) in the
Galactic bulge, *or* an intermediate mass BH about 500pc from us. Constraints
from an old ROSAT-PSPC observation are uninteresting (F_X<2*10^-13 erg/cm^2/s).
However, Chandra will be able to easily detect radiatively-efficient Bondi-Hoyle
accretion onto the BH. Even in the "worst case" of accretion from the hot ISM
with a column density of 1e21/cm^2 and a bolometric correction of 10, we would
expect to detect 20 photons. On the other hand, it is very unlikely that a
stellar mass BH in the bulge would be detectable. The requested observation,
therefore, provides a powerful way of determining whether the lensing object
really is an intermediate mass BH on our doorstep.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:05:05.30 -28:34:42.50 MACHO-99-BLG-22 ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03408113
Proposal Title: OBSERVATION OF CYG X-1 IN THE HIGH STATE WITH HETG/CHANDRA
PI: YUXIN FENG
Subject Category: BH AND NS BINARIES
Abstract: The 7 HETG/Chandra observations of Cyg X-1 covered the low(LS),
transition(TS) and high(HS) states that showed variable spectral features. Recent
3 observations (5ks) in HS showed an evidence for broad Fe K line which is
markedly different from that of LS and TS. It indicates that the disk line may be
distorted significantly by strong relativistic effects near the black hole in
HS.However, poor S/N line profiles in HS did not allow us to measure the
relativistic effects, the inner accretion disk radius which is generally believed
very close to the last stable orbit and can be used to determine the spin of the
hole, ionization states, inclination, etc. We propose 60 ks CC-mode HETG/Chandra
observation of Cyg X-1, which has settled in rare HS(HR2<0.7, ASM/RXTE since
April 2002) to detect the broad line. It is important also in understanding the
physical process which causes the state transition. A simultaneous RXTE
observation will also be planned to constrain the continuum above 5 keV.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:58:21.80 +35:12:06.50 CYG X-1 ACIS-S HETG 30.00
===================================================================================
Proposal Number: 03408114
Proposal Title: V4641 SGR DURING OUTBURST: FAST JETS & VARIABLE CORE
PI: MICHAEL RUPEN
Subject Category: BH AND NS BINARIES
Abstract: The black-hole X-ray binary (BHXB) V4641 Sgr was discovered in 1999;
0.5" radio jets were seen within 24h of the X-ray flare. Another outburst in May
has produced ongoing optical/radio/X-ray activity. The apparent jet velocities
(9.5c) are the highest yet known; in a few months they may easily extend over an
arcmin. With the past 2 months of activity, this is an ideal time to look for
such extended emission. The high quiescent luminosity (10x > BHXBs of similar
orbital period) and the strong, very wide Fe line seen in 1999 both suggest
X-rays from the jets: Doppler boosting may explain the luminosity, & the Fe line
suggests entrained/shocked material. We request ToO data to image these putative
X-ray jets, and to check for variability both in the jets & in the central
source. There is an accepted A04 proposal (Tomsick); but it is important also to
observe during the current outburst, given the extreme variability and high
proper motions. We'd be happy to share these data with Tomsick.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:19:21.60 -25:24:25.60 V4641SGR ACIS-S NONE 5.00
===================================================================================
Proposal Number: 03408116
Proposal Title: INVESTIGATION OF THE UNIQUE UNIDENTIFIED TEV SOURCE, TEV
J2032+4130, IN CYG OB2
PI: YOUSAF BUTT
Subject Category: BH AND NS BINARIES
Abstract: Observation by HEGRA at TeV energies has revealed the first, and only,
unidentified TeV source, TeV J2032+4130 at the 4.6sigma level in Cyg OB2
association. It is marginally consistent with the location of unidentified EGRET
(GeV) source 3EG J2033+4118 and has luminosity ~0.03 Crab in TeV. The source's
2sigma error location circle is just 6 arcmin in radius, well suited to CHANDRA
ACIS-I field of view. Chandra data on point-like vs. diffuse emission + spectra
will constrain source. In particular, we will resolve whether one of the sources
observed by ROSAT, 2RXP 203218.1+412807, seen in one of our Cyg OB2 datasets
could be related to the TeV emission -- we cannot tell if the ROSAT source is
intrinsically diffuse or point-like, nor can we yet constrain its spectrum. We
expect an ACIS-I ct rate of ~0.25 cts/sec from this source. There is some urgency
since the source may show variability on timescales of months. Please see
astro-ph/0207528 and Benaglia et al., A&A,366,605.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
20:32:07.00 +41:30:30.00 TEV J2032+4130 ACIS-I NONE 5.00
***********************************************************************************
SN, SNR AND ISOLATED NS
--------------------------------------------------
===================================================================================
Proposal Number: 03500014
Proposal Title: GAMMA-RAY BURST PROGENITORS: PROBING THEIR ENVIRONMENT
PI: SHRINIVAS KULKARNI
Subject Category: SN, SNR AND ISOLATED NS
Abstract: Gamma-ray burst astronomy is a field maturing at a phenomenal rate.
Only three years after the discovery of fading long-wavelength counterparts, we
now have distance measurements for dozens of events, we have developed a detailed
theoretical framework for understanding the X-ray -- radio afterglow lightcurves,
and observational evidence now ties the progenitors of long GRBs (those studied
to-date) to the collapse of massive stars. While progress has been rapid, three
important new observational and theoretical discoveries, formulated over the last
twelve months, allow us to address new and in many cases more sophisticated
questions than could have been posed a year ago.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
GRB TOO 1 ACIS-S HETG 55.00
===================================================================================
Proposal Number: 03500025
Proposal Title: AN X-RAY STUDY OF THE CENTER-FILLED SNR MSH11-61A AND ITS
NEUTRON STAR CANDIDATE RX J1102.9-6054
PI: PETER PREDEHL
Subject Category: SN, SNR AND ISOLATED NS
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:02:57.20 -60:54:34.00 MSH 11-61A ACIS-I NONE 30.00
11:02:57.20 -60:54:34.00 MSH 11-61A ACIS-I NONE 35.00
===================================================================================
Proposal Number: 03500072
Proposal Title: A SEARCH FOR PULSATIONS FROM THE CENTRAL CORE OF G21.5-0.9
PI: STEPHEN MURRAY
Subject Category: SN, SNR AND ISOLATED NS
Abstract: G21.5-0.9 is a Crab-like synchrotron nebula that is presumably powered
by a central pulsar. ACIS observations show that the power law index of the
nebula flattens with radius, indicative of the synchrotron burn-off of electrons
injected in the center. HRC observations show a central compact emission region
that is extended, with some indication of an embedded point source. We propose an
HRC timing observation with an exposure of 30 ks in order to search for
pulsations from the compact core of G21.5-0.9. The count rate of the compact
central region is 0.05 counts/s, so the proposed exposure would yield 1500
counts, thus providing sufficient statistics for a powerful timing search even if
the pulsations are somewhat dilluted by diffuse central emission. GTO Priority
"A"
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:33:34.00 -10:34:07.00 G21.5-0.9 HRC-S NONE 30.00
===================================================================================
Proposal Number: 03500076
Proposal Title: MEASUREMENT OF P-DOT IN 3C58
PI: STEPHEN MURRAY
Subject Category: SN, SNR AND ISOLATED NS
Abstract: An X-ray pulsar has been detected in the SNR 3C58. We propose a
follow-up observation to confirm the X-ray period and obtaina spin down rate
(P-dot) for this object. GTO Priority "A"
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
02:05:38.00 +64:49:24.00 3C58 HRC-S NONE 25.00
===================================================================================
Proposal Number: 03500096
Proposal Title: QUIESCENT RADIATION FROM MAGNETARS
PI: GORDON GARMIRE
Subject Category: SN, SNR AND ISOLATED NS
Abstract: The goals of this proposal are to (i) Measure the quiescent spectra of
magnetars (discriminate between thermal and nonthermal models and search for the
ion cyclotron lines.) (ii) Carry out phased resolved spectroscopy (iii) Resolve
the putative plerions (iv) make new measurement of periods
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:08:47.20 -40:08:51.00 RXJ J1708-4009 ACIS-S HETG 31.50
===================================================================================
Proposal Number: 03500098
Proposal Title: SNR 0103-72.6 : AN UNUSUALLY BRIGHT REMNANT IN THE SMC ALTERNATE
TARGET
PI: GORDON GARMIRE
Subject Category: SN, SNR AND ISOLATED NS
Abstract: The main goals of this proposal are to: search for a pulsar-powered
synchrotron nebular in the SMC
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:05:05.00 -72:22:60.00 SNR 0103-72.6 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03500136
Proposal Title: ACIS OBSERVATIONS OF THE CENTRAL OBJECT IN RCW103
PI: GORDON GARMIRE
Subject Category: SN, SNR AND ISOLATED NS
Abstract: We propose a 50 ks observation of the central object in the supernova
remnant RCW103 using the HETG. This object has been in a high intensity state
during the past two observations of it by the CXO. We propose to do a short
observation using the mode that we have employed during GTO2 to determine the
state of the source. If it is in a high state (~E-11 ergs/cm^2/s), then we would
propose to activate this TOO to do the grating observation. A grating observation
should help determine the nature of this unusual source, which has shown a 6 hour
periodic modlulation of its intensity, but with no optically detected
counterpart.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:17:36.30 -51:02:25.00 RCW103 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03500137
Proposal Title: CHANDRA TOO OBSERVATIONS OF TYPE IA SUPERNOVAE
PI: JOHN HUGHES
Subject Category: SN, SNR AND ISOLATED NS
Abstract: One of the major unsolved problems in supernova research concerns the
precise nature of the progenitor systems of Type Ia supernovae. We propose
Chandra target-of-opportunity observations of a bright Ia supernova in order to
better constrain the circumstellar environment of the progenitor and therefore
shed light on the nature of the precursor star. The ability of our team to
rapidly determine if a particular supernova meets our trigger criteria, coupled
with the broadband sensitivity and rapid response of Chandra, means that the
proposed observations will be more than an order of magnitude more sensitive than
any previous ones obtained in any waveband: X-ray, optical, or radio.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
SN IA TOO: INITIAL ACIS-S NONE 20.00
10:18:06.50 +21:49:41.70 SN2002BO ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03500138
Proposal Title: SNR 0506-68.0: A REMNANT TRANSITIONING FROM THE EJECTA-DOMINATED
TO THE SEDOV PHASE OF EVOLUTION
PI: JOHN HUGHES
Subject Category: SN, SNR AND ISOLATED NS
Abstract: SNR 0506-68.0 is the brightest LMC supernova remnant not yet observed
by Chandra. According to ASCA data it displays a higher mean metallicity than
nearly all of the other LMC remnants that are larger (e.g., DEM 71, N132D, and
N63A). On the other hand all LMC SNRs smaller than 0506-68.0 display evidence for
being young, i.e., a rapid pulsar, oxygen-rich optical emission or
ejecta-dominated X-ray emission. Thus 0506-68.0 appears to be a remnant in a
transitional phase of evolution between youth and middle age. We wish to use
Chandra to detect and study the ejecta emission that ASCA claims is there and
investigate how the metals from SNe ultimately mix into the ISM.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:05:54.00 -68:01:37.00 0506-68.0 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03500143
Proposal Title: YOUNG EJECTA-DOMINATED GALACTIC SUPERNOVA REMNANTS
PI: CARA RAKOWSKI
Subject Category: SN, SNR AND ISOLATED NS
Abstract: We propose a spectro-imaging study of two Galactic supernova remnants
(SNRs), G337.2-0.7 and G309.2-0.6, recently identified as being young and
ejecta-dominated by their ASCA X-ray spectra. The Chandra observations will be
critical for determining the spatial distribution of different X-ray emitting
materials, e.g. blast-wave, pulsar, synchrotron nebula, and ejecta knots. Given
the Si-rich nature of both these SNRs, we expect to see the nucleosynthetic
products of explosive O and Si-burning in their ejecta. Additionally, both SNRs
contain compact sources whose nature is currently unknown. Only Chandra has
sufficient spatial resolution to isolate their position and spectra, thereby
distinguishing between a small ejecta knot, a compact stellar remnant or a
foreground star.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:39:31.00 -47:49:30.00 G337.2 - 0.7 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03500193
Proposal Title: THE NEXT GEMINGA: A NEUTRON STAR IDENTIFICATION FOR THE EGRET
SOURCE 3EG J1835+5918
PI: JULES HALPERN
Subject Category: SN, SNR AND ISOLATED NS
Abstract: 3EG J1835+5918 is the brightest of the so-called unidentified EGRET
sources at intermediate galactic latitude (l,b)=(89,25). We obtained complete
radio, optical, and X-ray coverage of its error box, discovering a faint
ultrasoft X-ray source that can only be a nearby neutron star. 3EG J1835+5918 may
thus become the prototype of an hypothesized population of older pulsars, born in
the Gould belt, that can account for as many as 40 local EGRET sources. We
propose to prove that it is a neutron star and assess its point of origin by
obtaining precise coordinates with Chandra and deep HST images to measure its
color and proper motion. X-ray spectral information will address its temperature,
age, distance, and thus its gamma-ray efficiency.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:36:13.80 +59:25:30.40 3EG J1835+5918 ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03500195
Proposal Title: IS THE NEARBY ISOLATED NEUTRON STAR RX J0720.4-3125 A MAGNETAR?
PI: SHRINIVAS KULKARNI
Subject Category: SN, SNR AND ISOLATED NS
Abstract: Over the past few years, astronomers and physicists have realized that
X-ray spectroscopy of nearby neutron stars can be used to carry out tests of QED
and QCD under extreme conditions not accessible to laboratory experimentation. RX
J0720.4-3125 is the second brightest nearby neutron star and as such has and can
be expected to receive considerable attention. Unfortunately, the nature of the
source is unclear: an old magnetar, a weakly magnetized neutron star accreting
matter from the ISM, or a middle-aged pulsar. We show how with 29-ks of Chandra
time we can determine Pdot at a level to decisively unmask the nature of this
important source.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
07:20:24.90 -31:25:50.90 RX J0720.4-3125 ACIS-S NONE 1.00
07:20:24.90 -31:25:50.90 RX J0720.4-3125 ACIS-S NONE 3.88
07:20:24.90 -31:25:50.90 RX J0720.4-3125 ACIS-S NONE 9.88
07:20:24.90 -31:25:50.90 RX J0720.4-3125 ACIS-S NONE 14.40
===================================================================================
Proposal Number: 03500236
Proposal Title: NGC5471B: A HYPERNOVA REMNANT CANDIDATE IN M101
PI: Q. DANIEL WANG
Subject Category: SN, SNR AND ISOLATED NS
Abstract: We propose a Chandra ACIS-S observation of NGC5471B --- the best
X-ray-emitting hypernova remnant candidate recently identified in a giant HII
region of the nearby face-on spiral galaxy M101. With the superb pointing
accuracy and spatial resolution as well as the broad band coverage, this
observation will enable us to either confirm or reject this identification. If it
is confirmed, the remnant could have strong implications for understanding not
only Gamma-ray bursts observed at cosmological distances, but also various
energetic interstellar structures in nearby galaxies. The counting statistics
will further allow for a detailed morphological study of X-ray emission from the
giant HII region for spectral and timing analyses of point-like X-ray sources in
the field of the galaxy.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
14:04:29.10 +54:23:53.00 NGC5471B ACIS-S NONE 15.00
===================================================================================
Proposal Number: 03500259
Proposal Title: WHERE ARE THE SUPERNOVA REMNANTS AROUND YOUNG PULSARS?
PI: BRYAN GAENSLER
Subject Category: SN, SNR AND ISOLATED NS
Abstract: Young pulsars inside supernova remnants (SNRs) form a consistent
physical picture, in which the expanding blast wave from the supernova explosion
surrounds the central pulsar and its associated wind-driven synchrotron nebula.
However, many young pulsars have no associated SNR, a deficit which has no single
or obvious explanation. Here we propose ACIS observations of two young pulsars
which lack SNRs, PSRs J1105-6107 and B1046-58. Models which explain the absence
of SNRs around each pulsar make specific predictions for the morphology and
spectrum of high-resolution X-ray emission expected from these sources. With
Chandra, we will test both these specific models and the wider framework of our
understanding of pulsars which lack associated SNRs.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:05:26.20 -61:07:52.70 PSR J1105-6107 ACIS-S NONE 12.50
11:05:26.20 -61:07:52.70 PSR J1105-6107 ACIS-S NONE 12.50
===================================================================================
Proposal Number: 03500278
Proposal Title: AN UNIDENTIFIED ULTRA-STEEP SPECTRUM SOURCE
PI: JOSEPH LAZIO
Subject Category: SN, SNR AND ISOLATED NS
Abstract: Known classes of sources with radio spectra steeper than -1 (S ~
nu^alpha) include pulsars, high-z radio galaxies, fossil radio galaxies, and
cluster relics. As a routine process in our analysis of VLA 74 MHz images, we
look for, and generally find, higher frequency counterparts to all 74 MHz
sources. We have discovered a 74 MHz source with no higher frequency
counterparts, implying that its spectrum is steeper than -2.5. Although its
spectrum is consistent with that of many short-period pulsars, a 430 MHz
periodicity search at Arecibo Observatory was unsuccessful. However, pulse
broadening, scintillation, an ultra-steep radio spectrum, or orbital motion would
reduce our sensitivity. X-ray observations are immune to these effects. We
request 8 ks in an effort to detect this source.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
06:36:47.50 +18:38:48.84 VLA J0636+1838 ACIS-I NONE 8.00
===================================================================================
Proposal Number: 03500279
Proposal Title: THE MYSTERY OF COMPOSITE SUPERNOVA REMNANTS: THE CASE OF MSH
11-62
PI: ILANA HARRUS
Subject Category: SN, SNR AND ISOLATED NS
Abstract: Composite supernova remnants (SNRs) display the characteristics of both
a standard shell-type SNR as well as a compact nonthermal component powered by a
central object. A crucial aspect of their study is the ability to separate
spatially and spectrally these two components. We propose a 50 ks Chandra ACIS-S
observation of the composite SNR MSH 11-62. It has a Crab-like radio spectral
index and a strong linear polarization. Our ASCA observation has established the
existence of a thermal and a non-thermal component. The proposed observation
will: map the two contributions, characterize their respective properties and
constrain both the central engine and the dynamical state of the remnant, and
help build a general picture of the ever-growing class of composite supernova
remnants.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:11:52.00 -60:39:12.00 MSH 11-62 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03500282
Proposal Title: X-RAY SPECTROSCOPY OF SNR N157B, ITS PULSAR AND WIND NEBULA
PI: Q. DANIEL WANG
Subject Category: SN, SNR AND ISOLATED NS
Abstract: The remarkable SNR N157B contains the recently discovered 16 ms pulsar,
the most rapidly rotating young pulsar known. In addition to the large-scale
diffuse X-ray emission apparently associated with the SNR, three distinct
features have been spatially decomposed: the pulsar itself, a surrounding compact
wind nebula which is strongly elongated, and a long diffuse trail. We propose
Chandra ACIS observations for detailed X-ray spectroscopic measurements of these
components. These measurements are necessary for understanding the pulsar
emission mechanism, the pulsar wind, and the SNR. In particular, we will test our
proposed ram-pressure confined pulsar wind nebula model, which may provide
important constraints on the pulsar wind velocity and on the particle
acceleration at the shock front.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:37:47.60 -69:10:20.00 SNR N157B ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03500310
Proposal Title: THE PULSAR-POWERED NEBULA IN G322.5-0.1
PI: BRYAN GAENSLER
Subject Category: SN, SNR AND ISOLATED NS
Abstract: The current small sample of young pulsars shows a wide range of
properties. There is thus considerable motivation to discover new sources, both
to identify unusual and interesting pulsars for further study, and to establish
the properties of the overall population. Motivated by these issues, we here
propose ACIS observations of the pulsar-powered nebula in the supernova remnant
G322.5-0.1. We aim both to detect the central powering source and to use the
nebular morphology to probe the properties of the pulsar's relativistic wind.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
15:23:17.00 -57:06:37.00 G322.5-0.1 ACIS-I NONE 31.00
===================================================================================
Proposal Number: 03500339
Proposal Title: AN ACIS STUDY OF THE HIGH LUMINOSITY SNR G349.7+0.2
PI: PATRICK SLANE
Subject Category: SN, SNR AND ISOLATED NS
Abstract: G349.7+0.2 is one of the most X-ray luminous supernova remnants in the
Galaxy. CO measurements and the detection of OH masers clearly demonstrate that
the remnant is interacting with a molecular cloud, and provide a solid distance
measurement. Radio observations indicate a breakout into a lower density region
in the northwest. X-ray observations are consistent with this picture, indicating
a young SNR that has swept up considerable mass upon emerging from a wind-blown
cavity into dense material in the south. We propose an ACIS observation of
G349.7+0.2 in order to search for evidence of ejecta in the remnant, to study the
structure of the shocked material at the cloud interface, and to search for
temperature variations associated with the breakout into a lower density region.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:18:01.00 -37:26:49.00 G349.7+0.2 ACIS-S NONE 60.00
===================================================================================
Proposal Number: 03500343
Proposal Title: PROPOSAL FOR CHANDRA ACIS OBSERVATION OF THE THERMAL COMPOSITE
SNR 3C 391
PI: YANG CHEN
Subject Category: SN, SNR AND ISOLATED NS
Abstract: 3C391 is a supernova remnant interacting with a molecular cloud,
displaying a radio shell, X-ray bright interior, and mazer points. We propose a
65ks ACIS-S3 observation aiming to observe the source in arcsecond scales so as
to reveal much clearer information on the interaction and on the progenitor than
ROSAT and ASCA. The observation will yield X-ray fine structure, radial profile,
and element distribution. This information will be used to confront cloud
evaporation and breakout models for the emission and structure. We would answer
whether the poorly resolved X-ray bridge-like structure relates to the breakout
nozzle, what the NW sulphur arc is in nature, and why the NW abundance is
subsolar. Also, we hope to find a compact stellar remnant of an inferred massive
progenitor.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:49:28.30 -00:56:15.00 3C 391 ACIS-S NONE 65.00
===================================================================================
Proposal Number: 03500351
Proposal Title: IMAGING THE ENERGETIC PULSAR WIND NEBULA AROUND PSR J2229+6114
PI: JULES HALPERN
Subject Category: SN, SNR AND ISOLATED NS
Abstract: We discovered a new supernova remnant with an energetic 51.6 ms pulsar
in the error box of the EGRET source 3EG J2229+6122. With a spin-down power of
2.2x10**37 ergs/s, PSR J2229+6114 is the second most luminous gamma-ray pulsar
after the Crab, and more energetic than the Vela pulsar. A brief image that we
obtained with the Chandra ACIS-I in AO2 revealed a pulsar wind nebula with
features possibly quite similar to those of the Vela nebula. We propose to obtain
a long observation with ACIS-I in order to fully expose the variety of structures
that Chandra can resolve in these nebulae, and to search for additional diffuse
emission associated with the apparent bow-shock radio shell that surrounds the
X-ray source.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
22:29:05.30 +61:14:09.30 PSR J2229+6114 ACIS-I NONE 100.00
===================================================================================
Proposal Number: 03500363
Proposal Title: ASTROMETRIC STUDY OF ISOLATED NEUTRON STARS
PI: CHRISTIAN MOTCH
Subject Category: SN, SNR AND ISOLATED NS
Abstract: We propose to take advantage of the excellent imaging performance of
Chandra to measure accurate positions and proper motions of isolated neutron
stars discovered by ROSAT. First, the small error circles will considerably help
optical searches. Second, these observations will serve as first epoch
references. Observations a year or more after will provide determining
information on the X-ray powering mechanism, accretion from interstellar medium
or cooling. Optical studies are unpractical because of the extreme faintness of
the counterparts. Observing in the wavelength region of maximum emissivity
Chandra is the only observatory able to carry out this study.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
04:20:02.40 -50:22:49.50 RX J0420-5022 ACIS-S NONE 20.00
08:06:22.80 -41:22:33.00 RX J0806-4123 ACIS-I NONE 20.00
13:08:48.20 +21:27:07.50 RX J1308+2127 ACIS-I NONE 20.00
16:05:18.70 +32:49:19.70 RX J1605+3249 ACIS-I NONE 20.00
===================================================================================
Proposal Number: 03500389
Proposal Title: IMAGING AND TIMING STUDIES OF THE VERY ENERGETIC PSR J1420-6048
PI: ROGER ROMANI
Subject Category: SN, SNR AND ISOLATED NS
Abstract: We propose ACIS imaging and Continuous Clocking observations of the
recently discovered very energetic young pulsar PSR J1420-6048. This pulsar is
contained within the `Kookaburra' radio complex and is a likely counterpart of
the GeV source 3EG J1420-6038. ASCA observations of the region reveal an extended
hard X-ray source positionally coincident with the pulsar, and yield a marginal
X-ray pulse detection. The ACIS will be able to resolve the pulsar from the
nebula, and yield a good pulse profile and spectrum. We can simultaneously study
the nearby `Rabbit' radio/X-ray nebula, a potential plerion, to study its
morphology and spectrum, and to search for pulsations.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
14:19:32.00 -60:51:30.00 PSR J1420-6048 ACIS-S NONE 10.00
14:19:32.00 -60:51:30.00 PSR J1420-6048 ACIS-S NONE 10.00
14:19:32.00 -60:51:30.00 PSR J1420-6048 ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03500393
Proposal Title: CHANDRA OBSERVATIONS OF RXJ0806.3+1527: X-RAY STUDY OF A UNIQUE
X-RAY PULSATOR
PI: GIAN LUCA ISRAEL
Subject Category: SN, SNR AND ISOLATED NS
Abstract: We propose the first spectroscopic study of the unique X-ray pulsar
RXJ0806.3+1527. The currently known optical and X-ray characteristics of this
source are consistent both with a highly peculiar magnetic white dwarf in a
cataclysmic variable (CV), and an isolated accreting neutron star candidate, one
of the brightest discovered by ROSAT. This Chandra proposal represents the first
spectroscopic study of RXJ0806.3+1527 (in the X-ray band) and, together with the
requested spectroscopical Very Large Telescope (VLT) and photometric Telescopio
Nazionale Galileo (TNG) data (approved proposals) is expected to provide
important insights on the nature of RXJ0806.3+1527. A total exposure time of 20ks
is requested with ACIS-S
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
08:06:23.20 +15:27:30.40 RXJ0806.3+1527 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03500402
Proposal Title: PULSAR WIND TORI: NEUTRON STAR LINEAR AND ANGULAR MOMENTA
PI: ROGER ROMANI
Subject Category: SN, SNR AND ISOLATED NS
Abstract: The toroidal symmetry axis of isolated pulsar wind nebulae (PWN)
provides a model-independant measure of the spin orientation. We have selected a
set of PWN spanning the age range 10^4-10^6y, that are modeled to show resolvable
toroidal wind termination shocks. These objects can also provide proper motion
vectors and the angle between these momenta gives profound constraints on the
origin of pulsar velocities and a new probe of neutron star core collapse. Our
proposed spectral imaging study will provide new measurements of PWN energetics
and evolution and will additionally give spectrum and flux measurements to track
the cooling history of the young central neutron stars.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:38:25.10 +28:17:11.00 PSR J0538+2817 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03500415
Proposal Title: BRIDGING THE GAP: DISCOVERING THE INTER-PULSE EMISSION IN PSR
B1821-24
PI: ROBERT RUTLEDGE
Subject Category: SN, SNR AND ISOLATED NS
Abstract: With the requested observation, we will obtain an outstandingly high
S/N X-ray pulsed light-curve of the brightest recycled pulsar in the sky -- PSR
1821-24 -- to search for bridge emission, persistent emission, and to deliver an
important observational constraint for pulsar emission models; we will
demonstrate the end-to-end absolute timing capabilities of the HRC-S detector, up
to an accuracy of 8 micro-seconds, and provide the community with a calibration
resource; we will search for additional millisecond X-ray pulsars among the
resolved emission of M28; we will search for the optical counterparts of
identified X-ray sources with archival HST imaging; and we will search for the
unusual type-I X-ray burster housed in M28.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:24:32.00 -24:52:10.70 PSR B1821-24 HRC-S NONE 50.00
===================================================================================
Proposal Number: 03500419
Proposal Title: SEARCH FOR THE OUTER SHELL OF THE CRAB NEBULA
PI: FREDERICK SEWARD
Subject Category: SN, SNR AND ISOLATED NS
Abstract: The Crab Nebula is unique among supernova remnants in that there is no
evidence for rapidly moving debris from the explosion. We propose to search for
an outer shock with sensitivity 10-100 times that of previous X-ray observations.
