Chandra X-Ray Observatory
	(CXC)

Accepted Cycle 14 Large / X-ray Visionary Proposals

Proposal NumberSubject CategoryPI NameTypeTime
(Ks)
Title
14200176STARS AND WDHuenemoerderLP450Wolf-Rayet Winds at High Spectral Resolution
14200631STARS AND WDCorcoranLP500Occultation Measurements of the Embedded Wind Shock Distribution in the Nearest Eclipsing O-star Binary
14200801STARS AND WDKastnerLP670COMPACT AND DIFFUSE X-RAY SOURCES IN THE YOUNGEST PLANETARY NEBULAE
14400870BH AND NS BINARIESZezasXVP1100The Small Magellanic Cloud - A Case Study of X-ray Populations at Low Metallicity
14500153SN, SNR AND ISOLATED NSRomaniXVP1300A Legacy Study of the Relativistic Shocks of PWNe
14500702SN, SNR AND ISOLATED NSSlaneLP375A Detailed Study of the Composite Supernova Remnant MSH 11-62
14500725SN, SNR AND ISOLATED NSReynoldsLP400G11.2-0.3: Core-Collapse Supernova Progenitors, Cosmic Rays, and Pulsar-Wind Nebulae
14500928SN, SNR AND ISOLATED NSKargaltsevLP500A comparative study of two outstanding pulsar tails
14700473ACTIVE GALAXIES AND QUASARSKochanekLP810ENERGY DEPENDENT X-RAY MICROLENSING AND THE STRUCTURE OF QUASARS
14700824ACTIVE GALAXIES AND QUASARSHaggardLP300Joint Chandra/XMM/EVLA Monitoring of the Gas Cloud G2 as it Encounters Sgr A*
14700854ACTIVE GALAXIES AND QUASARSSandersLP435C-GOALS: The Chandra-RBGS Survey of a Complete Sample of Major-Merger LIRGs
14800360CLUSTERS OF GALAXIESTozziLP380Extreme constraints on ICM physics and cosmology: a deep observation of XMMUJ0044, the most distant massive cluster
14800365CLUSTERS OF GALAXIESJonesXVP988A Chandra-Planck Legacy Program for Massive Clusters of Galaxies
14800434CLUSTERS OF GALAXIESRandallLP350A Detailed Study of the Longest Known Ram Pressure Stripped Tail with Deep Chandra Observations of M86
14800815CLUSTERS OF GALAXIESWernerLP500Resolving the nearest cold front in the sky: the cleanest experimental tool to study detailed ICM physics
14900904EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYSCivanoXVP2800The COSMOS Legacy Survey

Subject Category: STARS AND WD

Proposal Number: 14200176

Title: Wolf-Rayet Winds at High Spectral Resolution

PI Name: David Huenemoerder

The physical origin of X-ray emission in single Wolf-Rayet (WR) stars is not known. We request 450 ks on WR 6 with HETGS to establish which mechanisms operate in the winds of massive stars at the end of their evolution, shortly before a supernova or gamma-ray burst explosion. High-spectral resolution above 1 kev with HETGS is required to resolve emission lines from the hottest X-ray emitting plasma and thereby determine the location of wind structures. Principal diagnostics of X-ray emission line profiles in conjunction with our state-of-the-art stellar atmospheres code will help unravel current uncertainties in wind generation.

R.A. Dec. Target Name Det. Grating Exp.Time
06:54:13.00-23:55:42.00WR 6ACIS-SHETG450

Subject Category: STARS AND WD

Proposal Number: 14200631

Title: Occultation Measurements of the Embedded Wind Shock Distribution in the Nearest Eclipsing O-star Binary

PI Name: Michael Corcoran

We propose four phase-constrained Chandra/HETGS observations of the massive, eclipsing, single-line spectroscopic binary $\delta$~Ori. Delta Ori is one of the fundamental calibrators of the mass-luminosity-radius relation in the upper HR diagram.These HETGS observations will, for the first time, provide an in-situ measurement of the distribution of the embedded, X-ray emitting shocks in the wind of an O star via radial velocity, occultation and $f/i$ ratio diagnostics, as well as determine the primary star's clumping-corrected mass loss rate. These observations will help resolve critical uncertainties in our understanding of the connection between stellar and mass loss parameters and pioneer new X-ray analysis methods in massive star astrophysics.

