Chandra X-Ray Observatory
	(CXC)

Accepted Cycle 4 Large Project Proposals

Proposal NumberSubject CategoryPI NameTypeTime
(Ks)
Title
04200312NORMAL STARS AND WDCorcoranLP500UNVEILING ETA CAR: CHANDRA OBSERVATIONS DURING THE 2003.5 EVENT
04200331NORMAL STARS AND WDFeigelsonLP780AN ULTRADEEP CHANDRA STUDY OF THE ORION NEBULA (GUEST OBSERVER PORTION)
04500141SN, SNR AND ISOLATED NSSlaneLP350A DETAILED STUDY OF 3C58 - THE YOUNGEST KNOWN PULSAR NEBULA IN THE GALAXY
04500223SN, SNR AND ISOLATED NSHughesLP370STUDYING HIGH MACH NUMBER SHOCKS IN YOUNG SUPERNOVA REMNANTS WITH CHANDRA
04500278SN, SNR AND ISOLATED NSSewardLP225SUPERNOVA REMNANTS IN THE MAGELLANIC CLOUDS
04500813SN, SNR AND ISOLATED NSPavlovLP300FIRST MEASUREMENT OF THE GRAVITATIONAL REDSHIFT AT THE SURFACE OF A NEUTRON STAR
04700532ACTIVE GALAXIES AND QUASARSKaastraLP360CONNECTING THE X-RAY AND UV IONIZED ABSORBERS IN MRK 279
04800280CLUSTERS OF GALAXIESScharfLP500SURVEYING THE FORNAX CLUSTER OF GALAXIES
04800927CLUSTERS OF GALAXIESHughesLP140CHANDRA OBSERVATIONS OF DLS SHEAR-SELECTED CLUSTERS
04900340EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYSJonesLP275A CHANDRA WIDE-FIELD SURVEY TO MAP THE COSMIC WEB AND INVESTIGATE THE EVOLUTION OF NUCLEAR ACCRETION
04901014EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYSJonesLP25A CHANDRA WIDE-FIELD SURVEY TO MAP THE COSMIC WEB AND INVESTIGATE THE EVOLUTION OF NUCLEAR ACCRETION

Subject Category: NORMAL STARS AND WD

Proposal Number: 04200312

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 information which may finally help us solve the riddle of this star.

R.A. Dec. Target Name Det. Grating Exp.Time
10:45:03.60-59:41:04.30ETA CARINAEACIS-SHETG100
10:45:03.60-59:41:04.30ETA CARINAEACIS-SHETG100
10:45:03.60-59:41:04.30ETA CARINAEACIS-SHETG100
10:45:03.60-59:41:04.30ETA CARINAEACIS-SHETG100
10:45:03.60-59:41:04.30ETA CARINAEACIS-SHETG100

Subject Category: NORMAL STARS AND WD

Proposal Number: 04200331

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.

R.A. Dec. Target Name Det. Grating Exp.Time
05:35:16.70-05:23:24.00ORION NEBULA CLUSTERACIS-INONE700

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 04500141

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.

R.A. Dec. Target Name Det. Grating Exp.Time
02:05:37.00+64:49:48.003C58ACIS-SNONE350

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 04500223

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.

R.A. Dec. Target Name Det. Grating Exp.Time
15:02:55.00-41:55:30.00SN1006ACIS-INONE220
00:25:19.00+64:08:10.00TYCHO'S SNRACIS-INONE150

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 04500278

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 aad will include some remnants with unique interesting features.

R.A. Dec. Target Name Det. Grating Exp.Time
05:40:00.00-69:44:15.000540-697ACIS-SNONE21
05:31:60.00-71:00:20.000532-710 [N206]ACIS-SNONE68
05:50:40.00-68:21:30.000550-683ACIS-SNONE68
04:54:33.00-67:12:48.000454-672 [N9]ACIS-SNONE68

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 04500813

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.

R.A. Dec. Target Name Det. Grating Exp.Time
12:10:00.80-52:26:25.101E 1207.4-5209ACIS-SNONE40
12:10:00.80-52:26:25.101E 1207.4-5209ACIS-SLETG260

Subject Category: ACTIVE GALAXIES AND QUASARS

Proposal Number: 04700532

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.

R.A. Dec. Target Name Det. Grating Exp.Time
13:53:03.50+69:18:29.20MRK 279HRC-SLETG360

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 04800280

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.

R.A. Dec. Target Name Det. Grating Exp.Time
03:38:30.00-35:27:04.00FORNAX CLUSTERACIS-INONE50
03:38:58.30-35:10:46.00FORNAX CLUSTERACIS-INONE50
03:39:53.30-35:21:50.00FORNAX CLUSTERACIS-INONE50
03:36:40.50-35:04:49.00FORNAX CLUSTERACIS-INONE50
03:37:35.10-35:16:03.00FORNAX CLUSTERACIS-INONE50
03:39:24.60-35:38:09.00FORNAX CLUSTERACIS-INONE50
03:35:45.90-35:15:45.00FORNAX CLUSTERACIS-INONE50
03:36:40.50-35:27:01.00FORNAX CLUSTERACIS-INONE50
03:37:35.30-35:37:57.00FORNAX CLUSTERACIS-INONE50
03:38:30.00-35:49:04.00FORNAX CLUSTERACIS-INONE50

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 04800927

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.

