Accepted Cycle 15 Observing Proposals

SN, SNR & ISOLATED NS

Proposal Number	Subject Category	PI Name	Type	Time (ks)	Title
15500072	SN, SNR AND ISOLATED NS	Halpern	GO	30	Measuring the Proper Motion of the Quiet Pulsar Calvera
15500090	SN, SNR AND ISOLATED NS	Halpern	GO	99	A Fifteen-Year Ephemeris for the CCO Pulsar in Puppis A
15500152	SN, SNR AND ISOLATED NS	Fong	TOO	60	Measuring the Explosion Geometry of Short GRBs: Implications for Energetics and Rates
15500155	SN, SNR AND ISOLATED NS	Burrows	GO	150	CHANDRA CYCLE 15 SPATIAL AND SPECTRAL MONITORING OF SN 1987A
15500176	SN, SNR AND ISOLATED NS	Tiengo	TOO	70	Measuring magnetar distance from the dust echo of a bright burst
15500190	SN, SNR AND ISOLATED NS	Weisskopf	TOO	70	Pre-Planned Target of Opportunity (ToO) Observations of the Crab Nebula upon the Occurrence of the Next Gamma-Ray Flare
15500198	SN, SNR AND ISOLATED NS	Weisskopf	GO	120	Joint Chandra and HST Monitoring and Studies of the Crab Nebula
15500264	SN, SNR AND ISOLATED NS	Maccarone	TOO	40	Calcium rich transients: tidal detonations of white dwarfs?
15500269	SN, SNR AND ISOLATED NS	Maccarone	GO	30	SN 2012hn: a tidal detonation event?
15500319	SN, SNR AND ISOLATED NS	Chandra	TOO	80	Tracing the X-ray emission from Type IIn supernovae
15500322	SN, SNR AND ISOLATED NS	Ofek	TOO	60	Testing the shock interaction hypothesis for hydrogen-poor super luminoius supernova
15500363	SN, SNR AND ISOLATED NS	Kaspi	TOO	105	Target-of-Opportunity Chandra Observations of Glitching High-B Radio Pulsars: Searching for Magnetar Metamorphoses
15500376	SN, SNR AND ISOLATED NS	Chandra	GO	40	The remarkable X-ray evolution of SN 2010jl
15500421	SN, SNR AND ISOLATED NS	Bernardini	GO	40	Unveiling the nature of cyclical behavior in the period evolution of the Anomalous X ray Pulsar XTE J1810-197
15500430	SN, SNR AND ISOLATED NS	Sakamoto	TOO	40	Identification of the Host Galaxy of Swift Short GRBs by the Chandra Sub-arcsecond Position
15500437	SN, SNR AND ISOLATED NS	Rea	TOO	85	PROMPT STUDY OF MAGNETAR OUTBURSTS WITH CHANDRA
15500567	SN, SNR AND ISOLATED NS	De Luca	GO	100	DEEP CHANDRA IMAGING OF THE GAMMA-RAY ONLY PULSAR PSR J1135-6055 AND ITS BENT JETS
15500573	SN, SNR AND ISOLATED NS	Slane	GO	30	Following the Temperature of a Neutron Star
15500577	SN, SNR AND ISOLATED NS	Gotthelf	GO	63	Where Have All The Central Compact Objects Gone?
15500590	SN, SNR AND ISOLATED NS	Troja	TOO	120	The collimation and energetics of short gamma-ray bursts
15500612	SN, SNR AND ISOLATED NS	Kaspi	GO	90	What is the Magnetic Field of Magnetar Swift J1822.3-1606?
15500616	SN, SNR AND ISOLATED NS	Racusin	TOO	120	Constraining the Energetics of Fermi-LAT GRBs with Chandra
15500621	SN, SNR AND ISOLATED NS	Williams	GO	150	Dynamics of a Type Ia SNR: Proper Motions in Tycho
15500730	SN, SNR AND ISOLATED NS	Dwarkadas	GO	115	REVISITING TWO OF THE BRIGHTEST TYPE IINS: HOW THE MIGHTY ARE FALLING - AND PERHAPS RISING AGAIN
15500737	SN, SNR AND ISOLATED NS	Ray	TOO	160	State of the shocked plasma: X-ray and radio signatures from type IIP supernovae
15500763	SN, SNR AND ISOLATED NS	Borkowski	GO	150	Dynamics of the Remnant of Kepler's Type Ia Supernova
15500831	SN, SNR AND ISOLATED NS	Soderberg	TOO	20	The Energetics and Environments of Type Ibc Supernovae
15500874	SN, SNR AND ISOLATED NS	Pavan	GO	250	DEEP STUDY OF THE 20PC-LONG PRECESSING JET IN IGR J11014-6103
15500895	SN, SNR AND ISOLATED NS	Fruchter	TOO	120	The Astrophysics of the Most Energetic Gamma-Ray Bursts

