Accepted Cycle 12 Observing Proposals

SN, SNR & ISOLATED NS

Proposal Number	Subject Category	PI Name	Title
12500006	SN, SNR AND ISOLATED NS	Burrows	Chandra Cycle 12 Spatial and Spectral Monitoring of SNR 1987A
12500075	SN, SNR AND ISOLATED NS	Halpern	Measuring the Spin-Down and Magnetic Field Strength of the CCO Pulsar in Puppis A
12500120	SN, SNR AND ISOLATED NS	Berger	Rapid Observations of Short Gamma-Ray Bursts: Accurate Positions Hold the Key to the Progenitor Population
12500138	SN, SNR AND ISOLATED NS	Romani	A Survey of PWNe around Narrow-Pulse Gamma-ray Pulsars
12500152	SN, SNR AND ISOLATED NS	Katsuda	X-Ray Time Variability of an Ejecta Filament in Puppis A
12500157	SN, SNR AND ISOLATED NS	Gotthelf	Spin-down of the 44 ms Pulsar Powering HESS J1813-178
12500182	SN, SNR AND ISOLATED NS	Racusin	Constraining the Energetics of Fermi-LAT GRBs with Chandra
12500202	SN, SNR AND ISOLATED NS	Vink	Detailed imaging of a pulsar wind nebula around a magnetar
12500216	SN, SNR AND ISOLATED NS	Park	Chandra HETGS Observation of the Oxygen-Rich Supernova Remnant G292.0+1.8
12500248	SN, SNR AND ISOLATED NS	Lorimer	PSRJ 1832+0029: a unique target for pulsar emission physics
12500261	SN, SNR AND ISOLATED NS	Bogdanov	PSR J1856+0245: Understanding the Connection Between Young Pulsars and TeV gamma-ray Sources
12500265	SN, SNR AND ISOLATED NS	Kaplan	Are long-period, strong-field radio pulsars progenitors of Isolated Neutron Stars?
12500373	SN, SNR AND ISOLATED NS	Fesen	X-ray Observations of the Optically Discovered Galactic Supernova Remnant G159.6+7.3
12500395	SN, SNR AND ISOLATED NS	Slane	Clumpy Winds and a Bursting X-ray Source: A Chandra Study of G296.1-0.5
12500440	SN, SNR AND ISOLATED NS	Tiengo	Measuring magnetar distance from the dust echo of a bright burst
12500476	SN, SNR AND ISOLATED NS	Kaspi	Grand Unification in Neutron Stars: The High-B Radio Pulsars
12500494	SN, SNR AND ISOLATED NS	Pooley	Chandra Observations of New X-ray Supernovae
12500495	SN, SNR AND ISOLATED NS	Pooley	Investigating the Emission of Extraordinarily Luminous and Unusual Supernovae
12500504	SN, SNR AND ISOLATED NS	Renaud	Imaging of the newly discovered composite SNR G310.6-1.6
12500511	SN, SNR AND ISOLATED NS	Kaspi	TINY HICCUPS TO TITANIC EXPLOSIONS: Tackling Transients in Anomalous X-ray Pulsars
12500549	SN, SNR AND ISOLATED NS	Troja	Jet-breaks in short GRBs
12500600	SN, SNR AND ISOLATED NS	Kaspi	Target-of-Opportunity Chandra Observations of Glitching High-B Radio Pulsars: Searching for Magnetar Metamorphoses
12500613	SN, SNR AND ISOLATED NS	Soderberg	The Energetics and Environments of Type Ibc Supernovae
12500619	SN, SNR AND ISOLATED NS	Rea	Exploring the unusual extended emission around the highly magnetic RRATJ1819-1458
12500631	SN, SNR AND ISOLATED NS	Uchiyama	A Deep Observation of Synchrotron X-ray Variability in SNR RX J1713.7-3946
12500646	SN, SNR AND ISOLATED NS	Rol	Constraining GRB physics through their afterglow light curves
12500668	SN, SNR AND ISOLATED NS	Seward	The Pulsar Wind Nebula in DEM L241
12500689	SN, SNR AND ISOLATED NS	Dwarkadas	The X-Ray Emission from SN 1993J: Resolving Almost Two Decades of Conflict with Detailed Spectral Modeling
12500786	SN, SNR AND ISOLATED NS	Theiling	VER J2019+407: UNIDENTIFIED TEV SOURCE IN THE GAMMA-CYGNI SNR
12500795	SN, SNR AND ISOLATED NS	Fox	Completing Identification of the Nearest and Brightest Neutron Stars
12500804	SN, SNR AND ISOLATED NS	Ng	Hunting for Anti-magnetars with Chandra
12500822	SN, SNR AND ISOLATED NS	Borkowski	Radioactivity, Particle Acceleration, and Supernova Ejecta in the Youngest Galactic SNR G1.9+0.3
12500852	SN, SNR AND ISOLATED NS	Patnaude	The Persistent X-ray Emission from the Type IIL SN 1979C
12500889	SN, SNR AND ISOLATED NS	Slane	A High Resolution Study of the Vela X Cocoon
12500918	SN, SNR AND ISOLATED NS	Fruchter	The Astrophysics of the Most Energetic Gamma-Ray Bursts
12500923	SN, SNR AND ISOLATED NS	Burrows	SEARCH FOR JET BREAKS IN LONG GRB X-RAY AFTERGLOWS