R.A. Dec. Target Name Det. Grating Exp.Time
05:32:00.40-00:17:56.70Delta OriACIS-SHETG125
05:32:00.40-00:17:56.70Delta OriACIS-SHETG125
05:32:00.40-00:17:56.70Delta OriACIS-SHETG125
05:32:00.40-00:17:56.70Delta OriACIS-SHETG125

Subject Category: STARS AND WD

Proposal Number: 14200801

Title: COMPACT AND DIFFUSE X-RAY SOURCES IN THE YOUNGEST PLANETARY NEBULAE

PI Name: Joel Kastner

The community of planetary nebula (PN) astronomers is undertaking ChanPLaNS, the first systematic X-ray survey of PNe in the solar neighborhood. ChanPlaNS is yielding such fundamental, new results as the frequency of appearance and range of X-ray spectral characteristics of X-ray-emitting PN central stars and the evolutionary timescales of wind-shock-heated bubbles within PNe. Here, we propose the next phase of the survey, in which we will observe all (24) remaining known compact (radius <= 0.4 pc), young PNe within ~1.5 kpc that have yet to be observed by Chandra. This LP represents the next step toward understanding the relationship between PN X-ray emission and PN shaping processes, and its results will have broad and profound impact on the study of binary stars and wind interactions.

R.A. Dec. Target Name Det. Grating Exp.Time
09:52:44.50-46:16:51.00PN G273.6+06.1ACIS-SNONE20
21:59:35.20-39:23:08.00IC 5148ACIS-SNONE20
17:22:15.70-38:29:03.50NGC 6337ACIS-SNONE20
19:31:07.20-03:42:31.50PN G034.1-10.5ACIS-SNONE20
15:51:40.90-51:31:28.60PN G329.0+01.9ACIS-SNONE30
08:37:08.00-39:25:05.40ESO 313-5ACIS-SNONE30
19:01:59.30+02:09:18.00LBN 036.00-01.26ACIS-SNONE30
19:46:34.20-23:08:12.90ESO 526-3ACIS-SNONE30
17:45:57.70-30:12:00.60ESO 455-33ACIS-SNONE30
18:54:37.20-08:49:39.10IC 1295ACIS-SNONE30
20:16:24.00+30:33:53.20NGC 6894ACIS-SNONE30
16:01:21.10-34:32:35.80NGC 6026ACIS-SNONE30
09:27:03.00-56:06:21.10NGC 2899ACIS-SNONE30
16:12:58.10-36:13:46.10NGC 6072ACIS-SNONE30
21:26:23.50+62:53:31.80NGC 7076ACIS-SNONE30
05:56:23.90+46:06:17.50IC 2149ACIS-SNONE30
17:29:20.40-23:45:34.80NGC 6369ACIS-SNONE30
22:40:19.80+61:17:08.70NGC 7354ACIS-SNONE30
17:47:56.20-29:59:41.90ESO 455-42ACIS-SNONE30
04:06:59.40+60:55:14.40NGC 1501ACIS-SNONE20
16:31:30.60-40:15:12.30NGC 6153ACIS-SNONE30
17:05:10.50-40:53:08.40IC 4637ACIS-SNONE30
18:09:29.90-24:12:23.50ESO 521-39ACIS-SNONE30
11:50:17.70-57:10:56.90NGC 3918ACIS-SNONE30

Subject Category: BH AND NS BINARIES

Proposal Number: 14400870

Title: The Small Magellanic Cloud - A Case Study of X-ray Populations at Low Metallicity

PI Name: Andreas Zezas

We propose a deep survey of 11 fields (100 ks each) in the SMC probing young (10-100 Myr) stellar populations of different ages down to a luminosity limit of 2E32 erg/s, well into the regime of quiescent X-ray binaries and X-ray emitting normal stars. These observations will provide the deepest luminosity functions (XLFs) of X-ray binaries ever recorded, enabling us to: (a) directly measure their formation efficiency as a function of age; (b) address the evolution of their XLF in the 10-100Myr range, (c) constrain the duty cycles of accreting pulsars; and (d) constrain parameters relevant to their formation and evolution. We will also observe for the first time low (0.2Zo) metallicity stars, and we will search for central compact objects in SNRs, and characterize their SN type.