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500072

Title: Measuring the Proper Motion of the Quiet Pulsar Calvera

Type: GO Total Time (ks): 30

PI Name: Jules Halpern

Calvera is a 59 ms X-ray pulsar at high Galactic latitude that was selected from the ROSAT All-Sky Survey. The absence of a PWN, radio, or gamma-ray emission, suggested that Calvera is a passively cooling NS and a nearby candidate for the elusive descendants of the central compact objects (an orphaned CCO). We recently measured the spin-down rate of Calvera, which, on the contrary, shows that it is surprisingly energetic. This makes it very difficult to understand its location and relative silence. In any scenario for Calvera's birth, whether in the Galactic disk or halo, its proper motion vector could be large and easily measured by Chandra, which will shed light on its origin. Deep optical images will help determine its distance and emission mechanisms.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
14:12:59.30	+79:19:58.20	CXOU J141259.3+791958	HRC-I	NONE	30

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500090

Title: A Fifteen-Year Ephemeris for the CCO Pulsar in Puppis A

Type: GO Total Time (ks): 99

PI Name: Jules Halpern

We detected spin-down of the pulsar in Puppis A, which requires a dipole magnetic field of only 2.8e10 G, the smallest of any young neutron star. This confirms the anti-magnetar scenario for CCOs. PSR J0821-4300 also has an X-ray spectral feature that is either an emission line at 0.75 keV or an absorption line at 0.46 keV, which is consistent with an electron cyclotron resonance at roughly the spin-down magnetic field strength. We propose to extend the time span of the ephemeris from 3 years to 15 years by linking new and archival data, measuring the spin-down rate to 0.1 percent and seeing if it is stable over this time span. This will test for any torque noise due to accretion of supernova ejecta, which is the most plausible mechanism for generating an emission line in the spectrum.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
08:21:57.30	-43:00:17.30	PSR J0821-4300	ACIS-S	NONE	99

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500152

Title: Measuring the Explosion Geometry of Short GRBs: Implications for Energetics and Rates

Type: TOO Total Time (ks): 60

PI Name: Wen-Fai Fong

Short GRB afterglows can provide a wealth of information on fundamental properties such as energy and geometry. The geometry is of particular interest because it affects the true energy scale and event rates, with implications for the explosion physics and progenitors. The collimation angles are measured from "jet breaks" in the afterglow light curves, yet only 2 short GRB jet breaks have been discovered so far (both with Chandra) due to the faintness of the optical and radio emission. To probe the relevant range of angles we require Chandra observations at ~5-20 days. Here we propose follow-up for a short GRB with a bright X-ray afterglow (determined from Swift/XRT at <1 day), which will allow us to measure angles of 5-15 deg, or place a meaningful lower bound of >10-20 deg.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
		Short-GRB-1	ACIS-S	NONE	60