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500006

Title: Chandra Cycle 12 Spatial and Spectral Monitoring of SNR 1987A

PI Name: David Burrows

Regular monitoring of SNR1987A, the only supernova remnant in which we can study the early developmental stages in detail, is critical to testing models of SNR evolution, nonequilibrium ionization processes, and thin plasma spectra. SNR1987A presents a unique opportunity to observe the birth and early evolution of a supernova remnant at high spatial and spectral resolution for the first time. We propose to continue our program of monitoring SNR1987A in Cycle 12 at roughly six month intervals.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
05:35:28.00	-69:16:11.10	SNR 1987A	ACIS-S	HETG	56
05:35:28.00	-69:16:11.10	SNR 1987A	ACIS-S	HETG	52

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500075

Title: Measuring the Spin-Down and Magnetic Field Strength of the CCO Pulsar in Puppis A

PI Name: Jules Halpern

This proposal is the second element of our two-year plan to measure the spin-down rate of the pulsar in Puppis A by obtaining a phase-coherent timing solution. If it is a weakly magnetized neutron star like the other CCO pulsars, this is the only practical way of measuring its spin-down. Our sensitivity to P-dot will correspond to a surface dipole B-field as small as 3.e10 G, comparable to our measured value for the CCO pulsar PSR J1852+0040 in Kes 79. Such a result would provide important support for the "anti-magnetar" model of CCOs. In addition, we will explore possible reasons for the unexplained surface hot spots, which are especially striking in Puppis A, using the energy-dependent pulse profiles and phase-resolved spectra.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
08:21:57.30	-43:00:17.60	PSR J0821-4300	ACIS-S	NONE	33
08:21:57.30	-43:00:17.60	PSR J0821-4300	ACIS-S	NONE	33

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500120

Title: Rapid Observations of Short Gamma-Ray Bursts: Accurate Positions Hold the Key to the Progenitor Population

PI Name: Edo Berger

Only 1/4 of all short GRBs are localized to sub-arcsecond accuracy, required for unambiguous host and redshift identifications, determination of the burst environment (disk, bulge, halo, IGM), and assessment of natal kicks. These properties determine the identity and ages of the progenitors, and the GRB explosion properties. Thus, much of our knowledge depends on a handful of events, which are moreover biased to high density environments by virtue of optical/radio detections. Here we propose to double the fraction of events with sub-arcsecond positions, and overcome the density bias, using rapid Chandra observations of bursts with only Swift/XRT positions (3-6"). Swift data will guarantee Chandra detections at <4 days, and follow-up work will delineate the burst/host properties.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
		Short-GRB-1	ACIS-S	NONE	20
		Short-GRB-2	ACIS-S	NONE	20

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500138

Title: A Survey of PWNe around Narrow-Pulse Gamma-ray Pulsars

PI Name: Roger Romani

We propose here, on behalf of the Fermi LAT team, ACIS observations of the X-ray counterparts of six unusual gamma-ray pulsars discovered by the LAT. The targets, four seen only in the gamma-rays, two also radio-detected, have unusual single or narrow double pulse profiles, which require particular emission geometries for different pulsar models. By measuring the arcsecond-scale structure of the wind nebula termination shocks of these young (<100kyr) objects, CXO can pin down the viewing angle and test the pulsar physics. All have known X-ray fluxes and we can also extract spectral and distance estimates needed to interpret the GeV gamma-rays. The survey sample covers a range of ages, spindown powers and expected inclinations, making it a powerful test of pulsar emission models.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
14:20:08.20	-60:48:16.60	J1420-6048	ACIS-I	NONE	90
18:09:50.20	-23:32:22.90	J1809-2332	ACIS-I	NONE	30
17:18:13.60	-38:25:18.10	J1718-3825	ACIS-S	NONE	40

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500152

Title: X-Ray Time Variability of an Ejecta Filament in Puppis A

PI Name: Satoru Katsuda

We recently found an X-ray--emitting filament associated with several O-rich fast-moving optically emitting knots (OFMKs) in the northeastern portion of the middle-aged supernova remnant Puppis A. Our spectral analysis of Chandra data revealed it to be O-Ne-Mg-rich ejecta. Archival Einstein, ROSAT, XMM-Newton, and Chandra data show an almost linear flux decrease for the filament over nearly 30 yr. This filament gives us an unusual opportunity to track X-ray variability of thermal emission. To measure spectral variability, we here propose a 40 ks observation of the filament with the Chandra ACIS. This observation will also provide us with a good opportunity to find nearby X-ray ejecta features.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
08:23:15.40	-42:50:54.20	Puppis A NE filament	ACIS-I	NONE	40