If found, the properties of the shock will determine properties of the progenitor
star. Chandra is very well suited for this observation. We will also obtain an
excellent image of the dust halo. Properties of the interstellar grains and their
distribution can be derived.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:34:32.00 +22:11:22.00 CRAB NEBULA HALO ACIS-I NONE 20.00
===================================================================================
Proposal Number: 03500461
Proposal Title: THE ENIGMATIC X-RAY PULSATOR IN THE PKS 1209-51/52 SUPERNOVA
REMNANT
PI: VYACHESLAV ZAVLIN
Subject Category: SN, SNR AND ISOLATED NS
Abstract: The Chandra Cycle 1 observations have allowed us to discover a 424 ms
period of the radio-quiet central source in the SNR PKS 1209-51/52, which proves
that the source is a neutron star. However, its true nature cannot be understood
until the period derivative is measured. For instance, an active pulsar with
unfavorably directed radio beam and a truly silent neutron star, whose X-ray
pulsations are caused by a nonuniform distribution of the surface temperature,
will show different values of the period derivative. The proposed 30 ks ACIS
observation in Continuous Clocking mode will allow us to measure the period
derivative, to check if there are long-term flux variations, to perform the
phase-resolved spectral analysis, and to elucidate the nature of compact central
objects in SNRs.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:10:00.80 -52:26:25.10 1E1207.4-5209 ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03500523
Proposal Title: PSR 0656+14 AND ITS PUTATIVE PULSAR-WIND NEBULA
PI: VYACHESLAV ZAVLIN
Subject Category: SN, SNR AND ISOLATED NS
Abstract: PSR 0656+14 is the brightest of the three middle-aged pulsars emitting
thermal radiation in the soft X-ray range. The previous X-ray and optical
observations have revealed three components of the pulsar radiation, with
different spectral and timing properties. Two thermal components (soft and hard)
are emitted from the neutron star surface. The nonthermal power-law component is
emitted from the pulsar's magnetosphere and/or a compact nebula which has not
been resolved. The proposed 30-ks ACIS-S observation will allow us to accurately
separate the components and establish their origins, to determine chemical
composition and distributions of temperature and magnetic field at the neutron
star surface, to constrain the pulsar mass and radius, and to search for the
synchrotron nebula.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
06:59:48.10 +14:14:21.50 PSR 0656+14 ACIS-S NONE 5.00
06:59:48.10 +14:14:21.50 PSR 0656+14 ACIS-S NONE 25.00
===================================================================================
Proposal Number: 03500538
Proposal Title: A CHANDRA SURVEY FOR COMPACT OBJECTS IN SUPERNOVA REMNANTS
PI: SHRINIVAS KULKARNI
Subject Category: SN, SNR AND ISOLATED NS
Abstract: It has become increasingly clear that the natal properties of young
neutron stars exhibit a rich diversity --- dramatically illustrated by the
enigmatic central object in Cas A and hinted at by early 3D modeling of
core-collapse. We propose a survey of an objectively constructed sample of nearby
SNRs which, when combined with archival data and our vigorous multi-wavelength
observation program, will give us a reliable view of the true variety of neutron
stars. The ensuing statistics and studies of the central objects will advance our
understanding of core-collapse and have bearing on related topics (supernova
energetics, natal kicks, etc). We believe that this comprehensive effort, a
census of such objects within 5 kpc, will be one of the enduring legacies of the
Chandra mission.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:28:32.00 +63:06:34.00 G127.1+0.5 ACIS-I NONE 20.00
05:26:49.00 +42:57:19.00 G166.0+4.2 ACIS-I NONE 30.00
13:50:30.00 -62:06:13.00 G309.8+0.0 ACIS-I NONE 40.00
14:42:50.00 -62:28:20.00 G315.4-2.3 ACIS-I NONE 10.00
19:33:20.00 +18:58:44.00 G054.4-0.3 ACIS-I NONE 25.00
19:38:24.00 +17:17:32.00 G053.6-2.2 ACIS-I NONE 35.00
20:52:14.00 +55:20:30.00 G093.3+6.9 ACIS-I NONE 15.00
20:53:22.00 +43:27:18.00 G084.2-0.8 ACIS-I NONE 25.00
23:59:17.00 +62:26:53.00 G116.9+0.2 ACIS-I NONE 50.00
===================================================================================
Proposal Number: 03500604
Proposal Title: SEARCHING FOR PROTON CYCLOTRON FEATURES IN TWO MAGNETAR
CANDIDATES
PI: LUIGI STELLA
Subject Category: SN, SNR AND ISOLATED NS
Abstract: Soft gamma-ray repeaters, SGRs, and anomalous X-ray pulsars, AXPs,
might contain ``magnetars'', young neutron stars endowed with ultra-high magnetic
fields, which shine as X-ray sources by releasing magnetic energy. Models
involving accretion are not ruled out yet. For the magnetic fields of magnetars,
proton cyclotron features, PCFs, are expected to lie in the X-ray band (E(PCFs) =
0.63 B/(10^{14} G) keV). Model atmosphere calculations predict that PCFs are
conspicuous and relatively broad. We propose here to search for PCFs in the X-ray
spectrum of a SGR (SGR1900+14) and an AXP (1E1048--59), by exploiting the unique
characteristics of the Chandra HETGS and METGS. These observation might provide
decisive evidence in favor of the existence of magnetars.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
10:50:07.80 -59:53:15.00 1E1048-59 ACIS-S HETG 30.00
19:07:16.40 +09:19:44.10 SGR 1900+14 ACIS-S HETG 30.00
===================================================================================
Proposal Number: 03500622
Proposal Title: THE DYNAMICAL PULSAR-WIND NEBULA IN THE VELA SNR
PI: GEORGE PAVLOV
Subject Category: SN, SNR AND ISOLATED NS
Abstract: The Chandra observations have shown the fine structure of the
synchrotron pulsar-wind nebula (PWN) around the Vela pulsar and an appreciable
change of the brightness and spectra of its elements in 7 months between two
ACIS-S observations. To understand the nature of the morphological and spectral
variations, we propose a series of eight logarithmically spaced ACIS-S
observations, 20 ks each, which will allow us to determine the time scale(s) and
the magnitude of the variations, to probe the properties of the relativistic
plasma in the PWN, and to study the interaction of the relativistic pulsar wind
with the ambient medium.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
08:35:20.70 -45:10:36.00 VELA PWN ACIS-S NONE 20.00
08:35:20.70 -45:10:36.00 VELA PWN ACIS-S NONE 20.00
08:35:20.70 -45:10:36.00 VELA PWN ACIS-S NONE 20.00
08:35:20.70 -45:10:36.00 VELA PWN ACIS-S NONE 20.00
08:35:20.70 -45:10:36.00 VELA PWN ACIS-S NONE 20.00
08:35:20.70 -45:10:36.00 VELA PWN ACIS-S NONE 20.00
08:35:20.70 -45:10:36.00 VELA PWN ACIS-S NONE 20.00
08:35:20.70 -45:10:36.00 VELA PWN ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03500712
Proposal Title: BALMER-DOMINATED SHOCKS IN THE CYGNUS LOOP: PROBING
COLLISIONLESS SHOCK PHYSICS
PI: TERRANCE GAETZ
Subject Category: SN, SNR AND ISOLATED NS
Abstract: We propose ACIS-S3 pointings at the two best-studied Balmer-dominated
shocks in the Cygnus Loop. Abundant optical and UV data are available (including
FUSE pointings). Because of its low extinction, the Cygnus Loop is one of only
five galactic remnants observable in the UV. One Balmer filament is a fast (~350
km/s) collisionless shock, the other a slower (~180 km/s), rapidly decelerating
shock on the verge of becoming radiative. These shocks sample two phases in the
evolution of the shock/wall interaction. Using Chandra's high resolution, we will
extract spectra for narrow regions paralleling the optical shocks to obtain the
postshock variation. This combination of Chandra, optical, and UV data will
greatly constrain models for collisionless shock physical properties and shock
evolution.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
20:54:30.96 +32:17:59.42 CYGNUS LOOP NE2 ACIS-S NONE 60.00
20:56:03.76 +31:57:02.63 CYGNUS LOOP NE1 ACIS-S NONE 60.00
===================================================================================
Proposal Number: 03500721
Proposal Title: LOCALIZATION OF "OPTICALLY-DARK" GAMMA-RAY BURSTS BY CHANDRA AND
HST
PI: GEORGE RICKER
Subject Category: SN, SNR AND ISOLATED NS
Abstract: We propose Chandra (CXO) observations of 4 GRBs detected by the HETE
soft X-ray camera, with contemporaneous observations with HST. These observations
are "relaxed" TOOs, performed 7-16 days after burst detection. To optimize the
chance of isolating Z > 10 GRBs, we will select "dark GRBs" for which no optical
counterpart has been found by ground-based searches within 2 days of GRB onset.
Previous CXO GRB searches have required that observations start within ~24 hours
of burst onset, placing an enormous strain on CXO operations. We have determined
that 30 ks observations made 7-16 days after burst onset will detect sufficient
photons to allow <0.7" localization of the GRB afterglow. We will immediately
place all CXO and HST positions and intensities in the public domain via the
GCN.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
03:05:27.30 +03:50:16.15 XRF011130 ACIS-I NONE 30.00
15:15:04.10 -19:24:48.50 GRB020531 ACIS-I NONE 10.00
15:15:04.10 -19:24:48.50 GRB020531 ACIS-I NONE 20.00
===================================================================================
Proposal Number: 03500727
Proposal Title: SOFT X-RAY SPECTROSCOPY OF A GAMMA-RAY BURST AFTERGLOW WITH
CHANDRA
PI: FREDERIK PAERELS
Subject Category: SN, SNR AND ISOLATED NS
Abstract: We propose to observe the afterglow of a bright, high latitude
Gamma-Ray Burst with Chandra/LETGS, for a total of 100 ksec. The key objective of
this observation is the acquisition of the first sensitive soft X-ray emission
spectrum of a GRB afterglow. With it, we will measure the relative abundances of
the alpha-elements with respect to Fe, and directly address the viability of
models that associate GRB's with the core collapse of massive stars.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
13:58:03.10 -31:22:22.00 GRB 020405 ACIS-S LETG 60.00
===================================================================================
Proposal Number: 03500728
Proposal Title: FINE FLUOROSCOPY ON MOLECULAR CLUMPS OVERTAKEN BY SUPERNOVA
BLAST WAVE
PI: YASUNOBU UCHIYAMA
Subject Category: SN, SNR AND ISOLATED NS
Abstract: By ASCA/BeppoSAX observations of the supernova remnant G78.2+2.1 and
IC443, there found three hard X-ray emitting clumps in which efficient electron
acceleration would be taking place at the transmitted shock driven by the
supernova blast wave. We propose Chandra observations of these newly discovered
hard X-ray clumps to uncover the spatial structure of the molecular clumps and to
study the particle acceleration in a dense and turbulent medium.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
20:20:12.00 +40:38:60.00 G78.2+2.1 CLUMP-2 ACIS-I NONE 20.00
20:21:24.00 +40:48:36.00 G78.2+2.1 CLUMP-1 ACIS-I NONE 10.00
===================================================================================
Proposal Number: 03500756
Proposal Title: RICH X-RAY STRUCTURES OF MIXED-MORPHOLOGY SNR W28 IN HARD AND
SOFT EMISSION
PI: JEONGHEE RHO
Subject Category: SN, SNR AND ISOLATED NS
Abstract: We propose ACIS-S observations of the archetype mixed-morphology SNR
W28, which shows center-filled X-rays within a radio shell. Two evolutionary
scenarios --evaporating clouds and radiative shocks -- are competing to explain
the central X-ray emission. Our studies of W28 show that the plasma conditions
are different from other MM SNRs with an extra high temperature component and
spectral variation across the remnant. The sub arcsec ACIS image will resolve
highly structured X-ray emission of W28 at the center and shells as it is
correlated with the chaotic, knoty optical emission. We are searching for
evidence of cloud interaction in the X-ray band, cosmic ray acceleration sites,
tracers of ejecta material, fate of clouds due to evaporations, and the radiative
X-ray filaments.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:00:24.80 -23:25:40.30 W28 ACIS-S NONE 90.00
===================================================================================
Proposal Number: 03500759
Proposal Title: THE TWO SHELLS OF DEM L 316
PI: ROSA WILLIAMS
Subject Category: SN, SNR AND ISOLATED NS
Abstract: The double-lobed system DEML316 is a particularly puzzling object.
Although it is known to be the remnant of one or more supernovae, the precise
nature of the structure remains mysterious. Suggestions to date include (1) the
collision of two supernova remnants (SNRs); (2) a supernova explosion into a
bipolar cavity; or (3) two SNRs superposed along the line of sight. To confirm or
rule out these scenarios, we are proposing observations of this system with
Chandra's ACIS. We will use spatially-resolved spectroscopy to determine where
the hot gas is located within the shells and discover the pattern of temperature
variations across the system. The resolution of this puzzle will add greatly to
our knowledge of the frequency, distribution, and evolution of SNRs.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:47:15.00 -69:42:25.00 DEM L 316 ACIS-S NONE 12.40
05:47:15.00 -69:42:25.00 DEM L 316 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03500783
Proposal Title: SPATIAL AND SPECTRAL STUDIES OF X-RAYS FROM PSR B1823-13 AND ITS
COMPACT NEBULA
PI: SACHIKO TSURUTA
Subject Category: SN, SNR AND ISOLATED NS
Abstract: We propose to carry out an observation of the Vela-like PSR B1823-13
with Chandra's ACIS-S. The primary goal is to separate the point source from the
surrounding nebula, so that we can conduct spectral analysis. We emphasize that
only Chandra's instruments can clearly eliminate the contamination of the point
source spectrum from the photons originating from the compact nebula. The
comparison of the results thus obtained with neutron star cooling theories will
help us determine the composition of the stellar interior, degree of
superfluidity, the equation of state, and stellar radius. We will also be able to
study the structural and spectral details of the compact nebula surrounding the
pulsar, that will also have direct impact on some of the areas of pulsar
astrophysics.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:26:13.17 -13:34:47.20 PSR B1823-13 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03500831
Proposal Title: THE RAPIDLY EVOLVING YOUNG SUPERNOVA REMNANT, SNR1987A
PI: DAVID BURROWS
Subject Category: SN, SNR AND ISOLATED NS
Abstract: SNR1987A presents a unique opportunity to observe the birth and early
evolution of a supernova remnant at high spatial resolution. The Chandra X-ray
Observatory affords the possibility of monitoring the expansion and evolution of
this remnant with high resolution images and spatially-resolved spectra. This
proposal follows on to our successful Cycle 1 and Cycle 2 observations with a
continued monitoring program. We propose two 50 ks monitoring observations of
SNR1987A in AO3, spaced 6 months apart, to continue the regular monitoring
program that we began in October 1999.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:35:28.00 -69:16:11.10 SNR 1987A ACIS-S NONE 50.00
05:35:28.00 -69:16:11.10 SNR 1987A ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03500856
Proposal Title: USING CHANDRA TO UNVEIL THE NATURE OF AN INTRIGUING
PULSAR-SUPERNOVA REMNANT SYSTEM: PSR J1119-6127 AND G292.2-0.5
PI: SAMAR SAFI-HARB
Subject Category: SN, SNR AND ISOLATED NS
Abstract: PSR J1119-6127 is a 1,700 year-old, high magnetic field radio pulsar
(PSR), discovered near the center of the supernova remnant: SNR G292.2-0.5. X-ray
observations revealed a point source ~1.5' from the radio pulsar and ~1' from an
IRAS source, making this system a unique target to better understand the PSR-SNR
association and the way pulsars dump their energy in their surroundings. The poor
statistics of available X-ray data preculdes determining the nature of the
underlying emission mechanism from any part of the remnant. We propose a 60 ksec
ACIS-S observation to image the immediate vicinity of the X-ray source, determine
whether it is an unresolved synchrotron nebula or a precursor LMXB, and get
reliable parameters for the SN explosion.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:19:03.40 -61:28:30.00 G292.2-0.5 ACIS-S NONE 60.00
===================================================================================
Proposal Number: 03500270
Proposal Title: BUILDING A BETTER MOUSE-TRAP: X-RAY IMAGING OF G359.23-0.92
PI: BRYAN GAENSLER
Subject Category: SN, SNR AND ISOLATED NS
Abstract: The source G359.23-0.92 ("the Mouse") is a spectacular object, with a
compact radio/X-ray head and a long cometary radio tail. This morphology strongly
suggests that the Mouse is the result of a young high-velocity pulsar interacting
with the ambient medium. We propose an ACIS-S observation of this source, with
the twin aims of detecting the unseen pulsar and imaging its surrounding nebula.
Any young and energetic pulsar thus identified would be an important addition to
the small number of such sources known, while imaging of the nebula presents an
opportunity to study the geometry and morphology of the bow shock produced by the
pulsar's motion.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:47:15.80 -29:58:01.00 MOUSE ACIS-S NONE 35.00
===================================================================================
Proposal Number: 03508073
Proposal Title: CHANDRA IDENTIFICATION OF THE X-RAY COUNTERPART OF GRB020127
PI: DEREK FOX
Subject Category: SN, SNR AND ISOLATED NS
Abstract: Roughly one-third of arcminute-scale gamma-ray burst (GRB) error boxes
fail to yield any optical transient in spite of intensive ground-based follow-up
efforts. These so-called "dark GRBs" are likely extinguished in the optical by
dust and gas in their host galaxy: in the one dark GRB identified (in the radio)
so far, GRB970828, modeling efforts indicate an extinction of >10 mags in R-band
(Djorgovski et al. 2001). Such large extinctions are characteristic of molecular
clouds and star-forming regions, and thus shed light on the nature of GRB
progenitors. The 8-arcminute-radius error circle of GRB020127 was reported by the
HETE-II team within 4.5 hours of the burst (GCN 1229), was well-placed for
immediate observations, and was observed from at least two facilities (GCNs 1230,
1234), without identification of a counterpart. Our best hope for counterpart
identification thus lies with the Chandra observations proposed here.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
08:15:07.02 +36:45:25.70 GRB020127 ACIS-I NONE 10.00
08:15:07.02 +36:45:25.70 GRB020127 ACIS-I NONE 10.00
===================================================================================
Proposal Number: 03508074
Proposal Title: AN EARLY OBSERVATION OF A NEARBY SUPERNOVA
PI: ERIC SCHLEGEL
Subject Category: SN, SNR AND ISOLATED NS
Abstract: The X-ray emission of supernovae is a young field with relatively
little data. The possible connection of supernovae with GRBs has been tantalizing
since the occurrence of SN1998bw. The debate over that source continues.
Observations of SN2002ap may go a long way to settling some of the debate. In
addition, the X-ray emission of Type Ic supernova other than SN1998bw is based on
the single detection of SN1994I in M51. X-rays provide information about the
circumstellar ejecta as the out- going shock runs into matter from previous
phases of mass loss. A reverse shock is created which generates low-energy X-rays
(~1 keV) while the outgoing shock generates harder events. The X-rays probe the
circumstellar matter and will provide measures of abundances. The X-ray light
curve provides a measure of the matter distribution. (Ref for SN: Schlegel 1995,
Reports Prog in Physics, 58, 1375)
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:36:23.80 +15:45:13.20 SN2002AP ACIS-S NONE 25.00
01:36:23.80 +15:45:13.20 SN2002AP ACIS-S NONE 25.00
01:36:23.80 +15:45:13.20 SN2002AP ACIS-S NONE 25.00
===================================================================================
Proposal Number: 03508075
Proposal Title: LOCALIZATION OF "OPTICALLY-DARK" GAMMA-RAY BURSTS BY CHANDRA
PI: GEORGE RICKER
Subject Category: SN, SNR AND ISOLATED NS
Abstract: Observation will be a second epoch ACIS-I image of the field of a HETE
X-ray rich GRB (XRF011130). The first epoch ACIS-I 30 ksec observation took place
on 10 December. It has been proposed that X-ray rich GRBs may be at redshifts Z >
~10. To date, no X-ray rich GRB counterpart has ever been identified. In the
first epoch observation, ~20 candidates were established. Since the Chandra X-ray
candidates were localized to <1 arcsec accuracy by Chandra, followup imaging by
HST and spectroscopy by ~8 meter-class ground-based telescopes can immediately
take place after the second epoch Chandra data is reduced.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
03:05:24.13 +03:47:54.00 XRF011130 ACIS-I NONE 15.00
===================================================================================
Proposal Number: 03508080
Proposal Title: TOO OBSERVATIONS OF SGR 1900+14 IN AN UNUSUAL ACTIVE STATE
PI: PETER WOODS
Subject Category: SN, SNR AND ISOLATED NS
Abstract: Previously, we have found that the counterpart to SGR 1900+14 underwent
extraordinary spectral changes during burst active episodes in 1998 and 2001. It
is during these epochs where we have gained the most insight into the nature of
this source. SGR 1900+14 recently entered a new phase of activity starting on
2/17. Our ToO observation of the SGR on 2/19 with the RXTE PCA found the flux
(2-10 keV) to be a factor of ~20 higher than expected. The pulsed signal of the
SGR is not seen in the data, nor is the pulsed signal of a nearby Be transient
(XTE J1906+09). There are no other catalogued X-ray transients in the 1 degree
radius FWZM fov of the PCA. The power spectrum did show an excess level of red
noise, similar to that seen in many BHCs. We conclude that we are observing
either (i) the rise of a new transient or (ii) new behavior from SGR 1900+14 in
an active state. A PCA raster scan has shown that the excess emission is
consistent with the direction of the SGR.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:07:14.33 +09:19:20.10 SGR 1900+14 ACIS-S NONE 3.00
===================================================================================
Proposal Number: 03508087
Proposal Title: CHANDRA ARCSECOND LOCALIZATION OF THE DARK BURST GRB020321
PI: DEREK FOX
Subject Category: SN, SNR AND ISOLATED NS
Abstract: Roughly 1 in 3 arcminute-scale GRB error boxes fail to yield an optical
transient despite intensive ground-based searches. These "dark bursts" must be
subject to severe optical extinction, either within their host galaxy or because
they are located at z>5. Well-localized dark bursts thus identify highly obscured
star-forming galaxies or galaxies close to the epoch of reionization - objects of
great interest in either case. We propose to localize the dark burst GRB020321
with a single 20-ks Chandra observation. Despite rapid notification and a small
error box (GCNs 1284, 1285), prompt observations have failed to reveal an optical
or radio afterglow of this burst (R<24; GCNs 1289, 1305). Given the 2'-radius
localization we anticipate at most two interloping X-ray sources; comparison with
optical datasets will thus allow a unique identification of the GRB afterglow.
The expected X-ray flux will be extrapolated from BeppoSAX observations to
further cement the source identification.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:11:02.40 -83:42:00.00 GRB020321 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03508095
Proposal Title: SN2001IG: DETECTING A MASS LOSS PHASE?
PI: ERIC SCHLEGEL
Subject Category: SN, SNR AND ISOLATED NS
Abstract: The X-ray emission of supernovae is a young field with relatively
little data. X-rays provide information about the circumstellar ejecta as the
outgoing shock runs into matter from previous phases of mass loss. A reverse
shock is created which generates low-energy X-rays (~1 keV) while the outgoing
shock generates harder events. The X-rays probe the circumstellar matter and are
expected to provide measures of abundances in spectral lines. The X-ray light
curve (LC) additionally provides a measure of the matter distribution (Ref for
SN: Schlegel 1995, Reports on Prog in Physics, 58, 1375). The radio LC of SN1979C
has been interpreted as revealing waves of mass loss (Weiler et al. 1992, ApJ,
399, 672) from the progenitor. No other SN has shown such behavior prior to the
recent increase in the radio LC of SN2001ig. We expect the hard and soft X-rays
to behave differently, directly testing shock/reverse shock theory.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
22:57:30.70 -41:02:25.00 SN2001IG ACIS-S NONE 25.00
22:57:30.70 -41:02:25.00 SN2001IG ACIS-S NONE 25.00
22:57:30.70 -41:02:25.00 SN2001IG ACIS-S NONE 25.00
===================================================================================
Proposal Number: 03508096
Proposal Title: CHANDRA ARCSECOND LOCALIZATION OF THE X-RAY FLASH XRF020427
PI: DEREK FOX
Subject Category: SN, SNR AND ISOLATED NS
Abstract: The X-ray flashes (XRFs) are identified in BeppoSAX observations as
fast X-ray transients that exhibit the properties of gamma-ray burst (GRB) prompt
X-ray counterparts while lacking detectable gamma-ray emission (Heise et al.
2001, astro-ph/0111246). The XRFs are distinguished from Galactic phenomena by
their nonthermal spectra, fast evolution, and near-isotropic sky distribution.
However, the absence of gamma-ray emission means that either (1) the XRFs
originate at very high redshifts, z>5; or (2) the XRFs are a GRB-like phenomenon
with Lorentz factors intermediate to GRBs (L>100) and supernovae (L~1). Chandra,
VLA, and HST observations of XRF011030 established for the first time that, in at
least this case, the XRF was the result of (2) a highly energetic explosion at a
cosmological distance z<3 (GCNs 1136, 1143, 1268). Chandra observations of the
XRF020427 will allow us to identify and study only the second such cosmological
X-ray flash.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
22:09:33.60 -65:19:36.50 XRF020427 ACIS-S NONE 15.00
22:09:33.60 -65:19:36.50 XRF020427 ACIS-S NONE 15.00
===================================================================================
Proposal Number: 03508118
Proposal Title: GRATING OBSERVATION OF GRB020813
PI: GEORGE RICKER
Subject Category: SN, SNR AND ISOLATED NS
Abstract: The SXC on HETE has just localized a very bright (>10 Crab) GRB to an
accuracy of 1 arcmin. Within minutes of the burst location being disseminated, an
optical transient was discovered in the SXC error box. HETE is expected to detect
only 2-3 such events per year with the SXC. Since this burst has some X-ray
characteristics reminescent of GRB011121 (Reeves et al 2002), a grating
observation with Chandra could establish definitively whether hydrogen-like
emission lines from non-iron metals are characteristic of bright GRBs, as is
predicted by the "supranova" model (Vietri and Stella 1999).
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:46:41.90 -19:36:05.10 GRB020813 ACIS-S HETG 80.00
===================================================================================
Proposal Number: 03508125
Proposal Title: SPECTROSCOPIC OBSERVATIONS OF THE BRIGHT AFTERGLOW OF GRB021004
PI: FIONA HARRISON
Subject Category: SN, SNR AND ISOLATED NS
Abstract: One of the holy grails of gamma-ray burst research is to detect X-ray
line signatures from an afterglow with high statistical significance. Of all
possible observations, this perhaps offers the best chance of constraining the
GRB mechanism and environment, and could provide the "smoking gun" signature
connecting GRBs to massive stellar deaths. In order to accomplish this, we know
long observations within one day of the event are necessary.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:26:54.40 +18:55:43.00 GRB021004 ACIS-S HETG 80.00
===================================================================================
Proposal Number: 03508128
Proposal Title: PROMPT CHANDRA OBSERVATION OF THE TYPE II SN 2002HH
PI: WALTER LEWIN
Subject Category: SN, SNR AND ISOLATED NS
Abstract: We propose to observe the Type II SN 2002hh. As we have shown, Chandra
data will constrain details of the pre-SN evolution and properties of the SN
ejecta and the circumstellar (cs) matter. In our simulations, we have assumed
1999em-type and 1998S-type spectra, with appropriate distance and absorption. If
02hh is like 99em, a 30 ksec obs can determine the flux to ~25% and the
temperature to ~50%, which would constrain cs interaction models. If 02hh is like
98S, we expect ~0.1 cts/sec. A 30ks obs would give us more counts than the >100ks
spent on 98S, and we would ALSO be able to determine elemental abundances to
~25-40%, which is even better than was done for 98S. This will constrain the
progenitor mass as it did for 98S. The ONLY REASON we wish to not trigger our
200ks A04 TOO is the high extinction to 02hh. If we could use 30ks (and save 170
for another occasion) WE WOULD, but that may not be allowed. A 30ks DDT obs is a
sensible and effective way to seize this rare opportunity.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
20:34:51.20 +60:09:17.50 SN 2002HH ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03508129
Proposal Title: PROMPT CHANDRA OBSERVATION OF THE TYPE IIN SN 2002HI
PI: WALTER LEWIN
Subject Category: SN, SNR AND ISOLATED NS
Abstract: We propose to observe the Type IIn (narrow emission line) SN 2002hi.
