Cycle 4 Large Projects

Subject Category	PI Name	Title
NORMAL STARS AND WD	MICHAEL CORCORAN	UNVEILING ETA CAR: CHANDRA OBSERVATIONS DURING THE 2003.5 EVENT
NORMAL STARS AND WD	ERIC FEIGELSON	AN ULTRADEEP CHANDRA STUDY OF THE ORION NEBULA (GUEST OBSERVER PORTION)
SN, SNR AND ISOLATED NS	PATRICK SLANE	A DETAILED STUDY OF 3C58 - THE YOUNGEST KNOWN PULSAR NEBULA IN THE GALAXY
SN, SNR AND ISOLATED NS	JOHN HUGHES	STUDYING HIGH MACH NUMBER SHOCKS IN YOUNG SUPERNOVA REMNANTS WITH CHANDRA
SN, SNR AND ISOLATED NS	FREDERICK SEWARD	SUPERNOVA REMNANTS IN THE MAGELLANIC CLOUDS
SN, SNR AND ISOLATED NS	GEORGE PAVLOV	FIRST MEASUREMENT OF THE GRAVITATIONAL REDSHIFT AT THE SURFACE OF A NEUTRON STAR
ACTIVE GALAXIES AND QUASARS	JELLE KAASTRA	CONNECTING THE X-RAY AND UV IONIZED ABSORBERS IN MRK 279
CLUSTERS OF GALAXIES	CALEB SCHARF	SURVEYING THE FORNAX CLUSTER OF GALAXIES
CLUSTERS OF GALAXIES	JOHN HUGHES	CHANDRA OBSERVATIONS OF DLS SHEAR-SELECTED CLUSTERS
EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS	CHRISTINE JONES	A CHANDRA WIDE-FIELD SURVEY TO MAP THE COSMIC WEB AND INVESTIGATE THE EVOLUTION OF NUCLEAR ACCRETION
EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS	CHRISTINE JONES	A CHANDRA WIDE-FIELD SURVEY TO MAP THE COSMIC WEB AND INVESTIGATE THE EVOLUTION OF NUCLEAR ACCRETION

NORMAL STARS AND WD

Proposal Title: UNVEILING ETA CAR: CHANDRA OBSERVATIONS DURING THE 2003.5 EVENT

PI Name: MICHAEL CORCORAN

Understanding the supermassive star Eta Car is important for a variety of topics: the formation and evolution of extremely massive stars and their influence on their environments. Eta Car has been a mystery since its giant eruption in the 1840s. A possible key to the puzzle is the identification of periodic changes in some near IR emission lines, and the discovery of repeatable X-ray eclipses. The next X-ray eclipse will occur during AO4, and we propose to use HETG to observe the variations in the spectral and spatial distribution of the emission during this event. In conjunction with scheduled HST/STIS, INTEGRAL, IR and optical spectroscopy, and radio observations, these HETG observation provide key in formation which may finally help us solve the riddle of this star.

Proposal #	Target Name	RA	DEC	Inst.	Grat.	Exp. Time	Seq. #	ObsID
04200312	ETA CARINAE	161.265000	-59.684528	ACIS-S	HETG	100.000000	200215	3745
04200312	ETA CARINAE	161.265000	-59.684528	ACIS-S	HETG	100.000000	200216	3746
04200312	ETA CARINAE	161.265000	-59.684528	ACIS-S	HETG	100.000000	200217	3747
04200312	ETA CARINAE	161.265000	-59.684528	ACIS-S	HETG	100.000000	200218	3748
04200312	ETA CARINAE	161.265000	-59.684528	ACIS-S	HETG	100.000000	200219	3749

NORMAL STARS AND WD

Proposal Title: AN ULTRADEEP CHANDRA STUDY OF THE ORION NEBULA (GUEST OBSERVER PORTION)

PI Name: ERIC FEIGELSON

We propose a 850 ks ACIS-I observation of the Orion Nebula spanning 11.5 contiguous days, with GTO Teams providing 150 ks of the time. The Orion Nebula is the best target in the sky for Chandra study of stellar magnetic activity and star formation with extensive multiwavelength support. Science goals include: addressing the mass- and age-dependence of magnetic activity in brown dwarfs; uncovering the low-mass members of the deeply embedded clusters; elucidating the absence of an activity-rotation relation in pre-main sequence stars; measuring flare frequencies, flare plasma conditions and coronal structures in dozens of active stars; investigate the nature of OB wind shocks; and studying X-ray effects on circumstellar environments.