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500157

Title: Spin-down of the 44 ms Pulsar Powering HESS J1813-178

PI Name: Eric Gotthelf

We have just discovered the pulsar in the faint shell-type supernova remnant SNR G12.82-0.02, coincident with the TeV gamma-ray source HESS J1813-178 and possibly the Fermi source 0FGL J1814.3-1739. PSR J1813-1749 is clearly one of the most energetic pulsars in the Galaxy, but its spin-down power is poorly measured. We need only a brief follow-up observation to measure the all important period derivative, critical for determining the energetics, dipole magnetic field strength, and spin-down age. This will allow us to infer the efficiency of emission in all high-energy wavebands from X-ray through TeV, and to search for GeV pulsations with Fermi. We can also constrain the age of the SNR and the birth period of the pulsar, important for modeling the radiation and evolution of the system.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
18:13:35.20	-17:49:57.50	CXO J181335.1-174957	ACIS-S	NONE	20

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500182

Title: Constraining the Energetics of Fermi-LAT GRBs with Chandra

PI Name: Judith Racusin

We propose to observe late-time X-ray afterglows of the most energetic subset of Fermi-LAT detected GRBs in order to constrain their jet break times, opening angles, and collimation corrected energy outputs. This new and exceptional population of GRBs demonstrate several new features not previously observed, and appear to be brighter on average than Swift era optical and X-ray afterglows, which makes them excellent candidates for broadband observations and detailed modeling. Observations of the X-ray afterglows by Swift-XRT do not reveal any jet break signatures in these objects, suggesting that they occur later when the afterglows are too faint for XRT, but possibly still observable by Chandra.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
		GRB AO12-1	ACIS-S	NONE	60
		GRB AO12-2	ACIS-S	NONE	60

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500202

Title: Detailed imaging of a pulsar wind nebula around a magnetar

PI Name: Jacco Vink

1E 1547.0-5408 is the only known AXP surrounded by a pulsar wind nebula (PWN). In addition, the AXP and PWN are embedded inside a supernova remnant (SNR). The PWN allows us to study the integrated relativistic electron outflows from a magnetar. If its nature is similar to that of regular PWNe, the PWN can be used to constrain the initial spin-period of a magnetar. This is important given the uncertainties about the origin of magnetar magnetic fields: turbulent amplification in a neutron star with initial periods of < 3 ms, or a strong field in the progenitor's core? The PWN is faint, and was only observed with Chandra for 10 ks. Here we propose a much deeper obser- vation of 100 ks, allowing us to search for substructure and to constrain the spectral properties of both PWN and SNR.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
15:50:54.10	-54:18:23.50	1E 1547.0-5408/PWN	ACIS-S	NONE	100

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500216

Title: Chandra HETGS Observation of the Oxygen-Rich Supernova Remnant G292.0+1.8

PI Name: Sangwook Park

While a significant progress on the detailed study of the O-rich supernova remnant (SNR) G292.0+1.8 is being made using our deep ACIS observation, the SNR dynamics and nucleosynthesis cannot be fully studied without locating its reverse shock. The deep ACIS data show the forward shock and contact discontinuity, but providing only a projected 2-D distribution of ejecta over the face of the SNR, the ACIS data are not useful to discriminate the reverse shock location (i.e., close to the SNR center vs near the contact discontinuity). The only way to reveal the reverse shock location along the line of sight is to measure Doppler shifts in the ejecta knots projected near the SNR center. Thus, we propose a 120 ks HETGS observation of G292.0+1.8 to reveal the 3-D structure of the reverse shock.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
11:24:39.50	-59:15:56.40	G292.0+1.8	ACIS-S	HETG	120

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500248

Title: PSRJ 1832+0029: a unique target for pulsar emission physics

PI Name: Duncan Lorimer

We have discovered very unusual behavior in PSR J1832+0029, a 533-ms radio pulsar which switches between on and off states on timescales of several hundred days. Remarkably, the pulsar's spin-down rate almost doubles when the radio emission is on. This is even more dramatic than observed for PSR B1931+24 for which no satisfactory theory presently exists. Unlike PSR B1931+24, J1832+0029 is nearby (1.3 kpc) and an excellent target for X-ray detection. Here we request a 23 ks ACIS TOO to study the X-ray emission of PSR J1832+0029 in its off state, triggered by radio monitoring. Together with our recent GO observation, this TOO will help distinguish between radio emission quenching mechanisms that are either intrinsic to the pulsar or caused by accretion from an orbiting companion.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
18:32:50.80	+00:29:27.20	J1832+0032	ACIS-S	NONE	23

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500261

Title: PSR J1856+0245: Understanding the Connection Between Young Pulsars and TeV gamma-ray Sources

PI Name: Slavko Bogdanov

We propose a Chandra ACIS-I observation of the recently discovered young, ``Vela-like'' pulsar PSR J1856+0245 in order to confirm the association between the pulsar and the positionally coincident TeV gamma-ray source HESS J1857+026. The superb angular resolution of Chandra will allow us to characterize the morphology and orientation of the pulsar wind nebula emission, which are important criteria for establishing the plausible connection between the TeV source and the pulsar. Confirming this association would offer valuable information about the composition of the pulsar wind, the injection history from the host pulsar, and the material into which the wind nebula is expanding.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
18:56:50.80	+02:45:52.20	PSR J1856+0245	ACIS-I	NONE	39

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500265

Title: Are long-period, strong-field radio pulsars progenitors of Isolated Neutron Stars?