R.A. Dec. Target Name Det. Grating Exp.Time
01:11:10.10-72:44:03.50SMC Deep Field 01ACIS-INONE100
01:13:33.20-72:32:41.80Deep Field 02ACIS-INONE100
01:13:56.90-73:20:34.00Deep Field 03ACIS-INONE100
01:13:39.90-73:08:37.20Deep Field 04ACIS-INONE100
00:56:08.60-72:35:02.50Deep Field 05ACIS-INONE100
00:52:46.60-72:42:11.80Deep Field 06ACIS-INONE100
00:51:52.00-73:00:24.60Deep Field 07ACIS-INONE100
00:49:43.20-72:49:16.30Deep Field 09ACIS-INONE100
00:41:00.00-73:19:60.00Deep Field 10ACIS-INONE100
00:47:09.60-73:07:33.00Deep Field 11ACIS-INONE100
00:56:35.90-72:20:06.30Deep Field 08ACIS-INONE100

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 14500153

Title: A Legacy Study of the Relativistic Shocks of PWNe

PI Name: Roger Romani

We propose deep ACIS observations of five pulsar wind nebulae (PWNe) with kyr-Myr ages. These carefully chosen targets show a high degree of axial symmetry in existing short ACIS images, so that the proposed imaging/spectroscopic studies can probe the geometry of the termination shock and the nature of the post-shock flow. Partitioning the exposure, we will also constrain instability growth and flow speed. By extending our view of PWN dynamics and evolution beyond the spectacular Crab and Vela nebulae, this legacy data set probes the mechanisms converting rotational energy to relativistic jet/torus outflow, key to astrophysical sources on many scales. Multiwavelength studies and modeling will also reveal parameters of the underlying pulsar accelerator and the wind-environment interaction.

R.A. Dec. Target Name Det. Grating Exp.Time
03:58:53.70+54:13:13.70PSR J0358+5413ACIS-INONE400
06:33:54.20+17:46:12.90PSR J0633+1746ACIS-INONE600
17:41:57.30-20:54:11.80PSR J1741-2054ACIS-SNONE300

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 14500702

Title: A Detailed Study of the Composite Supernova Remnant MSH 11-62

PI Name: Patrick Slane

MSH 11-62 is a remarkable example of an evolved core-collapse supernova remnant. It appears to be evolving in a wind-blown cavity created by its massive progenitor, shows evidence for energetic particles accelerated by the SNR shock and for ejecta heated by the reverse shock, and is accompanied by a neutron star powering a bright pulsar wind nebula that is apparently being disrupted by the supernova remnant reverse shock. We propose a deep Chandra observation to turn our qualitative picture of this remnant into a quantitative investigation of its ambient medium, ejecta profile, and pulsar wind nebula structure. We will use these measurements to model the evolution of the system, constrain the properties of its progenitor, and address the nature of its gamma-ray emission.

R.A. Dec. Target Name Det. Grating Exp.Time
11:11:48.00-60:37:60.00MSH 11-62ACIS-INONE375

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 14500725

Title: G11.2-0.3: Core-Collapse Supernova Progenitors, Cosmic Rays, and Pulsar-Wind Nebulae

PI Name: Stephen Reynolds

We propose a 400 ks observation of the young supernova remnant G11.2-0.3, a shell containing a pulsar-wind nebula and known pulsar, to address fundamental issues of core-collapse supernovae. Our observation should allow the determination of expansion proper motions and search for variability in the PWN; a sensitive search for thin rims of synchrotron X-ray emission; and greatly improved spectral characterization of shell emission, ejecta knots ahead of the blast wave, and mysterious interior thermal emission. G11.2-0.3 may be the remnant of a Type IIL/b (partially stripped) supernova, in which case our observations can constrain the nature of the progenitor wind, as well as give information on shock acceleration of electrons and the evolution of the interior pulsar-wind nebula.