Proposal #	Target Name	RA	DEC	Inst.	Grat.	Exp. Time	Seq. #	ObsID
04200331	ORION NEBULA CLUSTER	83.819583	-5.390000	ACIS-I	NONE	700.000000	200214	3744

SN, SNR AND ISOLATED NS

Proposal Title: A DETAILED STUDY OF 3C58 - THE YOUNGEST KNOWN PULSAR NEBULA IN THE GALAXY

PI Name: PATRICK SLANE

3C58 is the youngest known Crab-like SNR in the Galaxy. Chandra observations have uncovered its young pulsar, provided an upper limit to its surface temperature which challenges standard models of NS cooling, and identified the termination shock of its wind. Structures in the nebula indicative of jets and particle outflows have also been revealed. 3C58 thus possesses all of the standard traits of a young pulsar system, and may be a more appropriate "prototype" than the Crab. Based on the foundation built from our initial studies, we propose a definitive X-ray study of 3C58 to study structure on scales of the telescope resolution, perform spectral mapping of the complex emission regions, and obtain a template for future studies of this remnant of SN 1181 at other wavelengths.

Proposal #	Target Name	RA	DEC	Inst.	Grat.	Exp. Time	Seq. #	ObsID
04500141	3C58	31.404167	64.830000	ACIS-S	NONE	350.000000	500311	3832

SN, SNR AND ISOLATED NS

Proposal Title: STUDYING HIGH MACH NUMBER SHOCKS IN YOUNG SUPERNOVA REMNANTS WITH CHANDRA

PI Name: JOHN HUGHES

We propose deep imaging of the full extents of the young supernova remnants SN1006, Tycho, and G292.0+1.8. These images are optimized for proper motion measurements for which Chandra's superb angular resolution is uniquely suited and will yield significant results when compared to earlier Chandra, ROSAT, and Einstein images. The new X-ray data, in conjunction with our new radio observations, will address questions concerning the physics of ultra-high-Mach-number collisionless shocks, the efficiency of cosmic-ray acceleration, the dynamics of ejecta-dominated SNRs, and the small-scale structure of SN ejecta. These observations will serve as a legacy of the Chandra mission and will provide invaluable data for future research on SNRs and cosmic rays.

Proposal #	Target Name	RA	DEC	Inst.	Grat.	Exp. Time	Seq. #	ObsID
04500223	TYCHO'S SNR	6.329167	64.136111	ACIS-I	NONE	150.000000	500316	3837
04500223	SN1006	225.729167	-41.925000	ACIS-I	NONE	220.000000	500317	3838

SN, SNR AND ISOLATED NS

Proposal Title: SUPERNOVA REMNANTS IN THE MAGELLANIC CLOUDS

PI Name: FREDERICK SEWARD

Chandra has now observed 20 of the brightest remnants in the Magellanic Clouds. Because the distances are known and the absorption low, this set is going to yield definitive data on remnant characteristics and evolution. We propose to observe 6 more remnants in the LMC. All are fainter and some are larger than those in the observed sample. We expect to see faint central sources and previously unobserved structure. These observations will span a region of parameter space not covered in the presently-observed sample and will include some remnants with unique interesting features.

Proposal #	Target Name	RA	DEC	Inst.	Grat.	Exp. Time	Seq. #	ObsID
04500278	0454-672 [N9]	73.637500	-67.213333	ACIS-S	NONE	68.000000	500326	3847
04500278	0532-710 [N206]	83.000000	-71.005556	ACIS-S	NONE	68.000000	500327	3848
04500278	0540-697	85.000000	-69.737500	ACIS-S	NONE	21.000000	500328	3849
04500278	0550-683	87.666667	-68.358333	ACIS-S	NONE	68.000000	500329	3850

SN, SNR AND ISOLATED NS

Proposal Title: FIRST MEASUREMENT OF THE GRAVITATIONAL REDSHIFT AT THE SURFACE OF A NEUTRON STAR

PI Name: GEORGE PAVLOV

Chandra observations of 1E1207.4-5209, the neutron star (NS) in the PKS 1209-51/52 SNR, allowed us to discover absorption features in the NS thermal spectrum. This discovery provides a unique opportunity to measure the NS mass and radius and constrain the equation of state. We interpret the features as lines of once-ionized helium formed in the NS atmosphere with a magnetic field of 150 Teragauss, which implies a radius of 9-14 km for a one-solar-mass NS. To measure accurate line energies and resolve potentially multiple lines blended in the low-resolution CCD spectrum, we propose a deep observation with ACIS/LETG. This observation will provide a high-resolution phase-resolved spectrum, required for precise measurement of the NS mass and radius.