Its optical spectra show it is similar to the extremely X-ray luminous SN 1988Z
(IAUC 8006), which was observed at Lx=1e41 erg/s at an age of 6.5yr. It is
unknown what the early-time (first few weeks to months) Lx of such a SN would be.
A simple constant density model of the circumstellar (cs) material around 88Z
predicts an Lx of 1e43 erg/s at an age of a few months with a hard spectrum.
However, the cs interaction is complicated, and this naive model may not hold
(e.g., there could be absorption by the cs gas). It is difficult to make clear
predictions because of the lack of knowledge. A 10ks obs of 02hi (at 260 Mpc)
will reach a sensitivity as low as ~1e40 erg/s. This early obs would be unique
for this interesting and poorly understood class of SNe. Chandra may only see 2-3
SNe like this during its lifetime, and this opportunity should not be missed. In
the future, we will propose for these SNe under Peer Review.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
07:19:54.10 +17:58:18.20 SN 2002HI ACIS-S NONE 10.00
===================================================================================
Proposal Number: 03508130
Proposal Title: THE DECAYING X-RAY AFTERGLOW OF GRB021004
PI: MASAO SAKO
Subject Category: SN, SNR AND ISOLATED NS
Abstract: Observations of the afterglow of GRB021004 have provided us with a
unique opportunity to study the detailed physical conditions of the burst
environment. The optical light curves are densely sampled since ~9.5 minutes
after the burst and consist of multiple bumps and wiggles on various timescales.
The X-ray light curve, however, is sampled only during an earlier Chandra HETG
observation, which lasted ~1 day starting from ~20.5 hours after the burst. The
temporal slope during this observation was determined to be -1.0 +/- 0.2, and
there was no obvious change in spectral shape throughout the observation. As
stressed by Heyl & Perna (astro-ph/021004), the X-ray light curve is particularly
important for distinguishing between the various possible emission models. We
propose to measure the X-ray flux and the spectral shape of GRB021004 during its
late afterglow phases to address the long-term behaviour of this spectacular
afterglow.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:26:54.70 +18:55:41.30 GRB021004 ACIS-S NONE 30.00
***********************************************************************************
NORMAL GALAXIES
--------------------------------------------------
===================================================================================
Proposal Number: 03600029
Proposal Title: RESOLVING THE X-RAY BINARY POPULATION IN EARLY-TYPE GALAXIES
PI: CRAIG SARAZIN
Subject Category: NORMAL GALAXIES
Abstract: Our Chandra image of NGC4697 resolved this X-ray faint elliptical into
low mass X-ray binaries (LMXBs), plus a small fraction (23%) from ISM gas. New
Chandra observations will spatially resolve the emission from 3 more X-ray faint
early-type galaxies. We will determine the luminosity functions of LMXBs, which
provide direct evidence of the history of massive star formation, and a measure
of the relative numbers of NS and BH binaries. We will detect ~15 supersoft
sources, and ~40 LMXBs in globular clusters. The total X-ray spectra of the
sources and colors for individual sources will be used to constrain models for
LMXBs. The amount, distribution, and X-ray spectrum of any ISM gas emission will
be derived, and the luminosities, temperatures, and abundances compared to X-ray
bright galaxies.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
15:06:29.40 +55:45:49.30 NGC5866 (M102) ACIS-S NONE 36.00
===================================================================================
Proposal Number: 03600060
Proposal Title: STELLAR MASS LOSS VERSUS EXTERNAL ACCRETION IN X-RAY BRIGHT
ELLIPTICALS
PI: CRAIG SARAZIN
Subject Category: NORMAL GALAXIES
Abstract: Observations of NGC533, NGC1600, and NGC1332, X-ray-bright ellipticals
with extended emission line filaments and dust, will be used to study the
interaction between the hot, X-ray emitting gas and cooler (merger related?)
interstellar material. We will determine whether heat conduction into the cooler
gas or energy losses to grains affect the thermal state of the gas. The elemental
abundances and gradients in the hot gas will be derived and compared to the
stellar values. If the gas results from local stellar mass loss, the abundances
should be similar. If there is a cooling flow, the abundances at each radius
should reflect those of stars at larger radii. In these bright galaxies, inflow
of intergalactic gas may also be important; this would produce low abundances
with weak gradients.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:25:31.40 +01:45:32.80 NGC533 ACIS-S NONE 38.00
04:31:39.90 -05:05:10.10 NGC1600 ACIS-S NONE 28.50
04:31:39.90 -05:05:10.10 NGC1600 ACIS-S NONE 28.50
04:31:39.90 -05:05:10.10 NGC1600 ACIS-S NONE 57.00
===================================================================================
Proposal Number: 03600067
Proposal Title: NGC507 -- A GALAXY IN THE ACT OF MERGING
PI: STEPHEN MURRAY
Subject Category: NORMAL GALAXIES
Abstract: NGC507 exhibits sharp "edges" which are remarkably similar to those
seen in Chandra observations of merging clusters. These edges could represent
residual gas density discontinuties left behind as the central galaxy slowly
oscillates within the larger dark matter potential. We propose to study the
"edges" in detail and to detemine gas density and temperatures across the edges
to understand their origin. In addition, the high Chandra angular resolution
allows detailed study of the bright central cooling flow region which is well
resolved. Finally, Chandra's broad energy response coupled with the high angular
resolution will allow us to study the interaction between the radio source
emanating from NGC507 and the surrounding gaseous corona. GTO Priority "A"
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:23:38.00 +33:15:24.00 NGC507 ACIS-I NONE 45.00
===================================================================================
Proposal Number: 03600121
Proposal Title: THE TRANSFORMATION OF GALAXIES IN CLUSTERS
PI: CHRISTINE JONES
Subject Category: NORMAL GALAXIES
Abstract: We propose ACIS-S observations of galaxies that appear to be present
epoch analogs to the blue galaxies in distant clusters. We propose to study
NGC4438, the most disrupted spiral in Virgo and NGC1427A, an irregular galaxy
moving through Fornax at supersonic speed. The disruption of these galaxies is
attributed to interactions in their cluster environments. With Chandra's spatial
resolution, we will determine the distribution of the hot interstellar medium,
regions of star formation, and for NGC4438, the distribution of galactic sources
and the interaction of hot gas with the radio source. Understanding galaxy-galaxy
and galaxy-ICM interactions in these galaxies will provide a better understanding
of the environmental processes that transform blue galaxies to sedate elliptical
and SO's.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:27:45.60 +13:00:32.00 NGC 4438 ACIS-S NONE 25.00
===================================================================================
Proposal Number: 03600177
Proposal Title: ISOLATED ELLIPTICAL GALAXIES
PI: TREVOR PONMAN
Subject Category: NORMAL GALAXIES
Abstract: Isolated ellipticals provide a key 'control' sample for investigating
environmental influences on hot gas halos. We have carefully defined such a
sample and select three galaxies whose X-ray fluxes best suit them for Chandra
observations. We aim to accurately define the discrete source component, and
estimate the metallicity, temperature and mass of the hot gas. Surface brightness
profiles will be compared to models and to ellipticals in denser environments,
revealing the signatures of stripping or ICM containment.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:35:41.20 +26:31:23.20 NGC 4555 ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03600280
Proposal Title: LUMINOUS NON-NUCLEAR X-RAY SOURCES IN NEARBY GALAXIES
PI: PHILIP KAARET
Subject Category: NORMAL GALAXIES
Abstract: We propose observations of nearby galaxies, which when combined with
current or planned Chandra observations, will complete the sample of Chandra
observations of known non-nuclear point sources with luminosities above 2E38
erg/s in galaxies within 15 Mpc. The arcsecond resolution of Chandra is essential
for unambigious identification of these sources, measurement of their x-ray
properties, and for localization of the sources with sufficient accuracy to
permit counterpart searches at other wavelengths. The observations proposed here
will be made public immediately to encourage multiwavelength follow-up of these
observations.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
14:03:21.10 -41:22:44.00 NGC 5408 ACIS-S NONE 4.60
===================================================================================
Proposal Number: 03600281
Proposal Title: SEARCHING FOR X-RAY TRANSIENTS IN M31 WITH CHANDRA AND HST
PI: MICHAEL GARCIA
Subject Category: NORMAL GALAXIES
Abstract: We propose observations to allow 6 X-ray Transients (XRT) to be studied
in M31. The x-ray properties of these XRT (spectra, variability) will allow us to
determine whether the accreting object is a black hole or a neutron star. HST
observations of these XRT will determine the nature of the secondary star:
massive stars will show little (<2 mag) change in their UV luminosities during
outbursts, while low-mass stars will show large (>5 mag) changes in their UV
luminosities. This dataset will allow the first detailed study of evolution of
black hole and neutron star binaries in an external galaxy. As many of the XRT in
the Milky Way contain black hole primaries, we expect that a major result will be
an understanding of the formation of stellar mass black holes in another galaxy.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:40:27.10 +40:40:12.00 M31-S2 HRC-I NONE 1.00
00:40:27.10 +40:40:12.00 M31-S2 HRC-I NONE 1.00
00:40:27.10 +40:40:12.00 M31-S2 HRC-I NONE 1.00
00:40:27.10 +40:40:12.00 M31-S2 HRC-I NONE 1.00
00:41:54.67 +40:56:47.50 M31-T6 ACIS-I NONE 5.00
00:41:54.67 +40:56:47.50 M31-T6 ACIS-I NONE 5.00
00:41:54.69 +40:56:47.80 M31-T5 ACIS-I NONE 5.00
00:42:07.90 +40:55:15.60 M31-S1 HRC-I NONE 1.00
00:42:07.90 +40:55:15.60 M31-S1 HRC-I NONE 1.00
00:42:07.90 +40:55:15.60 M31-S1 HRC-I NONE 1.00
00:42:07.90 +40:55:15.60 M31-S1 HRC-I NONE 1.00
00:42:34.90 +40:57:21.01 M31-T1 ACIS-I NONE 5.00
00:42:44.40 +41:16:08.30 M31-CORE HRC-I NONE 1.00
00:42:44.40 +41:16:08.30 M31-CORE HRC-I NONE 1.00
00:42:44.40 +41:16:08.30 M31-CORE HRC-I NONE 1.00
00:42:44.40 +41:43:15.60 M31-CORE HRC-I NONE 1.00
00:43:05.50 +41:17:03.30 M31-T3 ACIS-I NONE 5.00
00:43:08.50 +41:18:20.00 M31-T2 ACIS-I NONE 5.00
00:43:09.80 +41:19:00.72 M31-T4 ACIS-I NONE 5.00
00:43:09.80 +41:19:00.72 M31-T4 ACIS-I NONE 5.00
00:44:07.00 +41:43:15.60 M31-N1 HRC-I NONE 1.00
00:44:07.00 +41:43:15.60 M31-N1 HRC-I NONE 1.00
00:44:07.00 +41:43:15.60 M31-N1 HRC-I NONE 1.00
00:44:07.00 +41:43:15.60 M31-N1 HRC-I NONE 1.00
00:44:28.40 +41:56:28.10 M31-N2 HRC-I NONE 1.00
00:44:40.08 +41:21:46.80 M31-T5 ACIS-S NONE 5.00
00:45:19.90 +41:49:48.00 M31-N2 HRC-I NONE 1.00
00:45:19.90 +41:49:48.00 M31-N2 HRC-I NONE 1.00
00:45:19.90 +41:49:48.00 M31-N2 HRC-I NONE 1.00
===================================================================================
Proposal Number: 03600335
Proposal Title: THE SHAPES OF DARK MATTER HALOS
PI: DAVID BUOTE
Subject Category: NORMAL GALAXIES
Abstract: We propose to measure the shape of the dark matter halo in the S0
galaxy NGC 1332. The X-ray isophote shapes of early-type galaxies probe both the
shape and radial mass distribution essentially independently of the temperature
profile of the hot gas. With an 80ks ACIS-S observation we will establish
definitively whether a non-spherical dark matter halo exists in a disk galaxy,
measure in detail the ellipticity and radial density profile of the halo, and
determine the mass of the galaxy to within +/- 10% interior to the faintest
isophotes detected by ROSAT. The high resolution of Chandra is vital for removing
any discrete sources, particularly near the center. These measurements will
provide crucial tests of models of the nature of the dark matter and the
formation of galactic structure.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
03:26:17.00 -21:20:09.00 NGC 1332 ACIS-S NONE 20.00
03:26:17.00 -21:20:09.00 NGC 1332 ACIS-S NONE 60.00
===================================================================================
Proposal Number: 03600365
Proposal Title: FURTHER PROBING THE NATURE OF SUPER-LUMINOUS X-RAY SOURCES IN
NEARBY GALAXIES
PI: TIMOTHY ROBERTS
Subject Category: NORMAL GALAXIES
Abstract: We propose the continuation of a programme of Chandra ACIS-S
observations of very luminous (L(x) > 10^39 erg/s) extra-nuclear X-ray sources in
nearby galaxies. Early results from this programme, combined with optical
spectro-imaging data, demonstrate the potential of Chandra data to reveal the
nature of these sources. The new observations will determine whether more of
these objects are truly point-like or whether they are groups of discrete sources
and/or truly diffuse emission, providing high quality CCD spectroscopy and
astrometry plus gross variability data in each case. This will reveal whether the
X-ray luminosity is derived from accreting black holes, recent supernovae,
complexes of sources or, perhaps, an entirely new class of astrophysical object.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
03:45:55.20 +68:04:56.00 IC 342 X-1 ACIS-S NONE 10.00
03:45:55.20 +68:04:56.00 IC 342 X-1 ACIS-S NONE 10.00
11:20:37.50 +13:34:28.00 NGC 3628 X-2 ACIS-S NONE 25.00
11:20:37.50 +13:34:28.00 NGC 3628 X-2 ACIS-S NONE 25.00
12:09:22.60 +29:55:49.00 NGC 4136 X-1 ACIS-S NONE 20.00
12:09:22.60 +29:55:49.00 NGC 4136 X-1 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03600360
Proposal Title: STUDY OF THE ISM-STRIPPING PROCESS IN THE VIRGO SPIRAL NGC 4501
(M88)
PI: HANS BOEHRINGER
Subject Category: NORMAL GALAXIES
Abstract: The stripping of the ISM of spiral galaxies falling into a galaxy
cluster is one of the most interesting environmental effects in galaxy evolution.
In the nearby Virgo cluster we may be able to observe this process in detail.
From 21 cm data and from ROSAT HRI X-ray observations there is strong evidence
that the spiral galaxy NGC 4501 is currently stripped from its interstellar gas.
CHANDRA is ideally suited to study this effect by high spatial resolution imaging
and spectroscopy. Different scenarios as e.g. interaction induced star formation,
or the mixing of warm ISM with the hot cluster ICM predict distinct spectral
signatures that can observed. In addition we will obtain information on the Sy2
nuclues and possible on SN1999cl in this galaxy.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:31:58.50 +14:25:20.00 NGC 4501 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03600404
Proposal Title: THE DYNAMICS OF THE HOT ISM IN EARLY-TYPE GALAXIES
PI: LAURENCE DAVID
Subject Category: NORMAL GALAXIES
Abstract: Chandra has already made a major contribution to our understanding of
the X-ray emission from early-type galaxies by resolving the X-ray binary
population in near-by ellipticals. While the diffuse X-ray emission from the most
luminous ellipticals almost certainly arises from hot gas in nearly hydrostatic
equilibrium, the dynamic state of the ISM in less luminous ellipticals is
essentially unknown. Using Chandra's subarcsecond resolution we propose to
observe three moderate luminosity ellipticals (N2434, N4203, and N4278) and
determine the dynamic state of the hot gas (i.e., cooling flow, partial wind,
total subsonic wind, or total transonic wind). This information is a key
diagnostic of the past chemical and thermodynamic history of the ISM in
elliptical galaxies.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
07:34:51.40 -69:17:01.00 NGC2434 ACIS-S NONE 46.00
===================================================================================
Proposal Number: 03600427
Proposal Title: NGC 520: AN ANOMALOUS GALAXY MERGER?
PI: ANDREW READ
Subject Category: NORMAL GALAXIES
Abstract: NGC 520 is one of the closest merging galaxy systems, and its
properties are clearly anomalous in comparison to other galaxies at a similar
merger stage. In testing our understanding of the important process of galaxy
merging, such an exceptional case is of great value. We propose to map the
properties of NGC 520 in detail with Chandra, in order to resolve the
contributions to its X-ray luminosity, and to compare it with a sample of
`normal' merging systems. This will help us to understand the diversity in the
properties of merging galaxies in terms of the nature of the progenitor galaxies
and the dynamics of the merger process.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:24:34.80 +03:47:39.70 NGC520 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03600450
Proposal Title: POPULATION STUDIES OF DWARF GALAXIES
PI: ALLYN TENNANT
Subject Category: NORMAL GALAXIES
Abstract: Chandra observations have revealed different luminosity functions for
elliptical and spiral galaxies, and even between the bulge and disk of a spiral.
The luminosity function can be produced by a birth-death model, with the
luminosity break being a consequence of either a star-formation epoch in the near
past or piling up of Eddington-limited accreting neutron stars. The model
predicts more sources in active galactic environments, while undistributed
galaxies host mainly primordial binaries. We propose to observe 3 dwarf galaxies.
Our objectives are to verify the prediction of the birth-death model, and to
quantify the difference between the properties of X-ray binary populations in
dwarf and normal galaxies.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:44:56.20 -14:48:04.00 NGC 6822 ACIS-I NONE 30.00
===================================================================================
Proposal Number: 03600460
Proposal Title: CHANDRA SURVEY OF GALAXIES WITH KNOWN BLACK HOLE MASSES
PI: ANDREW PTAK
Subject Category: NORMAL GALAXIES
Abstract: We propose a survey of nearby galaxies with known nuclear black hole
masses. We also have or will have extensive multi-wavelength data available for
these galaxies, allowing their spectral energy distributions (SEDs) to be studied
in unprecidented detail with arcsecond or better apertures. These SEDs will
constrain accretion models, and the X-ray fluxes will be a particularly strong
diagnostic. Our sample spans a range of nuclear activity and galaxy type, making
the results of our study applicable to galaxies in general.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
10:27:18.60 +28:30:25.00 NGC 3245 ACIS-S NONE 10.00
12:28:59.70 +13:58:44.00 NGC 4459 ACIS-S NONE 10.00
12:39:56.00 +10:10:35.10 NGC 4596 ACIS-S NONE 10.00
14:59:24.70 -16:41:36.00 NGC 5793 ACIS-S NONE 10.00
15:34:35.10 +15:12:01.00 NGC 5954 ACIS-S NONE 10.00
21:18:33.00 +26:26:48.00 NGC7052 ACIS-S NONE 10.00
===================================================================================
Proposal Number: 03600504
Proposal Title: RESOLVING THE ORIGIN OF X-RAY EMISSION IN A COMPLETE SAMPLE OF
LOCAL STARBURST-DRIVEN SUPERWINDS
PI: DAVID STRICKLAND
Subject Category: NORMAL GALAXIES
Abstract: Indirect evidence strongly suggests that starburst-driven outflows
(superwinds) are responsible for much of the enrichment and heating of the IGM.
X-ray observations of local superwinds are vital for studying this, as they
provide the most direct probe of the violent, high energy, processes that occur
in these outflows. We propose Chandra observations of 4 edge-on starbursts to
complete a flux-limited sample of 9 superwinds. Only Chandra has the spatial
resolution necessary to distinguish between different models for origin of the
X-ray emission in superwinds, as demonstrated by the existing Chandra data on a
few starbursts. The complete sample will permit general conclusions about the
X-ray emission from superwinds, and their role in IGM heating & enrichment, to be
made.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
03:54:39.50 -20:30:07.00 NGC 1482 ACIS-S NONE 30.00
09:55:52.60 +69:40:47.10 M82 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03600627
Proposal Title: A POSSIBLE NEW DISTANCE INDICATOR USING LOW MASS X-RAY BINARIES
IN THE NEAREST EARLY-TYPE GALAXIES
PI: JIMMY IRWIN
Subject Category: NORMAL GALAXIES
Abstract: Initial work with Chandra data of early-type systems indicates that the
amount of X-ray luminosity coming from LMXBs with luminosities below 10^38 ergs/s
appears to be constant from galaxy to galaxy once it is normalized by the optical
luminosity of the galaxy. If this is a general feature of galaxies it can be used
as a distance indicator to galaxies. A statistical analysis shows that this
method might be accurate to as little as 5%. We propose to observe four very
nearby early-type galaxies with accurately known distances with ACIS-S to confirm
that this method of distance determination is valid and can be used on more
distant galaxies. We will also detect any hot gas in these systems, and measure
its luminosity, temperature and metallicity.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
10:47:41.80 +13:58:60.00 NGC3377 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03600631
Proposal Title: UNVEILING THE NATURE OF ULTRA LUMINOUS X-RAY SOURCES IN NEARBY
SPIRAL GALAXIES - REALLY ~100 SOLAR MASS BLACK HOLES ? -
PI: MASAHIKO SUGIHO
Subject Category: NORMAL GALAXIES
Abstract: We propose 4 pointing observations (total 10 ksec) by Chandra HRC-I of
6 ultra luminous compact X-ray sources (ULXs) in the arm region of the nearby
spiral galaxies to determine their positions, for the purpose of optical
identification of ULXs and their dynamical mass measurement, which will unveil
the nature of ULXs as ~100 solar mass black holes.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
03:18:21.10 -66:32:35.00 NGC1313 SA AND SB HRC-I NONE 2.00
03:46:05.90 +68:08:06.00 IC342 S1 AND S2 HRC-I NONE 3.00
07:36:26.50 +65:35:37.00 NGC2403 S3 HRC-I NONE 3.00
09:55:33.05 +69:00:34.90 M81 X-6 HRC-I NONE 2.00
===================================================================================
Proposal Number: 03600684
Proposal Title: CHANDRA OBSERVATIONS OF THE X-RAY LUMINOUS STARBURST GALAXY
NGC3310
PI: ANDREAS ZEZAS
Subject Category: NORMAL GALAXIES
Abstract: We propose a 50Ks ACIS-S observation of NGC 3310, the most nearby X-ray
luminous starburst galaxy. Its X-ray luminosity places it (with the Antennae,
Arp299 and NGC3256) at the upper end of the luminosity function of nearby
star-forming galaxies. With Chandra we will determine if the same mechanisms are
responsible for the X-ray emission in both low and high X-ray luminosity
starbursts. We will study the nature of the resolved sources and determine the
relative contribution of the diffuse and point source components. By extending
the range of starburst galaxies observed by Chandra to higher X-ray luminosities
it will be possible to perform statistical studies of their properties, which
will help the understanding of high redshift starbursts which cannot be observed
in comparable detail
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
10:38:45.90 +53:30:12.00 NGC 3310 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03600687
Proposal Title: DIFFUSE X-RAY EMISSION IN EDGE-ON DISK GALAXIES: NGC 5775 AND
NGC 3044
PI: PHILIP MALONEY
Subject Category: NORMAL GALAXIES
Abstract: We propose 65 ksec ACIS-S observations of the edge-on disk galaxies NGC
5775 and NGC 3044, both of which show bright, extraplanar ionized gas in H alpha
and have extensive radio continuum halos. The primary goal is to image the
diffuse soft X-ray emission expected (and already observed with ROSAT in the case
of NGC 5775) to result from injection of energy and momentum into the halo by
stellar winds and supernovae. The physical parameters (e.g. luminosity, mass,
scaleheight, density and temperature) of X-ray emitting gas will be derived. The
X-ray data will be compared with existing optical and radio data to constrain the
physics of disk-halo interactions in these galaxies.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
14:53:57.50 +03:32:42.00 NGC 5775 ACIS-S NONE 65.00
===================================================================================
Proposal Number: 03600843
Proposal Title: CLUSTER-GALAXY INTERACTIONS IN THE COMA CLUSTER
PI: MICHAEL GREGG
Subject Category: NORMAL GALAXIES
Abstract: The vigorously star forming galaxy NGC 4911 provides a spectacular
example of a luminous spiral on its first passage through the hot intracluster
medium of the Coma cluster. ACIS-I imaging of NGC 4911 and its environs will
complement HST Cycle 8 WFPC2 imaging and reveal the role of the X-ray gas in
driving star formation and generating tidal debris. To further explore this
connection, we request 4 orbits of HST/WFPC2 H-alpha imaging. The ACIS-I image
will also contain the giant spiral NGC 4921, another X-ray source interacting
with the intracluster medium. In addition, the ACIS-I image will provide a deep,
high resolution look at the Coma intracluster medium over a wide range of X-ray
surface brightness.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
13:00:56.10 +27:47:26.00 NGC 4911 ACIS-I NONE 65.00
===================================================================================
Proposal Number: 03600865
Proposal Title: NGC1404: INTERACTION WITH FORNAX GAS, COOLING FLOWS, AND THE
METALLICITY PROBLEM
PI: JIMMY IRWIN
Subject Category: NORMAL GALAXIES
Abstract: We propose a 30 ksec ACIS-S observation of NGC1404. Its small projected
distance from the center of Fornax makes it a prime candidate for studying the
interaction of galactic X-ray gas with cluster gas. We will search for a bow
shock-like structure on the side of NGC~1404 facing Fornax and also derive
temperature information on an elongated tail on the opposite side of the galaxy.
We will compare the cooling rate of the central gas with limits set by FUSE and
search for evidence of a rotating cooling flow. We will investigate why the X-ray
temperature is much greater than the stellar velocity dispersion temperature, as
well as derive detailed temperature and metallicity maps. Finally, we will
determine if the metallicity of the gas is truly as low as previous studies have
indicated.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
03:38:52.00 -35:35:34.00 NGC1404 ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03600940
Proposal Title: MONITORING THE EXTREME X-RAY FLARING OF SAGITTARIUS A* AND A
DEEP SURVEY OF THE CENTRAL 40 PC OF THE GALAXY
PI: FREDERICK BAGANOFF
Subject Category: NORMAL GALAXIES
Abstract: In Cycle 1, we discovered the first clear evidence of X-ray emission
from Sgr A*, the compact radio source associated with the massive black hole
(MBH) at the dynamical center of the Milky Way. In Cycle 2, we made the first
detection of rapid, large-amplitude X-ray variability of Sgr A*. To gather
unprecedented information about the immediate environment of an MBH, we propose a
510-ks ACIS-I observation of Sgr A* to measure the quiescent-state emission
spectrum and to characterize the timescales, duty cycle, energetics, and spectral
evolution of the flares. Simultaneous monitoring with OVRO and VLBA are being
proposed to search for correlated variations and lags predicted by theory to
characterize the flaring state emission process. We will also obtain a deep
survey in this rich field.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:45:40.00 -29:00:28.00 SGR A* ACIS-I NONE 38.50
17:45:40.00 -29:00:28.00 SGR A* ACIS-I NONE 40.00
17:45:40.00 -29:00:28.00 SGR A* ACIS-I NONE 100.00
17:45:40.00 -29:00:28.00 SGR A* ACIS-I NONE 170.00
17:45:40.00 -29:00:28.00 SGR A* ACIS-I NONE 170.00
===================================================================================
Proposal Number: 03600966
Proposal Title: A CHANDRA SURVEY OF THE SMC
PI: ANDREAS ZEZAS
Subject Category: NORMAL GALAXIES
Abstract: We propose to perform a survey of a large portion of the Small
Magellanic Cloud with ACIS-I. These observations will allow us to determine the
X-ray stellar populations down to low luminosity limits (LX = 1E34 erg/s), 10
times deeper than ROSAT.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:49:26.60 -72:44:38.00 SMC FIELD 7 ACIS-I NONE 9.00
00:49:27.10 -73:16:47.00 SMC FIELD 4 ACIS-I NONE 12.00
00:53:03.40 -72:42:34.50 SMC FIELD 6 ACIS-I NONE 10.00
00:53:09.50 -72:26:44.00 SMC FIELD 5 ACIS-I NONE 8.00
00:56:45.20 -72:18:27.00 SMC FIELD 3 ACIS-I NONE 10.00
===================================================================================
Proposal Number: 03600574
Proposal Title: MULTI-COMPONENT X-RAY EMISSION IN THE S0 GALAXY NGC 5102
PI: RALPH KRAFT
Subject Category: NORMAL GALAXIES
Abstract: We propose to observe the nearby (3.1 Mpc) S0 galaxy NGC 5102 with the
ACIS-S for 35 ks to resolve the diffuse emission from the point source
population. For many early galaxies, particularly X-ray underluminous galaxies
(class 1 galaxies by the definition of Irwin and Sarazin 1998) such as NGC 5102,
a significant fraction of their X-ray luminosity comes from an LMXB population.