R.A. Dec. Target Name Det. Grating Exp.Time
18:11:29.40-19:25:25.00G11.2-0.3ACIS-SNONE400

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 14500928

Title: A comparative study of two outstanding pulsar tails

PI Name: Oleg Kargaltsev

Long pulsar tails detected in X-rays and radio are believed to result from the supersonic motion of pulsars through the ISM. The processes responsible for the tail formation, collimation, and stability are poorly understood. Short Chandra observations of two outstanding pulsar tails allowed us to characterize their general properties, but much remains to be learned about the complex physics of magnetized collimated flows. We propose much deeper observations of these two tails which show very different properties. We will measure their shapes and internal structures, perform definitive spatially-resolved spectroscopy, and study the connection with the radio tails. The results will advance our understanding of magnetized collimated outflows and their interaction with the ambient medium.

R.A. Dec. Target Name Det. Grating Exp.Time
15:09:27.10-58:50:56.10PSR J1509-5850 nebulaACIS-INONE380
17:47:25.90-29:59:58.00The MouseACIS-INONE120

Subject Category: ACTIVE GALAXIES AND QUASARS

Proposal Number: 14700473

Title: ENERGY DEPENDENT X-RAY MICROLENSING AND THE STRUCTURE OF QUASARS

PI Name: Christopher Kochanek

The structure of the X-ray emitting regions of quasars remains an open question. Using microlensing in lensed quasars, we can now constrain the sizes, finding that they are compact compared to the UV emission (2500A) with 1/2 light radii of ~10-30 gravitational radii. We propose measuring the relative sizes of the hard and soft X-ray emission, better constraining the overall X-ray sizes and comparing them to the hottest regions of the accretion disk by coarsely monitoring 6 lenses with CXO (6 epochs each) and 5 with HST/UV (2 epochs). In essence, the variability amplitudes of the X-ray/UV compared to our well-sampled optical light curves allows us to measure the sizes. We request ~2/3 (1/3) of the time in Cycle 14 (15) for a total of 864~ks (with slew tax) and 12 HST orbits.

R.A. Dec. Target Name Det. Grating Exp.Time
01:58:41.40-43:25:04.20QJ0158-4325ACIS-SNONE114
04:38:14.90-12:17:14.40HE0435-1223ACIS-SNONE222
10:04:34.20+41:12:44.00SDSS1004+4112ACIS-SNONE150
11:06:33.50-18:21:24.20HE1104-1805ACIS-SNONE84
22:40:30.30+03:21:28.80Q2237+0305ACIS-SNONE180
11:31:51.60-12:31:57.00RXJ1131-1231ACIS-SNONE60

Subject Category: ACTIVE GALAXIES AND QUASARS

Proposal Number: 14700824

Title: Joint Chandra/XMM/EVLA Monitoring of the Gas Cloud G2 as it Encounters Sgr A*

PI Name: Daryl Haggard

A dense, cold cloud (G2) is on a collision course with Sgr A*, the radio source at our Galactic Center. G2 is on an eccentric orbit and already shows signs of tidal disruption by the black hole. High-energy emission from Sgr A* will likely increase significantly due to this encounter, peaking at pericenter (summer 2013). We propose simultaneous Chandra, XMM, and EVLA monitoring observations to constrain the rates and emission mechanisms of faint X-ray flares, study the radiation properties of Sgr A* as G2 breaks up and feeds gas to the central accretion flow, and detect G2 itself as it is shocked and heated. Multiwavelength observations of this encounter will have a profound impact on our understanding of radiatively inefficient accretion flows into, and outflow from, massive black holes.