PI Name: David Kaplan

The 7 Isolated Neutron Stars intrigue both because of the hope of determining neutron-star parameters and because of their large inferred population. Regarding the latter, from timing we found remarkably similar field strengths and consistently long characteristic ages, suggestive of initially stronger fields that decayed, a result reproduced theoretically. There should then be slowly rotating, strong-field progenitors heated by field decay. Five pulsars with P>3s & B>3e13G might be such objects. X-ray observations of four exist; two are indeed anomalously hot, and two are undetected, but too distant and extincted. The remaining one, PSR J0726-2612, is likely the nearest and least extincted. In 20 ks, we can determine whether it is hotter or not than expected from standard cooling.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
07:26:08.10	-26:12:38.10	PSR J0726-2612	ACIS-S	NONE	20

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500373

Title: X-ray Observations of the Optically Discovered Galactic Supernova Remnant G159.6+7.3

PI Name: Robert Fesen

Before the advent of radio astronomy, only two Galactic supernova remnants were known from optical studies: the Crab Nebula and Kepler's SN. Instances where a Galactic remnant was first identified through its optical emission are rare, and at present most new remnants are discovered through X-ray emission. Here we propose for Chandra ACIS-I observations of the recently discovered remnant G159.6+7.3. This remnant appears as a large shell of H-alpha emission in the Virginia Tech Spectral Line Survey of the Galactic plane, with regions of faint, Balmer emission reminiscent of remnants such as the Cygnus Loop and SN 1006. This proposed observation will firmly dispel any uncertainty about its nature, measure the gas temperature behind the shock, and be used to estimate its age and distance.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
05:34:18.70	+49:57:54.00	G159.6+7.3	ACIS-I	NONE	30

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500395

Title: Clumpy Winds and a Bursting X-ray Source: A Chandra Study of G296.1-0.5

PI Name: Patrick Slane

G296.1-0.5 is a bright SNR that, based on our recent studies, appears to be expanding into the wind of a Wolf-Rayet progenitor star. The composition shows unique signatures of CNO-cycle material, and the X-ray emission is suggestive of the clumpy structure expected in such winds. We have also discovered a bursting X-ray source in the field whose properties are similar to those of magnetars in outburst. Magnetars are thought to originate in massive stars such as the inferred progenitor of G296.1-0.5. Here we propose an ACIS observation to characterize the clumpy structure of the swept-up wind in G296.1-0.5 and to establish a high-precision location and/or an extremely sensitive limit on the quiescent luminosity of the variable X-ray source.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
11:50:36.00	-62:21:23.00	G296.5-0.1	ACIS-I	NONE	30

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500440

Title: Measuring magnetar distance from the dust echo of a bright burst

PI Name: Andrea Tiengo

We recently discovered around the magnetar 1E 1547.0-5408 three bright X-ray expanding rings due to scattering of the radiation of a strong burst by three dust layers in our Galaxy. We propose rapid follow-up observations with Chandra in the case that a similar phenomenon is again detected in a magnetar. This would provide the first high resolution two-dimensional images of an X-ray expanding ring around an astrophysical object and would constrain the source distance and energetics of the emission producing the dust echo. Moreover, the time evolution of the ring intensity and spectrum, depending on the dust grains composition and size, is a powerful tool to test the different interstellar dust models.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
		Magnetar scattering halo	ACIS-I	NONE	70

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500476

Title: Grand Unification in Neutron Stars: The High-B Radio Pulsars

PI Name: Victoria Kaspi

The past decade has revealed a bewildering diversity in NS properties. From rotation-powered pulsars (RPs) to magnetars to the so-called isolated neutron stars (INSs), the leading physical characteristic in defining a NS's observational behavior has been argued, increasingly convincingly, to be magnetic field, B. We request Chandra observations PSRs J0726-2612 and PSR J1001-5939, 2 very nearby, high-B RPs having properties very similar to those of INSs, in order to test whether B is truly the `grand unification' parameter for RPs, magnetars and INSs. Indeed this is predicted in recent models of NS thermomagneto-evoluion, and if correct, explains the long-standing puzzle of the nature of the INSs.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
10:01:32.20	-59:39:17.80	PSR J1001-5939	ACIS-S	NONE	19

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500494

Title: Chandra Observations of New X-ray Supernovae

PI Name: David Pooley

We propose to continue our X-ray studies of Type II and Type Ib/c supernovae (SNe). The Swift satellite has ushered in a new era of studying SNe in the X-rays, obtaining densely sampled X-ray lightcurves for the first time. However, its spatial resolution is often not good enough to separate a SN from nearby sources. We propose short Chandra observations to alleviate this. These observations will assess the X-ray environment of newly discovered Swift SNe to determine any possible source confusion or contamination of the SN flux. Our strategy makes the best use of the capabilities of each observatory.