NGC 5102 is considerably less massive and less X-ray luminous than early galaxies
previously observed with Chandra, but its proximity permits detailed observation.
We will determine the relationship between the diffuse and point like components,
measure the temperature and density of the diffuse component, and investigate the
nature of the soft X-ray excess seen in this and other X-ray underluminous
galaxies.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
13:21:57.00 -36:37:49.00 NGC 5102 ACIS-S NONE 35.00
===================================================================================
Proposal Number: 03601013
Proposal Title: AN X-RAY STUDY OF NGC 1313
PI: STEPHEN MURRAY
Subject Category: NORMAL GALAXIES
Abstract: NGC 1313 is a prime target for Chandra for several reasons. Previous
observations have discovered 8 galactic X-ray sources, 5 of them with
luminosities between 6x10^{37} and 6x10^{38. One of these is the supernova
remnant SN 1978K. NGC 1313 is an interacting galaxy with evidence of widespread
star formation. Our ACIS-S observations are designed to study several of these
special features, but will focus on the galactic center, which has so far not
been detected in X-rays. Our observations will either discover a central X-ray
source (or sources), or will place an upper limit approximately an order of
magnitude below the previous upper limit, which was obtained with about180 ksec
of observations with the ROSAT HRI. GTO Priority "A"
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
03:18:32.00 -66:31:10.00 NGC 1313 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03601019
Proposal Title: SIMULTANEOUS X-RAY/RADIO MONITORING OF SAGITTARIUS A*
PI: GORDON GARMIRE
Subject Category: NORMAL GALAXIES
Abstract: In Cycle 1, we discovered the first clear evidence of X-ray emission
from Sagittarius A* (Sgr A*), the compact nonthermal radio source associated with
the massive black hole at the dynamical center of the Milky Way. In Cycle 2, we
reported the first detection of large-amplitude X-ray variability of Sgr A*. We
propose 4x12.5-ks (50-ks total) GTO observations with ACIS-I spanning a reported
106-day radio cycle. Simultaneous monitoring with the VLA, OVRO, SMA, and VLBA
will be proposed: 1) to search for correlated variations and lags between the
wavebands and 2) to produce the first simultaneous broad-band spectra of Sgr A*
at multiple epochs in order to constrain the emission processes and the sizes and
structures of the emitting regions.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:45:40.00 -29:00:28.00 SGR A* ACIS-I NONE 12.50
17:45:40.00 -29:00:28.00 SGR A* ACIS-I NONE 12.50
17:45:40.00 -29:00:28.00 SGR A* ACIS-I NONE 12.50
17:45:40.00 -29:00:28.00 SGR A* ACIS-I NONE 12.50
===================================================================================
Proposal Number: 03600380
Proposal Title: THE HALPHA - X-RAY CONNECTION IN DWARF STARBURST GALAXIES.
PI: IAN STEVENS
Subject Category: NORMAL GALAXIES
Abstract: We propose to observe 6 dwarf starburst galaxies showing Halpha
evidence of nuclear outflows. Chandra observations of these galaxies, utilizing
the excellent spatial and spectral resolution, will allow us to measure X-ray
temperatures and map the sources of X-ray emission, and so determine the
kinematics and morphologies of the outflows. We will also be able to distinguish
between regions of diffuse emission and point-source emission (probably X-ray
binaries). These observations will lead to a better understanding of the
evolution of starbursts in dwarf galaxies and their effects on both the host
galaxies and their surroundings. This sample of 6 galaxies will also allow us to
better determine the X-ray luminosity function of these galaxies and their X-ray
binary populations.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:53:57.00 -23:09:50.00 NGC 3955 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03608117
Proposal Title: SEARCHING FOR THE X-RAY SIGNATURE TO CURRENT RADIO ACTIVITY IN
M31*
PI: FRANCIS PRIMINI
Subject Category: NORMAL GALAXIES
Abstract: M31*, the radio source identified with the super-massive black hole in
M31, has recently brightened significantly, from ~50+/-9 microJy on July 5 to
~90+/-9 microJy on July 29 (5 GHz, VLA). This is the first significant evidence
for radio variability. We request a 5 ksec ACIS-I observation to determine how
this variability is reflected in x-rays. The typical luminosity of the x-ray
counterpart, in several Chandra observations, is ~4e36 ergs/sec (0.5-7 keV) but
it has occasionally brightened by a factor of 2-4. However, there are no
contemporary radio observations and thus the x-ray/radio correlation is unknown.
A Chandra observation of unusual activity in the x-ray counterpart NOW would: 1)
strengthen the x-ray identification with M31*, which is now based only on
position; 2) constrain source emission models, some of which predict
anti-correlated radio and x-ray variability.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:42:44.40 +41:16:08.90 M31 ACIS-I NONE 5.00
***********************************************************************************
ACTIVE GALAXIES AND QUASARS
--------------------------------------------------
===================================================================================
Proposal Number: 03700010
Proposal Title: SIMULTANEOUS HST, CHANDRA AND FUSE OBSERVATIONS OF INTRINSIC
ABSORBERS IN AGN
PI: GERARD KRISS
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: Photoionized, warm absorbing gas is an important component of the
nuclear structure of AGN. Approximately half of all low-z AGN show
high-ionization UV absorption lines and X-ray warm absorbers, but the
relationship of the UV-absorbing gas to the even higher ionization X-ray
absorbing material is not yet understood. Only a handful of
high-spectral-resolution observations with HST, Chandra or FUSE currently exist
(NGC4151, NGC3516, NGC3783, NGC5548, Mrk 509). These show a diversity of
kinematic structure and ionization states in the absorbers. We propose to
increase significantly the sample of low-redshift AGN studied at high spectral
resolution in the UV and the X-ray by obtaining simultaneous HST, Chandra, and
FUSE spectra of NGC7469.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
23:03:15.70 +08:52:26.60 NGC7469 ACIS-S HETG 80.00
===================================================================================
Proposal Number: 03700011
Proposal Title: EXPLORATORY OBSERVATIONS OF A NEW BRIGHT QUASAR
PI: KAREN LEIGHLY
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: The VLA FIRST radio survey recently discovered a new, extremely bright
quasar that is the second brightest optical object in the sky at z>0.1. Optically
classified as a Narrow-line Seyfert 1 galaxy (NLS1), PHL 1811 is not typical of
this class of objects because it is a very weak X-ray source. We propose short
exploratory UV spectroscopic observations of this new bright quasar that will
reveal its true nature and permit us to identify potential applications of future
deeper observations. PHL~1811 may be the brightest luminous NLS1, in which case
the study of the profiles and ratios of the emission lines will be valuable.
Alternatively, PHL 1811 may be the brightest BALQSO, and the structure and
composition of the BAL flow may be studied. (abridged)
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
21:55:01.50 -09:22:24.70 PHL 1811 ACIS-S NONE 10.00
21:55:01.50 -09:22:24.70 PHL 1811 ACIS-S NONE 10.00
===================================================================================
Proposal Number: 03700015
Proposal Title: THE PHYSICS OF X-RAY/OPTICAL JETS
PI: MEG URRY
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: (truncated) An important new probe of the physics of large-scale radio
jets is possible with the discovery of resolved X-ray/optical jets. To probe jet
energetics and physics generally, and to test the ``Compton/CMB'' interpretation
specifically, we propose deep HST imaging of three X-ray/optical jets
(PKS~1127--145, PKS~0637--752, 3C~371) and one optical jet (PKS~2201+044), plus
Chandra observations of the latter two. The multiwavelength spectra of individual
knots differ significantly, as does one jet from another, indicating the need for
detailed high-resolution study of more than 1 or 2 jets. Along with the
well-observed 3C~273 and M~87 jets, the 4 proposed targets are the only known (or
likely) nonthermal X-ray jets readily detected with Chandra and HST.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:06:50.60 +69:49:28.10 3C371.0 ACIS-S NONE 40.00
22:04:17.70 +04:40:02.30 PKS2201+044 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03700016
Proposal Title: A SNAPSHOT SURVEY OF THE OPTICALLY SELECTED TYPE-2 QUASARS
PI: S. DJORGOVSKI
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We identified a population of emission-line objects in DPOSS, which can
be plausibly interpreted as the long-sought type-2 quasars. They have
high-ionization Seyfert-2 like spectra, but with narrow-line luminosities
comparable to those of the luminous type-1 quasars in the same redshift range.
Keck spectropolarimetry confirms the presence of hidden QSO nuclei in them. This
provides a major piece of evidence in favor of the unified schemes for AGN, and
it should help extend our understanding of AGN in general. This population may be
a major contributor to the cosmic hard x-ray background. It is complementary to
the optically dull hard x-ray sources found by $Chandra$.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
09:02:46.70 +16:40:01.00 PSS 0902+1640 ACIS-S NONE 5.00
11:46:40.60 +30:15:09.00 PSS 1146+3015 ACIS-S NONE 5.00
13:42:42.50 +49:44:40.00 PSS 1342+4944 ACIS-S NONE 5.00
16:05:51.10 +44:05:41.00 PSS 1605+4405 ACIS-S NONE 5.00
23:11:51.30 +16:44:57.00 PSS 2311+1644 ACIS-S NONE 5.00
===================================================================================
Proposal Number: 03700027
Proposal Title: THE QUASAR MR2251-178 AND ITS WARM ABSORBER
PI: PETER PREDEHL
Subject Category: ACTIVE GALAXIES AND QUASARS
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
22:54:05.80 -17:34:55.00 MR2251-178 HRC-S LETG 80.00
===================================================================================
Proposal Number: 03700032
Proposal Title: J2310-437, AN X-RAY BRIGHT, RADIO-LOUD,OPTICALLY DULL GALAXY
PI: STEPHEN MURRAY
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose Chandra observations for J2310-437, an x-ray bright,
radio-loud, optically dull galaxy. ACTA maps of J2310-437 show substantial
structure (jets and knots) on the few arcsec scale - extremely well-matched to
Chandra's angular resolution. This optically dull galaxy (little or no nuclear
optical continuum and weak or absent emission lines) differs significantly from
other classes of AGNs. The proposed Chandra observations will map structures and
determine the spectral properties of the core and brighter extended features,
with the goal of understanding the physical processes at work. GTO Priority "A"
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
23:10:41.80 -43:47:34.30 J2310-437 ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03700033
Proposal Title: A CHANDRA OBSERVATION OF THE UNUSUAL RADIO GALAXY 3C 403
PI: STEPHEN MURRAY
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: VLA observations (8 GHz) of the nearby (z=0.089) FR II radio galaxy 3C
403 show a very unusual twisted X structure in the diffuse radio emission. In
addition, the hotspots that make up two legs of the X are not collinear with the
nucleus. One possible explanation for the unusual radio morphology of 3C 403
could be a significant asymmetry in the hot ISM of the host galaxy. We will test
this hypothesis by mapping the spatial morphology of the X-ray emitting plasma to
understand the relationship between the radio plasmas and the ISM. Lack of
detection of such an asymmetry could imply that the source axis has changed in
the recent past, and the unusual shape is a result of backflow of jet material
into an old cocoon. GTO Priority "A"
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:52:16.00 +02:30:28.00 3C403 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03700042
Proposal Title: PROBING THE INTERGALACTIC MEDIUM AT LOW REDSHIFT
PI: CLAUDE CANIZARES
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: Cosmological hydrodynamic simulations predict that a substantial
fraction of the baryonic material at low redshift should be in the form of a
warm/hot (log T = 5-7) intergalactic medium (WHIM). We propose to observe three
X-ray bright quasars (3C 279, 1H 0414+009, 1ES 1028+511) with the Chandra HETGS
to search for the absorption produced by this WHIM gas and determine whether it
can account for the apparent baryon deficit in the present-day universe. Our
simulations show that we should be able to detect several resonant absorption
lines from highly-ionized metals (such as O VII and O VIII) in the WHIM gas.
These data will also be useful for studying absorption and/or emission lines
intrinsic to the quasars.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
04:16:52.40 +01:05:24.00 1H 0414+009 ACIS-S HETG 41.00
04:16:52.40 +01:05:24.00 1H 0414+009 ACIS-S HETG 52.00
10:31:18.40 +50:53:36.00 1ES 1028+511 ACIS-S HETG 25.00
10:31:18.40 +50:53:36.00 1ES 1028+511 ACIS-S HETG 75.00
12:56:11.10 -05:47:22.00 3C 279 ACIS-S HETG 107.00
===================================================================================
Proposal Number: 03700051
Proposal Title: A COMPLETE X-RAY SAMPLE OF BROAD ABSORPTION LINE QSOS
PI: GORDON GARMIRE
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: The main goals of this proposal are: (i)obtain a complete X-ray sample
of BALQSO's (ii) provide by far the best characterization of the relationship
between UV and X-ray properties of BALQSO's currently available. (iii) identify
the X-ray bright ones; these observations will identify the X-ray bright BALQSOs
so that they can be studied in subsequent, spectroscopic observations.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:37:36.40 +14:36:40.00 LBQS 1235+1453 ACIS-S NONE 7.00
12:43:03.60 +15:50:47.00 LBQS 1240+1607 ACIS-S NONE 7.00
12:45:51.40 +01:05:04.00 LBQS 1243+0121 ACIS-S NONE 7.00
13:17:14.20 +01:00:13.00 LBQS 1314+0116 ALTER ACIS-S NONE 7.00
===================================================================================
Proposal Number: 03700052
Proposal Title: FOLLOW-UPS TO THE LLAGN SURVEY
PI: GORDON GARMIRE
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: The main goal of this proposal is to: Study the nature of the weak
Seyfert 1.9 active nucleus of NGC 4565
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:50:26.60 +25:30:06.00 NGC 4725 ALTERNATE ACIS-S NONE 25.00
===================================================================================
Proposal Number: 03700062
Proposal Title: PROBING WARM ABSORPTION IN THE RADIO QUIET QSO MR2251-17.8
PI: CLAUDE CANIZARES
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose a 150ks observation of the QSO MR2251-17.8 in order to probe
the warm absorption and extended line region reported in this object. High
resolution Chandra data will allow us to determine the nature and physical
properties of the circum source material and compare them to those seen in lower
luminosity AGN. Variable column densities which can be a few orders of magnitude
greater than the Galactic column strongly suggests that partially ionized
material is intrinsic to the source. We intend to propose for simultaneous HST
time if the Chandra observation is approved in order to further investigate the
optical/UV spectrum and in particular the C IV feature that has been reported.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
22:54:05.90 -17:34:54.30 MRC 2251-178 ACIS-S HETG 150.00
===================================================================================
Proposal Number: 03700075
Proposal Title: FOLLOW-UP OBSERVATIONS OF THE RADIO GALAXY CEN-A
PI: STEPHEN MURRAY
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to observe Cen-A with the ACIS-S to continue our monitoring
program of galactic x-ray binaries. We will posiiotn the observation to place the
inner jet at the best focus and we will obtain spectral data on the extended SW
lobe. GTO Priority "A"
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
13:25:28.69 -43:00:59.70 CEN-A ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03700092
Proposal Title: FOLLOW-UP TO CHANDRA GL SURVEY OF GRAVITATIONAL LENSES
PI: GORDON GARMIRE
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: The main goals of this proposal are: (i) Measure short time delays to
accuracies of a few percent in GL systems with small image separations. (ii)
Determine the nature of the X-ray absorption associated with BAL systems.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
08:31:41.60 +52:45:16.80 APM08279+5255 ACIS-S NONE 90.00
===================================================================================
Proposal Number: 03700094
Proposal Title: COLLIDING GALAXIES
PI: GORDON GARMIRE
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: The main goal of these observations is to explore the production of
black holes in the colliding material. A number of interacting galaxies have
shown point sources of emission that exceed the Eddington limited luminosity by
an order of magnitude. These observations will extend this work to other
colliding galaxies.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
22:20:44.77 -24:40:41.83 NGC 7252 ALTERNATE ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03700112
Proposal Title: STUDY OF THE Z=3.572 QUASAR PKS 2215+020
PI: LEON VANSPEYBROECK
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: Lobanov et al. (2001 Ap J, 547, 714) have presented a VSOP study of
this quasar; the proposed observation will determine the possible existence of
related X-ray properties.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
22:17:48.20 +02:20:11.00 PKS 2215+020 ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03700166
Proposal Title: HOT GAS, STAR FORMATION, AND NUCLEAR ACTIVITY IN THE PECULIAR
LOW LUMINOSITY RADIO GALAXY NGC 4410A
PI: BEVERLY SMITH
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to use the Chandra ACIS-S instrument to obtain high
resolution X-ray maps of the nearby radio galaxy NGC 4410A. NGC 4410A has a very
distorted radio structure, a ring of extremely luminous HII regions, stellar
tidal tails and bridges, and abundant interstellar matter. ROSAT X-ray maps of
this system suggest three X-ray components: a compact nuclear source, an extended
halo 10 arcsec in diameter, approximately coincident with the most luminous of
the HII regions, and a faint extended X-ray `tail' 2 arcmin long aligned with a
stellar bridge. We propose to use Chandra to resolve these components spatially
and spectrally, to distinguish X-ray emission from shocks, intracluster gas,
nuclear jets, and stellar winds.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:26:28.20 +09:01:10.80 NGC 4410A ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03700205
Proposal Title: HIGH RESOLUTION SPECTROSCOPY OF AGN IN OUTBURST:THE GASEOUS
NUCLEAR ENVIRONMENT AND THE WIGM
PI: FABRIZIO NICASTRO
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to observe up to 3 AGNs in exceptionally high states for 100
ks each with the Chandra ACIS-LETG, to study efficiently both their gaseous
nuclear environment as well as possible intervening high ionization metal
absorption systems. The observations will be triggered by the Rossi-XTE ASM and
will require rapid response times. This observing strategy will guarantee
exceptionally high quality spectra containing at least one milion counts in the
first orders of the LETGS. Given the unique high quality scientific rewards of
this program, we propose that the data from this program be made immediately
public to ensure their widest utilization.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:25:46.70 +12:39:44.00 SY1 IN OUTBURST ACIS-S LETG 100.00
===================================================================================
Proposal Number: 03700230
Proposal Title: UNVEILING THE POWERFUL QUASAR HIDDEN IN THE NUCLEUS OF THE FRII
RADIO GALAXY 3C 265
PI: MARCO BONDI
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: Optical and near IR observations of the radio galaxy 3C 265 suggest the
presence of a powerful quasar hidden in its nucleus. In order to test this
possibility we propose a Chandra observation of this target. Our aim is to unveil
the absorbed nucleus obtaining the intrinsic X-ray luminosity and spectrum and,
at the same time, to study the effect of the nuclear photons on the relativistic
electrons in the radio lobes. These electrons are directly illuminated by the
nuclear photons and can efficiently up-scatter them into the X-ray band via
inverse Compton. The proposed Chandra observation will also allow to constrain
the energy spectrum of these scattering electrons.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:45:29.00 +31:33:49.00 3C 265 ACIS-S NONE 60.00
===================================================================================
Proposal Number: 03700232
Proposal Title: THE PATTERN OF HEAVY ELEMENT ABUNDANCES IN A HIGH REDSHIFT
GALAXY
PI: JILL BECHTOLD
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to measure the X-ray absorbing column associated with the
intervening z=2.04 absorption line system of PKS 0458-020. We estimate that an
accurate measurement can be made if the O/H is 1/8 solar or greater. Oxygen and
the alpha-process elements are the main contributors to the X-ray cross-section;
this will be the first measurement of their abundance in any high redshift
galaxy. We will see directly whether the absorber shares the same nucleosynthetic
history as the Pop II metal-poor halo stars and globular clusters of the Milky
Way, or whether it has an abundance pattern like current-day disk stars and gas.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:01:12.80 -01:59:15.00 PKS 0458-020 ACIS-S NONE 77.00
===================================================================================
Proposal Number: 03700239
Proposal Title: CHANDRA OBSERVATIONS OF A POPULATION OF TYPE 2 QUASARS
DISCOVERED IN THE DPOSS
PI: S. DJORGOVSKI
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We have identified a population of emission-line objects in DPOSS,
which can be plausibly interpreted as the long-sought type-2 quasars. This
provides a major piece of evidence in favor of th eunified schemes for AGN, and
it should help extend our understanding of AGN in general. This population may be
a major contributor to the cosmic x-ray background. X-ray observations are a key
in confirming the nature of these objects through measurements of the intrinsic
cuclear luminosity as well as the absorbing column. We propose CXO observations
on a sample of ten of these, to complement our extensive Keck/Palomar/HST/VLA
followup program.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:08:47.90 +19:23:16.00 PSS 0008+1923 ACIS-S NONE 15.00
00:16:10.10 +32:09:08.00 PSS 0016+3209 ACIS-S NONE 15.00
03:11:22.40 +04:07:14.00 PSS 0311+0407 ACIS-S NONE 15.00
09:46:44.30 +66:11:30.00 PSS 0946+6611 ACIS-S NONE 15.00
09:58:44.50 +07:40:27.00 PSS 0958+0740 ACIS-S NONE 15.00
13:38:52.10 +22:18:36.00 PSS 1338+2218 ACIS-S NONE 15.00
15:07:14.40 +56:03:44.00 PSS 1507+5603 ACIS-S NONE 15.00
15:39:45.20 +43:12:02.00 PSS 1539+4312 ACIS-S NONE 15.00
22:22:39.10 +23:07:56.00 PSS 2222+2307 ACIS-S NONE 15.00
22:37:48.60 +18:37:43.00 PSS 2237+1837 ACIS-S NONE 15.00
===================================================================================
Proposal Number: 03700241
Proposal Title: CHANDRA SNAPSHOT OBSERVATIONS OF SOFT X-RAY TRANSIENT AGN
PI: RICK EDELSON
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose short Chandra observations of 4 known soft X-ray transient
AGN and 4 candidate transient objects. These new measurements will provide tight
constraints on the X-ray luminosity of these sources and, when combined with
previous ROSAT measurements, will give ``corrected'' light curves spanning ten
years, providing a key test of Rees' t^-5/3 decay model for stellar disruption
events in galactic nuclei. If alternatively the transient behavior is due the
episodic nature of an otherwise normal AGN, then it is plausible that the spatial
distribution of extended X-ray emission in the nucleus could provide evidence of
earlier activity cycles. Finally, if the candidate transient sources show the
predicted factor of ~100 fading this will double the number of known transients.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:39:15.80 -51:17:03.00 WPVS 007 ACIS-S NONE 10.00
12:36:51.00 +45:39:03.00 MCG+08-23-067 ACIS-S NONE 2.00
12:36:51.00 +45:39:03.00 MCG+08-23-067 ACIS-S NONE 10.00
12:37:41.20 +26:42:29.00 IC 3599 ACIS-S NONE 10.00
12:42:10.60 +33:17:03.00 WAS 61 ACIS-S NONE 2.00
12:42:10.60 +33:17:03.00 WAS 61 ACIS-S NONE 10.00
12:58:51.40 +23:55:32.00 RX J1258+23 ACIS-S NONE 2.00
12:58:51.40 +23:55:32.00 RX J1258+23 ACIS-S NONE 10.00
13:54:19.90 +32:55:47.00 MRK 663 ACIS-S NONE 2.00
13:54:19.90 +32:55:47.00 MRK 663 ACIS-S NONE 10.00
15:15:23.40 +55:30:57.00 NGC 5905 ACIS-S NONE 10.00
16:24:56.50 +75:54:56.00 RX J1624+75 ACIS-S NONE 10.00
===================================================================================
Proposal Number: 03700246
Proposal Title: NGC4698: A SEYFERT-2 GALAXY WITH NO OBSCURING COLUMN
PI: IOANNIS GEORGANTOPOULOS
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to observe NGC4698 one of the brightest Seyfert-2s in the
spectroscopic sample of galaxies. NGC4698, despite its unambiguous optical
classification, presents no obscuring column in the ASCA X-ray spectra. The
possibility that this is a Compton thick object is ruled out by both the absence
of a strong FeK line and the large value of the fx/f[OIII] ratio. A few Seyfert-2
galaxies with similar properties have been discovered and they may represent the
prototypes of a new class of Seyfert-2s which challenges the standard AGN
unification schemes. Chandra spatially resolved spectroscopy and timing analysis
will help constraining the nature of the X-ray emission in this object.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:48:22.30 +08:29:20.00 NGC4698 ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03700247
Proposal Title: INVERSE COMPTON SCATTERING IN POWERFUL RADIO GALAXIES:
CONSTRAINING THE ELECTRON SPECTRUM
PI: GIANFRANCO BRUNETTI
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to exploit the high spatial resolution and sensitivity of
Chandra to observe 3 powerful radio galaxies with the aim to study the extended
inverse Compton (IC) emission from the radio lobes. In the framework of the
unified scheme linking powerful radio galaxies and quasars, the IC scattering of
nuclear radiation from relativistic electrons with Lorentz factor of about
100-300 results in soft X-ray emission coincident with radio lobes (Brunetti et
al., 1997). Furthermore, due to the scattering configuration, the IC X-ray
brightness is expected to be much higher in the radio lobe associated with the
counter-jet. The study of the resulting X-ray spectrum and luminosity allows to
measure the low energy electron spectrum and to constrain the energetics of radio
lobes.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:16:31.60 +79:16:52.00 3C 6.1 ACIS-S NONE 20.00
00:16:31.60 +79:16:52.00 3C 6.1 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03700252
Proposal Title: THE HIGH RESOLUTION VIEW OF THE COMPLEX WARM ABSORBER/EMITTER OF
NGC 985
PI: FABRIZIO NICASTRO
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to observe with the HETGS the Sy1 NGC 985 for 80 ks. This is
the brightest (F[2-10] = 2e-11 cgs) Sy1 known to host a warm absorber, not yet
observed with the Chandra gratings. BeppoSAX data of NGC 985 clearly demonstrate
that, the X-ray ionized absorber in this object is complex. NGC 985 is also one
of the biggest known ring-galaxies, interacting with another fainter galaxy,
whose nucleus is only 3'' away from the Seyfert nucleus. With the proposed
observation we will be able to detect X-ray sources associated with starburst
activity in the ring, and to resolve thermal X-ray emission. Finally, if hot gas
in the ring absorbs the Seyfert continuum along our line of sight, we will derive
important astrophysical properties of the ISM in the host galaxy.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
02:34:37.80 -08:47:15.00 NGC 985 ACIS-S HETG 80.00
===================================================================================
Proposal Number: 03700294
Proposal Title: AN ABSORPTION STUDY OF PG 2112+059: THE X-RAY BRIGHTEST BAL QSO
KNOWN
PI: SARAH GALLAGHER
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: Broad Absorption Line (BAL) QSOs allow us to observe substantial gas
outflows that are probably present in most QSOs, but the nature of their X-ray
absorption remains poorly understood. In an ASCA/BeppoSAX survey of BAL QSOs, we
have recently discovered that PG 2112+059 is the X-ray brightest BAL QSO known
and shows X-ray absorption suggestive of ionized gas. Furthermore, X-ray spectral
variability is apparent by comparison of ASCA and ROSAT data. We propose a 60 ks
ACIS-S observation of PG 2112+059 that will provide the best constraints yet on
the column density, ionization state, covering fraction, and outflow velocity of
the X-ray gas in a BAL QSO. We will also obtain a simultaneous HST STIS spectrum
to test UV/X-ray absorber models and monitor UV line variability.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
21:14:52.60 +06:07:42.50 PG 2112+059 ACIS-S NONE 60.00
===================================================================================
Proposal Number: 03700317
Proposal Title: DIFFUSE X-RAY EMISSION, SUPERWINDS, AND STELLAR X-RAY SOURCES IN
THE STARBURST GALAXIES NGC 2146 AND NGC 1808
PI: PHILIP MALONEY
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose 44 ksec observations of the starburst galaxies NGC 2146 and
NGC 1808, both of which show evidence for large-scale superwinds driven by the
active star formation. This will allow us to map the spatial structure of the
winds on approximately arcsecond scales, to distinguish the contributions of
stellar (accreting neutron star and black hole) sources from the thermal emission
of the winds, and to perform spatially-resolved spectroscopy on roughly 11''
scales (NGC 2146) and 3'' scales (NGC 1808). The physical parameters in the winds
(pressure, density, etc.) will be derived and compared with superwind theory.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:07:42.30 -37:30:46.00 NGC 1808 ACIS-S NONE 44.00
===================================================================================
Proposal Number: 03700333
Proposal Title: ORIENTATION VS. EVOLUTION FROM A UNIQUE BALQSO
PI: PAUL GREEN
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose deep ACIS-S imaging spectroscopy of the brightest Broad
Absorption Line (BAL) QSO from our Chandra AO1 snapshot survey. BALs are caused
by highly ionized outflows from the quasar nucleus with velocities commonly
reaching 0.1c. The ionization of their X-ray warm absorbers has never been
constrained, but directly affects best estimates of their possibly huge kinetic
luminosities. BALQSOs may exist in every quasar when seen at the proper
orientation, or they may represent an early or high L/LEdd phase of quasar
evolution. High S/N hard X-ray spectra have proven difficult to obtain from bona
fide BALQSOs, but UM425 provides the best opportunity yet to test the competing
models and provide crucial insight into conditions near the nucleus.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:23:20.60 +01:37:47.20 UM425 ACIS-S NONE 120.00
===================================================================================
Proposal Number: 03700369
Proposal Title: SUPERWIND EVOLUTION: THE YOUNG STARBURST-DRIVEN WIND GALAXY NGC
2782
PI: IAN STEVENS
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: NGC2782 is a starburst galaxy of particular note because of the stage
of development of its superwind. NGC2782 shows clear evidence of a bipolar
outflow, and its superwind is believed to be on the verge of breaking out into
free-flow into the IGM. The southern lobe of the outflow appears to be still
contained within a Halpha bubble, while the northern lobe has probably just
ruptured. Consequently, this object is intermediate between mature superwinds
(such as M82) and nascent superwinds still contained within the galaxy, and X-ray
observations of this system will yield insights into the development of
superwinds. Consequently, we propose to observe the superwind galaxy NGC2782 with
the ACIS-S instrument on Chandra for 30ksec.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
09:14:05.10 +40:06:49.00 NGC 2782 ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03700392
Proposal Title: DECONVOLUTION OF THE RELATIVISTIC FE-K LINES IN ACTIVE GALAXIES
AND PHYSICS FROM THE NARROW EMISSION COMPONENT
PI: TAHIR YAQOOB
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: Chandra has enabled the unambiguous deconvolving of narrow Fe-K
emission lines in a number of broad-line AGN. Measuring the narrow-line (NL)
parameters, (even a non-detection) is important to better understanding and model
XMM and existing ASCA data on the relativistically broadened Fe-K lines. The NL
is itself a tracer of the temperature, location and velocity field of
circumnuclear matter. Without knowledge of the NL, constraints derived from the
relativistic Fe lines will always be uncertain. We propose to continue a
systematic program to deconvolve the NL to understand the different physics
operating in broad Fe-K line AGN. Only Chandra can do this until 2005. We will
also propose simultaneous XMM observations to measure the broad Fe-K line
component.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
04:33:11.10 +05:21:15.10 3C 120 ACIS-S HETG 60.00
22:35:46.10 -26:03:02.20 NGC 7314 ACIS-S HETG 30.00
22:35:46.10 -26:03:02.20 NGC 7314 ACIS-S HETG 70.00
===================================================================================
Proposal Number: 03700397
Proposal Title: A SYSTEMATIC X-RAY SURVEY OF SUBMILLIMETRE-LUMINOUS QUASARS
PI: ROBERT PRIDDEY
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to obtain X-ray fluxes for a sample of the most optically
luminous quasars at high redshift (z>4 and z=2), as part of a campaign to study
in detail the SEDs of these objects. All the targets have either bright
detections, or deep upper limits, at submm wavelengths, obtained during our
recent SCUBA quasar survey. Sensitive X-ray observations are a crucial part of
this project, because they give an insight into the central engine of the AGN
itself, and could help clarify to what extent the submm emission is powered by
dust heated by the AGN, or by a starburst in the quasar's primeval host galaxy.