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500155

Title: CHANDRA CYCLE 15 SPATIAL AND SPECTRAL MONITORING OF SN 1987A

Type: GO Total Time (ks): 150

PI Name: David Burrows

Regular monitoring of SN 1987A, the only supernova remnant in which we can study the early developmental stages in detail, is critical to testing models of remnant evolution, nonequilibrium ionization processes, thin plasma spectra, and physical processes in dusty plasmas. SN 1987A 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 SN 1987A at roughly six month intervals in Cycle 15.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
05:35:28.00	-69:16:11.10	SN 1987A	ACIS-S	HETG	75
05:35:28.00	-69:16:11.10	SN 1987A	ACIS-S	HETG	75

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500176

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

Type: TOO Total Time (ks): 70

PI Name: Andrea Tiengo

In 2009 we 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 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. This proposal was accepted in Cycle 12, 13 and 14, but it has not been triggered yet.

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

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500190

Title: Pre-Planned Target of Opportunity (ToO) Observations of the Crab Nebula upon the Occurrence of the Next Gamma-Ray Flare

Type: TOO Total Time (ks): 70

PI Name: Martin Weisskopf

The Crab Nebula (with its central pulsar) has been an emblematic source in high-energy astrophysics for nearly fifty years and remains a continuing source of scientific stimulus. The recent stunning discovery of rapid g-ray variability (up to 1 GeV) demonstrates that the nebula differs from the description found in most recent theoretical models. Our scientific objective is to locate the source of these g-ray flares, which would be a giant step toward understanding them.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
05:34:31.60	+22:00:56.40	Crab	HRC-S	LETG	70

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500198

Title: Joint Chandra and HST Monitoring and Studies of the Crab Nebula

Type: GO Total Time (ks): 120

PI Name: Martin Weisskopf

The scientific purpose of this proposal is three-fold: (1) Continue to quantify and correlate the Crab s X-ray and optical, temporal and spatial variations, developing a legacy database for high-spatial-resolution studies of this astrophysical archetype; (2) identify and explore phenomena responsible for the recently discovered fact that the Crab is not a standard candle in hard X-rays; and (3) establish X-ray and optical baselines, to aid in determining the location and physics of the Crab s gamma-ray flares.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
05:34:31.60	+22:00:56.40	Crab	ACIS-S	NONE	120

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500264

Title: Calcium rich transients: tidal detonations of white dwarfs?

Type: TOO Total Time (ks): 40

PI Name: Thomas Maccarone

We propose for a 40 kilosecond TOO observation of a new Ca-rich gap transient. These enigmatic objects, with properties intermediate between those of classical novae and Type Ia supernovae, can be well-explained by tidal detonations of low mass white dwarfs by intermediate mass black holes. In such a case, fall-back accretion of the tidal debris would power an X-ray source for which we propose to search. Because supermassive black holes will swallow white dwarfs whole, a successful outcome to this proposal would both explain the Ca-rich gap transients *and* establish the existence of intermediate mass black holes.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
		Ca-rich gap transient	ACIS-S	NONE	40

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500269

Title: SN 2012hn: a tidal detonation event?

Type: GO Total Time (ks): 30

PI Name: Thomas Maccarone

We propose for a 30 kilosecond observation of SN 2102hn, a Ca-rich gap transient. These enigmatic objects, with properties intermediate between those of classical novae and Type Ia supernovae, can be well-explained by tidal detonations of low mass white dwarfs by intermediate mass black holes. In such a case, fall-back accretion of the tidal debris would power an X-ray source for which we propose to search. Because supermassive black holes will swallow white dwarfs whole, a successful outcome to this proposal would both explain the Ca-rich gap transients *and* establish the existence of intermediate mass black holes.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
06:42:42.60	-27:26:49.80	SN 2012hn	ACIS-S	NONE	30