R.A. Dec. Target Name Det. Grating Exp.Time
17:45:40.00-29:00:27.90Sgr AACIS-INONE50
17:45:40.00-29:00:27.90Sgr AACIS-INONE50
17:45:40.00-29:00:27.90Sgr AACIS-INONE50
17:45:40.00-29:00:27.90Sgr AACIS-INONE50
17:45:40.00-29:00:27.90Sgr AACIS-INONE50
17:45:40.00-29:00:27.90Sgr AACIS-INONE50

Subject Category: ACTIVE GALAXIES AND QUASARS

Proposal Number: 14700854

Title: C-GOALS: The Chandra-RBGS Survey of a Complete Sample of Major-Merger LIRGs

PI Name: David Sanders

We propose to finish our Chandra-ACIS survey of a statistically complete sample of 87 major-merger LIRGs [log(Lir/Lsun)=11.0-12.57], from the IRAS RBGS. Our proposed Cycle-14 observations of the 29 lower-luminosity objects (11.0-11.72) will allow us to have a uniform and complete census of AGN and X-ray luminous starbursts in the nearest and brightest major-merger LIRGs, and will complement our existing Spitzer-IRAC/MIPS/IRS, HST-ACS, GALEX and Herschel observations of the same sample. The results will be used to address the following key questions: are binary AGN a common feature of these LIRGs, and if so, when and at what level is the AGN activity triggered in each nucleus? And can the fueling and growth of massive black holes be correlated in time with the merger phase?

R.A. Dec. Target Name Det. Grating Exp.Time
01:51:14.00+22:34:55.00NGC 0695ACIS-SNONE15
01:20:01.40+14:21:35.00CGCG 436-030ACIS-SNONE15
13:01:49.90+04:20:01.00CGCG 043-099ACIS-SNONE15
18:33:35.60+59:53:20.00NGC 6670A/BACIS-SNONE15
13:52:16.60+02:06:08.00NGC 5331ACIS-SNONE15
06:09:45.10-21:40:22.00IRAS F06076-2139ACIS-SNONE15
11:25:47.30+14:40:23.00IC 2810ACIS-SNONE15
18:11:37.30+01:31:40.00IRAS 18090+0130ACIS-SNONE15
16:42:39.20-09:43:11.00IRAS F16399-0937ACIS-SNONE15
18:13:38.60-57:43:36.00IC 4687/6ACIS-SNONE15
16:19:10.30-07:53:57.00IRAS F16164-0746ACIS-SNONE15
23:16:01.70+25:33:33.00IC 5298ACIS-SNONE15
04:21:20.00-18:48:48.00ESO 550-IG025ACIS-SNONE15
00:11:06.60-12:06:27.00NGC 0034ACIS-SNONE15
00:54:04.00+73:05:13.00MCG+12-02-001ACIS-SNONE15
17:16:36.30-10:20:40.00IRAS F17138-1017ACIS-SNONE15
12:06:53.00-31:57:08.00ESO 440-IG058ACIS-SNONE15
13:01:25.90+29:18:46.00NGC 4922ACIS-SNONE15
09:36:39.30+48:28:19.00MCG+08-18-013ACIS-SNONE15
02:46:17.00+13:05:45.00UGC 02238ACIS-SNONE15
10:04:02.70-06:28:35.00NGC 3110ACIS-SNONE15
09:46:20.30+03:03:22.00IC 563/4ACIS-SNONE15
03:54:16.40+15:55:44.00CGCG 465-012ACIS-SNONE15
13:02:20.50-15:46:05.00MCG-02-33-098/9ACIS-SNONE15
21:36:10.80-38:32:38.00ESO 343-IG013ACIS-SNONE15
04:34:00.10-08:34:46.00NGC 1614ACIS-SNONE15
20:37:18.60+25:31:42.00IRAS 20351+2521ACIS-SNONE15
00:42:46.50-23:33:31.00NGC 0232ACIS-SNONE15
08:44:27.60-31:41:41.00ESO 432-IG006ACIS-SNONE15

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 14800360

Title: Extreme constraints on ICM physics and cosmology: a deep observation of XMMUJ0044, the most distant massive cluster

PI Name: Paolo Tozzi

We propose a deep (380 ks) Chandra observation of the distant galaxy cluster XMMUJ0044 at z=1.58. With this observation we will push detailed studies of X-ray clusters to the edge of the current discovery limit, by measuring global temperature and Fe abundance, gas and total mass, putting strong constraints on the time formation of cool core, on the chemical enrichment time scale, on the relation between ICM and galaxy population, and deriving the best constraint to the standard Lambda-CDM model attainable at present. These results, achievable only with Chandra, are secured by a first X-ray characterization of XMMUJ0044 based on XMM data, and will constitute an unrivaled reference for distant cluster studies until the next generation of high-angular resolution X-ray satellites.