The targets shall become an important reference sample for studies of quasar
SEDs, across the spectrum from X-rays to radio.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:21:27.37 -02:03:32.80 LBQS0018-0220 ACIS-S NONE 5.00
01:34:21.48 +33:07:55.90 PSS0134+3307 ACIS-S NONE 5.00
02:21:05.52 +37:20:46.20 HS0218+3707 ACIS-S NONE 5.00
02:22:31.71 +15:06:28.60 HS0219+1452 ACIS-S NONE 5.00
02:51:27.78 +34:14:42.10 HS0248+3402 ACIS-S NONE 5.00
08:08:49.42 +52:15:15.30 PSS0808+5215 ACIS-S NONE 5.00
08:13:31.30 +25:45:02.90 HS0810+2554 ACIS-S NONE 5.00
11:42:54.27 +26:54:57.80 HS1140+2711 ACIS-S NONE 5.00
12:05:23.12 -07:42:32.30 BR1202-0725 ACIS-S NONE 10.00
16:03:20.91 +07:21:04.60 BR1600+0724 ACIS-S NONE 5.00
22:38:22.50 -02:45:53.10 BRI2235-0301 ACIS-S NONE 5.00
23:22:07.17 +19:44:23.10 PSS2322+1944 ACIS-S NONE 5.00
===================================================================================
Proposal Number: 03700401
Proposal Title: A CHANDRA AND XMM-NEWTON STUDY OF THE MOST DISTANT QUASARS:
X-RAYING THE FIRST MASSIVE BLACK HOLES
PI: WILLIAM BRANDT
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to continue our systematic Chandra and XMM-Newton study of
the most distant known quasars, with our ultimate goals being to learn about the
central power sources and environments of the first quasars to form in the
Universe. We request exploratory observations of 12 quasars with z > 4.8 and one
with z = 4.78. These data, combined with our previous programs, will provide
nearly complete X-ray coverage of all known z > 4.8 quasars. We will constrain
the X-ray luminosity function of optically selected quasars at the highest
redshifts, and we will define the broad-band spectral energy distributions of
these quasars. Count stacking will give basic spectral constraints. These
observations will provide the key flux information needed for effective planning
of future X-ray spectroscopy.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
02:06:51.40 +12:16:24.40 SDSS020651+121624 ACIS-S NONE 6.00
02:31:37.60 -07:28:54.50 SDSSJ023137-072854 ACIS-S NONE 4.50
03:07:22.90 -49:45:48.00 BR B0305-4957 ACIS-S NONE 4.00
07:56:18.10 +41:04:08.60 SDSS075618+410408 ACIS-S NONE 7.50
07:56:52.10 +45:02:58.90 SDSS075652+450258 ACIS-S NONE 7.30
09:13:16.60 +59:19:21.50 SDSS091316+591921 ACIS-S NONE 10.00
09:41:08.40 +59:47:25.80 SDSS094108+594725 ACIS-S NONE 4.50
09:51:51.20 +59:45:56.20 SDSS095151+594556 ACIS-S NONE 5.00
10:23:32.10 +63:35:08.10 SDSS102332+633508 ACIS-S NONE 4.80
17:37:44.90 +58:28:29.50 SDSS173744+582829 ACIS-S NONE 4.50
22:16:44.00 +00:13:48.30 SDSS221644+001348 ACIS-S NONE 8.00
===================================================================================
Proposal Number: 03700413
Proposal Title: AN IN-DEPTH STUDY OF THE X-RAY SOURCE POPULATION AND HOT ISM OF
THE ANTENNAE GALAXIES
PI: GIUSEPPINA FABBIANO
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose a deep 375~ks observation of the prototypical merger
galaxies NGC~4038/39 (``The Antennae''), divided into 5 time segments. Together
with the archival data, we will obtain a deep 450ks ACIS-S exposure and time
monitoring over 3 yrs. The unique significance of the Antennae for our
understanding of mergers and the extraordinary characteristics of the X-ray
emission of this system, make this study essential for probing a wide range of
fundamental questions on the properties and evolution of XRBs, the range of black
hole masses implied by the rich ULX population, the properties of the multiphase
ISM, and the evolution of galaxy mergers, that cannot be addressed by looking at
more normal galaxies.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:01:53.70 -18:52:35.50 NGC 4038/NGC 4039 ACIS-S NONE 37.00
12:01:53.70 -18:52:35.50 NGC 4038/NGC 4039 ACIS-S NONE 38.00
12:01:53.70 -18:52:35.50 NGC 4038/NGC 4039 ACIS-S NONE 75.00
12:01:53.70 -18:52:35.50 NGC 4038/NGC 4039 ACIS-S NONE 75.00
12:01:53.70 -18:52:35.50 NGC 4038/NGC 4039 ACIS-S NONE 75.00
12:01:53.70 -18:52:35.50 NGC 4038/NGC 4039 ACIS-S NONE 75.00
===================================================================================
Proposal Number: 03700438
Proposal Title: RESOLVING THE WARM ABSORBER IN NGC 5548
PI: JELLE KAASTRA
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to map the ionization and velocity structure of the X-ray
and UV absorbers in NGC 5548 with the LETGS and HETGS of Chandra and STIS/HST.
NGC 5548 is an important target for this kind of study because 1) it shows
multiple kinematic components in the UV characterized by a range in ionization
parameter and effective column, 2) it shows evidence for multiple kinematic and
ionization components in previous Chandra X-ray spectra, and 3) it has a low
Galactic column, which permits coverage of spectral lines out to 80 Angstrom with
the LETGS. These data yield the ionization parameter and column density of the
absorption-line regions as a function of radial velocity, and constrain the
elemental abundances and shape of the unobserved EUV continuum.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
14:17:59.60 +25:08:12.40 NGC 5548 HRC-S LETG 175.00
14:17:59.60 +25:08:12.40 NGC 5548 HRC-S LETG 175.00
14:17:59.60 +25:08:12.40 NGC 5548 ACIS-S HETG 170.00
===================================================================================
Proposal Number: 03700502
Proposal Title: X-RAY IMAGING OF QUASAR JETS
PI: ALAN MARSCHER
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to observe 5 quasars with arcsecond-scale radio jets. Three
of these point almost directly at us, as indicated by several observed
characteristics, while the other two are likely to be less well aligned. If the
jets remain relativistic out to kpc-scales, we expect to see X-ray emission from
inverse Compton scattering of Cosmic Microwave Background photons (IC-CMB), as
appears to be the case in X-ray jets already observed in FR II galaxies and
quasars (often offset from radio/optical knots). The ratio of X-ray to radio flux
for IC-CMB should depend on the jet orientation, magnetic field direction,
Lorentz factor, and redshift. The extent to which the proposed observations
confirm these expectations will provide a test of the IC-CMB X-ray emission model
in quasar jets.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
08:30:52.10 +24:10:59.80 0827+243 ACIS-S NONE 20.00
09:27:03.00 +39:02:20.80 0923+392 ACIS-S NONE 20.00
12:24:54.40 +21:22:47.10 1222+216 ACIS-S NONE 20.00
13:19:46.20 +51:48:08.20 1317+520 ACIS-S NONE 20.00
22:12:01.60 +08:19:17.00 2209+080 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03700526
Proposal Title: REVEALING THE NATURE OF THE X-RAY ABSORPTION IN NGC 4151
PI: STEVEN KRAEMER
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: Determining the nature of the soft X-ray absorption in the Seyfert
galaxy NGC 4151 has proved elusive. Currently, the strong downturn below 3 keV is
thought to be a blend of absorption edges from highly ionized species in an
unusually large column of gas. However, it has been impossible to test this
explanation or constrain physical models of the gas due to the inability of
previous X-ray missions to resolve the expected absorption lines. We propose
simultaneous Chandra and HST/STIS observations of NGC 4151 to detect the X-ray
absorption lines, determine the ionization state, column, and kinematics of the
X-ray absorbers, and determine the connection to the UV absorbers.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:10:32.70 +39:24:19.60 NGC 4151 ACIS-S HETG 90.00
12:10:32.70 +39:24:19.60 NGC 4151 ACIS-S HETG 160.00
===================================================================================
Proposal Number: 03700563
Proposal Title: THE DYNAMICS OF CLASSICAL DOUBLE RADIO SOURCES: TESTING
SELF-SIMILAR MODELS
PI: MARTIN HARDCASTLE
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: Although well-accepted models for the dynamics of classical double
radio sources have been current for many years, it is only recently that they
have progressed to the point at which they can be directly tested against
observations. Kaiser (2000) has developed a model which predicts parameters of
the hot-gas environment of well-behaved double sources from their observed radio
spatial and spectral structure. We propose to test this model by observing the
cluster environments of two intermediate-redshift radio sources. The observations
will help to resolve important outstanding questions relating to the energy
budget and particle content of these objects.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
07:09:18.20 +74:48:31.80 3C173.1 ACIS-S NONE 25.00
09:06:31.90 +16:46:11.70 3C215 ACIS-S NONE 35.00
===================================================================================
Proposal Number: 03700593
Proposal Title: FRUSTRATED GPS QUASARS
PI: WILLEM DE VRIES
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: Gigahertz Peaked Spectrum (GPS) radio sources constitute a key class of
objects in the study of radio source evolution: they are the most compact, and
therefore, the youngest radio sources. Understanding the triggering of nuclear
radio activity and the subsequent expansion of the radio structure through the
ambient medium of the host galaxy requires a detailed understanding of the GPS
class. GPS galaxies, however, have small radio sizes because they are most likely
"young", whereas GPS quasars are thought to be small because they are confined by
an unusually dense medium; they would be "old". To settle this age issue we
propose to assess the existence of the putative dense quasar medium with Chandra.
Either outcome will be crucial to the understanding of powerful radio source
evolution.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:34:13.30 +47:53:50.80 Q1231+481 ACIS-S NONE 5.00
18:15:36.70 +61:27:11.50 Q1815+614 ACIS-S NONE 5.00
===================================================================================
Proposal Number: 03700582
Proposal Title: X-RAY STUDIES OF HIGH REDSHIFT RADIO GALAXIES
PI: CHRIS CARILLI
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose spectroscopic imaging with Chandra of five high z radio
galaxies. These data represent a critical extension of our long-standing
observational program on these sources. We will study the hot gas environments to
constrain source dynamics and magnetic fields in the hot gas. We hope to
determine whether the alignment between this hot gas and the radio source axis,
as is seen in the two high z sources studied with Chandra thus far, is a general
feature of high z radio galaxies. We will also study the Xray emission from the
AGN in order to test quasar-radio galaxy unification models, and to probe the
immediate gaseous environments of the AGN. We will search for Xray emission from
other cluster galaxies, and for non-thermal Xray emission from the radio
structures.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:58:33.50 -24:59:32.20 0156-252 ACIS-S NONE 20.00
04:08:51.50 -24:18:16.50 0406-244 ACIS-S NONE 20.00
08:30:53.40 +19:13:15.60 0828+193 ACIS-S NONE 20.00
20:39:24.50 -25:14:30.40 2036-254 ACIS-S NONE 20.00
20:51:03.40 -27:03:04.60 2048-272 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03700611
Proposal Title: SIMULTANEOUS CHANDRA, HST AND FUSE OBSERVATIONS OF WARM
ABSORBERS IN AGN
PI: GERARD KRISS
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: Photoionized, warm absorbing gas is an important component of the
nuclear structure of AGN. About half of all low-z AGN show X-ray warm absorbers
and high-ionization UV absorption lines, but the relationship of the X-ray
absorber to the UV-absorbing gas is not clear. Only a handful of
high-spectral-resolution observations with Chandra, HST, or FUSE currently exist
(NGC4151, NGC3516, NGC3783, NGC5548, Mrk 509). These show a diversity of
kinematic structure and ionization states in the absorbers. We propose to
increase significantly the sample of low-redshift AGN studied at high spectral
resolution in the X-ray and the UV by obtaining simultaneous HST, Chandra, and
FUSE spectra of NGC5548 and Mrk279. Our HETGS spectra will also probe the origin
of narrow Fe Kalpha emission in Seyfert 1s.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
13:53:03.40 +69:18:29.90 MRK279 ACIS-S HETG 120.00
===================================================================================
Proposal Number: 03700668
Proposal Title: X-RAY WEAK BROAD-LINE QUASARS: ABSORPTION OR INTRINSIC X_RAY
WEAKNESS ?
PI: GUIDO RISALITI
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to observe a sample of 23 soft X-ray weak, optically red
quasars, discovered by the Hamburg Quasar Survey. The lack of detection in the
ROSAT PSPC, despite their relatively bright optical emission make them a peculiar
class of quasars, classified as type 1 in the optical but type 2 in the X-rays.
Establishing the X-ray properties of these objects is important for (1) the X-ray
background synthesis models (they could be the missing "QSO2s"), (2) the unified
models (they challenge the traditional torus model) and (3) the long debated
problem on the discrepancy between optical and X-ray luminosity functions. With
180 ks with ACIS-S we can observe a well defined sample of sources and measure
their absorption column density in many cases.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:20:10.80 +21:32:51.00 HS 0017+2116 ACIS-S NONE 10.00
08:14:22.10 +51:48:39.50 HS 0810+5157 ACIS-S NONE 8.00
08:32:55.60 +18:23:00.50 HS 0830+1833 ACIS-S NONE 7.00
08:50:45.70 +11:08:40.30 HS 0848+1119 ACIS-S NONE 6.00
08:57:24.00 +09:03:49.00 HS 0854+0915 ACIS-S NONE 4.00
10:39:34.10 +39:52:57.80 HS 1036+4008 ACIS-S NONE 7.00
11:13:50.80 +40:17:21.00 HS 1111+4033 ACIS-S NONE 10.00
12:05:04.40 +35:22:08.10 HS 1202+3538 ACIS-S NONE 7.00
12:31:38.10 +47:50:53.00 HS 1229+4807 ACIS-S NONE 7.00
12:33:01.80 +47:24:55.50 HS 1230+4741 ACIS-S NONE 10.00
12:40:06.70 +47:40:03.30 HS 1237+4756 ACIS-S NONE 5.00
12:54:22.90 +26:20:05.90 HS 1251+2636 ACIS-S NONE 6.00
14:17:34.30 +26:47:52.00 HS 1415+2701 ACIS-S NONE 9.00
14:19:51.80 +47:09:00.90 HS 1417+4722 ACIS-S NONE 8.00
14:24:36.00 +42:10:30.60 HS 1422+4224 ACIS-S NONE 6.00
18:24:46.70 +65:09:25.20 HS 1824+6507 ACIS-S NONE 7.00
19:39:29.50 +70:07:49.00 HS 1939+7000 ACIS-S NONE 5.00
21:38:05.30 +13:39:53.50 HS 2135+1326 ACIS-S NONE 6.00
21:48:32.20 +04:42:15.80 HS 2146+0428 ACIS-S NONE 7.00
22:53:38.50 +29:57:12.10 HS 2251+2941 ACIS-S NONE 7.00
===================================================================================
Proposal Number: 03700685
Proposal Title: ACIS-S IMAGING-SPECTROSCOPY OF THREE INTERMEDIATE FRI/FRII RADIO
GALAXIES
PI: CHRISTOPHER REYNOLDS
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose ACIS-S imaging of three intermediate FRI/FRII radio galaxies
which are embedded in the centers of rich galaxy clusters. These objects are good
candidates for fading/dying radio galaxies. We request 50ks observations of both
3C346 and 3C401 with the intention of comparing the radio and X-ray morphologies.
In particular, we will search for X-ray shells and cavities that have been seen
in many low-redshift radio-galaxy/cluster systems. These data will constrain the
kinetic power and history of these sources. We will also be able to easily
resolve the ICM emission from any central AGN component, even in the presence of
a central cooling flow cusp. A 10ks exploratory observation of 3C173.1 is
requested in order to perform the same decomposition.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:40:25.10 +60:41:35.00 3C401 ACIS-S NONE 25.00
19:40:25.10 +60:41:35.00 3C401 ACIS-S NONE 25.00
===================================================================================
Proposal Number: 03700691
Proposal Title: X-RAY VARIABILITY IN THE JET AND CORE OF M87
PI: DANIEL HARRIS
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: M87 is the nearest galaxy with a bright radio / optical / X-ray jet,
and affords an unparalleled opportunity to study extragalactic jet phenomena at
high resolution. We propose the initial phase of a long-term variability study of
the core and jet of M87 with 5 ACIS observations at intervals of 2 months. We
will correlate X-ray brightness variations in both time and place with
morphological features (shocks within knots) and structural changes (emergence of
new superluminal features) seen in our high resolution radio / optical studies of
the 20" jet. Our ultimate goal is to learn what processes and phyical conditions
are responsible for producing X-rays in AGN jets.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:30:49.00 +12:23:30.00 M87 ACIS-S NONE 5.00
12:30:49.00 +12:23:30.00 M87 ACIS-S NONE 5.00
12:30:49.00 +12:23:30.00 M87 ACIS-S NONE 5.00
12:30:49.00 +12:23:30.00 M87 ACIS-S NONE 5.00
12:30:49.00 +12:23:30.00 M87 ACIS-S NONE 5.00
===================================================================================
Proposal Number: 03700772
Proposal Title: PROBING THE HOT AGN OUTFLOW IN NGC 4151
PI: PATRICK OGLE
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We will use Chandra LETGS to study the soft X-ray emission line
spectrum from the narrow-line region (NLR) of the Seyfert 1.5 galaxy NGC 4151.
This is a follow-up to a successful HETGS observation of NGC 4151 in March 2000.
The goal of this proposal is to distinguish between emission from hot(1E7 K)
plasma and resonance scattering as the sources of the unusually strong resonance
emission lines. If we can verify the existence of a hot plasma, it will provide
the necessary pressure to confine the optical and cool X-ray emitting NLR clouds.
It will also indicate a very large mass outflow rate for the nucleus, much larger
than inferred from optical and UV observations. This study will have important
implications for the warm absorbers in Seyfert 1 galaxies and the AGN unification
paradigm.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:10:32.60 +39:24:20.60 NGC 4151 ACIS-S LETG 90.00
===================================================================================
Proposal Number: 03700780
Proposal Title: THE POWERFUL RADIO GALAXY PICTOR A
PI: ANDREW WILSON
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose a 100 ksec observation of the western hot spot and jet of
the nearby, FRII, powerful radio galaxy Pictor A. Our goals are to: (i) measure
the change of the spatially-integrated spectral index of the hot spot through the
Chandra band, in order to confirm or reject one model of the X-ray emission; (ii)
map the spatial distribution of the X-ray spectral index over the hot spot; (iii)
compare the X-ray, optical and radio morphologies; (iv) provide a more accurate
spectral index of the jet to check the synchrotron self-Compton model of its
X-ray emission; and (v) try to detect the jet all the way from the nucleus to the
hot spot.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:19:26.20 -45:45:53.50 PICTOR A - WEST ACIS-S NONE 50.00
05:19:26.20 -45:45:53.50 PICTOR A - WEST ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03700742
Proposal Title: THE X-RAY SPECTRA OF RED QUASARS SELECTED FROM 2MASS AND FIRST
PI: MARK LACY
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We have identified a sample of very red (R-K>4.9) quasars at redshifts
~1-2 through matching the 2MASS and FIRST surveys. We believe that these are high
luminosity analogues of the red quasars found in deep Chandra surveys which make
up ~30% of the X-ray background. Chandra observations of our quasars will allow
us to test this hypothesis through measurements of the absorbing columns and
spectral slopes. We also wish to establish the gas:dust ratio in the absorbing
material, and compare our objects to broad absorption line quasars, which also
show high columns and reddening. If, as we expect, our red quasars do indeed have
similar X-ray spectra to those which contribute to the X-ray background, we can
define a large sample of bright objects to study in detail.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:34:35.60 -09:31:03.00 FTM0134-0931 ACIS-S NONE 1.00
07:29:10.40 +33:36:34.00 FTM0729+3336 ACIS-S NONE 2.00
07:38:20.10 +27:50:45.50 FTM0738+2750 ACIS-S NONE 4.00
09:06:51.50 +49:52:36.00 FTM0906+4952 ACIS-S NONE 6.00
10:12:30.50 +28:25:27.20 FTM1012+2825 ACIS-S NONE 3.50
10:36:33.50 +28:28:21.60 FTM1036+2828 ACIS-S NONE 4.00
===================================================================================
Proposal Number: 03700781
Proposal Title: X-RAY IMAGING OF GPS AND CSS QUASARS
PI: ANETA SIEMIGINOWSKA
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose the first survey of GPS and CSS radio-loud quasars with
ACIS-S. We will study their arcsecond structure in the X-rays, search for X-ray
jets, and search for signatures of intermittent AGN activity. Our AO1
observations of two GPS sources revealed long (300 kpc) X-ray jets, challenging
the notion that GPS sources are young and/or "frustrated" FRI radio sources. Our
observations will confirm or refute current theories of radio quasar evolution.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:37:41.30 +33:09:34.00 Q0134+329 ACIS-S NONE 10.00
07:44:17.50 +37:53:17.10 Q0740+380 ACIS-S NONE 42.00
09:43:36.90 -08:19:31.00 Q0941-080 ACIS-S NONE 5.00
11:46:08.10 -24:47:33.00 Q1143-245 ACIS-S NONE 5.00
12:48:24.00 -19:59:19.60 Q1245-197 ACIS-S NONE 5.00
12:52:26.40 +56:34:19.70 Q1250+568 ACIS-S NONE 15.00
13:30:37.80 +25:09:10.80 Q1328+254 ACIS-S NONE 40.00
14:19:08.20 +06:28:34.80 Q1416+067 ACIS-S NONE 20.00
14:59:07.60 +71:40:20.00 Q1458+718 ACIS-S NONE 20.00
18:31:14.90 +29:07:10.10 Q1829+290 ACIS-S NONE 5.00
21:30:32.90 +05:02:17.00 Q2127+040 ACIS-S NONE 5.00
===================================================================================
Proposal Number: 03700786
Proposal Title: A COMPLETE SURVEY FOR X-RAY EMISSION FROM RADIO JETS
PI: HERMAN MARSHALL
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to obtain high resolution X-ray images for a well defined
complete sample of quasar jets. Selection is based on the flux density in
extended emission which should give a sample that is unbiased with regard to
orientation and possible beaming. We also select objects in which the morphology
gives an indication that beaming may be important, by way of contrast. We will
find good targets for detailed X-ray imaging and optical followup so that we can
measure the spectral energy distributions and then test models such as the
synchrotron and synchrotron self-Compton emission mechanisms. In addition, we
will measure the X-ray spectra of the quasar cores in order to model the origins
of jets and examine the relationship between cores and kpc scale jets.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
02:10:46.20 -51:01:01.90 0208-512 ACIS-S NONE 5.00
02:31:45.90 +13:22:54.70 0229+131 ACIS-S NONE 5.00
04:16:04.40 -20:56:27.60 0413-210 ACIS-S NONE 5.00
07:48:36.10 +24:00:24.10 0745+241 ACIS-S NONE 5.00
08:57:42.50 -77:19:31.90 0858-771 ACIS-S NONE 5.00
09:04:52.60 -57:35:09.00 0903-573 ACIS-S NONE 5.00
09:22:46.40 -39:59:35.10 0920-397 ACIS-S NONE 5.00
10:33:07.70 -36:01:56.90 1030-357 ACIS-S NONE 5.00
10:48:38.30 -41:13:59.60 1046-409 ACIS-S NONE 5.00
11:47:33.60 -67:53:41.70 1145-676 ACIS-S NONE 5.00
12:05:33.30 -26:34:04.10 1202-262 ACIS-S NONE 5.00
13:01:00.80 -32:26:29.20 1258-321 ACIS-S NONE 5.00
13:46:49.00 -60:24:30.00 1343-601 ACIS-S NONE 5.00
14:27:56.30 -42:06:19.40 1424-418 ACIS-S NONE 5.00
16:58:09.00 +07:41:27.50 1655+077 ACIS-S NONE 5.00
17:02:42.00 -77:41:57.30 1655-776 ACIS-S NONE 5.00
18:29:31.80 +48:44:46.60 1828+487 ACIS-S NONE 5.00
20:56:16.40 -47:14:47.60 2052-474 ACIS-S NONE 5.00
21:05:01.30 -48:48:49.00 2101-490 ACIS-S NONE 5.00
22:53:57.70 +16:08:53.60 2251+158 ACIS-S NONE 5.00
===================================================================================
Proposal Number: 03700795
Proposal Title: 3C 346, 3C 78, AND THE X-RAY EMISSION MECHANISM FROM OPTICAL
JETS
PI: MARK BIRKINSHAW
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: The radio to X-ray spectral energy distributions of radio-galaxy jets,
and the offsets between the positions of the radio/optical and X-ray knots, show
that the X-ray emission is mostly of synchrotron origin, unlike the
inverse-Compton emission from quasar jets. Imaging and spectral data from Chandra
can provide crucial new information on jet physics, specifically the electron
energy distribution and jet speed. Here we propose a 50 ksec Chandra observation
of the longest optical jet not yet observed, 3C 346, and a short exploratory
image of the anomalously bright jet source 3C 78. Existing VLA, HST, and ROSAT
data suggest that 3C 346 will show structures like those in the X-ray jets of M
87 and 3C 66B, and possibly also a thermal envelope like that seen around the jet
in 3C 15.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
03:08:26.20 +04:06:39.30 3C78 ACIS-S NONE 5.00
16:43:48.70 +17:15:49.00 3C346 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03700814
Proposal Title: STRONG LYMAN ALPHA SOURCES AT REDSHIFTS Z>4: GALAXIES OR
QUASARS?
