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Proposal Title: The Extended Chandra Deep Field-South Survey: A Public Chandra Legacy

Proposal Number: 05900218

PI: William Brandt

Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS

Abstract: We propose to extend the 1 Ms Chandra Deep Field-South (CDF-S) survey with six public 330 ks flanking observations: the Extended CDF-S (E-CDF-S). Using these, we will study the detailed cosmic history of accretion onto supermassive black holes, the role of moderate-luminosity AGN at high redshift, AGN clustering, and X-ray groups and low-luminosity clusters. The proposed observations are optimized to fill the X-ray luminosity/redshift plane at z > 1.5 where the AGN source statistics are still limited. Follow-up studies will exploit the superb E-CDF-S multiwavelength coverage including VLT/Keck spectroscopy (6000+ VLT redshifts), HST imaging (GEMS, GOODS, ACS Ultradeep Field; 734 HST orbits), intensive ground-based imaging, and scheduled SIRTF observations.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
03:33:03.64	-27:41:20.68	Extended CDF-S #1	ACIS-I	TE	NONE	250.00	000.100
03:31:50.54	-27:41:18.28	Extended CDF-S #2	ACIS-I	TE	NONE	250.00	000.100
03:31:50.31	-27:57:31.89	Extended CDF-S #3	ACIS-I	TE	NONE	250.00	000.100
03:33:03.69	-27:57:33.23	Extended CDF-S #4	ACIS-I	TE	NONE	250.00	000.100

Proposal Title: A Megasecond Image of the Core of the Perseus Cluster

Proposal Number: 05800170

PI: Andrew Fabian

Subject Category: CLUSTERS OF GALAXIES

Abstract: We propose a further 800 ks observation of the Perseus cluster, A426, the X-ray brightest cluster of galaxies in the sky. By combining this observation with our current data we will obtain a 1 Ms "ultimate image" of the cluster. Our main goal is to quantify the ripples due to the propagating sound waves seen in our 200 ks image. A detailed understanding of the mechanisms in the nearby Perseus cluster will unable us to fully understand the solution to the "cooling flow problem". The Perseus cluster is the only extragalactic source with such a high ACIS-S surface brightness over many sq arcmin. We propose that it should be observed as deeply as possible with Chandra and before any further degradation takes place in the performance of the detectors or spacecraft.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
03:19:48.20	+41:30:42.20	Abell 426	ACIS-S	TE	NONE	200.00	089.600
03:19:48.20	+41:30:42.20	Abell 426	ACIS-S	TE	NONE	200.00	089.600
03:19:48.20	+41:30:42.20	Abell 426	ACIS-S	TE	NONE	200.00	089.600
03:19:48.20	+41:30:42.20	Abell 426	ACIS-S	TE	NONE	200.00	089.600

Proposal Title: The Cassiopeia A Explosion: Getting at the Core Issues

Proposal Number: 05500623

PI: Una Hwang

Subject Category: SN, SNR AND ISOLATED NS

Abstract: We propose a deep 1 Ms observation of the core-collapse remnant Cas A as a unique and important legacy of the Chandra Observatory. These data may be used to construct an observational nucleosynthesis curve giving composition by mass for all the X-ray emitting ejecta, and to study explosion asymmetries, turbulent mixing, particle acceleration, and the compact remnant. Particularly for a detailed study of the various processes that produce and distribute the heavy elements in a core-collapse explosion, Cas A is perhaps the best candidate target. Important results have been obtained with the existing <50 ks observations, but true breakthroughs may be expected with a much deeper exposure that allows us to study nucleosynthesis and core-collapse using Chandra's full spatial resolution.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
23:23:26.70	+58:49:03.00	Cassiopeia A	ACIS-S	TE	NONE	1000.00	280.000

Proposal Title: An Ultra-Deep Study of M101

Proposal Number: 05600587

PI: K. Kuntz

Subject Category: NORMAL GALAXIES

Abstract: We propose a multi-segmented 1 Ms observation of M101, a near-by face-on spiral in a direction of low Galactic absorption. The observation will detect point sources to L(0.5-2.0 keV)=4x10^35 ergs/s, detect nearly all young to middle-aged SNR, detect and resolve super-bubbles typical of the Milky Way, and provide an unprecedented view of the hot ISM in a spiral galaxy. Coupled with our HST-ACS images, we will be able to measure directly the X-ray output of individual stellar clusters, and better determine the galactic energy budget. The resulting images will bring a wealth of material to a broad range of galactic, stellar, and ISM studies.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
14:03:12.90	+54:20:55.60	M101	ACIS-S	TE	NONE	858.00	003.000
14:03:33.60	+54:20:55.60	M101	ACIS-S	TE	NONE	142.00	003.000

Proposal Title: A Chandra HETGS & HST view of the Warm and Lukewarm absorbers in IRAS 13349+2438

Proposal Number: 05700535

PI: Julia Lee

Subject Category: ACTIVE GALAXIES AND QUASARS

Abstract: We propose 300~ks Chandra HETGS simultaneous with 4 HST orbits primarily to study the warm absorber environment (chemical compositions, velocities, absorbing column) of the archetypal infrared quasar IRAS 13349+2438. We will look for associations between the X-ray and UV absorbers, and study the properties of dust extinction in this source. Inner shell excitation lines from low ionization ions (previously only probed in the UV) will be compared with HST measurements. We will resolve many of the individual lines of the UTA to put ionization limits on a possible `lukewarm' absorber. The HST spectrum will give us a first view of Ly-alpha and Si IV in this source at shorter wavelengths.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
13:37:18.70	+24:23:03.00	IRAS 13349+2438	ACIS-S	TE	HETG	300.00	000.321