R.A. Dec. Target Name Det. Grating Exp.Time
00:44:05.20-20:33:59.70XMMUJ0044.0-2033ACIS-SNONE380

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 14800365

Title: A Chandra-Planck Legacy Program for Massive Clusters of Galaxies

PI Name: Christine Jones

ESA's Planck Mission has provided a large, statistically representative sample of very massive clusters, detected over the full sky through their SZ effect. The Planck clusters are sufficiently X-ray bright that for all 165 z<0.35 clusters, Chandra will collect 10,000 source counts to characterize each cluster's dynamical state, including merger properties, measure cluster masses and mass proxies and define local cluster mass and temperature functions. Chandra observations will provide a benchmark at low redshifts for comparison to high redshift clusters and to cosmological N-body simulations. Our team is expert in the analysis of X-ray and SZ data and in theory, simulations, lensing, and radio studies of clusters. We plan to make our cluster analysis products available to the community.

R.A. Dec. Target Name Det. Grating Exp.Time
10:43:24.80-20:37:18.00G106.73-83.22ACIS-INONE12
21:35:19.90+01:23:14.50G055.97-34.88ACIS-INONE20
18:04:29.70+18:04:29.70G036.72+14.92ACIS-INONE10
05:16:37.50-54:31:31.80G262.25-35.36ACIS-INONE22
06:16:19.80-21:57:35.00G229.21-17.24ACIS-INONE24
22:18:41.30-38:54:16.80G002.74-56.18ACIS-INONE11
19:47:09.30-76:23:52.00G318.13-29.57ACIS-INONE20
21:27:03.50-12:09:19.00G039.85-39.98ACIS-INONE15
19:38:19.70+54:09:26.30G086.45+15.29ACIS-INONE15
10:22:27.30+50:06:16.30G163.72+53.53ACIS-INONE14
22:23:49.30-01:37:13.20G062.42-46.41ACIS-INONE9
20:23:24.30-55:34:26.50G342.31-34.90ACIS-INONE21
09:45:26.20-08:40:06.00G244.69+32.49ACIS-INONE16
02:25:56.00-41:54:53.00G256.45-65.71ACIS-INONE15
05:32:59.40-37:01:39.60G241.74-30.88ACIS-INONE25
03:03:53.10-77:52:14.40G294.66-37.02ACIS-INONE34
10:23:44.10+49:08:17.00G165.08+54.11ACIS-INONE10
22:17:46.10-35:43:22.20G008.44-56.35ACIS-INONE12
10:39:28.10+05:10:06.00G241.85+51.53ACIS-INONE14
17:47:18.00+45:13:30.70G071.61+29.79ACIS-INONE21
11:59:23.00+49:47:39.00G143.24+65.21ACIS-INONE22
19:34:54.00-50:53:18.80G347.18-27.35ACIS-INONE25
05:25:50.00-47:14:38.30G253.47-33.72ACIS-INONE18
13:15:06.60+51:49:27.20G114.33+64.87ACIS-INONE31
23:39:44.00-85:10:33.00G304.67-31.66ACIS-INONE23
06:16:29.50-39:48:28.80G247.17-23.32ACIS-INONE17
12:36:57.40+63:11:08.00G125.70+53.85ACIS-INONE29
09:20:24.80+30:30:09.20G195.62+44.05ACIS-INONE38
14:14:05.30+71:17:36.50G113.82+44.35ACIS-INONE19
18:19:55.30+57:09:57.30G085.99+26.71ACIS-INONE35
10:00:02.10-30:15:55.80G264.41+19.48ACIS-INONE31
20:51:50.20-58:45:23.00G345.40-39.34ACIS-INONE30
12:01:04.00-39:52:11.00G292.51+21.98ACIS-INONE45
19:14:36.90-59:28:19.90G337.09-25.97ACIS-INONE25
09:38:21.40+52:02:38.40G164.61+46.39ACIS-INONE42
12:59:37.60+60:04:41.90G121.11+57.01ACIS-INONE44
06:21:55.00+74:41:38.40G139.59+24.18ACIS-INONE18
11:11:37.10+40:50:01.90G172.88+65.32ACIS-INONE12
05:10:13.00-45:19:29.00G250.90-36.25ACIS-INONE16
05:31:34.70-75:11:26.40G286.58-31.25ACIS-INONE24
18:54:06.00+68:22:15.00G098.95+24.86ACIS-INONE17
06:37:19.50-48:28:50.40G257.34-22.18ACIS-INONE25
21:04:22.90-41:21:46.00G000.44-41.83ACIS-INONE14
11:42:37.40+58:32:14.30G139.19+56.35ACIS-INONE33
12:15:28.80-39:01:47.00G295.33+23.33ACIS-INONE15