PI: SANGEETA MALHOTRA
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: Strong Lyman Alpha line emission is expected both from primordial
galaxies and from the type II quasars required to explain the hard x-ray
background. We have identified ~200 Lyman alpha emitting candidates at redshifts
4.5 and 5.7. Of these, 60% show rest equivalent widths EW>200 Angstroms, which
require active nuclei, or extreme populations of massive stars. Our Lyman Alpha
survey is a unique resource for determining the space density of type II quasars
efficiently. X-ray imaging with Chandra ACIS will determine the fraction of type
II quasars among the Lyman alpha sources. This has implications for composition
of the X-ray background, background radiation at other wavelengths, and structure
formation (stars vs black holes) in the early universe.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
14:25:38.88 +35:35:49.20 FIELD-142549+353248 ACIS-I NONE 58.00
14:25:38.88 +35:35:49.20 FIELD-142549+353248 ACIS-I NONE 122.00
===================================================================================
Proposal Number: 03700855
Proposal Title: SEARCH FOR AN INTERMEDIATE MASS BLACK HOLE IN THE STARBURST
GALAXY NGC2146
PI: HIRONORI MATSUMOTO
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We discovered an Intermediate Mass Black Hole (IMBH) of $10^3$ --
$10^6$ $M_\odot$ in the starburst galaxy M82 with Chandra HRC. Our follow-up
ground-based observations found a near-infrared star cluster in the vicinity of
the IMBH as well as an Expanding Molecular Super Bubble (EMSB) which surrounds
the IMBH and has a kinematic energy of $10^{55}$ erg. Based on these results, we
propose a scenario that an IMBH is produced by starburst activity and it grows to
become a Super Massive Black Hole (SMBH). We believe this scenario can explain
the formation of SMBHs in other galaxies universally. We propose a CXO monitoring
observation of another starburst galaxy NGC2146 to examine our scenario.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
06:18:37.30 +78:21:23.60 NGC2146 ACIS-S NONE 10.00
06:18:37.30 +78:21:23.60 NGC2146 ACIS-S NONE 10.00
06:18:37.30 +78:21:23.60 NGC2146 ACIS-S NONE 10.00
06:18:37.30 +78:21:23.60 NGC2146 ACIS-S NONE 10.00
06:18:37.30 +78:21:23.60 NGC2146 ACIS-S NONE 10.00
06:18:37.30 +78:21:23.60 NGC2146 ACIS-S NONE 10.00
===================================================================================
Proposal Number: 03700871
Proposal Title: SEARCHING FOR MISSING LINK BETWEEN ULTLALUMINOUS INFRARED
GALAXIES AND OPTICALLY-SELECTED QUASARS
PI: NAOHSIA ANABUKI
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: Ultraluminous infrared Galaxies(ULIRGs) are the most luminous active
galaxies. The evolutionary relation with optically-selected quasars(optical-QSOs)
are suggested so far. From our recent study of ULIRGs observed with ASCA,
however, we found some evidences which suggest a connection between ULIRGs and
narrow-line quasars (NLQSOs) rather than optical-QSOs, and the relation between
ULIRGs and QSOs are yet unclear. Hence, in order to reveal the nature and the
evolution of AGN in ULIRGs, we propose Chandra observations to serach for missing
link between these objects.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:14:38.90 +32:41:33.30 IRAS 11119+3257 ACIS-S NONE 18.90
===================================================================================
Proposal Number: 03700892
Proposal Title: MASSIVE GAS INFLOW IN RADIO GALAXIES
PI: MAKOTO KISHIMOTO
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to take a deep X-ray image of the nearby aligned radio
galaxy 3C321 with Chandra ACIS-S. There has been a big controversy over the
nature of the huge scattering regions observed in the aligned radio galaxies.
These scattering regions can have enormous amount of gas which is possibly
flowing into the central part of the radio galaxies, analogous to the cooling
flow seen in the cluster of galaxies, if the scatterers are electrons. A number
of observations have actually pointed the scatterers to be electrons. We propose
that this can be robustly addressed simply by spatially resolving the scattering
region in X-ray, since the electron scattering region should still be detected
while dust scattering region will be essentially gone in the X-ray.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
15:31:42.70 +24:04:25.00 3C321 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03700891
Proposal Title: PROBING THE X-RAY EMISSION OF HIGH LUMINOSITY EMISSION LINE
GALAXIES: QUASAR 2'S AND THE STARBURST-AGN CONNECTION
PI: PAOLO COPPI
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose Chandra observations for a sample of 8 highly luminous,
local (M_B < -23, z<0.5) emission line galaxies discovered by the QUEST large
area objective prism survey. The objects selected have spectra indicative of
extremely strong star formation and/or obscured AGN activity. The objects
represent the rare (less than 0.1 per square degree) local counterparts to the
luminous and more common objects we preferentially see at higher redshifts and
could be examples of obscured quasars with hard spectra, the long-sought "Quasar
2's" invoked to explain the X-ray background. Chandra's exquisite angular
resolution and sensitivity above 2 keV is key for disentangling the star
formation and AGN activity in these objects and measuring the obscuration of any
AGN found.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
09:28:56.50 -02:13:35.50 QUEST 0928-0213 ACIS-S NONE 10.00
11:55:44.60 -01:47:39.80 QUEST 1155-0147 ACIS-S NONE 30.00
12:20:04.40 -00:25:39.00 QUEST 1220-0025 ACIS-S NONE 20.00
15:33:45.20 -03:46:24.60 QUEST 1533-0346 ACIS-S NONE 10.00
===================================================================================
Proposal Number: 03700923
Proposal Title: PROBING UNIFICATION WITH ACIS-HETG OBSERVATION OF COMPTON-THIN
SEYFERT 2 NGC 2110
PI: JULIA LEE
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: NGC 2110 is a well-studied Seyfert which display many enigmatic
properties. We propose a 150ks HETG observation as the next scientific step &
complement to the 50ks ACIS (imaging) observation, which shows soft emission from
both the core & extent. HETG observation will unambiguously resolve the nature of
the soft excess, and allow for detailed measurements of velocity profiles &
ionization states of the surrounding gas. Detection of the iron K narrow core
will resolve geometry-related arguments which have direct bearing on Unification.
The properties of NGC 2110 which are distinct from many of the canonical Seyferts
will allow for a comprehensive study (when compared with AO1 HETG/LETG
observations) of the high resolution X-ray properties of the range of Seyferts.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:52:11.40 -07:27:22.00 NGC2110 ACIS-S HETG 35.00
05:52:11.40 -07:27:22.00 NGC2110 ACIS-S HETG 35.00
05:52:11.40 -07:27:22.00 NGC2110 ACIS-S HETG 80.00
===================================================================================
Proposal Number: 03700998
Proposal Title: SOFT X-RAY EMISSION AND ABSORPTION IN NGC 4051
PI: ALBERT BRINKMAN
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to observe the bright Narrow Line Seyfert 1 galaxy NGC 4051
with the LETG/HRC-S of Chandra. The spectral resolution of the LETGS and its
wavelength coverage up to 100 Angstrom allows us to disentangle the contributions
of emission features arising from the accretion disk and/or from continuum
absorption edges produced by the warm absorber. Both components will be studied
in detail, using the spectrosopic as well as the time variability data.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:03:09.60 +44:31:53.20 NGC 4051 HRC-S LETG 100.00
===================================================================================
Proposal Number: 03701000
Proposal Title: SOFT X-RAY EMISSION AND ABSORPTION IN TON 1388
PI: ALBERT BRINKMAN
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to observe the bright Quasi Stellar Object Ton 1388 with the
LETG/HRC-S of Chandra. The spectral resolution of the LETGS and its wavelength
coverage up to 100 Angstrom allows us to disentangle the contributions of
emission features arising from the accretion disk as opposed to continuum
absorption edges produced by the warm absorber. Both components will be studied
in detail spectroscopically.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:19:08.80 +21:19:17.90 TON 1388 HRC-S LETG 90.50
===================================================================================
Proposal Number: 03700211
Proposal Title: MAPPING THE REFLECTING REGIONS IN THE SEYFERT 2 GALAXY TOLOLO
0109-383
PI: GIORGIO MATT
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to observe for 10 ks with ACIS-S the Compton-thick Seyfert 2
galaxy Tololo 0109-383 in order to study the spatial extent of the warm reflector
discovered by ASCA and BeppoSAX, and its correlation with the extended (about 5")
High Ionization Nuclear Emission-Line Region. This observation will shed light on
the nature and distribution of the ionized circumnuclear matter, and will help
clarify the relation between its X-ray and optical properties.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:11:27.50 -38:05:01.00 TOLOLO 0109-383 ACIS-S NONE 10.00
===================================================================================
Proposal Number: 03701014
Proposal Title: SIMULTANEOUS CHANDRA-HST OBSERVATIONS OF SEYFERT 1 GALAXY NGC
7469
PI: CLAUDE CANIZARES
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to add 70ks of Chandra GTO HETGS time (through Canizares) to
the approved 80ks Chandra--HST observation of the Seyfert galaxy NGC 7469 (PI:
Kriss). This will nearly double the number counts in the HETGS spectrum,
improving S/N on emission and absorption lines and revealing weaker lines from
the intrinsic absorber in this source. This will allow a better determination of
the column densities vs. ionization state, resolve any separate kinematic
components, and look for evidence of any collisionally ionized (versus
photoionized) material. Understanding the circumnuclear absorbing gas and its
influence on the radiation escaping from AGN has additional important
implications for the radiative input to the IGM and the origins of the X-ray
background.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
23:03:15.70 +08:52:26.60 NGC 7469 ACIS-S HETG 70.00
===================================================================================
Proposal Number: 03701015
Proposal Title: CHANDRA HETG OBSERVATION OF THE SEYFERT 2 GALAXY IRAS 18325-5926
PI: CLAUDE CANIZARES
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose a 112ks GTO (through Canizares) observation of the enigmatic
Seyfert 2 galaxy IRAS 18325-5926 with the Chandra HETGS to complement our
BeppoSAX (PI: Lee who is a Co-I on this proposal) 150ks long look, and scheduled
150ks XMM (PI: Iwasawa, also a Co-I) observations. HETGS observations will
unambiguously resolve the nature of the soft excess presumably from circumnuclear
material, and allow for a thorough assessment of the geometry and nature of the
accretion disk and corona. The strong Fe K line and lack of associated reflection
component argues for a highly ionized disk. We will look for multiple peaks in
the line expected from ionization, and/or individual lines due to high
ionizations of Fe.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:36:58.00 -59:24:10.00 IRAS 18325-5926 ACIS-S HETG 56.00
18:36:58.00 -59:24:10.00 IRAS 18325-5926 ACIS-S HETG 56.00
===================================================================================
Proposal Number: 03700784
Proposal Title: CHANDRA OBSERVATIONS OF TYPE-2 LINERS: STARBURSTS OR AGNS ?
PI: ANDREAS ZEZAS
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose to observe with ACIS-S3 (BI) for 40Ks each, four nearby
LINER-2 type objects. The optical spectra of two of these objects are found to be
reproduced by shocks in gas poor environments based on theoretical models,
whereas the other two are classical type-2 LINERS. Our primary goal is to study
the nature of this class of objects which has been a matter of debate over the
last few years. With these observations we will be able to determine the
mechanism which powers these galaxies: distinguish between an advection dominated
AGN, a classical AGN, shocks or starburst activity.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:03:25.40 +18:08:13.00 NGC 3507 ACIS-S NONE 40.00
12:28:59.10 +03:34:14.00 NGC4457 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03701002
Proposal Title: A CHANDRA SURVEY OF THE MOST LUMINOUS QUASARS AT Z > 4
PI: GORDON GARMIRE
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose exploratory 4 ks observations of ten of the most luminous
and optically brightest quasars at z > 4. Our science goals are (1) to determine
the X-ray fluxes, X-ray luminosities, optical-to-X-ray slopes, and broad-band
spectral energy distributions (SEDs) of these quasars, (2) to constrain X-ray
spectral properties using hardness ratios and stacking analyses, (3) to
facilitate spectroscopic observations with XMM-Newton, and (4) to lay key
groundwork for future high-redshift X-ray efforts with Constellation-X and XEUS.
We will obtain supporting optical and near-infrared spectroscopy with the
queue-scheduled 8-m Hobby-Eberly Telescope. The proposed project will complement
our other studies of z > 4 quasars using Chandra, XMM-Newton, and archival data.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:21:26.20 +03:47:07.00 PSS0121+0347 ACIS-S NONE 6.00
01:33:40.40 +04:00:59.00 PSS0133+0400 ACIS-S NONE 6.00
02:09:44.70 +05:17:14.00 PSS0209+0517 ACIS-S NONE 6.00
03:11:15.20 -17:22:47.40 BR0308-1734 ACIS-S NONE 6.00
09:26:36.30 +30:55:06.00 PSS0926+3055 ACIS-S NONE 6.00
09:55:11.30 +59:40:32.00 PSS0955+5940 ACIS-S NONE 6.00
09:57:44.50 +33:08:23.00 PSS0957+3308 ACIS-S NONE 6.00
13:26:11.90 +07:43:59.00 PSS1326+0743 ACIS-S NONE 6.00
13:47:43.40 +49:56:21.00 PSS1347+4956 ACIS-S NONE 6.00
14:43:40.80 +58:56:53.00 PSS1443+5856 ACIS-S NONE 6.00
===================================================================================
Proposal Number: 03700302
Proposal Title: AN X-RAY MICROLENSING TEST OF THE AU-SCALE CENTRAL STRUCTURE OF
THE QUADRUPLE QUASAR 2237+0305
PI: SHIN MINESHIGE
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: We propose Chandra observation of the gravitationally lensed quasar
Q2237+0305 (Einstein Cross) during a microlensing event. We will monitor the four
images of the QSO from the ground regularly to ascertain the onset of a
microlensing event. As the microlensing event occurs, we will measure the
variations of X-ray intensity and spectra with AXAF and compare with those taken
after the event. Since only a small region of the QSO accretion disk is strongly
magnified during a microlensing event, we will be able to limit the size of X-ray
emitting regions of the QSO and thus the mass which is contained on scales of
several AUs. If observed simultaneously with ground-based telescopes and with
HST, furthermore, we will also be able to probe multi-wavelength emission
properties of QSOs.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
22:40:30.30 +03:21:31.00 Q2237+0305 ACIS-S NONE 15.00
22:40:30.30 +03:21:31.00 Q2237+0305 ACIS-S NONE 15.00
22:40:30.30 +03:21:31.00 Q2237+0305 ACIS-S NONE 15.00
22:40:30.30 +03:21:31.00 Q2237+0305 ACIS-S NONE 15.00
22:40:30.30 +03:21:31.00 Q2237+0305 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03708070
Proposal Title: CHANDRA MONITORING OF A MICROLENSING EVENT IN MG J0414+0534
PI: GEORGE CHARTAS
Subject Category: ACTIVE GALAXIES AND QUASARS
Abstract: Recent Chandra monitoring of the gravitational lens (GL) system MG
J0414+0534 indicate that images C and B are possibly undergoing microlensing
events. The microlensing event in image B is of particular interest since it is
accompanied by a five-fold increase of the equivalent width of a reprocessed
narrow Fe Ka line in the spectrum of image B. This sudden increase can be
explained with a caustic crossing that selectively enhances a strip of the
reflection emission region of the accretion disk. The main goal of the proposed
DDT observations is to directly probe the various emission regions of an
accretion disk from scales of a few hundred gravitational radii down to the event
horizon of the black hole. We expect to achieve this goal by monitoring changes
in the line energy, intensity, and profile of an Fe Ka line in image B as a
magnification caustic is traversing the accretion disk of the distant z = 2.64
radio loud quasar MG J0414+0534.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
04:14:37.70 +05:34:44.00 MG J0414+0534 ACIS-S NONE 30.00
04:14:37.70 +05:34:44.00 MG J0414+0534 ACIS-S NONE 30.00
04:14:37.70 +05:34:44.00 MG J0414+0534 ACIS-S NONE 100.00
***********************************************************************************
CLUSTERS OF GALAXIES
--------------------------------------------------
===================================================================================
Proposal Number: 03800004
Proposal Title: MEASURING THE MASS DISTRIBUTION IN THE MOST DISTANT,VERY X-RAY
LUMINOUS GALAXY CLUSTER KNOWN
PI: HARALD EBELING
Subject Category: CLUSTERS OF GALAXIES
Abstract: We propose to obtain a mosaic of deep HST/WFPC2 images to conduct a
weak lensing analysis of the mass distribution in the massive, distant galaxy
cluster ClJ1226.9+3332, recently discovered by us. At z=0.888 this exceptional
system is more X-ray luminous and more distant than both MS1054.4-0321 and
ClJ0152.7-1357, the previous record holders, thus providing yet greater leverage
for cosmological studies of cluster evolution. ClJ1226.9+3332 differs markedly
from all other currently known distant clusters in that it exhibits little
substructure and may even host a cooling flow, suggesting that it could be the
first cluster to be discovered at high redshift that is virialized. We propose
joint HST and Chandra observations to investigate the dynamical state of this
extreme object.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:26:58.20 +33:32:48.00 CLJ1226.9+3332 ACIS-I NONE 32.00
===================================================================================
Proposal Number: 03800013
Proposal Title: A NEW GALAXY CLUSTER STRONG LENS
PI: MIKE GLADDERS
Subject Category: CLUSTERS OF GALAXIES
Abstract: In the course of the Red-Sequence Cluster Survey, we have discovered a
stunning new example of strong lensing by a relatively high redshift (z~0.7)
cluster. At least 4 separate arcs are detected in our initial survey data, at 3-4
different cluster-centric radii and hence likely corresponding to at least 3
different background sources at 3 different redshifts. The proposed HST WFPC2
imaging, in conjunction with proposed VLT spectroscopy, offers an unprecedented
opportunity to measure the core mass distribution of a cluster at such a high
redshift. In combination with requested coordinated Chandra X-ray imaging, this
will enable a direct comparison of the dark matter and baryonic components of the
cluster, and enable a measure of cosmology via sources at different z.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
02:24:34.10 -00:02:30.90 RCS0224-0002 ACIS-S NONE 15.00
===================================================================================
Proposal Number: 03800021
Proposal Title: MERGER SHOCKS IN CLUSTERS OF GALAXIES
PI: CRAIG SARAZIN
Subject Category: CLUSTERS OF GALAXIES
Abstract: Major mergers of clusters are the most energetic events in the present
Universe. We propose Chandra observations of 2 merging clusters to detect shocks
in the intracluster gas. We will use these shocks to determine the global
dynamics and local physics of the intracluster medium. Shock physics will
determine: (a) if the kinetic energy is effectively thermalized in shocks or if
much of the shock energy goes into turbulence, magnetic fields, or cosmic rays;
(b) if electrons undergo collisionless heating in the shocks; (c) whether the
acceleration of relativistic electrons is effective in these shocks; and (d) what
the persistence of small cooling cores tells us about the dynamics of mergers and
peaks in the dark matter distribution in clusters.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
15:22:28.99 +27:42:29.88 A2065 ACIS-I NONE 50.00
===================================================================================
Proposal Number: 03800034
Proposal Title: DEEP X-RAY IMAGE OF A133
PI: STEPHEN MURRAY
Subject Category: CLUSTERS OF GALAXIES
Abstract: We propose to obtain a deep high resolution X-ray image of A133. We
will measure the X-ray surface brightness profile and gas temperature at a large
radius from the center and use this information to measure the baryon fraction at
half the virial radius. We will constrain the clumpiness of the intracluster
medium. GTO Priority "A"
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:02:40.80 -21:52:40.80 A133 OFFSET ACIS-I NONE 45.00
01:02:40.80 -21:52:40.80 A133 OFFSET ACIS-I NONE 45.00
===================================================================================
Proposal Number: 03800039
Proposal Title: A DETAILED STUDY OF THE CLUSTER 1E 0657-56
PI: STEPHEN MURRAY
Subject Category: CLUSTERS OF GALAXIES
Abstract: Abstract: 1E 0657-56 is the hottest known cluster. A short ACIS
exposure has also revealed that it has the most compelling (if not the only)
example of a merger bow shock. The proposed additional long exposure will be used
to derive the detailed temperature and pressure profiles across the shock front
and the interface between the cool moving subcluster and the shocked gas. GTO
Priority "A"
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
06:58:19.70 -55:56:20.00 1E 0657-56 ACIS-I NONE 90.00
===================================================================================
Proposal Number: 03800040
Proposal Title: A DETAILED STUDY OF THE CLUSTER A907
PI: STEPHEN MURRAY
Subject Category: CLUSTERS OF GALAXIES
Abstract: A short ACIS exposure of A907 has revealed sharp features in the X-ray
brightness distribution that may be shock fronts. If true, this would be only the
second example of a clear shock front in a galaxy cluster. The proposed exposure
will provide an accurate temperature profile across these features and a
definitive answer to this question. GTO Priority "B"
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
09:58:22.00 -11:03:50.40 A907 ACIS-I NONE 50.00
===================================================================================
Proposal Number: 03800069
Proposal Title: OLEGS OR FOSSIL GROUPS -- STUDYING EVOLVED GALAXY SYSTEMS
PI: STEPHEN MURRAY
Subject Category: CLUSTERS OF GALAXIES
Abstract: Recent studies identified an unusual class of compact groups in which
most of the optical light arises from a single dominant elliptical and yet the
X-ray gas has an extent and luminosity characteristic of a bright galaxy group.
These systems may be ``fossil'' groups in which the member galaxies have merged
into a single, central galaxy. We propose to observe the two X-ray brightest
objects, ESO3060170 and NGC1550. We will determine the total gravitating mass and
the mass in heavy elements. Combined with optical photometry, we will derive the
mass-to-light ratio and use the heavy element abundance to test the idea that
these systems are either ``fossil'' groups or possibly a new class of optically
``dim'' systems. GTO Priority "A"
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
04:19:38.25 +02:23:42.00 NGC1550-A ACIS-I NONE 10.00
04:19:38.25 +02:23:42.00 NGC1550-B ACIS-I NONE 10.00
05:40:07.20 -40:47:60.00 ESO3060170-A ACIS-I NONE 15.00
05:40:12.00 -40:51:54.00 ESO3060170-B ACIS-I NONE 15.00
===================================================================================
Proposal Number: 03800071
Proposal Title: COLLIDING GROUPS
PI: STEPHEN MURRAY
Subject Category: CLUSTERS OF GALAXIES
Abstract: ACIS-I observations of the X-ray groups around NGC6868 and NGC6861 will
allow us to investigate the possible merger of these groups into a larger system.
Both groups have extended, symmetric X-ray emission, centered on the bright NGC
galaxies. Both have been extensively studied at other wavelengths. Of note,
NGC6868 has a central radio source and studies of the stellar and ionized gas
show unusual kinematics, particularly in the core. With Chandra we will search
for interactions in the region between the groups, map the gas temperature and
abundance within each group and study the morphology and gas temperature in the
central regions to determine if cooling flows are present.\ GTO Priority "A"
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
20:07:19.10 -48:22:12.00 NGC6861 ACIS-I NONE 25.00
20:09:54.10 -48:22:47.00 NGC6868 ACIS-I NONE 25.00
===================================================================================
Proposal Number: 03800102
Proposal Title: THE INTERACTION BETWEEN CLUSTER CENTRAL RADIO SOURCES AND
COOLING FLOWS
PI: CRAIG SARAZIN
Subject Category: CLUSTERS OF GALAXIES
Abstract: Central galaxies in rich clusters are sites of cluster cooling flows,
with large masses of gas cooling through X-ray temperatures. Many of these
galaxies host powerful radio sources. Our Chandra image of A2052 and others show
strong interactions between X-ray gas and radio plasma. The X-ray gas may confine
radio lobes, deflect radio jets, and produce Faraday rotation. The radio lobes
may displace and compress the X-ray gas; this may lead to enhanced cooling and
star formation. We propose Chandra observations of three bright cooling flows
with radio sources to image the interaction region with the radio source, and to
determine the physical state of the X-ray gas. We will also derive the overall
cooling flow properties, including abundance gradients and excess absorption, if
any.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
23:36:30.50 +21:08:45.50 A2626 ACIS-S NONE 26.00
===================================================================================
Proposal Number: 03800104
Proposal Title: THE FATE OF MATTER IN THE MODERATE COOLING FLOW CLUSTER ABELL
1991
PI: BRIAN MCNAMARA
Subject Category: CLUSTERS OF GALAXIES
Abstract: Using Chandra imaging, ground based U, R, I, and VLA radio imaging for
Abell 1991, we will reevaluate the proposition that large quantities of
intracluster gas are cooling and accreting onto its central cluster galaxy (CDG)
and fueling star formation. In addition, we will study in detail the role of its
radio source on the dynamics of the hot gas, and in triggering star formation.
Measurements of the physical state of the keV gas will be made on the same
arcsecond spatial scales as the star formation regions, permitting the cooling
rates and star formation rates to be directly compared and perhaps reconciled.
Abell 1991 is an excellent example of a bright cooling flow with a moderately
small cooling rate and radio power, which is the most abundant type of cooling
flow cluster.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
14:54:31.50 +18:38:32.00 ABELL 1991 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03800108
Proposal Title: CHANDRA AND HST OBSERVATIONS OF THE BRIGHTEST, RELAXED CLUSTER
LENSES
PI: STEVEN ALLEN
Subject Category: CLUSTERS OF GALAXIES
Abstract: We propose coordinated observations, using the Chandra Observatory and
Hubble Space Telescope, of three of the X-ray brightest, cooling-flow clusters
with bright gravitational arcs newly identified from the ROSAT XBACS/BCS lensing
study. Our primary aim is to measure the cluster mass profiles using both the
X-ray and lensing data. Secondary goals include measurements of the X-ray
gas/total mass ratio as a function of radius, and the properties and ages of the
cooling flows. Our targets are the X-ray brightest, dynamically-relaxed lensing
clusters not yet studied with Chandra or HST and are amongst the most massive and
X-ray luminous clusters known.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
08:00:56.90 +36:03:26.00 ABELL 611 ACIS-S NONE 40.00
09:52:49.20 +51:53:06.00 ZWICKY 2701 ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03800113
Proposal Title: OBSERVATION OF MACS CLUSTERS, Z>0.5
PI: LEON VANSPEYBROECK
Subject Category: CLUSTERS OF GALAXIES
Abstract: Observe these clusters to determine distances using the SZ effect.