Proposal Number: 05800890

PI: Maxim Markevitch

Subject Category: CLUSTERS OF GALAXIES

Abstract: The galaxy cluster 1E0657-56 is a treasure trove of information on just about every problem in cluster physics. It is the only cluster known to have a shock front with M substantially greater than 1. The proposed 500 ks observation, combined with the existing 90 ks, will allow us to determine whether electrons are heated adiabatically or dissipatively in a shock and whether the electron-ion equilibration is efficient. We will search for an electron temperature precursor to the shock to estimate thermal conductivity. We also will determine the importance of gas turbulence and study the destruction of a cooling flow remnant by ram pressure. Combined with data from other wavelengths, this observation can also shed light on the nature of dark matter and the origin of cluster radio halos.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
06:58:19.70	-55:56:20.00	1E0657-56	ACIS-I	TE	NONE	500.00	001.100

Proposal Number: 05500645

PI: Richard Mccray

Subject Category: SN, SNR AND ISOLATED NS

Abstract: We propose to obtain spatially resolved spectra of the newborn supernova remnant SNR1987A with the ACIS-S/LETG on Chandra. The spectra will provide sufficient counts in several emission lines so that we can, for the first time, directly measure the velocity of the supernova blast wave through line profiles, and the electron temperature through line ratios, as functions of position. We will develop hydrodynamical models to interpret the dispersed X-ray spectra as well as complementary X-ray imaging data and UV and optical images and spectra from the HST and radio images from the Australia Telescope Compact Array.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
05:35:28.00	-69:16:11.10	SNR1987A	ACIS-S	TE	LETG	300.00	000.050

Proposal Number: 05900888

PI: Fabrizio Nicastro

Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS

Abstract: We propose to extend our highly succesful Chandra-AO4 TOO program to the 5th Chandra cycle, to observe up to 2 blazars in exceptionally high states with the Chandra HRCS-LETG (hereinafter HLETG) for a total exposure time of 350 ks. We shall study the ``warm'', low-redshift, phase of the intergalactic medium, where most of the baryonic matter of the local (z < 1-2) Universe is believed to hide.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
		Class A Blazar in Ou	HRC-S		LETG	100.00	010.000
		Class B Blazar in Ou	HRC-S		LETG	250.00	005.000

Proposal Number: 05400594

PI: Frederik Paerels

Subject Category: BH AND NS BINARIES

Abstract: Recently, we discovered narrow absorption features in the spectrum of 28 X-ray bursts from the neutron star in the LMXB EXO0748-676, whose properties point to a photospheric origin. The transition wavelengths are consistent with the n=2-3 lines in H- and He-like Fe, exhibiting a gravitational redshift of z=0.35. The measured line strengths indicate that the lines are significantly broadened by the Stark effect, and this will ultimately provide an opportunity to determine both the mass and the radius of this neutron star. Here we propose a very deep spectroscopic observation with Chandra HETGS, to detect the Fe Lyman spectrum and obtain crucial independent spectroscopic confirmation for the Balmer line identification, and to measure the spin period of the neutron star.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
07:48:33.30	-67:45:00.00	EXO 0748-676	ACIS-S	TE	HETG	300.00	010.000

Proposal Number: 05900547

PI: Belinda Wilkes

Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS

Abstract: We propose a moderate-depth (70 ksec), 0.6 sq.deg. Chandra survey, the deepest/largest CONTIGUOUS area to date, in the Lockman Field of the SIRTF/SWIRE Legacy Survey coincident with a completed, ultra-deep VLA survey with deep optical and near-IR imaging in-hand. SWIRE, the largest SIRTF program, will detect >500 000 dusty galaxies to z > 2.5 in 7 fields covering 65 sq.degs. The prime science goal is to study the structure, evolution and environments of AGN, starbursts and ellipsoids over the SAME SPATIAL VOLUME out to z > 2.5. Key to this study is an X-ray survey deep enough to distinguish starbursts and AGN, including the significant, highly obscured (log Nh>22) subset. Chandra will secure X-ray identification and fluxes for ~550 (0.6 sq deg) of the field's ~7000 SWIRE sources.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
10:46:00.00	+59:00:60.00	SWIRE LOCKMAN 5 (cen	ACIS-I	TE	NONE	070.00	000.000
10:43:60.00	+58:45:60.00	SWIRE LOCKMAN 1	ACIS-I	TE	NONE	070.00	000.000
10:46:00.00	+58:45:60.00	SWIRE LOCKMAN 2	ACIS-I	TE	NONE	070.00	000.000
10:48:00.00	+58:45:60.00	SWIRE LOCKMAN 3	ACIS-I	TE	NONE	070.00	000.000
10:43:60.00	+59:00:60.00	SWIRE LOCKMAN 4	ACIS-I	TE	NONE	070.00	000.000
10:48:00.00	+59:00:60.00	SWIRE LOCKMAN 6	ACIS-I	TE	NONE	070.00	000.000
10:43:60.00	+59:15:60.00	SWIRE LOCKMAN 7	ACIS-I	TE	NONE	070.00	000.000
10:46:00.00	+59:15:60.00	SWIRE LOCKMAN 8	ACIS-I	TE	NONE	070.00	000.000
10:48:00.00	+59:15:60.00	SWIRE LOCKMAN 9	ACIS-I	TE	NONE	070.00	000.000

Last modified: 12/02/10

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