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500319

Title: Tracing the X-ray emission from Type IIn supernovae

Type: TOO Total Time (ks): 80

PI Name: Poonam Chandra

Type IIn supernovae (SNe IIn) are a heterogeneous class of supernovae believed to be powered by dense circumstellar interaction. However, neither their evolutionary status nor the origin of the tremendous mass loss from their progenitors is known. X-ray emission from shock heated gas is crucial for the energetics of the interaction and serve as a crucial diagnostic. X-rays combined with multiwavelength studies can constrain the progenitor systems and lead to a wealth of information about the surrounding medium, ejecta density, and structure of SNe IIn. Here we request joint Chandra and Swift-XRT time and propose to do Chandra-ACIS Spectroscopy at two epochs, of one Type IIn supernova that has optical emission brighter than $-19$ absolute magnitude and has been detected by Swift-XRT.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
		SN-IIN	ACIS-S	NONE	80

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500322

Title: Testing the shock interaction hypothesis for hydrogen-poor super luminoius supernova

Type: TOO Total Time (ks): 60

PI Name: Eran Ofek

SLSN-I are a class of bright supernovae (SNe) with peak absolute magnitude in excess of -21, relatively long rise time, and no hydrogen or helium signature in their spectra. The nature of these SNe is unclear. Here we suggest a Chandra 60ks Target of Opportunity program that will enable to test if SLSN-I are powered by interaction of a SN ejecta with massive circum-stellar matter. The goal of the proposed Chandra observations is to look for X-ray emission at both early and late times, and to resolve the puzzle of their power source. We suggest to observe a single SLSN-I event which luminosity distance is smaller than 500 Mpc.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
		ToO-early	ACIS-S	NONE	60

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500363

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

Type: TOO Total Time (ks): 105

PI Name: Victoria Kaspi

In 2006 observations of a high-magnetic-field rotation-powered pulsar (RPP), we observed a sudden "magnetar metamorphosis" simultaneous with a rotation glitch. The RPP's X-ray flux increased by a factor of 10, its spectrum changed dramatically, and it emitted magnetar-like X-ray bursts. After <8 weeks, it returned to its normal state. This amazing event, caught serendipitously, suggests that all high-magnetic-field RPPs may undergo 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 RPP when it has a large glitch or X-ray burst in order to test this hypothesis.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
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
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
10:01:32.20	-59:39:17.80	PSR J1001-5939	ACIS-S	NONE	105
17:40:33.80	-30:15:43.50	PSR B1737-30	ACIS-S	NONE	105

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500376

Title: The remarkable X-ray evolution of SN 2010jl

Type: GO Total Time (ks): 40

PI Name: Poonam Chandra

SN 2010jl is a bright Type IIn (narrow line) supernova (SN) shown to have luminous X-ray emission. Our three Chandra ACIS-S observations taken at 2, 12, and 20 months after the SN discovery show dramatically different spectra primarily due to strong evolution of the X-ray absorption. The spectra indicate high temperatures and high absorbing column densities. This is the first time an external circumstellar X-ray absorption has been clearly observed in a SN, giving us a rare opportunity to follow the evolution of the external column density and obtain unique information on circumstellar structure and the shock interaction. In this proposal we request a 40 ks of Chandra ACIS-S observation of SN 2010jl during Cycle 15.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
09:42:53.30	+09:29:41.80	SN 2010jl	ACIS-S	NONE	40

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500421

Title: Unveiling the nature of cyclical behavior in the period evolution of the Anomalous X ray Pulsar XTE J1810-197

Type: GO Total Time (ks): 40

PI Name: Federico Bernardini

This program is aimed at obtaining a phase-coherent timing solution for the period evolution of XTEJ1810-197 (XTEJ), continuing the successful X-ray monitoring of this unique Anomalous X-ray Pulsar (AXP).AXPs are Magnetars, isolated neutron star (NS) whose emission is likely due to the decay of an extremely strong magnetic field, 10e+(14-15) G.The requested pointings are aimed at studying the period evolution of XTEJ, by means of phase connected timing analysis, with the goal of demonstrating the presence of a long term (5 yr) precession of its rotation axis. XTEJ could be a unique precessing Magnetar (only 3 candidate precessing NSs are known).This would shed light on the physical properties of the NS crust/core core and on the physical properties of matter at extremely high density.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
18:09:51.10	-19:43:51.90	XTEJ 1810-197	ACIS-S	NONE	40