Target Name	Det.	Grating	Exp.Time
SN1	ACIS-S	NONE	10
SN2	ACIS-S	NONE	10
SN3	ACIS-S	NONE	10
SN4	ACIS-S	NONE	10

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500495

Title: Investigating the Emission of Extraordinarily Luminous and Unusual Supernovae

PI Name: David Pooley

In the past few years, the Texas Supernova (SN) Search and its successor the ROTSE SN Verification Project (RSVP) have found several of the most luminous SNe ever detected. Explaining such high luminosities has been challenging, and, in each case, one must consider the "standard" interaction of the SN ejecta with the surrounding material as a (partial) source of this extraordinary luminosity before considering more exotic scenarios (e.g., pair-formation instability). Deep Chandra observations are the most sensitive probes of interaction and are the only way to detect or set meaningful limits on the X-ray flux from such a SN given the typical distances involved. The continuation of RSVP as well as the new Palomar Transient Factory ensure a reliable stream of sources for future discovery.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
		Luminous SN	ACIS-S	NONE	100

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500504

Title: Imaging of the newly discovered composite SNR G310.6-1.6

PI Name: Matthieu Renaud

We recently discovered a small diameter shell-type supernova remnant (SNR) in a 5 ks Chandra survey field of INTEGRAL sources. At the center of G310.6-1.6 lies one of the most energetic pulsar (PSR) in the Milky Way, powering a bright radio and X-ray wind nebula (PWN). Initial studies of this system suggests a young (< 1kyr) and distant (~ 10 kpc) SNR, but many questions remain unanswered by the short snapshot. We propose a deep (54 ks) imaging observation of G310.6-1.6 to provide spectral diagnostics of the spatial components of this evidently complex system and map its SNR and PWN structure, to identify possible tori and jet-like structures. A detailed study of G310.6-1.6 will provide an important new example of the interaction of PSR/PWN/SNR in an extreme system.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
14:00:45.70	-63:25:42.60	IGR J14003-6326	ACIS-S	NONE	54

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500511

Title: TINY HICCUPS TO TITANIC EXPLOSIONS: Tackling Transients in Anomalous X-ray Pulsars

PI Name: Victoria Kaspi

The past decade has seen major progress in neutron star astrophysics, with the discovery of magnetars in general, and the recognition that the Anomalous X-ray Pulsars (AXPs) fall in this class. AXPs have recently revealed surprising and dramatic variability behavior, which theorists have begun to show are highly constraining of physical models of magnetars, including their crusts, atmospheres, coronae and magnetospheres. In this proposal, we request Chandra/ACIS-S Target-of-Opportunity observations of one major Anomalous X-ray Pulsar (AXP) outburst in AO12, in order to study in detail the evolution of the spectrum, pulsed fraction and pulse profile, for quantitative confrontation with recently developed models for the structure and electrodynamics of magnetars.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
10:50:08.90	-59:53:20.40	1E 1048.1-5937	ACIS-S	NONE	75
23:01:07.90	+58:52:46.00	1E 2259+586	ACIS-S	NONE	75
17:08:47.20	-40:08:50.70	RXS J1708-4009	ACIS-S	NONE	75
01:46:22.30	+61:45:07.00	4U 0142+61	ACIS-S	NONE	75
18:41:19.20	-04:56:12.50	1E 1841-045	ACIS-S	NONE	75
18:44:53.00	-02:56:40.00	AX J1845-0258	ACIS-S	NONE	75
01:00:43.10	-72:11:33.80	CXOU J0110043.1-721134	ACIS-S	NONE	75
18:09:51.10	-19:43:51.70	XTE J1810-197	ACIS-S	NONE	75
16:47:10.20	-45:52:17.00	CXOU J164710.2-455216	ACIS-S	NONE	75
18:46:24.50	-02:58:28.00	PSR J1846-0258	ACIS-S	NONE	75
15:50:55.30	-54:19:02.00	1E 1547.0-5408	ACIS-S	NONE	75
		New AXP	ACIS-S	NONE	75

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500549

Title: Jet-breaks in short GRBs

PI Name: Eleonora Troja

The degree of collimation in short GRBs is a key issue, bearing important information on the true energy release, the event rate and the nature of their progenitors. The detection of highly energetic short GRBs makes this issue more compelling. The intrinsic faintness of short GRB afterglows prevents jet-breaks to be detected with Swift/XRT observations. We propose to overcome this observational limit by triggering Chandra ToOs for a bright short GRB, carefully selected on the basis of its X-ray and optical afterglow properties at t=1d.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
		short GRB	ACIS-S	NONE	100