Also, study cluster evolution
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
06:47:50.20 +70:14:55.00 MACS-J0647.7+7015 ACIS-I NONE 20.00
07:44:53.00 +39:27:26.00 MACS-J0744.8+3927 ACIS-I NONE 20.00
08:25:24.70 +61:57:14.00 MACS-J0825.5+6157 ACIS-I NONE 20.00
21:29:26.20 -07:41:27.00 MACS-J2129.4-0741 ACIS-I NONE 20.00
===================================================================================
Proposal Number: 03800123
Proposal Title: CHANDRA OBSERVATION OF THE COMPRESSED WARM INTERSTELLAR MEDIUN
IN THE OPHIUCHUS CD GALAXY
PI: ALEXEY VIKHLININ
Subject Category: CLUSTERS OF GALAXIES
Abstract: The ROSAT HRI image of the Ophiuchus cluster reveals that its cD galaxy
harbors the compact, but extended, X-ray source. The properties of this source
appear very similar to those in Coma cD galaxies, which we have recently
demonstrated to be the remnants of the warm interstellar medium compressed by the
hot intracluster gas. The existence of such objects is possible only if there is
a delicate balance of radiative cooling, heat conduction from the hot cluster
gas, and stellar feedback. This provides a unique possibility to study these
crucial physical processes in detail. We request a 50 ksec observation with
ACIS-I.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:12:27.80 -23:22:11.50 OPHIUCHUS CLUSTER ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03800124
Proposal Title: GAS DENSITY DISCONTINUITIES IN MERGING CLUSTERS
PI: MAXIM MARKEVITCH
Subject Category: CLUSTERS OF GALAXIES
Abstract: One of the new and unexpected Chandra discoveries is the existence of
sharp edges, or gas density discontinuities, in the ICM of several clusters.
Depending on the sign of the temperature jump across the discontinuity, the edges
correspond to two different phenomena: either a sharp boundary of a moving,
stripped subcluster remnant, or a bow shock (in only one known case). With
Chandra's angular resolution, both phenomena offer unique insights into the
cluster physics, including determining the gas bulk velocity, its acceleration,
growth of plasma instabilities, strength and structure of magnetic fields, and
thermal conductivity. We propose deep ACIS observations of three bright clusters
whose images show the presence of such contact discontinuities and shock fronts.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
03:42:43.90 -53:38:27.60 A3158 ACIS-I NONE 27.00
03:42:43.90 -53:38:27.60 A3158 ACIS-I NONE 33.00
06:02:10.00 -39:57:20.99 A3376 ACIS-I NONE 22.00
06:02:10.00 -39:57:20.99 A3376 ACIS-I NONE 48.00
===================================================================================
Proposal Number: 03800125
Proposal Title: ABELL 168, A RARE MERGER WITH THE SIMPLEST GEOMETRY
PI: MAXIM MARKEVITCH
Subject Category: CLUSTERS OF GALAXIES
Abstract: Mergers provide a unique laboratory for studying cluster physics. For
example, using the gas temperature and density upstream and downstream of a
merger shock, one can determine the shock velocity that defines the merger
timescale and energetics. If shock fronts are discernible (with the help of
Chandra's arcsecond resolution), one can use them to study microscopic properties
of the intracluster plasma, including the magnetic field. While many clusters
exhibit signs of merging, most have complicated geometries and projections that
preclude unambiguous interpretation. We propose to obtain a detailed temperature
map of A168 whose image suggests a head-on collision of two similar cool
subclusters occurring in the plane of the sky - the simplest possible merger
scenario.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:14:52.30 +00:23:58.00 A168_OFFSET1 ACIS-I NONE 40.00
01:15:25.00 +00:16:15.00 A168_OFFSET2 ACIS-I NONE 40.00
===================================================================================
Proposal Number: 03800127
Proposal Title: DETAILED STUDY OF CLUSTER A907
PI: LEON VANSPEYBROECK
Subject Category: CLUSTERS OF GALAXIES
Abstract: A short ACIS exposure of A907 has revealed sharp features in the X-ray
brightness distribution that may be shock fronts. If true, this would be only the
second example of a clear shock front in a galaxy cluster. The proposed exposure
will provide an accurate temperature profile across these features and a
definitive answer to this question.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
09:58:22.10 -11:03:50.00 A907 ACIS-I NONE 50.00
===================================================================================
Proposal Number: 03800130
Proposal Title: OVER-LUMINOUS ELLIPTICAL GALAXIES (AKA FOSSIL GROUPS)
PI: WILLIAM FORMAN
Subject Category: CLUSTERS OF GALAXIES
Abstract: Recent studies identified a new class of groups in which most of the
optical light arises from a single, dominant elliptical and yet the X-ray gas has
an extent and luminosity characteristic of a bright galaxy group. These systems
may be ``fossil'' groups in which the member galaxies have merged into a single
galaxy. We propose to observe two low redshift, X-ray bright members of this
class, ESO5520200 and NGC4936. We will determine baryon fractions, mass-to-light
ratios, and mass and abundance distributions to test if these systems are either
``fossil'' groups or a new optically ``dim'' class. By studying sharp surface
brightness ``edges'', Chandra's high angular resolution will allow us to catch
galaxies in the act of merging and measure gas motions and magnetic field
strengths.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
04:54:52.20 -18:06:56.00 ESO5520200 ACIS-I NONE 26.00
===================================================================================
Proposal Number: 03800131
Proposal Title: THE Z=1.786 CLUSTER AROUND 3C294
PI: ANDREW FABIAN
Subject Category: CLUSTERS OF GALAXIES
Abstract: With a 19.5 ks Chandra exposure we have imaged the intracluster medium
around the radio galaxy 3C294 at redshift z=1.786. The temperature of the gas is
5 +/- 1.5 keV. We propose here to observe the cluster for ten times longer in
order to determine the temperature to within 0.5 keV, measure the metallicity to
0.2 solar, and search for any large temperature gradient in the gas - the
temperature profile may be similar to that in nearby clusters with high surface
brightness and decrease inward. We shall also measure the X-ray spectrum of the
emission from the (highly absorbed) central active galaxy and hotspots. The 3C294
cluster is at a redshift twice that of any other known cluster for which such
precise measurements are likely to be obtained.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
14:06:44.10 +34:11:24.80 3C294 ACIS-S NONE 75.00
14:06:44.10 +34:11:24.80 3C294 ACIS-S NONE 125.00
===================================================================================
Proposal Number: 03800269
Proposal Title: A SEARCH FOR X-RAY EMISSION FROM A PROTO-CLUSTER AT Z=3.8
PI: CALEB SCHARF
Subject Category: CLUSTERS OF GALAXIES
Abstract: Structure formation theories predict that massive galaxies at high-z
should act as signposts to high-density environments, which evolve into the cores
of rich clusters. These regions contain over-densities of young galaxies,
including dusty, interaction-driven starbursts - the progenitors of massive
ellipticals. Submm observations can identify these systems. Our submm survey
around the z=3.8 radio galaxy, 4C41.17, reveals a clear excess of super-luminous
galaxies, consistent with the star formation rate needed to form a massive galaxy
in 10^8 years. We propose searching for the expected X-ray emission from this
collapsed structure, placing stringent emission limits on the submm galaxies, and
evaluating the obscured AGN and star formation contributions to their prodigious
luminosities.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
06:50:52.10 +41:30:30.80 4C41.17 ACIS-S NONE 70.00
06:50:52.10 +41:30:30.80 4C41.17 ACIS-S NONE 80.00
===================================================================================
Proposal Number: 03800286
Proposal Title: A DETAILED STUDY OF THE CORE OF THE PERSEUS CLUSTER
PI: ANDREW FABIAN
Subject Category: CLUSTERS OF GALAXIES
Abstract: We request a deep 200 ks observation of the Perseus cluster core. The
Perseus cluster is the brightest cluster in the X-ray sky. The Chandra view of
the core of the Perseus cluster offers the unique opportunity to study the
interaction between the radio source and the intracluster gas on scales matching
the intensity gradients in the interface. The proposed observations will increase
our effective ACIS-S exposure by a factor 6-8 so that we can study the detailed
properties of the X-ray gas, such as temperature, metallicity and multiphase
character, on scales as small as 3 arcsec (1.5\,h$_{50}^{-1}$ kpc). In addition,
we request a further 10 ks observation in fast readout mode of the nucleus to
measure its spectrum without the effect of pile-up.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
03:19:47.60 +41:30:37.00 ABELL 426 ACIS-S NONE 5.00
03:19:47.60 +41:30:37.00 ABELL 426 ACIS-S NONE 96.50
03:19:47.60 +41:30:37.00 ABELL 426 ACIS-S NONE 97.00
===================================================================================
Proposal Number: 03800338
Proposal Title: CLUSTER DARK MATTER ON THE SMALLEST SCALES
PI: DAVID BUOTE
Subject Category: CLUSTERS OF GALAXIES
Abstract: We propose to observe the cluster A2589 for 15ks with ACIS-S to measure
the slope of its dark matter density profile at the smallest possible radii.
A2589 is an ideal target for analysis of its core dark matter profile because it
is bright, nearby (z=0.042), has a smooth, relaxed morphology, and does not
possess a central radio source. Our proposed observation of A2589 will provide an
important test of theories of dark matter and cosmology at the smallest fraction
of a virial radius (0.010r_vir) to date.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
23:23:57.20 +16:46:43.00 A2589 ACIS-S NONE 15.00
===================================================================================
Proposal Number: 03800400
Proposal Title: COMPLEX CLUSTERS: MERGERS AND NARROW ANGLE TAILED RADIO SOURCES
PI: WILLIAM FORMAN
Subject Category: CLUSTERS OF GALAXIES
Abstract: We propose deep ACIS observations of two nearby clusters, A514 and
A2147, both of whose X-ray emission show unusually complex structures, that are
likely related to ongoing mergers. Since both are nearby, Chandra's angular
resolution will allow these structures to be studied with unprecedented detail.
In particular for A2147, we will determine if the sharp ``edge'' in its surface
brightness is due to a merger or to the motion of a central gas cloud in the
cluster ICM. We will map the temperature, as well as the density, across the
edge. The cluster A514 has head-tail radio sources, for which we plan to
investigate if a cluster-subcluster merger, rather than the galaxies own motion
through the intracluster medium, is responsible for bending the tails.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:02:07.20 +15:57:36.00 ABELL 2147 ACIS-I NONE 20.00
===================================================================================
Proposal Number: 03800443
Proposal Title: THE X-RAY STRUCTURE OF OLD, HIGH LUMINOSITY FOSSIL GALAXY GROUPS
PI: LAURENCE JONES
Subject Category: CLUSTERS OF GALAXIES
Abstract: A class of `fossil' groups has been discovered. Most L* galaxies in
these groups have merged into a normal, relaxed, giant elliptical galaxy. Fossil
groups thus appear to be very old. They represent an end-point of galaxy merging
and may be the evolutionary link between compact groups and giant elliptical
galaxies. We propose an ACIS study of these old groups to (a) study the
environment of giant elliptical formation and (b) to understand their high X-ray
luminosities (Lx). Their properties have important implications for the impact of
preheating at early epochs and the merger origin of giant ellipticals. Here we
propose to study a sample of high Lx systems: accompanying proposals are for a
single high Lx system (PI Jones), and nearby low Lx systems (PI Ponman).
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:56:03.40 +25:56:48.00 RXJ1256.0+2556 ACIS-S NONE 28.00
13:31:30.20 +11:08:03.00 RXJ1331.5+1108 ACIS-S NONE 31.00
15:52:12.50 +20:13:32.00 RXJ1552.2+2013 ACIS-S NONE 15.00
===================================================================================
Proposal Number: 03800470
Proposal Title: EARLY-TYPE GALAXIES IN GROUPS: STRIPPING AND STIFLING
PI: TREVOR PONMAN
Subject Category: CLUSTERS OF GALAXIES
Abstract: Isolated early-type galaxies are rare, and it appears that most
non-dwarf ellipticals form within groups, though some of these are later
incorporated into clusters. An understanding of the formation and evolution of
early-type galaxies requires a study of the way in which they are affected by the
group environment. Gas and dark matter can be stripped from galaxies, or
conversely surrounding intergalactic gas can stifle galaxy winds, leading to
enhanced gas retention. Our most recent ROSAT studies show that much previous
work on the X-ray properties of early-type galaxies has been confused by
inclusion of cooling flows focussed on the brightest group galaxies, which are
anomalously bright. We propose to study the X-ray components of a sample of
normal early-type galaxies in groups.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
10:00:21.80 -19:38:60.00 HCG 42 ACIS-S NONE 35.00
13:29:25.00 +11:44:30.00 NGC 5171 ACIS-S NONE 35.00
===================================================================================
Proposal Number: 03800474
Proposal Title: THE ASSEMBLY OF GALAXY GROUPS
PI: TREVOR PONMAN
Subject Category: CLUSTERS OF GALAXIES
Abstract: The most interesting phase in the evolution of a galaxy group is the
virialisation stage, at which the infall velocities of the galaxies are
randomised and the interstellar gas compressed and heated. The violently
fluctuating environment experienced by galaxies during this phase may have
long-lasting effects on their properties. Such virialising groups appear to be
quite rare, since the phase is transient, but we have identified three strong
candidates from an extensive study of groups with ROSAT. We propose to obtain
high quality spectral images of these with ACIS in order to study the way in
which the intergalactic medium is heated, and the effects of strong interactions
on galaxy properties.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:10:10.80 -37:33:23.00 NGC 3557 ACIS-I NONE 40.00
===================================================================================
Proposal Number: 03800488
Proposal Title: FOSSIL GROUPS IN THE LOCAL UNIVERSE
PI: TREVOR PONMAN
Subject Category: CLUSTERS OF GALAXIES
Abstract: Fossil groups are believed to be rare examples of galaxy systems which
collapsed at an early epoch, but have not yet been incorporated into clusters. If
this idea is correct, then they offer us a direct view of the first generation of
galaxy groups, undisturbed by subsequent merging. A direct test of this idea is
available from the shape of their dark matter distribution, which should be
strongly peaked. We have located the closest fossil groups in the Universe, and
propose to image them at high resolution with ACIS-S, in order to map the core of
the potential, and to study the cooling and metallicity of some of the least
disturbed gas in existence.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:51:48.90 +23:04:19.00 NGC 6482 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03800489
Proposal Title: GALAXY WAKES: THE FIRST SAMPLES
PI: TREVOR PONMAN
Subject Category: CLUSTERS OF GALAXIES
Abstract: Wakes generated as galaxies move through hot intracluster gas are
important in their own right, since stripping and accretion can have profound
effects on galaxy evolution. Wakes also provide valuable diagnostics of galaxy
properties and cluster dynamics. Previous X-ray observatories have been able to
study only a small number of especially bright and nearby galaxy wakes. With
Chandra, we have the possibility for the first time, of imaging a whole sample of
wakes within a single cluster, allowing us to examine their properties and
scaling relations. We have chosen two clusters with optimal temperatures and
distances but strongly contrasting morphologies: A160 is a relaxed cluster,
whilst A194 is currently merging. We expect to detect at least seven wakes in
each system.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:13:05.00 +15:29:48.00 ABELL 160 ACIS-I NONE 60.00
===================================================================================
Proposal Number: 03800498
Proposal Title: THE PUZZLING DUMB-BELL GALAXY NDC 4782/3: GALACTIC WAKES VERSUS
BENT JETS
PI: IRINI SAKELLIOU
Subject Category: CLUSTERS OF GALAXIES
Abstract: Galactic wakes and bent radio jets are the only means to disclose the
motion of galaxies on the sky: in combination with the X-ray and optical
properties of their surroundings they provide accurate measurements of the
cluster's gravitational potential, and its dynamical state. It is therefore very
alarming when one finds a system in which the wakes and bent jets disagree. We
propose to study this puzzling system: the dumb-bell galaxy NGC 4782/3. The
Chandra observation will enable us to disclose the fine structure and spectral
properties of the small-scale wakes and compare them with our simulations. We
will also be able to assess the bending mechanisms for the radio jets, and
finally establish the universality of one (or both) methods in unveiling the
motion of galaxies.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:54:36.00 -12:33:50.00 NGC 4782/3 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03800519
Proposal Title: CHANDRA OBSERVATIONS OF A Z=0.84 GALAXY CLUSTER AND ITS CENTRAL
HST QSO
PI: ROBERT SCHMIDT
Subject Category: CLUSTERS OF GALAXIES
Abstract: We request 20ks of Chandra observations of the galaxy cluster around
the z=0.84 quasar NVSS J003942-352803. The cluster was discovered in the course
of an imaging program at the ESO NTT carried out to study the connection between
Ly-alpha absorbers and galaxies in the field of intermediate-redshift (z~1) pairs
of quasars. HST-STIS spectra of the two quasars in the field reveal several
Ly-alpha absorbers around the quasar redshift of z=0.84. Chandra's superb spatial
resolution will be able to separate the X-ray emission of the quasar from the
X-ray emission of the galaxy cluster. By combining our STIS spectra with the
proposed Chandra observations we will be able to probe both the warm gas in the
UV, and the hot gas in the X-rays.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:39:42.44 -35:28:01.00 Q0037-3544 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03800533
Proposal Title: THE ORIGIN OF X-RAY EMISSION FROM LOW VELOCITY DISPERSION GROUPS
PI: TREVOR PONMAN
Subject Category: CLUSTERS OF GALAXIES
Abstract: Low velocity dispersion ($\sigma$) groups have shallow potentials, and
should retain rather little hot gas if the intergalactic medium has been
preheated during the process of galaxy formation, as has been suggested recently.
However, some groups with low $\sigma$ have X-ray luminosities so high, that the
$L$:$\sigma$ relation is observed to be {\it flatter} in groups than in clusters.
If this `excess' luminosity is truly diffuse gas, then the preheating model is in
serious difficulty. Alternatively, there could be new sources of X-ray emission
in these groups such as intergalactic shocks, which may be related to their
evolutionary state. We propose to image three of the most extreme low
$\sigma$/high $L_X$ groups with ACIS to find out.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:24:43.20 +38:45:36.00 NGC 3665 GROUP ACIS-I NONE 20.00
===================================================================================
Proposal Number: 03800536
Proposal Title: THE X-RAY STRUCTURE OF THE PROTOTYPE FOSSIL GROUP
PI: LAURENCE JONES
Subject Category: CLUSTERS OF GALAXIES
Abstract: We discovered the first `fossil' group, which contains a normal,
relaxed giant elliptical galaxy but almost no L* galaxies. It appears to be very
old, and may represent an end-point of galaxy merging. We propose an ACIS study
of the prototype fossil group to (a) study the environment of giant elliptical
formation and (b) to understand the unusual properties: a very high X-ray
luminosity for the temperature, and a remarkably elongated X-ray surface
brightness, indicative of a very anisotropic dark matter distribution. These
properties have important implications for the impact of preheating at early
epochs and the formation of structures within dark matter filaments. Accompanying
proposals are for a sample of high Lx fossil groups (PI Jones), and nearby, low
Lx fossil groups (PI Ponman)
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
13:40:32.80 +40:17:40.00 RXJ1340.6+4018 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03800537
Proposal Title: RXJ1720.1+2638: A NEARLY RELAXED CLUSTER WITH A FAST MOVING
CORE?
PI: PASQUALE MAZZOTTA
Subject Category: CLUSTERS OF GALAXIES
Abstract: Observed with previous X-ray missions, RXJ1720.1+2638 looks like the
prototype of a "relaxed cluster of galaxies". The cluster appears azimuthally
symmetric and the X-ray brightness peak coincides with the cluster central
galaxy. Thanks to its unprecedented spatial resolution, the Chandra observation
of this cluster shows a far more complex structure. In particular it shows two
X-ray features, on the opposite sides of the X-ray peak, that strongly indicate
motion of the cluster core. Because of the low exposure of the previous
observation several issues relative to the cluster formation and evolution are
answered. We propose a 52ks ASCI-I observation to study the details of the dual
structure in the gravitational potential of this cluster.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:20:09.91 +26:37:30.00 RXJ1720.1+2638 ACIS-I NONE 25.00
17:20:09.91 +26:37:30.00 RXJ1720.1+2638 ACIS-I NONE 27.00
===================================================================================
Proposal Number: 03800587
Proposal Title: ANATOMY OF THE X-RAY GROUP NGC 5044
PI: STEVEN KAHN
Subject Category: CLUSTERS OF GALAXIES
Abstract: We propose a 150 ks observation of the brightest X-ray group of
galaxies NGC 5044. By using the ACIS-S+HETG instrument, we will obtain a fully
resolved zero-order image, large-scale images of some emission lines, and a high
resolution spectrum of the core of the group. We expect to study a low
temperature homogenous cooling flow in detail, measure the distribution of oxygen
and iron throughout the group, map the dark matter potential and baryon fraction,
and examine the apparent cooling flow wake. We argue that some of the unsolved
problems in X-ray clusters can best be studied with an X-ray group.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
13:15:24.10 -16:23:06.00 NGC 5044 ACIS-S HETG 60.00
13:15:24.10 -16:23:06.00 NGC 5044 ACIS-S HETG 90.00
===================================================================================
Proposal Number: 03800590
Proposal Title: DETECTION OF HIGH REDSHIFT CLUSTER OF GALAXIES AROUND 3CR184
PI: TATEHIRO MIHARA
Subject Category: CLUSTERS OF GALAXIES
Abstract: This proposal is to separate the cluster gas and AGN components in the
high redshift cluster of galaxies of 3CR184. ASCA observation of 3CR184 has
suggested the existence of the large cluster of galaxies and/or AGN. The good
spatial resolution of Chandra is the only way to separate the two components, and
to prove the existence of a large cluster of galaxies at $z=1$. The flux and
metal abundance of high redshift clusters of galaxies are particularly important
to understand the evolution of clusters and the structure formation in the
universe.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
07:39:24.50 +70:23:10.90 3CR184 CLUSTER ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03800599
Proposal Title: A SEARCH FOR SMALL-SCALE STRUCTURE IN THE RASSCALS GALAXY GROUPS
PI: MARGARET GELLER
Subject Category: CLUSTERS OF GALAXIES
Abstract: Chandra has the necessary resolution to pick out small-scale structure
within the ROSAT All Sky Survey---Center for Astrophysics Loose Systems
(RASSCALS). This catalog of 260 nearby galaxy groups contains several objects
that are too X-ray luminous for their small (< 150 km/s) velocity dispersions.
The excess emission could be due to a central cooling flow or to embedded sources
similar to those seen in rich clusters such as Abell 2256 and 3C295. We propose
to use the ACIS-I to observe the two RASSCALS with the lowest dispersions (60 +/-
18 and 80 +/- 27 km/s) for a total of 70 ksec. Besides finding density
enhancements in the gas, the observations can reveal the temperature and
metallicity structures of these very low mass systems of galaxies.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
09:33:27.10 +34:03:02.00 NRGB045 ACIS-I NONE 35.00
===================================================================================
Proposal Number: 03800610
Proposal Title: THE CLUSTER ENVIRONMENTS OF OLD GALAXIES IN QUASAR FIELDS AT Z ~
1.5
PI: ALAN STOCKTON
Subject Category: CLUSTERS OF GALAXIES
Abstract: Current direct X-ray surveys for clusters of galaxies find essentially
no objects at z > 1. One can seek higher-redshift clusters in pointed
observations of radio source fields, but powerful radio sources are found not
only in rich clusters, but in a wide range of environments. We propose that one
can "stack the deck" by selecting radio-loud QSO fields at high redshift that
also show galaxies at the quasar redshift that both are luminous and formed
virtually their entire stellar populations early in the history of the Universe.
Such a selection favors regions where galaxy evolution has proceeded most
rapidly, and thus likely the regions of strongest overdensity. We propose to
investigate the X-ray properties of 4 quasar fields for which we have identified
such galaxies.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:48:24.40 +38:54:05.00 TXS 0145+386 FIELD ACIS-I NONE 63.00
16:25:14.40 +15:45:22.00 4C 15.55 FIELD ACIS-I NONE 52.00
===================================================================================
Proposal Number: 03800615
Proposal Title: A STUDY OF MERGER SIGNATURES IN NEARBY GALAXY CLUSTERS:
CONSTRAINTS ON ICM PHYSICS AND STRUCTURE FORMATION SCENARIOS
PI: JOSEPH MOHR
Subject Category: CLUSTERS OF GALAXIES
Abstract: High angular resolution imaging and spectroscopy with Chandra has led
to the discovery of arcsecond-scale discontinuities in the projected temperature
and surface brightness maps of the merging clusters A2142 and A3667. We propose
to build on these results by observing three other nearby clusters currently
undergoing major mergers. Observations of shock features in these clusters will
provide important insights into the physical state of the intracluster medium.
Together with archival targets, these three new clusters will allow us to measure
the range of shock strengths in merging systems and compare those measurements
directly to hydro simulations of cluster evolution in various structure formation
scenarios.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
02:57:55.20 +13:02:04.00 ABELL 399 ACIS-I NONE 50.00
19:21:12.00 +43:56:43.70 ABELL 2319 ACIS-I NONE 15.00
===================================================================================
Proposal Number: 03800624
Proposal Title: REHEATING IN COOLING FLOWS
PI: TREVOR PONMAN
Subject Category: CLUSTERS OF GALAXIES
Abstract: One of the most interesting early discoveries of Chandra and XMM, is
the lack of really cool gas in cluster cooling flows. Since many cooling flows
contain embedded radio galaxies, an attractive explanation holds that cooling
flows fuel central AGN, which inject energy, reducing the gas cooling rate.
Cooling flows are self-regulating. The same phenomenon has been seen in one of
the first galaxy groups to be studied by Chandra. HCG~62 shows both a lack of
cool ($<0.5$ keV) gas, and the unexpected presence of two lobe-like structures,
probably related to the presence of a central radio source. We propose to target
two bright group cooling flows known to contain {\it no} radio source. Comparison
between these systems and HCG~62 will provide a conclusive test of the AGN
reheating hypothesis.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:23:06.70 +10:37:16.30 NGC 4325 GROUP ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03800625
Proposal Title: RESOLVING THE HIGH TEMPERATURE REGION BETWEEN THE SUBCLUSTERS OF
ABELL 115 AND INTRACLUSTER MEDIUM INTERACTIONS OF 3C 28
PI: HENRIC KRAWCZYNSKI
Subject Category: CLUSTERS OF GALAXIES
Abstract: We propose a 50 ksec observation of the galaxy cluster Abell 115 with
the ACIS I detector. This very X-ray luminous cluster is a unique laboratory to
study shock heated gas between two merging cluster components. Chandra's combined
imaging and spectroscopic capabilities will make it possible to extract highly
resolved maps of the Intracluster Medium (ICM) density, temperature, and chemical
composition. Furthermore, it will be possible to study in detail the interaction
of the ICM with the powerful radio galaxy 3C 28.0, the Brightest Cluster Galaxy.