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500430

Title: Identification of the Host Galaxy of Swift Short GRBs by the Chandra Sub-arcsecond Position

Type: TOO Total Time (ks): 40

PI Name: Takanori Sakamoto

We propose a continuation of our successful ToO program to observe short GRBs detected by Swift to identify the afterglow in X-rays by a sub-arcsecond position from Chandra. Our ToO program will increase the number of short GRBs having an unambiguous host galaxy identification, and also should provide a much less biased sample host galaxies of short GRBs. We request a maximum of 2 ToOs for 20 ksec each based on the estimation of previous Swift short GRB observations. Our trigger criteria are 1) Swift short GRBs localized by Swift/XRT and 2) no afterglow confirmation in optical within 5 hours after the burst. We request <1-3 days response to our ToO, so that the afterglow can be observed while still bright.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
		Short GRB ToO	ACIS-S	NONE	20
		Short GRB ToO	ACIS-S	NONE	20

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500437

Title: PROMPT STUDY OF MAGNETAR OUTBURSTS WITH CHANDRA

Type: TOO Total Time (ks): 85

PI Name: Nanda Rea

The discovery of transient magnetars has opened a new perspective in the field confirming that a relatively large number of members of this class has not been discovered yet, and suggesting that others would manifest themselves in the future through outbursts. This proposal is aimed at gathering new insights on the physics of magnetars through the study of their outbursts. In particular, we are asking for 85ks of Chandra time divided in 4 observations throughout the outburst from a known or still unknown magnetar candidate.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
		NEWMAGNETAR	ACIS-S	NONE	85
10:50:07.10	-59:53:21.40	1E1048.1-5937	ACIS-S	NONE	85
17:08:46.00	-40:08:53.00	RXSJ170849-400910	ACIS-S	NONE	85
18:41:19.40	-04:56:10.90	1E1841-04	ACIS-S	NONE	85
18:44:54.70	-02:56:53.40	AXJ1844-0256	ACIS-S	NONE	85
20:13:52.80	+34:19:55.20	SGR 2013+34	ACIS-S	NONE	85
23:01:08.30	+58:52:44.50	1E 2259+584	ACIS-S	NONE	85
19:07:14.30	+09:19:20.10	SGR 1900+14	ACIS-S	NONE	85
16:35:51.80	-47:35:23.30	SGR 1627-41	ACIS-S	NONE	85
18:08:39.30	-20:24:39.50	SGR 1806-20	ACIS-S	NONE	85
05:26:00.90	-66:04:36.30	SGR 0526-66	ACIS-S	NONE	85
05:01:06.20	+45:16:35.00	SGR 0501+4516	ACIS-S	NONE	85
15:50:55.30	-54:19:02.00	1E 1547.0-5408	ACIS-S	NONE	85
18:46:24.50	-02:58:28.00	PSR J1846-0258	ACIS-S	NONE	85
18:33:44.40	-08:31:07.70	SGR 1833-0832	ACIS-S	NONE	85
16:22:44.80	-49:50:54.40	PSR 1622-4950	ACIS-S	NONE	85
17:14:05.70	-38:10:30.90	CXO 171405-381031	ACIS-S	NONE	85
18:22:18.00	-16:04:26.80	Swift 1822-1606	ACIS-S	NONE	85
16:47:10.20	-45:52:17.00	CXO J164710.2-455216	ACIS-S	NONE	85
04:18:33.90	+57:32:22.90	SGR 0418+4729	ACIS-S	NONE	85
01:46:22.40	+61:45:03.30	4U0142+614	ACIS-S	NONE	85
18:34:52.10	-08:45:56.00	Swift 1834-0836	ACIS-S	NONE	85
01:00:43.10	-72:11:34.00	CXOUJ0100-7211	ACIS-S	NONE	85

