Chandra Large and Very Large Projects

Proposal Number: 07701072

Title: High-resolution spectroscopy of 'binary' AGN in the colliding galaxies of NGC 6240

PI Name: Claude Canizares

We propose to measure the kinematics of the AGNs inside the two colliding spiral galaxies in NGC 6240, by conducting an emission line analysis with the High Energy Transmission Grating Spectrometer (HETGS). Measuring the black hole kinematics will provide new constraints for models of galactic mergers with AGNs, which in turn are important to understand the link between the growth of supermassive black holes and their host galaxies. We can also extract HETGS spectra of the interface between the AGNs and the starburst region, in order to determine whether or not the predicted quenching of the starburst has started occurring near the AGNs.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
16:52:58.90	2:24:03.30	NGC 6240	ACIS-S	HETG	140
16:52:58.90	2:24:03.30	NGC 6240	ACIS-S	HETG	160

Proposal Number: 02700294

Title: DETERMINING THE NATURE OF THE VARIABLE ABSORPTION IN NGC 3783 WITH CHANDRA/HST

PI Name: Ian George

We propose 5 Chandra/HETG observations of NGC 3783, each simultaneous with HST/STIS observations already approved. The observations will allow the accurate determination of the variable continuum, absorption & emission line properties known to exist in this Seyfert, and constitute the most comprehensive study possible of the nature, origin and evolution of the X-ray & UV absorbers in an AGN. Such absorbers constitute a major component of the circumnuclear gas in AGN, and only the HETG has the resolution to make these measurements. It is vital to perform such a detailed study early in the mission to facilitate the correct interpretation of the Chandra & XMM observations of this and other AGN. We also ask the TAC to approve a restructuring of Chandra time already awarded to this study.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
11:39:02.40	-37:44:24.00	NGC 3783	ACIS-S	HETG	170
11:39:02.40	-37:44:24.00	NGC 3783	ACIS-S	HETG	170
11:39:02.40	-37:44:24.00	NGC 3783	ACIS-S	HETG	170
11:39:02.40	-37:44:24.00	NGC 3783	ACIS-S	HETG	170
11:39:02.40	-37:44:24.00	NGC 3783	ACIS-S	HETG	170

Proposal Number: 03700413

Title: AN IN-DEPTH STUDY OF THE X-RAY SOURCE POPULATION AND HOT ISM OF THE ANTENNAE GALAXIES

PI Name: Giuseppina Fabbiano

We propose a deep 375~ks observation of the prototypical merger galaxies NGC~4038/39 (``The Antennae''), divided into 5 time segments. Together with the archival data, we will obtain a deep 450ks ACIS-S exposure and time monitoring over 3 yrs. The unique significance of the Antennae for our understanding of mergers and the extraordinary characteristics of the X-ray emission of this system, make this study essential for probing a wide range of fundamental questions on the properties and evolution of XRBs, the range of black hole masses implied by the rich ULX population, the properties of the multiphase ISM, and the evolution of galaxy mergers, that cannot be addressed by looking at more normal galaxies.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
12:01:53.70	-18:52:35.50	NGC 4038/NGC 4039	ACIS-S	NONE	37
12:01:53.70	-18:52:35.50	NGC 4038/NGC 4039	ACIS-S	NONE	38
12:01:53.70	-18:52:35.50	NGC 4038/NGC 4039	ACIS-S	NONE	75
12:01:53.70	-18:52:35.50	NGC 4038/NGC 4039	ACIS-S	NONE	75
12:01:53.70	-18:52:35.50	NGC 4038/NGC 4039	ACIS-S	NONE	75
12:01:53.70	-18:52:35.50	NGC 4038/NGC 4039	ACIS-S	NONE	75