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500600

Title: Target-of-Opportunity Chandra Observations of Glitching High-B Radio Pulsars: Searching for Magnetar Metamorphoses

PI Name: Victoria Kaspi

We recently discovered a high-magnetic-field rotation-powered pulsar undergoing a "magnetar metamorphosis" simultaneously with a rotation glitch, transforming from an ordinary rotation-powered pulsar into a much brighter X-ray source with very different spectrum, and even possibly impacting on its nebular surroundings. After <8 weeks, the source returned to its normal state. This amazing event, caught serendipitously, suggests that all high-magnetic-field radio pulsars undergo such transient metamorphoses at glitch epochs, but have not been so recognized because of the absence of a sensitive X-ray all-sky monitor. We therefore request Chandra ToO observations of one high-magnetic-field radio pulsar when it has a large glitch or large X-ray burst in order to test this hypothesis.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
01:57:49.90	+62:12:25.90	PSR B0154+61	ACIS-S	NONE	105
07:26:08.10	-26:12:38.10	PSR J0726-2612	ACIS-S	NONE	105
08:47:57.00	-43:16:57.20	PSR J0847-4316	ACIS-S	NONE	105
10:01:32.20	-59:39:17.80	PSR J1001-5939	ACIS-S	NONE	105
11:19:14.30	-61:27:49.50	PSR J1119-6127	ACIS-S	NONE	105
16:32:39.70	-48:18:52.60	PSR J1632-4818	ACIS-S	NONE	105
17:18:10.00	-37:18:53.00	PSR J1718-3718	ACIS-S	NONE	105
17:26:07.50	-35:29:58.00	PSR J1726-3530	ACIS-S	NONE	105
17:34:26.60	-33:33:22.00	PSR J1734-3333	ACIS-S	NONE	105
18:14:43.10	-17:44:48.00	PSR J1814-1744	ACIS-S	NONE	105
18:19:33.80	-14:58:01.00	PSR J1819-1458	ACIS-S	NONE	105
18:21:34.30	-14:19:26.00	PSR 1821-1419	ACIS-S	NONE	105
18:47:35.20	-01:30:46.00	PSR J1847-0130	ACIS-S	NONE	105
19:13:50.80	+04:46:06.00	PSR J1913+0446	ACIS-S	NONE	105
19:18:23.60	+14:45:06.00	PSR B1916+14	ACIS-S	NONE	105
		New High-B pulsar	ACIS-S	NONE	105

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500613

Title: The Energetics and Environments of Type Ibc Supernovae

PI Name: Alicia Soderberg

Twenty-five years have passed since the peculiar class of Type Ibc supernovae were first recognized as a distinct flavor of core-collapse explosions. However, it is only recently that SNe Ibc have enjoyed a surge of interest thanks to their association with GRBs. Today, the most crucial question is whether SNe Ibc and GRBs arise from similar or distinct progenitor systems. Progress requires a detailed study of ordinary SNe Ibc which out-number GRBs by a factor of 100. Here we propose to continue our successful Chandra ToO program for SNe Ibc that is complemented by Swift/XRT and EVLA observations from our on-going programs.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
		SNIbc1	ACIS-S	NONE	10
		SNIbc2	ACIS-S	NONE	10

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500619

Title: Exploring the unusual extended emission around the highly magnetic RRATJ1819-1458

PI Name: Nanda Rea

We ask for a Chandra ACIS-S 90ks observation of RRATJ1819-1458 in order to search for variability and perform a detailed study of the extended X-ray emission discovered in a previous short Chandra observation. This RRAT has a 5x10^{13} Gauss magnetic field and is the only RRAT with a known X-ray counterpart and PWN. The relatively low rotational power and large characteristic age of RRATJ1819-1458 (\dot{E} = 3x10^{32} erg/s and tau = 117 kyr) makes the detection of this PWN very surprising, possibly pointing to an additional power for the pulsar wind, rather than the \dot{E} alone. The recent discovery of variability in the PWN of the high-B pulsar PSR J1846-0258 suggest that a similar behaviour might be observed for RRATJ1819-1458 and in fact be common among high magnetic field sources.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
18:19:34.10	-14:58:04.00	RRAT J1819-1458	ACIS-S	NONE	90

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500631

Title: A Deep Observation of Synchrotron X-ray Variability in SNR RX J1713.7-3946

PI Name: Yasunobu Uchiyama

The detection of synchrotron X-ray variability in SNR RX J1713.7-3946 has suggested that the interstellar magnetic field can be largely amplified at the expanding shock of a young SNR through magnetohydrodynamic waves generated by cosmic-rays themselves. We have conduced new Chandra ACIS-I observations (Cycle 10) of the northwestern shell of RX J1713.7-3946 in 2009, with a total exposure of 90 ks. Here we propose another 90 ks observation in 2010-2011, as a straightforward extension of the Cycle-10 program to largely enhance its scientific return. By comparing the images taken in Cycles 10 and 12, we will explore time variability in lower surface brightness regions thanks to increased statistics.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
17:11:45.50	-39:33:23.20	RX J1713.7-3946 NW	ACIS-I	NONE	90