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500567

Title: DEEP CHANDRA IMAGING OF THE GAMMA-RAY ONLY PULSAR PSR J1135-6055 AND ITS BENT JETS

Type: GO Total Time (ks): 100

PI Name: Andrea De Luca

The Large Area Telescope (LAT) onboard the Fermi mission opened a new era for pulsar astronomy, detecting pulsations from more than 100 gamma-ray pulsars, about 30% of which are not seen at radio wavelengths. One of the most recent entries in the -ray only family is PSR J1135-6055, an energetic pulsar located at a few kpc, likely associated to the radio supernova remnant G293.8+0.6. An archival 35ks observation unveils a peculiar pulsar wind nebula, reminiscent of a pair of anti-podal jets originating from the pulsar and bending in the ISM.We propose a deep ACIS-S observation of the system, in order to assess the morphology of the diffuse features. Chandra imaging and spatially-resolved spectroscopy of this nebula could teach us a lot about pulsar winds.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
11:35:08.30	-60:55:36.50	PSR J1135-6055	ACIS-S	NONE	100

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500573

Title: Following the Temperature of a Neutron Star

Type: GO Total Time (ks): 30

PI Name: Patrick Slane

Chandra observations of the neutron star in Cas A have revealed a stunning decrease in its X-ray flux and surface temperature over the course of less than 10 years. This rapid cooling implies the onset of a phase change to neutron superfluidity in the neutron star interior, and places strong constraints on nucleon pairing and the neutron star mass. We propose an observation of 1WGA J1713.4-3949, the young neutron star in the supernova remnant G347.3-0.5, to search for any evidence of a similar associated flux decline since its initial observation in Chandra Cycle 1. Detection of such cooling will strengthen constraints on the complex physics of neutron star interiors.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
17:13:28.00	-39:49:48.00	1WGA J1713.4-3949	ACIS-I	NONE	30

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500577

Title: Where Have All The Central Compact Objects Gone?

Type: GO Total Time (ks): 63

PI Name: Eric Gotthelf

The central compact object class of young neutron stars in supernova remnants are detected only as thermal X-ray sources. Characterized by weak magnetic fields, a fundamental puzzle of their evolution is the absence of any evidence for their numerous descendants in X-ray or radio surveys. We know that their characteristic timing ages are much older than their real ages, which implies that some apparently old radio pulsars may actually be "orphaned CCOs" that are young enough to detect as cooling X-ray sources. Here we propose a small survey of radio pulsars with similarly weak B-fields as CCOs to see if we can find young, bright ones that qualify as immediate descendants of CCOs.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
00:51:30.10	+04:22:49.00	PSR J0051+0423	ACIS-S	NONE	3.5
01:37:23.80	+16:54:42.10	PSR J0137+1654	ACIS-S	NONE	3.5
03:35:16.60	+45:55:53.40	PSR J0335+4555	ACIS-S	NONE	3.5
05:20:36.10	-25:53:12.20	PSR J0520-2553	ACIS-S	NONE	3.5
06:56:48.90	-54:49:14.90	PSR J0656-5449	ACIS-S	NONE	3.5
14:10:07.30	-74:04:53.30	PSR J1410-7404	ACIS-S	NONE	3.5
16:07:48.70	-64:49:43.00	PSR J1607-6449	ACIS-S	NONE	3.5
16:27:52.50	-59:36:55.30	PSR J1627-5936	ACIS-S	NONE	3.5
16:52:16.60	-14:00:27.40	PSR J1652-1400	ACIS-S	NONE	3.5
18:07:38.00	-08:47:43.20	PSR J1807-0847	ACIS-S	NONE	3.5
18:13:38.70	+18:22:15.00	PSR J1813+1822	ACIS-S	NONE	3.5
19:11:55.30	+17:58:45.70	PSR J1911+1758	ACIS-S	NONE	3.5
21:56:23.70	+26:18:30.40	PSR J2156+2618	ACIS-S	NONE	3.5
22:23:03.20	+29:23:58.60	PSR J2222+2923	ACIS-S	NONE	3.5
23:07:41.20	+22:25:50.10	PSR J2307+2225	ACIS-S	NONE	3.5
13:34:30.10	-58:39:16.50	PSR J1334-5839	ACIS-S	NONE	3.5
17:55:41.80	-27:25:45.00	PSR J1755-2725	ACIS-S	NONE	3.5
20:48:45.80	+22:55:05.30	PSR J2048+2255	ACIS-S	NONE	3.5