Proposal Number: 03700438

Title: RESOLVING THE WARM ABSORBER IN NGC 5548

PI Name: Jelle Kaastra

We propose to map the ionization and velocity structure of the X-ray and UV absorbers in NGC 5548 with the LETGS and HETGS of Chandra and STIS/HST. NGC 5548 is an important target for this kind of study because 1) it shows multiple kinematic components in the UV characterized by a range in ionization parameter and effective column, 2) it shows evidence for multiple kinematic and ionization components in previous Chandra X-ray spectra, and 3) it has a low Galactic column, which permits coverage of spectral lines out to 80 Angstrom with the LETGS. These data yield the ionization parameter and column density of the absorption-line regions as a function of radial velocity, and constrain the elemental abundances and shape of the unobserved EUV continuum.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
14:17:59.60	25:08:12.40	NGC 5548	HRC-S	LETG	175
14:17:59.60	25:08:12.40	NGC 5548	HRC-S	LETG	175
14:17:59.60	25:08:12.40	NGC 5548	ACIS-S	HETG	170

Proposal Number: 05700535

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

PI Name: Julia Lee

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.	Grating	Exp.Time
13:37:18.70	24:23:03.00	IRAS 13349+2438	ACIS-S	HETG	130
13:37:18.70	24:23:03.00	IRAS 13349+2438	ACIS-S	HETG	170

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	69:18:29.20	MRK 279	HRC-S	LETG	27.5
13:53:03.50	69:18:29.20	MRK 279	HRC-S	LETG	27.5
13:53:03.50	69:18:29.20	MRK 279	HRC-S	LETG	50
13:53:03.50	69:18:29.20	MRK 279	HRC-S	LETG	50
13:53:03.50	69:18:29.20	MRK 279	HRC-S	LETG	50
13:53:03.50	69:18:29.20	MRK 279	HRC-S	LETG	55
13:53:03.50	69:18:29.20	MRK 279	HRC-S	LETG	100

Proposal Number: 02700728

Title: FINDING THE BARYONS IN THE LOW REDSHIFT UNIVERSE.

PI Name: Smita Mathur

Recent estimates of the primordial deuterium abundance, combined with the theory of big bang nucleosynthesis (BBN), imply a baryon density parameter $\Omega_b \approx 0.04 h_{70}^{-2}$. The main reservoir of low redshift baryons is still ``missing''. All the observed stellar and gaseous components add up to only $\Omega_b \approx 0.004h_{70}^{-1}$, a factor of ten below the BBN abundance. Hydrodynamic cosmological simulations predict that a large fraction of the low redshift baryons should reside in a hot diffuse intergalactic medium (IGM). We propose to exploit the excellent spectral resolution of Chandra gratings to probe the low redshift IGM with sensitive X-ray spectroscopy. We expect to detect the main reservoir of low redshift baryons with observations of OVII absorption lines.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
18:21:57.30	64:20:36.40	H1821+643	ACIS-S	LETG	66
18:21:57.30	64:20:36.40	H1821+643	ACIS-S	LETG	100
18:21:57.30	64:20:36.40	H1821+643	ACIS-S	LETG	167
18:21:57.30	64:20:36.40	H1821+643	ACIS-S	LETG	167

Proposal Number: 08700916

Title: The Definitive Chandra Observations of NGC 4258

PI Name: Michael Nowak

We propose a 320 ksec HETG observation of NGC 4258. This will yield a high S/N nuclear spectra that is uncontaminated by extended emission or pileup. We will measure the fluorescent Kalpha line strength and width, search for low energy emission lines as expected in some ADAF models, and accurately measure the absorbing column. The latter may be probing the warped disk structure. We will search for nuclear flaring, as observed in Sgr A*. The S/N for observations of the `anomalous arms' will be increased over previous observations. The binary population will be surveyed down to an implied isotropic luminosity of 10^36 erg/s. Our observation will be coordinated with the VLA, to further test the "fundamental plane" of black hole radio/X-ray activity.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
12:18:57.50	47:18:14.00	NGC 4258	ACIS-S	HETG	160
12:18:57.50	47:18:14.00	NGC 4258	ACIS-S	HETG	160

Proposal Number: 08700551

Title: The Chandra-RBGS Survey of a Complete Sample of Luminous Infrared Galaxies

PI Name: David Sanders

We propose a Chandra-ACIS survey of a complete sample of Luminous Infrared Galaxies (LIRGs) with Lir >10^11.5, from the IRAS Revised Bright Galaxy Sample (RBGS). All of these objects are interacting/merging gas-rich spirals. Our new observations will provide a uniform and complete census of AGN and X-ray luminous starbursts in the nearest and brightest LIRGs, and will complement approved Spitzer-IRAC+MIPS, and HST-ACS imaging of the same sample. The results will be used to address the following key questions: are binary AGN a common feature of these LIRGs, and if so, when and at what level is the AGN activity triggered in each nucleus ? and can the fueling and growth of massive black holes be correlated in time with the merger phase ?