R.A. Dec. Target Name Det. Grating Exp.Time
05:22:17.00-48:20:10.00DLS J0522-4820ACIS-INONE20
10:49:41.00-04:17:44.00DLS J1049-0417ACIS-INONE20
10:54:08.00-05:49:44.00DLS J1054-0549ACIS-INONE20
10:55:12.00-05:03:43.00DLS J1055-0503ACIS-INONE20
14:02:12.00-10:28:14.00DLS J1402-1028ACIS-INONE20
09:16:00.00+29:31:34.00DLS J0916+2931ACIS-INONE20
14:02:03.00-10:19:44.00DLS J1402-1019ACIS-INONE20

Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS

Proposal Number: 04900340

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.

R.A. Dec. Target Name Det. Grating Exp.Time
14:25:44.40+32:56:47.40SS1ACIS-INONE5
14:27:00.60+32:56:47.40SS2ACIS-INONE5
14:28:16.90+32:56:47.40SS3ACIS-INONE5
14:29:33.20+32:56:47.40SS4ACIS-INONE5
14:30:49.50+32:56:47.40SS5ACIS-INONE5
14:33:22.00+32:56:47.40SS7ACIS-INONE5
14:34:38.30+32:56:47.40SS8ACIS-INONE5
14:35:54.50+32:56:47.40SS9ACIS-INONE5
14:37:10.80+32:56:47.40SS10ACIS-INONE5
14:38:27.00+32:56:47.40SS11ACIS-INONE5
14:25:43.20+33:12:47.50SS12ACIS-INONE5
14:26:59.70+33:12:47.50SS13ACIS-INONE5
14:28:16.20+33:12:47.50SS14ACIS-INONE5
14:29:32.70+33:12:47.50SS15ACIS-INONE5
14:30:49.20+33:12:47.50SD16ACIS-INONE5
14:32:05.70+33:12:47.50SD17ACIS-INONE5
14:34:38.70+33:12:47.50SS19ACIS-INONE5
14:35:55.20+33:12:47.50SS20ACIS-INONE5
14:37:11.70+33:12:47.50SS21ACIS-INONE5
14:38:28.20+33:12:47.50SS22ACIS-INONE5
14:25:42.10+33:28:47.60SS23ACIS-INONE5
14:26:58.80+33:28:47.60SS24ACIS-INONE5
14:28:15.50+33:28:47.60SS25ACIS-INONE5
14:29:32.30+33:28:47.60SS26ACIS-INONE5
14:30:49.00+33:28:47.60SD27ACIS-INONE5
14:32:05.70+33:28:47.60SD28ACIS-INONE5
14:33:22.50+33:28:47.60SD29ACIS-INONE5
14:35:55.90+33:28:47.60SS31ACIS-INONE5
14:37:12.60+33:28:47.60SS32ACIS-INONE5
14:38:29.40+33:28:47.60SS33ACIS-INONE5
14:25:40.90+33:44:47.40SS34ACIS-INONE5
14:26:57.80+33:44:47.40SS35ACIS-INONE5
14:28:14.80+33:44:47.40SS36ACIS-INONE5
14:29:31.80+33:44:47.40SS37ACIS-INONE5
14:30:48.70+33:44:47.40SD38ACIS-INONE5
14:32:05.70+33:44:47.40SD39ACIS-INONE5
14:33:22.70+33:44:47.40SD40ACIS-INONE5
14:34:39.60+33:44:47.40SD41ACIS-INONE5
14:37:13.60+33:44:47.40SS43ACIS-INONE5
14:38:30.60+33:44:47.40SS44ACIS-INONE5
14:25:39.70+34:00:47.50SS45ACIS-INONE5
14:26:56.90+34:00:47.50SS46ACIS-INONE5
14:28:14.10+34:00:47.50SS47ACIS-INONE5
14:29:31.30+34:00:47.50SS48ACIS-INONE5
14:30:48.50+34:00:47.50SD49ACIS-INONE5
14:32:05.70+34:00:47.50SD50ACIS-INONE5
14:33:22.90+34:00:47.50SD51ACIS-INONE5
14:34:40.20+34:00:47.50SD52ACIS-INONE5
14:35:57.40+34:00:47.50SS53ACIS-INONE5
14:37:14.60+34:00:47.50SS54ACIS-INONE5
14:38:31.80+34:00:47.50SS55ACIS-INONE5
14:33:22.20+33:12:47.50SD18ACIS-INONE5
14:34:39.20+33:28:47.60SD30ACIS-INONE5
14:35:56.60+33:44:47.40SS42ACIS-INONE5
14:32:05.70+32:56:47.40SS6ACIS-INONE5

Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS

Proposal Number: 04901014

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.

R.A. Dec. Target Name Det. Grating Exp.Time
14:26:59.40+32:41:23.00SS57ACIS-INONE5
14:28:12.00+32:41:32.00SS58ACIS-INONE5
14:25:41.80+32:41:09.00SS56ACIS-INONE5
14:29:29.70+32:41:40.00SS59ACIS-INONE5
14:30:42.20+32:41:44.00SS60ACIS-INONE5
Smithsonian Institute Smithsonian Institute

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 © 1998-2017. All rights reserved.