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500646

Title: Constraining GRB physics through their afterglow light curves

PI Name: Evert Rol

Our current understanding of gamma-ray burst afterglow light curves has become increasingly confused, and the validity of the standard synchrotron fireball model for GRBs is nowadays increasingly questioned. In particular, achromatic breaks due to the the lateral expansion of the GRB jet are not substantiated by Swift X-ray observations. It is only through this that the true energies of GRBs are constrained, and questions such as the true rate of GRBs and the determination of cosmological parameters are based upon it. We propose to use CXO to construct the late time X-ray light curves for several Swift bursts. These observations will search for evidence of achromatic jet breaks, providing the necessary insight into the GRB evolution, and the energy and activity of the central engine.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
		GRB	ACIS-S	NONE	22

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500668

Title: The Pulsar Wind Nebula in DEM L241

PI Name: Frederick Seward

DEM L241 is a moderately bright SNR in the Large Magellanic Cloud. XMM has revealed but not resolved a PWN inside this remnant. Chandra's arcsec resolution makes possible a search for structure within the PWN and for the PSR itself as a point source. Any structure observed in the thermal part of the remnant will help determine age and evolution. Results will be particularly useful added to Chandra observations of 33 other MC remnants, 8 of which contain compact sources or PWN.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
05:35:60.00	-67:35:09.00	DEM L241	ACIS-S	NONE	50

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500689

Title: The X-Ray Emission from SN 1993J: Resolving Almost Two Decades of Conflict with Detailed Spectral Modeling

PI Name: Vikram Dwarkadas

Supernova (SN) 1993J is one of the closest, and consequently best observed SN in the Northern hemisphere. The large dataset has provided an unprecedented look into the dynamics, kinematics and evolution of the shock structures. Unfortunately the last good spectral quality observation of SN 1993J was in 2005-2006. We propose a 79 kilo-second observation of SN 1993J in Cycle 12. We will use this in conjunction with previous spectra to tune our hydrodynamic model and compute synthetic spectra using non-equilibrium ionization conditions,that can be compared directly to observed data. This will help us to precisely calibrate the circumstellar medium into which the SN is propagating, and discriminate between conflicting density profiles derived from radio VLBI data.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
09:55:24.80	+69:01:13.70	SN 1993J	ACIS-S	NONE	79

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500786

Title: VER J2019+407: UNIDENTIFIED TEV SOURCE IN THE GAMMA-CYGNI SNR

PI Name: Mark Theiling

VER J2019+407 is a newly discovered TeV source whose nature is unknown. Spatial coincidence with the complex NW region of the gamma-Cygni SNR (G78.2+2.1) implies possible cosmic-ray acceleration a the SNR shock. We propose a deep Chandra observation (50 ks) at the position of VER J2019+407 to reveal the nature of the X-ray counterpart to this new source, and to better understand its environment.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
20:19:52.80	+40:47:24.00	VER J2019+407	ACIS-I	NONE	50

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500795

Title: Completing Identification of the Nearest and Brightest Neutron Stars

PI Name: Derek Fox

Having completed a multi-year program of observations, including over 400 ksec of Swift X-ray and UV observations, we have identified 28 candidate neutron stars from among the 18,811 sources of the ROSAT Bright Source Catalog. With one of these confirmed as the eighth known isolated neutron star, and 20 others queued for observation, we request Chandra observations of seven final candidates to collect sub-arcsec positions and modest-quality X-ray spectra. Sub-arcsec X-ray positions are vital to confirm these objects as neutron stars by demonstrating the absence of optical counterparts to faint magnitudes (V > 25 mag), and yield blackbody temperatures and radii. Completion of this study has the potential to dramatically increase the number of bright, nearby neutron stars that are known.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
04:40:48.50	+29:24:34.50	1RXSJ044048.0+292440	ACIS-S	NONE	2
22:14:05.00	+39:39:03.40	1RXSJ221405.0+393855	ACIS-S	NONE	2
13:02:05.20	+15:51:34.80	1RXSJ130205.2+155122	ACIS-S	NONE	2
06:43:47.30	-39:12:54.40	1RXSJ064348.7-391256	ACIS-S	NONE	2
05:30:52.10	+52:15:58.30	1RXSJ053051.9+521606	ACIS-S	NONE	2
23:03:32.20	+15:20:17.10	1RXSJ230334.0+152019	ACIS-S	NONE	2
17:32:53.60	-37:12:00.00	1RXSJ173253.6-371200	ACIS-S	NONE	2