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500590

Title: The collimation and energetics of short gamma-ray bursts

Type: TOO Total Time (ks): 120

PI Name: Eleonora Troja

The degree of collimation in short GRBs is a key issue, bearing critical information on the true energy release, the event rate and the nature of the GRB progenitor. The geometry of the GRB outflow can be constrained through afterglow observations, and, in particular, through the measurement of the so-called ``jet-breaks''. The intrinsic faintness of short GRB afterglows prevents jet-breaks to be detected with Swift/XRT observations. We propose to overcome this limit by triggering deep Chandra ToOs observations of short GRB afterglows.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
		GRB	ACIS-S	NONE	60
		GRB	ACIS-S	NONE	60

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500612

Title: What is the Magnetic Field of Magnetar Swift J1822.3-1606?

Type: GO Total Time (ks): 90

PI Name: Victoria Kaspi

In recent years, the mean magnetic field of known magnetars has been lowered by discoveries of sources with magnetic fields < 1x10^14 G. In particular, Swift J1822.3-1606 and SGR 0418+5729 appear to have fields that are ~1x10^13 G. This begs the question of how low the true magnetic field distribution of magnetars stretches and whether it is in fact distinct from that of the main pulsar population. Here we propose to perform phase-coherent timing of Swift J1822.3-1606 with Chandra. With our proposed timing campaign we will be able to distinguish between ambiguous measurements now present in the literature and determine the true spin-inferred magnetic field of this interesting object.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
18:22:18.10	-16:04:25.50	Swift J1822.3-1606	ACIS-S	NONE	90

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500616

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

Type: TOO Total Time (ks): 120

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 usually do not reveal 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 (ks)
		GRB AO15-1	ACIS-S	NONE	60
		GRB AO15-2	ACIS-S	NONE	60

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500621

Title: Dynamics of a Type Ia SNR: Proper Motions in Tycho

Type: GO Total Time (ks): 150

PI Name: Brian Williams

Type Ia SNe are of fundamental importance in astrophysics, yet the nature of their environments and progenitor systems is poorly understood. We propose a new epoch of imaging of Tycho's SNR, with the goal of expanding the baseline for proper motions to as many as 14 years. In a recent work, we have shown that the ISM surrounding Tycho is non-uniform, in agreement with the limited proper motion studies that have been done in radio and X-rays. The dynamics of the forward shock can be used to localize the explosion site. A new epoch will also allow the first ever study of ejecta dynamics in a Type Ia SNR, including the proper motion of individual elements, which reflect the ejecta structure at the time of explosion and can distinguish between various explosion models for Type Ia SNe.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
00:25:19.30	+64:07:55.60	Tycho	ACIS-I	NONE	150

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500730

Title: REVISITING TWO OF THE BRIGHTEST TYPE IINS: HOW THE MIGHTY ARE FALLING - AND PERHAPS RISING AGAIN

Type: GO Total Time (ks): 115

PI Name: Vikram Dwarkadas

Type IIn Supernovae (SNe) form the highest luminosity class of X-ray SNe, excluding those associated with gamma-ray bursts. Yet their progenitors remain a mystery. In this proposal we aim to investigate two of the brightest Type IIn SNe, SN 2005kd and SN 2006jd. SN 2005kd appeared to be fading most rapidly, but then brightened again last year, leading to a very interesting evolution. SN 2006jd has a reasonably well-sampled light curve, although the high-temperature spectrum has been difficult to constrain. Coupling this spectrum with previous data, and hydrodynamical simulations, we will model the evolution of the X-ray emission, use it to place limits on the ambient medium density, and thereby the SN progenitor, providing clues to the progenitors of Type IIn SNe.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
04:03:16.90	+71:43:18.90	SN 2005kd	ACIS-S	NONE	30