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
1:38:52.90	-10:27:11.40	IRAS F01364-1042	ACIS-S	NONE	15
4:46:49.50	-48:33:32.90	ESO 203-IG001	ACIS-S	NONE	15
5:16:46.40	79:40:12.60	VII Zw 031	ACIS-S	NONE	15
6:27:23.10	-47:10:47.00	ESO 255-IG007	ACIS-S	NONE	15
7:27:37.60	-2:54:54.10	IRAS 07251-0248	ACIS-S	NONE	15
8:52:29.90	-69:01:58.00	ESO 60-IG016	ACIS-S	NONE	15
9:04:12.70	-36:27:01.10	IRAS 09022-3615	ACIS-S	NONE	15
9:13:38.80	-10:19:20.30	IRAS F09111-1007	ACIS-S	NONE	15
10:06:04.80	-33:53:15.00	IC 2545	ACIS-S	NONE	15
10:20:00.20	8:13:34.00	IRAS F10173+0828	ACIS-S	NONE	15
13:15:06.40	-55:09:22.70	IRAS 13120-5453	ACIS-S	NONE	15
13:15:35.00	62:07:28.80	VV 250a	ACIS-S	NONE	15
13:20:35.30	34:08:22.20	UGC 08387	ACIS-S	NONE	15
14:40:59.00	-37:04:32.00	IRAS F14378-3651	ACIS-S	NONE	15
14:57:00.70	24:37:02.70	VV 340a	ACIS-S	NONE	15
16:38:13.20	-68:26:42.80	ESO 069-IG006	ACIS-S	NONE	15
17:14:20.00	53:10:30.00	IRAS F17132+5313	ACIS-S	NONE	15
18:32:41.10	-34:11:27.50	IRAS F18293-3413	ACIS-S	NONE	15
19:14:30.90	-21:19:07.00	ESO 593-IG008	ACIS-S	NONE	15
19:32:21.20	-3:59:56.30	IRAS F19297-0406	ACIS-S	NONE	15
19:56:35.40	11:19:02.60	IRAS 19542+1110	ACIS-S	NONE	15
20:57:23.30	17:07:34.30	CGCG 448-020	ACIS-S	NONE	15
21:11:30.40	58:23:03.20	IRAS 21101+5810	ACIS-S	NONE	15
22:49:39.90	-48:50:58.10	ESO 239-IG002	ACIS-S	NONE	15
22:51:49.30	-17:52:23.50	IRAS F22491-1808	ACIS-S	NONE	15
23:21:04.30	-69:12:54.00	ESO 077-IG014	ACIS-S	NONE	15

Proposal Number: 08700512

Title: Jets, Bubbles, Binaries, and Hot Gas: A Deep Observation of Centaurus A

PI Name: Ralph Kraft

We propose to observe Centaurus A, the nearest radio galaxy and the nearest massive early-type galaxy, for 1.2 Ms. We will probe the particle acceleration processes of the jet to an unprecedented sensitivity, by measuring its spectrum and morphology on the scale of radiative energy losses. We also will measure the proper motions and velocity shear of X-ray knots. We will measure the temperature and density structure of the shock around the SW radio lobe to study the hydrodynamics of the lobe/ISM interaction to a level previously seen only in Galactic SNRs. We will detect hundreds of X-ray binaries, probe the GC/LMXB link, and investigate their temporal properties. Finally, we will measure the thermodynamic paramters of the gas and the elemental abundance throughout the ISM.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
13:25:18.79	-43:03:01.72	Centaurus A Jet	ACIS-I	NONE	100
13:25:19.15	-43:02:42.40	Centaurus A Jet	ACIS-I	NONE	100
13:25:32.79	-43:01:35.13	Centaurus A Jet	ACIS-I	NONE	100
13:25:46.00	-42:58:14.58	Centaurus A Jet	ACIS-I	NONE	100
13:25:51.80	-43:00:04.43	Centaurus A Jet	ACIS-I	NONE	100
13:25:51.80	-43:00:04.43	Centaurus A Jet	ACIS-I	NONE	100