Proposal #	Target Name	RA	DEC	Inst.	Grat.	Exp. Time	Seq. #	ObsID
04500813	1E 1207.4-5209	182.503333	-52.440306	ACIS-S	NONE	20.000000	500392	3913
04500813	3 1E 1207.4-5209	182.503333	-52.440306	ACIS-S	NONE	20.000000	500393	3914
04500813	1E 1207.4-5209	182.503333	-52.440306	ACIS-S	LETG	260.000000	500394	3915

ACTIVE GALAXIES AND QUASARS

Proposal Title: CONNECTING THE X-RAY AND UV IONIZED ABSORBERS IN MRK 279

PI Name: JELLE KAASTRA

We propose a deep X-ray/UV spectroscopy campaign on the bright Seyfert 1 galaxy Mrk 279, using Chandra LETGS, HST/STIS, and FUSE. Our main scientific goal is to study the AGN outflow seen as an ionized absorber in this galaxy, focusing on the crucial connection between the X-ray and UV manifestations of the outflows. We will map the ionization and velocity structure, measure the elemental abundances and then determine the mass and kinetic luminosity flux of the outflow - all stepping stones for studying the importance of outflows in the evolution of AGN and their host galaxies. In addition we will use the LETGS data to determine the existence of relativistic CNO emission lines in the spectrum.

Proposal #	Target Name	RA	DEC	Inst.	Grat.	Exp. Time	Seq. #	ObsID
04700532	MRK 279	208.264583	69.308111	HRC-S	LETG	360.000000	700706	4027

CLUSTERS OF GALAXIES

Proposal Title: SURVEYING THE FORNAX CLUSTER OF GALAXIES

PI Name: CALEB SCHARF

Low luminosity X-ray clusters of galaxies are the dominant reservoirs of bound matter in the Universe. At a distance of 20 Mpc, the Fornax cluster has an immense collection of the highest quality multi-wavelength data, making it an exceptional laboratory for studying the astrophysics of these systems. We propose surveying an inner region of Fornax with Chandra's unprecedented combination of spatial and spectral resolution to produce a keystone dataset with a long-term legacy. We will investigate the interactions of cluster galaxies with the ICM, their populations of globular clusters, search for emission from dwarf galaxies, ultra-compact systems, and intra-cluster planetary nebulae, and compare the ICM metal contents with the detailed history of stellar populations in Fornax.

Proposal #	Target Name	RA	DEC	Inst.	Grat.	Exp. Time	Seq. #	ObsID
04800280	FORNAX CLUSTER	53.941250	-35.262500	ACIS-I	NONE	50.000000	800324	4168
04800280	FORNAX CLUSTER	54.168750	-35.080278	ACIS-I	NONE	50.000000	800325	4169
04800280	FORNAX CLUSTER	54.168750	-35.450278	ACIS-I	NONE	50.000000	800326	4170
04800280	FORNAX CLUSTER	54.396250	-35.267500	ACIS-I	NONE	50.000000	800327	4171
04800280	FORNAX CLUSTER	54.397083	-35.632500	ACIS-I	NONE	50.000000	800328	4172
04800280	FORNAX CLUSTER	54.625000	-35.451111	ACIS-I	NONE	50.000000	800329	4173
04800280	FORNAX CLUSTER	54.625000	-35.817778	ACIS-I	NONE	50.000000	800330	4174
04800280	FORNAX CLUSTER	54.742917	-35.179444	ACIS-I	NONE	50.000000	800331	4175
04800280	FORNAX CLUSTER	54.852500	-35.635833	ACIS-I	NONE	50.000000	800332	4176
04800280	FORNAX CLUSTER	54.972083	-35.363889	ACIS-I	NONE	50.000000	800333	4177

CLUSTERS OF GALAXIES

Proposal Title: CHANDRA OBSERVATIONS OF DLS SHEAR-SELECTED CLUSTERS

PI Name: JOHN HUGHES

We propose Chandra observations of the most massive clusters currently identified from the Deep Lens Survey (DLS). The DLS is a deep multicolor (BVRz') imaging survey of 28 square degree being carried out at the 4-m telescopes of the US National Observatories (KPNO and CTIO). The DLS shear-selected cluster sample makes it possible for the first time to study clusters in a baryon-independent way. We are pursuing detailed investigations of this sample with HST and ground-based Keck spectroscopy. Chandra observations will meet multiple high-impact scientific goals, specifically, testing the ``fair sample'' hypothesis, calibrating the relationships between cluster mass, size, X-ray luminosity and temperature, and studying the evolution of these relationships with look-back time.