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500804

Title: Hunting for Anti-magnetars with Chandra

PI Name: Chi-Yung Ng

Central compact objects (CCOs) are an enigmatic class of neutron stars whose X-ray emission mechanism remains a mystery. Recent spin-down measurements revealed the CCO PSR J1852 as an "anti-magnetar", a pulsar with a very weak surface magnetic field, which is hard to reconcile with the high surface temperature and large pulsed fraction observed. We propose a complete Chandra census of all weak-field radio pulsars within 8kpc to search for more anti-magnetars. Any detection would confirm CCOs as a subset of radio pulsars, strongly constraining the physics of anti-magnetars.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
19:54:22.60	+29:23:17.30	PSR B1952+29	ACIS-S	NONE	5
17:39:38.30	-39:52:00.30	PSR J1739-3951	ACIS-S	NONE	5
14:25:36.60	-57:23:30.80	PSR J1425-5723	ACIS-S	NONE	5
06:09:58.90	+21:30:02.80	PSR J0609+2130	ACIS-S	NONE	5
11:07:34.50	-59:07:18.70	PSR J1107-5907	ACIS-S	NONE	5

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500822

Title: Radioactivity, Particle Acceleration, and Supernova Ejecta in the Youngest Galactic SNR G1.9+0.3

PI Name: Kazimierz Borkowski

X-rays in G1.9+0.3 are produced primarily by energetic electrons accelerated in its very fast blast wave. However, the radio-bright but X-ray faint northern shell shows prominent thermal emission from supernova ejecta. Doppler broadening velocities are of order 26,000 km/s. An additional spectral line at 4.1 keV is emitted by radioactive 44Sc produced by the electron-capture decay of 44Ti. The line flux implies an initial mass of 44Ti synthesized in the explosion of 1.9 x 10-5 solar masses. The spatial distribution of 44Sc hints at an asymmetric explosion. We propose a 1 Ms Chandra observation, with the primary goal of mapping 44Sc emission. This observation will establish the degree of asymmetry of the explosion, and may distinguish between core-collapse and Type Ia origin for G1.9+0.3.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
17:48:45.00	-27:10:00.10	G1.9+0.3	ACIS-S	NONE	1000

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500852

Title: The Persistent X-ray Emission from the Type IIL SN 1979C

PI Name: Daniel Patnaude

Models for the evolution of supernova that expand into stellar winds predict that the X-ray emission will drop with time. However, since it was first observed with ROSAT, the X-ray emission from SN 1979C in M100 has remained remarkably constant. Here we propose for a short, 15 ks Chandra ACIS-S observation of SN 1979C to monitor its evolution and to see if the X-ray emission has dropped since it was last observed, in 2008. We will combine these new observations with existing archival data to compare to models for supernova evolution and to models for emission from central compact objects.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
12:22:58.60	+15:47:51.70	SN 1979C	ACIS-S	NONE	15

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500889

Title: A High Resolution Study of the Vela X Cocoon

PI Name: Patrick Slane

Vela X is a nearby PWN which has undergone a reverse shock interaction with its host SNR. A distinct region in the central portions of the nebula, known as the cocoon, shows complex filament-like structure in the radio, and evidence of similar structure in XMM images. This region of the nebula also shows a concentration of TeV gamma-ray emission, and evidence for emission from ejecta that has been mixed into the nebula. We propose a 25~ks ACIS-I observation of the central cocoon region of Vela X to search for evidence of filamentary structure that may represent the Rayleigh-Taylor mixing zones, or perhaps regions of enhanced magnetic field associated with the reverse shock interaction.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
08:34:31.00	-45:45:33.00	Vela X Cocoon	ACIS-I	NONE	25

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500918

Title: The Astrophysics of the Most Energetic Gamma-Ray Bursts

PI Name: Andrew Fruchter

The Large Area Telescope (LAT) of Fermi has found a sample of highly relativistic gamma-ray bursts (GRBs), which may be among the most energetic bursts ever discovered. Here we propose to use Chandra and HST to follow the late time X-ray and optical light curves of a LAT detected burst that also has excellent early multiwavelength coverage. Our observations, in conjunction with the Fermi data, will allow us to measure the energy and the bulk Lorentz factor of the explosion. Recent work on some of the most powerful GRBs begins to substantially constrain physical models of the progenitors. The energetics of the highly relativistic LAT bursts may greatly strengthen these constraints and provide new insight into the currently unknown mechanism that determines the energy in a GRB.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
		LAT Burst 1	ACIS-I	NONE	120

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 12500923

Title: SEARCH FOR JET BREAKS IN LONG GRB X-RAY AFTERGLOWS

PI Name: David Burrows

In the standard fireball model for GRB afterglows, the jet opening angle can be determined from the achromatic jet break time by measuring the time at which this break in the light curve occurs. Swift XRT observations have shown that jet breaks are not observed in the first several days or weeks of a typical X-ray afterglow. This has important implications for the derived energetics of the GRB itself that cannot be resolved without a more complete sample of observed jet breaks. We propose to follow 4 carefully chosen long GRB afterglows with late-time Chandra observations in order to search for jet breaks occurring after the Swift observations end.

Target Name	Det.	Grating	Exp.Time
GRB AO12-01	ACIS-S	NONE	60
GRB AO12-02	ACIS-S	NONE	60
GRB AO12-03	ACIS-S	NONE	60
GRB AO12-04	ACIS-S	NONE	60

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