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 14800434

Title: A Detailed Study of the Longest Known Ram Pressure Stripped Tail with Deep Chandra Observations of M86

PI Name: Scott Randall

We propose deep Chandra observations of the ram pressure stripped tail in M86, the longest ram pressure stripped tail known. M86 is nearby, in the Virgo cluster (~17 Mpc), and is X-ray bright. With Chandra's high spatial resolution we will image fine detail in the tail, and map the temperature and abundance structure along the tail. We will determine the origin of the stripped gas, place limits on gas mixing in the tail with the ICM, and ultimately place constrains on ICM microphysics through comparisons with detailed hydrodynamical simulations.

R.A. Dec. Target Name Det. Grating Exp.Time
12:25:45.90+13:04:52.00M86 Inner TailACIS-INONE150
12:25:02.30+13:16:54.60M86 Outer TailACIS-INONE200

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 14800815

Title: Resolving the nearest cold front in the sky: the cleanest experimental tool to study detailed ICM physics

PI Name: Norbert Werner

We propose a very deep legacy-class observation of the nearest, best resolved cold front in the sky which lies 90 kpc to the North of M87. Cold fronts are known to be remarkably sharp, with gas density and temperature discontinuities several times sharper than the Coulomb mean free path. The proposed observation will provide an extraordinary improvement in resolution (resolving ~80 pc scales), allowing to study the cold front interface in unprecedented detail. Cold fronts provide a relatively simple experimental setup - a unique tool to study ICM physics. The proposed observation will place crucial constraints on fundamental physical processes shaping cold fronts, such as: growth of instabilities in the ICM, intra-cluster magnetic fields, gas velocities, conduction and viscous stresses.

R.A. Dec. Target Name Det. Grating Exp.Time
12:29:56.30+12:38:39.60Virgo cold frontACIS-INONE500

Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS

Proposal Number: 14900904

Title: The COSMOS Legacy Survey

PI Name: Francesca Civano

We propose the COSMOS-Legacy Survey covering the entire 1.7deg2 COSMOS/HST area to a uniform depth of ~160ks, expanding the current deep C-COSMOS area by a factor 3, with 56x50 ks pointings for a total of 2.8 Ms. This area and depth proposed are designed to detect~40 z>4, and ~4 z>5 Large Scale Structures on >15' scales, connecting luminous Chandra quasars (among over 200 z>3 quasars) and sub-mm galaxies, a method already proven in C-COSMOS. The area/depth combination also probes mini-quasars at z>7 using anistotropies of the unresolved XRB and the masses of the DM halos hosting X-ray AGN up to z~3 via autocorrelation functions on ~30' scales. Large programs with SCUBA2, NuSTAR, Subaru and Keck over the COSMOS field will identify and get redshifts for all COSMOS-Legacy sources.

R.A. Dec. Target Name Det. Grating Exp.Time
10:00:29.90+02:12:40.00COSMOS LegacyACIS-INONE2800
Smithsonian Institute Smithsonian Institute

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