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500737

Title: State of the shocked plasma: X-ray and radio signatures from type IIP supernovae

Type: TOO Total Time (ks): 160

PI Name: Alak Ray

Type IIP Supernovae arise from massive stars that end their lives as Red Supergiants. Shock wave from the explosion interacts with a complex circumstellar medium originating from the parent star in winds or episodic ejections. Particles can be accelerated to relativistic energies which radiate by synchrotron process in the shock-amplified magnetic fields and inverse Compton scattering against optical/ UV photons from the supernova. Thermal emission can result from the reverse shock reheating the expanding cold ejecta. These processes have different signatures in radio and X-ray bands which can be disentangled in bright events. Multiple Chandra observations can probe the history of variable mass loss from the progenitor star.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
		SN IIP ToO	ACIS-S	NONE	160

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500763

Title: Dynamics of the Remnant of Kepler's Type Ia Supernova

Type: GO Total Time (ks): 150

PI Name: Kazimierz Borkowski

The remnant of Kepler's Type Ia SN shows an interaction of SN ejecta with a highly asymmetric ambient circumstellar medium (CSM). This material was ejected by a single-degenerate progenitor prior to the explosion, and its complex spatial distribution contains invaluable information about the progenitor itself. We propose a third-epoch observation of Kepler's SNR that will provide us with much improved expansion rates, allowing for measurements of shock speeds along the whole periphery of the remnant. These measurements will be compared with 3-D hydrodynamic simulations, thus unraveling the true shape of the CSM in a Type Ia progenitor. They will also advance our knowledge of poorly-understood particle acceleration and magnetic field amplification processes in fast SNR shocks.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
17:30:41.20	-21:29:31.40	Kepler's Supernova Remnant	ACIS-S	NONE	150

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500831

Title: The Energetics and Environments of Type Ibc Supernovae

Type: TOO Total Time (ks): 20

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. Their low volumetric rate and optical heterogeneity did not initially motivate strong observational programs. SNe Ibc have enjoyed a surge of interest thanks to the observational realization that most long-duration gamma-ray bursts (GRBs) are accompanied by SNe Ibc. The converse, however, is not true: we recently measured the fraction of SNe Ibc harboring relativistic GRB jets to be just 1%. The progenitors of SNe Ibc and their relation to those of GRB-SNe have yet to be observationally identified. Here we propose a modest Chandra program to enable progress.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
		SN1	ACIS-S	NONE	10
		SN2	ACIS-S	NONE	10

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500874

Title: DEEP STUDY OF THE 20PC-LONG PRECESSING JET IN IGR J11014-6103

Type: GO Total Time (ks): 250

PI Name: Lucia Pavan

IGR J11014-6103 is a unique X-ray emitter comprising: (1) a run-away pulsar with the highest known kick velocity to date, (2) an elongated wind nebula trailing behind it (detected in radio and X-rays), and (3) a collimated jet-like feature extending over 20 parsecs. The peculiar shape and orientation of this feature suggests this could be the most elongated precessing pulsar jet ever detected in our Galaxy. Due to the limited exposure time of the data available so far however two competing scenarios still remain to be investigated. With this proposal, we aim at unveiling the real nature of the jet through a 250 ksec observation of IGR J11014-6103 with Chandra/ACIS-I, fully exploiting the unique high angular resolution and large field-of-view capabilities of this instrument.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
11:01:45.00	-61:01:39.60	IGR J11014-6103	ACIS-I	NONE	250

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 15500895

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

Type: TOO Total Time (ks): 120

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 of a GRB.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time (ks)
		LAT Burst 1	ACIS-S	NONE	120

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