The ROSAT HRI image clearly shows extended structure which is correlated with the
lobes of the radio source and which will be resolved by Chandra.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:55:46.60 +26:24:37.30 3C 28.0 ACIS-I NONE 50.00
===================================================================================
Proposal Number: 03800689
Proposal Title: STUDY OF METAL ENRICHMENT PROCESSES AROUND THE CENTRAL GALAXY IN
THE MKW4 CLUSTER
PI: YASUSHI FUKAZAWA
Subject Category: CLUSTERS OF GALAXIES
Abstract: ASCA revealed that many clusters of galaxies exhibit a metal abundance
increment at the center of clusters of galaxies. BeppoSAX, Chandra, and Newton
have also confirmed it. The mass and abundance ratio of excess metals indicate
that these were produced by recent SNe Ia in the central galaxies and ejected
into the intracluster space. Therefore, we are just seeing the metal ejection
from galaxies. Here, we propose to observe a poor cluster of galaxies MKW4 with
high stellar to ICM mass ratio at the cluster center, in order to map the Fe with
$4''\times4''$ resolution and study the processes of metal enrichments in the
intracluster medium.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:04:26.70 +01:53:43.30 MKW4 ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03800699
Proposal Title: A DETAILED STUDY OF THE SUPERCLUSTER SC1120-1202 AT $Z$=0.43
PI: ANTHONY GONZALEZ
Subject Category: CLUSTERS OF GALAXIES
Abstract: We propose to use ACIS-I to observe the recently discovered
supercluster SC 1120-1202 at $z=0.43$. This region is extreme within the 130 sq.
degrees probed by the Las Campanas Distant Cluster Survey (LCDCS), is compact
(containing four clusters within a single ACIS field-of-view), and includes three
clusters with expected temperatures in excess of 5 keV. In an effort to study
this unique environment, we will use our proposed observations to 1) identify
additional collapsed objects within the supercluster2) detect shocks and
distortions in the X-ray isophotes indicative of mergers and cluster
interactions, and 3) measure the properties (metallicity and mass) of the
gravitationally collapsed objects to determine whether this extreme environment
affects the clusters and groups within.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:20:09.00 -12:01:58.00 SC 1120-1202 ACIS-I NONE 70.00
===================================================================================
Proposal Number: 03800748
Proposal Title: SEARCH FOR HOT PRIMORDAL GAS IN A FAILED CLUSTER OF GALAXIES
CANDIDATE 0806+20
PI: KIYOSHI HAYASHIDA
Subject Category: CLUSTERS OF GALAXIES
Abstract: Failed cluster of galaxies is a hypothetical object of large gas cloud
of which collapse time exceeds the Hubble time. Such cloud, if exists, failed to
form galaxies in it and should not have metal in it. 0806+20 is the prime
candidate of such objetct, extracted from the Einstein data base as an extended
source without optical counterpart. Although ASCA observation of this source did
not reveal spatial extenstion, ASCA X-ray spectrum is fitted with a power law or
thin thermal model, with a marginal detection of redshifted (z or 0.5-0.6) iron
line. No optical counterpart was detected with a limiting R mag of 24. From
these, 0806+20 may be 1) a distant (usual or failed) cluster, 2) a unusually
optically faint quasar. Chandra X-ray image will reveal which is the solution.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
08:09:08.00 +20:24:20.00 0806+20 ACIS-S NONE 5.00
===================================================================================
Proposal Number: 03800763
Proposal Title: HEAD-TAIL GALAXIES AS PROBES OF SUBSTRUCTURE IN THE PERSEUS
CLUSTER OF GALAXIES
PI: DIAB JERIUS
Subject Category: CLUSTERS OF GALAXIES
Abstract: Narrow angle tail (NAT) radio galaxies offer intriguing hints as to the
nature of the interaction of galaxies with the intra-cluster medium (ICM). They
frequent areas of enhanced X-ray emission in clusters of galaxies; there are
strong indications that ram pressure forces associated with merging subclusters
bend the galaxies' jets. We propose to observe two NAT galaxies in the Perseus
cluster, exploring their intrinsic X-ray emission and their interactions with the
cluster gas. Chandra's arcsecond resolution will permit direct comparisons of
X-ray and radio structures, the separation of galactic and ICM spectroscopic
signatures, and probes of the effects of merging subclusters on NAT morphology,
and thus the role of these galaxies as diagnostics of the underlying cluster
substructure.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
03:18:15.70 +41:51:28.00 NGC 1265 ACIS-S NONE 95.00
===================================================================================
Proposal Number: 03800797
Proposal Title: THE CORE STRUCTURE OF THE LOWEST REDSHIFT STRONG LENSING CLUSTER
PI: HARUYOSHI KATAYAMA
Subject Category: CLUSTERS OF GALAXIES
Abstract: We propose a Chandra ACIS-S observation of the cluster of galaxies
A2124. The redshift of A2124 is z=0.066, which is the lowest among the clusters
showing strong lensing arcs. The strong lensing arc of A2124 is located at about
27$''$($=$46h$^{-1}$kpc) from the cluster center. Chandra observations will
provide the X-ray emission profile and the gas temperature in the core region of
the cluster for the first time and will also provide the gravitational mass
profile, under the assumption of hydrostatic equilibrium. Because the projected
mass of the matter within the arc is determined from the arc radius, we will be
able to examine and construct the detailed mass profile of the cluster. A2124
provides us with an exceptional opportunity for such study.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
15:45:00.00 +36:06:33.00 ABELL 2124 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03800798
Proposal Title: RICH, OPTICALLY-SELECTED GALAXY CLUSTERS AT Z~1 FROM THE RCS
SURVEY
PI: ERICA ELLINGSON
Subject Category: CLUSTERS OF GALAXIES
Abstract: We propose deep ACIS-I observations of three rich clusters discovered
by the Red-sequence Cluster Survey (RCS) with redshifts 0.6 < z < 1.2. These
observations will allow us to address three important scientific goals: the
accurate calibration of the RCS mass function, a preliminary study of properties
of optically selected clusters at high redshift, and an investigation of
gravitational lensing by very high redshift clusters.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
14:16:59.80 +53:05:12.20 RCS1417+5305 ACIS-I NONE 65.00
14:19:12.10 +53:26:11.00 RCS1419+5326 ACIS-S NONE 10.00
16:20:10.00 +29:29:21.50 RCS1620+2929 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03800884
Proposal Title: CHANDRA OBSERVATIONS OF A GALAXY CLUSTER AT Z=1.11
PI: DANIEL STERN
Subject Category: CLUSTERS OF GALAXIES
Abstract: We propose a 45 ksec exposure with ACIS-I of the narrow-lined radio
galaxy MG0442+0202 at z=1.11 and its associated cluster, one of the most distant
galaxy clusters known. The system has been detected in archival ROSAT data, which
we argue is dominted by emission from hot intracluster gas. The spatial and
energy resolution of Chandra will be critical for these observations: we expect
to see unresolved X-ray emission from the AGN embedded within diffuse, soft X-ray
emission from the cluster ICM. Observations of the radio galaxy will provide
basic data for AGN unification schemes. Observations of the cluster ICM will
conclusively demonstrate the existence of a massive, bound structure and allow us
to probe the cosmologically-informative L-T relation at early cosmic epoch.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
04:42:23.70 +02:02:19.80 CL 0442+0202 ACIS-I NONE 45.00
===================================================================================
Proposal Number: 03800927
Proposal Title: THE INTRAGROUP MEDIUM IN X-RAY LUMINOUS GALAXY GROUPS: RADIO
SOURCES AND THE DISTRIBUTION OF HEAVY ELEMENTS
PI: JAN VRTILEK
Subject Category: CLUSTERS OF GALAXIES
Abstract: Most galaxies in the present-day Universe are in groups and poor
clusters. Groups are the building blocks from which clusters form, and they
accordingly occupy an important niche in the continuum between isolated galaxies
and rich clusters. We here propose to exploit the high X-ray brightnesses of
three selected groups with central radio sources to study the interactions
between the intragroup medium and the radio sources -- in particular, to
understand better the possible role of the radio sources in regulation of cooling
flows -- and to examine the metallicity distribution of the intragroup gas at a
level of detail not possible prior to the availability of Chandra's high angular
resolution.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
10:50:26.90 -12:50:26.00 SS2B153 ACIS-S NONE 31.00
===================================================================================
Proposal Number: 03800994
Proposal Title: OBSERVATION OF BCS CLUSTERS, SECOND SET
PI: LEON VANSPEYBROECK
Subject Category: CLUSTERS OF GALAXIES
Abstract: Observe these clusters to determine distances using the SZ effect.
Also, study cluster evolution
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
13:06:57.40 +46:32:42.00 A1682 ACIS-I NONE 10.00
17:20:09.60 +27:40:08.00 A2259 ACIS-I NONE 10.00
17:23:55.20 +85:53:24.00 A2294 ACIS-I NONE 10.00
22:00:54.50 +20:57:32.00 A2409 ACIS-I NONE 10.00
23:37:40.10 +00:16:33.00 A2631 ACIS-I NONE 10.00
===================================================================================
Proposal Number: 03800997
Proposal Title: OBSERVATION OF BCS CLUSTERS, FIRST SET
PI: LEON VANSPEYBROECK
Subject Category: CLUSTERS OF GALAXIES
Abstract: Observe these clusters to determine distances using the SZ effect.
Also, study cluster evolution
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:27:45.90 +26:16:25.00 RXJ0027.6+2616 ACIS-I NONE 10.00
00:37:05.30 +09:09:10.00 A68 ACIS-I NONE 10.00
===================================================================================
Proposal Number: 03800996
Proposal Title: OBSERVATION OF MACS CLUSTERS, 0.450.3
PI: HARALD EBELING
Subject Category: CLUSTERS OF GALAXIES
Abstract: We propose ACIS-I and HST observations of 30 distant and very X-ray
luminous clusters (z>0.3, Lx>1e45) detected in the MAssive Cluster Survey (MACS).
22 of these 30 are new discoveries. Our targets are the high-z counterparts of
the best-studied local systems and, combined with 4 others scheduled for
observation, form a statistical sample >10 times larger than any previous one in
this redshift and luminosity range. Chandra's unique capabilities will allow us
to obtain spatially resolved gas temperature and density maps to constrain both
the cosmological and physical parameters governing the evolution of the most
massive clusters at z<0.5. The proposed observations are complemented by
extensive groundbased follow-up studies of weak gravitational lensing, galaxy
dynamics and the SZ effect.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:11:42.90 -15:23:22.00 MACSJ0011.7-1523 ACIS-I NONE 22.00
00:35:26.10 -20:15:44.00 MACSJ0035.4-2015 ACIS-I NONE 22.00
00:47:21.60 -08:09:21.00 MACSJ0047.3-0810 ACIS-I NONE 14.00
01:52:32.60 -28:53:22.00 MACSJ0152.5-2852 ACIS-I NONE 18.00
01:59:49.30 -08:49:59.00 MACSJ0159.8-0849 ACIS-I NONE 18.00
02:42:35.90 -21:32:26.00 MACSJ0242.5-2132 ACIS-I NONE 12.00
02:57:41.70 -22:09:11.99 MACSJ0257.6-2209 ACIS-I NONE 20.00
03:08:56.00 +26:45:37.00 MACSJ0308.9+2645 ACIS-I NONE 25.00
04:04:33.20 +11:07:58.00 MACSJ0404.6+1109 ACIS-I NONE 24.00
04:17:34.70 -11:54:33.00 MACSJ0417.5-1154 ACIS-I NONE 12.00
04:29:36.10 -02:53:07.00 MACSJ0429.6-0253 ACIS-I NONE 24.00
05:20:42.00 -13:28:48.00 MACSJ0520.7-1328 ACIS-I NONE 20.00
05:47:01.50 -39:04:28.00 MACSJ0547.0-3904 ACIS-I NONE 22.00
09:49:51.80 +17:07:09.00 MACSJ0949.8+1708 ACIS-I NONE 15.00
11:15:51.90 +01:29:54.00 MACSJ1115.8+0129 ACIS-I NONE 16.00
11:31:54.20 -19:55:42.00 MACSJ1131.8-1955 ACIS-I NONE 15.00
12:06:12.20 -08:48:04.00 MACSJ1206.2-0847 ACIS-I NONE 24.00
13:20:08.50 +70:04:39.00 MACSJ1319.9+7003 ACIS-I NONE 20.00
14:27:39.50 -25:21:03.00 MACSJ1427.6-2521 ACIS-I NONE 17.00
17:20:16.90 +35:36:25.00 MACSJ1720.2+3536 ACIS-I NONE 21.00
17:31:40.00 +22:51:58.00 MACSJ1731.6+2252 ACIS-I NONE 21.00
19:31:49.70 -26:34:34.00 MACSJ1931.8-2634 ACIS-I NONE 14.00
20:49:55.90 -32:16:49.00 MACSJ2049.9-3217 ACIS-I NONE 24.00
22:11:46.00 -03:49:45.00 MACSJ2211.7-0349 ACIS-I NONE 18.00
22:28:33.90 +20:37:16.00 MACSJ2228.5+2036 ACIS-I NONE 21.00
22:29:45.40 -27:55:37.00 MACSJ2229.7-2755 ACIS-I NONE 17.00
22:45:04.80 +26:38:04.00 MACSJ2245.0+2637 ACIS-I NONE 17.00
23:11:33.30 +03:38:04.00 MACSJ2311.5+0338 ACIS-I NONE 14.00
===================================================================================
Proposal Number: 03800394
Proposal Title: REHEATING THE GAS IN CLUSTER COOLING FLOWS
PI: LAURENCE DAVID
Subject Category: CLUSTERS OF GALAXIES
Abstract: Some of the first results from Chandra show that the central regions of
cooling flow clusters are morphologically complex. Chandra and XMM-Newton also
find little spectroscopic evidence for cool gas as expected in clusters that were
previously thought to contain massive cooling flows. One possible resolution to
this problem is that the gas is shocked heated by a central radio source which
prevents the gas from cooling. To investigate this hypothesis, we propose to
observe the cooling flow clusters A576 and A2626. The central dominant galaxy in
these clusters are associated with small scale radio emission, which may indicate
that the nuclear activity was triggered recently and the shock front has not yet
propagated beyond the cooling flow region.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
07:21:29.30 +55:45:35.00 ABELL 576 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03801021
Proposal Title: MAPPING DARK MATTER IN A COLLING FLOW CLUSTER AND A DARK CLUMP
PI: GORDON GARMIRE
Subject Category: CLUSTERS OF GALAXIES
Abstract: We propose a 35 ks ACIS-I observation of the field of Abell 1942, a
relaxed, luminous (Lx ~ 1.e45 erg/s, 2-10 keV) cluster at z=0.22. We have two
objectives. We will measure the cluster's dark matter profile to within 50 kpc of
the cluster core, with the aim of constraining the cross-section for dark matter
self-interaction. We will also look for low-surface brightness X-ray emission
from an intriguing, dark (M/L > 450) mass concentration lying near Abell 1942 on
the sky which was recently discovered in a weak lensing study by Erben and
co-workers. Our failure to detect X-ray emission from the clump would rule out
its association with a poor group at the cluster redshift or with a moderately
luminous cluster at z=1.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
14:38:21.80 +03:36:25.00 ABELL 1942 AND CLUMP ACIS-I NONE 60.00
===================================================================================
Proposal Number: 03800097
Proposal Title: MAPPING DARK MATTER IN A COLLING FLOW CLUSTER AND A DARK CLUMP
PI: GORDON GARMIRE
Subject Category: CLUSTERS OF GALAXIES
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
13:26:31.07 +29:03:19.80 RCS1325+2858 ACIS-S NONE 31.50
13:26:31.07 +29:03:19.80 RCS1325+2858 ACIS-S NONE 45.00
***********************************************************************************
EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS
--------------------------------------------------
===================================================================================
Proposal Number: 03900164
Proposal Title: THE CHANDRA SURVEY OF THE HUBBLE DEEP FIELD NORTH AREA: A PUBLIC
RESOURCE FOR THE PRESENT AND FUTURE OF X-RAY ASTRONOMY
PI: WILLIAM BRANDT
Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS
Abstract: We propose to extend the Chandra deep survey of the HDF-N and its
vicinity. The ultimate goal is to obtain 5 Ms of coverage over the next 5 years;
currently we have 1 Ms coverage. Here we propose two public 500 ks observations.
This project will fulfill one of Chandra's central design goals and will be a
long-lasting legacy of Chandra, laying the groundwork for the next generation of
X-ray observatories. We should remain nearly photon limited for point-sources
near the aim point. We will study obscured and high-redshift AGN, starbursts,
normal galaxies, clusters, groups, and diffuse X-ray emission. The HDF-N field is
the ideal region for multiwavelength follow-up studies due to the enormous
database already in place. Our ACIS team expertise will be extensively utilized.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:36:49.40 +62:12:58.00 HDF-N ACIS-I NONE 50.00
12:36:49.40 +62:12:58.00 HDF-N ACIS-I NONE 67.00
12:36:49.40 +62:12:58.00 HDF-N ACIS-I NONE 90.00
12:36:49.40 +62:12:58.00 HDF-N ACIS-I NONE 126.70
12:36:49.40 +62:12:58.00 HDF-N ACIS-I NONE 166.70
12:36:49.40 +62:12:58.00 HDF-N ACIS-I NONE 166.70
12:36:49.40 +62:12:58.00 HDF-N ACIS-I NONE 166.70
12:36:49.40 +62:12:58.00 HDF-N ACIS-I NONE 166.70
===================================================================================
Proposal Number: 03900446
Proposal Title: A CHEAP COMPLETE WIDE BRIGHT SURVEY
PI: FABIO LA FRANCA
Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS
Abstract: We propose to observe with Chandra the 17 sources of the HELLAS (the
High Energy LLarge Area Survey from BeppoSAX) for which no obvious optical
counterpart was possible to find. With the proposed 57 Ksec of observations we
will end up with a total complete sample of 81 sources covering an area 55 deg^2
down ~7x10^-14 cgs. This will result in the largest complete wide field bright
hard X-ray survey available so far at these fluxes. The 17 sources are on average
harder than the total sample, and probably are either faint type 2 AGNs or the
new discovered X-ray emitting "normal" galaxies. This survey will be of great
interest to evolutionary studies, allowing a link at brighter fluxes with the
faint surveys at moment underway with Chandra.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
09:46:05.30 -14:02:59.00 H094605 ACIS-I NONE 2.50
09:46:32.80 -14:06:15.40 H094633 ACIS-I NONE 1.50
13:48:24.30 -30:25:47.00 H134824 ACIS-I NONE 1.50
13:55:55.70 +18:14:16.70 H135556 ACIS-I NONE 1.50
14:11:58.70 -03:07:02.00 H141159 ACIS-I NONE 1.50
16:26:57.10 +55:13:34.10 H162657 ACIS-I NONE 1.50
18:36:11.30 -65:07:19.90 H183611 ACIS-I NONE 1.50
22:03:00.50 -32:04:18.00 H220301 ACIS-I NONE 2.50
23:02:30.10 +08:37:06.00 H230230 ACIS-I NONE 2.50
23:02:36.20 +08:56:42.00 H230236 ACIS-I NONE 1.50
===================================================================================
Proposal Number: 03900462
Proposal Title: THE X-RAY UNIVERSE AT HIGH REDSHIFT
PI: KIRPAL NANDRA
Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS
Abstract: Deep optical surveys show a population of star-forming galaxies at high
z. These are probably in the process of formation, evolving into local
ellipticals and spirals. X-ray observations can determine the influence of AGN
activity on their evolution, and gives an independent measure of the star
formation rate. We propose a 200ks observation of the Groth-Westphal Survey area
to determine the X-ray emission and AGN content of galaxies out to z=3. This is a
very intensively studied region of the sky; notably for our purposes it contains
over 200 spectroscopically confirmed Lyman Break Galaxies. It is targeted for
numerous future deep surveys (e.g. SIRTF, GALEX) and a huge spectroscopic survey
by the DEEP consortium, offering enormous archival potential beyond our own
exploitation of the data.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
14:17:43.60 +52:28:41.20 GROTH-WESTPHAL FIELD ACIS-I NONE 30.00
14:17:43.60 +52:28:41.20 GROTH-WESTPHAL FIELD ACIS-I NONE 84.68
14:17:43.60 +52:28:41.20 GROTH-WESTPHAL FIELD ACIS-I NONE 85.32
===================================================================================
Proposal Number: 03900496
Proposal Title: A COMBINED CHANDRA/XMM ATTACK ON THE ASTROPHYSICS OF THE HARD
X-RAY BACKGROUND.
PI: IAN MCHARDY
Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS
Abstract: We propose a Chandra survey of the minimum exposure to provide
arcsecond positions and unambiguous identifications for the ~175 sources with
high quality X-ray spectra in our second 200ksec XMM survey, completing a
programme begun in Chandra AO2. We need the 350 sources from both XMM/Chandra
surveys for evolutionary studies. The powerful combination of XMM spectra with
CHANDRA positions, with extensive observations in other bands, enables us to
understand the astrophysics of the hard X-ray background; ie do the contributors
have absorbed, or intrinsically flat, spectra? how do QSO spectra, including
black body components, evolve? what is the X-ray emission mechanism of optically
inactive galaxies and of narrow emission line galaxies? which non-gravitational
source heated galaxy groups?
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:45:02.38 -04:38:35.21 XMM 1HR - FIELD 2 ACIS-I NONE 30.00
01:45:49.63 -04:32:24.26 XMM 1HR - FIELD 1 ACIS-I NONE 30.00
===================================================================================
Proposal Number: 03900608
Proposal Title: THE SHEEP SURVEY: WHAT KIND OF OBJECTS MAKE THE X-RAY
BACKGROUND?
PI: KIRPAL NANDRA
Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS
Abstract: Chandra deep surveys have detected the discrete source populations that
make up the X-ray background, but the objects are too faint to characterize in
detail. Much brighter example have been found in our large area 5-10 keV survey
with ASCA (SHEEP). Many are difficult to identify optically, however, given the
large positional uncertainty. We propose to use Chandra to determine unambiguous
optical counterparts with 5ks snapshots of the 35 sources not detected by ROSAT.
We further propose to spectroscopically identify these counterparts using the
NOAO 4m telescopes. Our scientific goals are to determine the nature of the new
populations making up the X-ray background, and revisit the phenomenology of AGN
in the light of these new classes of object.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:43:47.00 +00:54:36.00 AX J0043.7+0054 ACIS-S NONE 5.00
00:58:43.00 +30:19:45.00 AX J0058.7+3019 ACIS-S NONE 5.00
01:40:08.10 +06:28:05.80 AX J0140.1+0628 ACIS-S NONE 5.00
01:44:54.20 -03:45:19.00 AX J0144.9-0345 ACIS-S NONE 5.00
01:46:15.00 -03:54:53.00 AX J0146.2-0354 ACIS-S NONE 5.00
03:35:16.70 -15:05:55.00 AX J0335.2-1505 ACIS-S NONE 5.00
03:35:40.40 -36:09:18.00 AX J0335.6-3609 ACIS-S NONE 5.00
04:40:02.90 -45:34:59.00 AX J0440.0-4534 ACIS-S NONE 5.00
08:36:13.90 +55:38:48.00 AX J0836.2+5538 ACIS-S NONE 5.00
08:36:36.20 +55:29:42.00 AX J0836.6+5529 ACIS-S NONE 5.00
08:44:50.10 +50:04:37.00 AX J0844.8+5004 ACIS-S NONE 5.00
10:35:10.10 +39:38:09.00 AX J1035.1+3938 ACIS-S NONE 5.00
11:07:00.20 -11:50:45.00 AX J1107.0-1150 ACIS-S NONE 5.00
11:15:24.10 +53:08:07.00 AX J1115.4+5308 ACIS-S NONE 5.00
12:18:40.10 +05:46:17.00 AX J1218.6+0546 ACIS-S NONE 5.00
12:30:51.90 +14:33:23.00 AX J1230.8+1433 ACIS-S NONE 5.00
12:31:33.50 +14:22:50.00 AX J1231.5+1422 ACIS-S NONE 5.00
12:43:50.00 +13:05:17.30 AX J1243.8+1305 ACIS-S NONE 5.00
13:25:50.00 -39:20:40.00 AX J1325.8-3920 ACIS-S NONE 5.00
13:54:01.00 +33:46:27.00 AX J1354.0+3346 ACIS-S NONE 5.00
14:06:08.30 +22:33:02.00 AX J1406.1+2233 ACIS-S NONE 5.00
14:06:13.60 +22:28:22.00 AX J1406.2+2228 ACIS-S NONE 5.00
14:25:13.70 +23:03:19.00 AX J1425.2+2303 ACIS-S NONE 5.00
15:00:09.20 +33:25:06.00 AX J1500.1+3325 ACIS-S NONE 5.00
15:11:43.60 +07:58:54.00 AX J1511.7+0758 ACIS-S NONE 5.00
15:11:47.90 +57:02:42.00 AX J1511.7+5702 ACIS-S NONE 5.00
15:12:04.40 +57:08:05.00 AX J1512.0+5708 ACIS-S NONE 5.00
15:31:51.10 +24:14:43.00 AX J1531.8+2414 ACIS-S NONE 5.00
15:31:56.50 +24:20:22.00 AX J1531.9+2420 ACIS-S NONE 5.00
15:32:19.10 +24:01:13.00 AX J1532.3+2401 ACIS-S NONE 5.00
15:32:33.10 +24:15:13.00 AX J1532.5+2415 ACIS-S NONE 5.00
15:45:13.60 +48:55:06.00 AX J1545.2+4855 ACIS-S NONE 5.00
16:17:05.90 +35:06:38.00 AX J1617.0+3506 ACIS-S NONE 5.00
16:18:10.70 +34:59:46.00 AX J1618.1+3459 ACIS-S NONE 5.00
20:02:47.10 -33:00:15.00 AX J2002.7-3300 ACIS-S NONE 5.00
===================================================================================
Proposal Number: 03900812
Proposal Title: WIDE-FIELD CHANDRA SURVEY OF THE LOCKMAN HOLE-NORTHWEST
PI: AMY BARGER
Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS
Abstract: We propose a wide-field Chandra survey of a contiguous region in the
Lockman Hole-Northwest (LH-NW). The two complementary science goals of our
proposed observations are to determine the overlap of the hard X-ray and
far-infrared (FIR) populations and to determine the correlation function of X-ray
selected AGN. The advantages of the LH-NW are its extremely low neutral hydrogen
column density, existing deep FIR observations with ISO, scheduled Legacy Program
observations with SIRTF, and 160 Ks of Chandra GTO observations. We propose to
waive any proprietary period to provide the community with immediate access to
this valuable dataset.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
10:32:06.00 +57:37:24.99 LH-NW-4 ACIS-I NONE 40.00
10:32:46.00 +57:46:24.99 LH-NW-7 ACIS-I NONE 40.00
10:33:22.00 +57:55:25.00 LH-NW-6 ACIS-I NONE 40.00
10:34:02.10 +57:28:25.00 LH-NW-5 ACIS-I NONE 40.00
10:34:38.00 +57:55:25.00 LH-NW-8 ACIS-I NONE 40.00
10:35:16.00 +57:46:24.99 LH-NW-9 ACIS-I NONE 40.00
===================================================================================
Proposal Number: 03900836
Proposal Title: CHANDRA OBSERVATIONS OF OPTICALLY FAINT SOURCES DISCOVERED WITH
ASCA
PI: YOSHIHIRO UEDA
Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS
Abstract: The origin of the Cosmic X-ray background (CXB) has been one of the key
issues of X-ray astronomy. We propose Chandra observations of 5 selected
unidentified X-ray sources with fluxes larger than 3 x 10^(-13) erg/cm2/s
discovered by the serendipitous source survey project with ASCA. They do not have
any optical counterparts with the R band magnitude brighter than 19.5 and could
be a luminous class of type-2 QSOs. For the determination of the nature of the
2-10 keV source population excellent X-ray positions are absolutely vital to
obtain reliable identifications, in particular if one does not know a priori the
nature of the optical objects.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:33:31.70 -21:39:54.40 1AXG J003331-2139 ACIS-I NONE 3.00
01:09:52.20 -12:52:58.10 1AXG J010952-1252 ACIS-I NONE 1.00
11:07:13.10 -18:39:51.50 1AXG J110713-1839 ACIS-I NONE 2.00
13:18:32.20 +32:59:14.30 AX J131832+3259 ACIS-I NONE 2.70
13:56:29.60 +77:24:42.80 1AXG J135629+7724 ACIS-I NONE 2.90
***********************************************************************************
GALACTIC DIFFUSE EMISSION AND SURVEYS
--------------------------------------------------
===================================================================================
Proposal Number: 03910054
Proposal Title: PROBING THE INTERSTELLAR MEDIUM: X-RAY ABSORPTION AT IRON AND
OXYGEN WITH GX 349+2
PI: CLAUDE CANIZARES
Subject Category: GALACTIC DIFFUSE EMISSION AND SURVEYS
Abstract: Photoelectic absorption of X-rays in neutral matter was based on atomic
absorption cross sections derived from optical constants which were largely
adequate to describe K-edge structure. Recent observations with Chandra in at
first glace fully compliant very recent laboratory measurements found significant
narrow structures in the Fe L, which clearly show that the currently in use Henke
optical contants are inadequat to descibe Fe L absorption, but also indicate
mixing with other molecular components. The latter is very much evident at
O-edges as well. We propose a high resolution survey of GX 349+2 to probe
absoption in the Fe and O region.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:05:44.50 -36:25:22.00 GX 349+2 ACIS-S HETG 35.00
===================================================================================
Proposal Number: 03910326
Proposal Title: X-RAY EMISSION MECHANISMS AND EVOLUTION OF SUPERBUBBLES
PI: SALLY OEY
Subject Category: GALACTIC DIFFUSE EMISSION AND SURVEYS
Abstract: We propose Chandra ACIS observations of four young superbubbles
generated by stellar winds and supernovae of OB associations in the Large
Magellanic Cloud. The imaging data will resolve the structure of the X-ray
emission, allowing us to discriminate between the three principal models for
superbubble X-ray emission. Since the X-ray luminosity is the most direct probe
of the superbubble energy budgets, these data will strongly constrain models for
superbubble evolution and resulting consequences for the multiphase ISM and
galaxy evolution.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
04:59:49.00 -70:10:28.00 DEM L50 ACIS-S NONE 40.00
05:22:17.00 -67:56:38.00 DEM L152 ACIS-S NONE 20.00