Proposal #	Target Name	RA	DEC	Inst.	Grat.	Exp. Time	Seq. #	ObsID
04800927	DLS J0522-4820	80.570833	-48.336111	ACIS-I	NONE	20.000000	800364	4208
04800927	DLS J0916+2931	139.000000	29.526111	ACIS-I	NONE	20.000000	800365	4209
04800927	DLS J1049-0417	162.420833	-4.295556	ACIS-I	NONE	20.000000	800366	4210
04800927	DLS J1054-0549	163.533333	-5.828889	ACIS-I	NONE	20.000000	800367	4211
04800927	DLS J1055-0503	163.800000	-5.061944	ACIS-I	NONE	20.000000	800368	4212
04800927	DLS J1402-1019	210.512500	-10.328889	ACIS-I	NONE	20.000000	800369	4213
04800927	DLS J1402-1028	210.550000	-10.470556	ACIS-I	NONE	20.000000	800370	4214

EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS

Proposal Title: A CHANDRA WIDE-FIELD SURVEY TO MAP THE COSMIC WEB AND INVESTIGATE THE EVOLUTION OF NUCLEAR ACCRETION

PI Name: CHRISTINE JONES

We propose a wide-field X-ray imaging survey with deep and shallow components in order to map the structure and evolution of the Universe to redshift unity, and to probe the nature, environment and evolutionary history of AGN. The observations will cover the Bootes field of the NOAO Deep Wide-Field Survey, that is unique in its wide-field coverage and availability of deep multiwavelength imaging (including VLA and SIRTF) and optical spectroscopy. The Chandra survey is designed to sample volumes appropriate for statistical investigations of cluster environments, the space density of groups, biases in the optical and X-ray selection of groups and clusters, and AGN phenomena in relation to galaxy host properties and their evolution.

Proposal #	Target Name	RA	DEC	Inst.	Grat.	Exp. Time	Seq. #	ObsID
04900340	SS45	216.415417	34.013194	ACIS-I	NONE	5.000000	900261	4218
04900340	SS34	216.420417	33.746500	ACIS-I	NONE	5.000000	900262	4219
04900340	SS23	216.425417	33.479889	ACIS-I	NONE	5.000000	900263	4220
04900340	SS12	216.430000	33.213194	ACIS-I	NONE	5.000000	900264	4221
04900340	SS1	216.435000	32.946500	ACIS-I	NONE	5.000000	900265	4222
04900340	SS46	216.737083	34.013194	ACIS-I	NONE	5.000000	900266	4223
04900340	SS35	216.740833	33.746500	ACIS-I	NONE	5.000000	900267	4224
04900340	SS24	216.745000	33.479889	ACIS-I	NONE	5.000000	900268	4225
04900340	SS13	216.748750	33.213194	ACIS-I	NONE	5.000000	900269	4226
04900340	SS2	216.752500	32.946500	ACIS-I	NONE	5.000000	900270	4227
04900340	SS47	217.058750	34.013194	ACIS-I	NONE	5.000000	900271	4228
04900340	SS36	217.061667	33.746500	ACIS-I	NONE	5.000000	900272	4229
04900340	SS25	217.064583	33.479889	ACIS-I	NONE	5.000000	900273	4230
04900340	SS14	217.067500	33.213194	ACIS-I	NONE	5.000000	900274	4231
04900340	SS3	217.070417	32.946500	ACIS-I	NONE	5.000000	900275	4232
04900340	SS48	217.380417	34.013194	ACIS-I	NONE	5.000000	900276	4233
04900340	SS37	217.382500	33.746500	ACIS-I	NONE	5.000000	900277	4234
04900340	SS26	217.384583	33.479889	ACIS-I	NONE	5.000000	900278	4235
04900340	SS15	217.386250	33.213194	ACIS-I	NONE	5.000000	900279	4236
04900340	SS4	217.388333	32.946500	ACIS-I	NONE	5.000000	900280	4237
04900340	SD49	217.702083	34.013194	ACIS-I	NONE	5.000000	900281	4238
04900340	SD38	217.702917	33.746500	ACIS-I	NONE	5.000000	900282	4239
04900340	SD27	217.704167	33.479889	ACIS-I	NONE	5.000000	900283	4240
04900340	SD16	217.705000	33.213194	ACIS-I	NONE	5.000000	900284	4241
04900340	SS5	217.706250	32.946500	ACIS-I	NONE	5.000000	900285	4242
04900340	SS6	218.023750	32.946500	ACIS-I	NONE	5.000000	900286	4243
04900340	SD17	218.023750	33.213194	ACIS-I	NONE	5.000000	900287	4244
04900340	SD28	218.023750	33.479889	ACIS-I	NONE	5.000000	900288	4245
04900340	SD39	218.023750	33.746500	ACIS-I	NONE	5.000000	900289	4246
04900340	SD50	218.023750	34.013194	ACIS-I	NONE	5.000000	900290	4247
04900340	SS7	218.341667	32.946500	ACIS-I	NONE	5.000000	900291	4248
04900340	SD18	218.342500	33.213194	ACIS-I	NONE	5.000000	900292	4249
04900340	SD29	218.343750	33.479889	ACIS-I	NONE	5.000000	900293	4250
04900340	SD40	218.344583	33.746500	ACIS-I	NONE	5.000000	900294	4251
04900340	SD51	218.345417	34.013194	ACIS-I	NONE	5.000000	900295	4252
04900340	SS8	218.659583	32.946500	ACIS-I	NONE	5.000000	900296	4253
04900340	SS19	218.661250	33.213194	ACIS-I	NONE	5.000000	900297	4254
04900340	SD30	218.663333	33.479889	ACIS-I	NONE	5.000000	900298	4255
04900340	SD41	218.665000	33.746500	ACIS-I	NONE	5.000000	900299	4256
04900340	SD52	218.667500	34.013194	ACIS-I	NONE	5.000000	900300	4257
04900340	SS9	218.977083	32.946500	ACIS-I	NONE	5.000000	900301	4258
04900340	SS20	218.980000	33.213194	ACIS-I	NONE	5.000000	900302	4259
04900340	SS31	218.982917	33.479889	ACIS-I	NONE	5.000000	900303	4260
04900340	SS42	218.985833	33.746500	ACIS-I	NONE	5.000000	900304	4261
04900340	SS53	218.989167	34.013194	ACIS-I	NONE	5.000000	900305	4262
04900340	SS10	219.295000	32.946500	ACIS-I	NONE	5.000000	900306	4263
04900340	SS21	219.298750	33.213194	ACIS-I	NONE	5.000000	900307	4264
04900340	SS32	219.302500	33.479889	ACIS-I	NONE	5.000000	900308	4265
04900340	SS43	219.306667	33.746500	ACIS-I	NONE	5.000000	900309	4266
04900340	SS54	219.310833	34.013194	ACIS-I	NONE	5.000000	900310	4267
04900340	SS11	219.612500	32.946500	ACIS-I	NONE	5.000000	900311	4268
04900340	SS22	219.617500	33.213194	ACIS-I	NONE	5.000000	900312	4269
04900340	SS33	219.622500	33.479889	ACIS-I	NONE	5.000000	900313	4270
04900340	SS44	219.627500	33.746500	ACIS-I	NONE	5.000000	900314	4271
04900340	SS55	219.632500	34.013194	ACIS-I	NONE	5.000000	900315	4272

EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS

Proposal Title: A CHANDRA WIDE-FIELD SURVEY TO MAP THE COSMIC WEB AND INVESTIGATE THE EVOLUTION OF NUCLEAR ACCRETION

PI Name: CHRISTINE JONES

We propose a wide-field X-ray imaging survey with deep and shallow components in order to map the structure and evolution of the Universe to redshift unity, and to probe the nature, environment and evolutionary history of AGN. The observations will cover the Bootes field of the NOAO Deep Wide-Field Survey, that is unique in its wide-field coverage and availability of deep multi- wavelength imaging (including VLA and SIRTF) and optical spectroscopy. The Chandra survey is designed to sample volumes appropriate for statistical investigations of cluster environments, the space density of groups, biases in the optical and X-ray selection of groups and clusters, and AGN phenomena in relation to galaxy host properties and their evolution.

Proposal #	Target Name	RA	DEC	Inst.	Grat.	Exp. Time	Seq. #	ObsID
04901014	SS56	216.424167	32.685833	ACIS-I	NONE	5.000000	900321	4278
04901014	SS57	216.747500	32.689722	ACIS-I	NONE	5.000000	900322	4279
04901014	SS58	217.050000	32.692222	ACIS-I	NONE	5.000000	900323	4280
04901014	SS59	217.373750	32.694444	ACIS-I	NONE	5.000000	900324	4281
04901014	SS60	217.675833	32.695556	ACIS-I	NONE	5.000000	900325	4282

Last modified: 12/02/10

The Chandra X-Ray Center (CXC) is operated for NASA by the Smithsonian Astrophysical Observatory. 60 Garden Street, Cambridge, MA 02138 USA. Email: cxchelp@head.cfa.harvard.edu Smithsonian Institution, Copyright © 1998-2026. All rights reserved.