Proposal Number: 07400810

Title: CHAZSS: The Chandra HETGS Atoll/Z Spectroscopic Survey

PI Name: Jon Miller

High-res. X-ray spectroscopy of accretion-powered sources in the Chandra era has focused on black holes. Neutron stars with low magnetic fields - "Z" and "atoll" binaries - have largely been ignored and/or poorly observed at high resolution. We propose a survey of 6 "Z" and "atoll" neutron star binaries. In a total of only 300 ksec, we can observe each of the 6 sources in our sample twice, obtaining consistent, robust, and constraining spectra free from photon pile-up. High-res. spectroscopy will break degeneracies in X-ray timing-based models for the accretion flows in these systems, and provide new insights into both the origin of the "kHz" QPOs seen in these sources and the nature of the "Z" and "atoll" tracks they trace in color-color diagrams.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
16:40:55.50	-53:45:05.00	4U 1636-53	ACIS-S	HETG	25
16:40:55.50	-53:45:05.00	4U 1636-53	ACIS-S	HETG	25
16:45:47.70	-45:36:40.00	GX 340+0	ACIS-S	HETG	25
16:45:47.70	-45:36:40.00	GX 340+0	ACIS-S	HETG	25
17:02:44.50	-36:25:23.00	GX 349+2	ACIS-S	HETG	25
17:05:44.50	-36:25:23.00	GX 349+2	ACIS-S	HETG	12.5
17:05:44.50	-36:25:23.00	GX 349+2	ACIS-S	HETG	12.5
17:38:58.30	-44:27:00.00	4U 1735-44	ACIS-S	HETG	25
17:38:58.30	-44:27:00.00	4U 1735-44	ACIS-S	HETG	25
18:16:01.40	-14:02:11.00	GX 17+2	ACIS-S	HETG	25
18:16:01.40	-14:02:11.00	GX 17+2	ACIS-S	HETG	25
18:23:40.50	-30:21:40.00	4U 1820-30	ACIS-S	HETG	25
18:23:40.50	-30:21:40.00	4U 1820-30	ACIS-S	HETG	25

Proposal Number: 05400594

Title: High Resolution Photospheric Spectroscopy of the Neutron Star in EXO0748-676

PI Name: FREDERIK PAERELS

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.	Grating	Exp.Time
7:48:33.30	-67:45:00.00	EXO 0748-676	ACIS-S	HETG	130
7:48:33.30	-67:45:00.00	EXO 0748-676	ACIS-S	HETG	170

Proposal Number: 03400837

Title: COMPLETE COMPACT OBJECT AND BINARY SURVEY OF 47TUC

PI Name: Jonathan Grindlay

Our cycle 1 observation of 47Tuc has shown its promise as the ultimate laboratory for study of the production and evolution of compact binaries and compact objects in globular clusters. We propose a deep (4 x 75ksec) ACIS-S observation to measure the complete populations of millisecond pulsars (MSPs) and cataclysmic variables (CVs) by their variability and spectra and to constrain the main sequence binary population. Coordinated HST (ACS) data would provide unique identifications of CVs and many MSPs and allow the full population of quiescent low mass x-ray binaries to be distinguished from CVs. This dataset would provide fundamental constraints for the origins of neutron stars, millisecond pulsars, magnetic white dwarfs and compact binaries in globular clusters.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
0:24:05.80	-72:04:51.20	47 TUCANAE	ACIS-S	NONE	5
0:24:05.80	-72:04:51.20	47 TUCANAE	ACIS-S	NONE	5
0:24:05.80	-72:04:51.20	47 TUCANAE	ACIS-S	NONE	5
0:24:05.80	-72:04:51.20	47 TUCANAE	ACIS-S	NONE	5
0:24:05.80	-72:04:51.20	47 TUCANAE	ACIS-S	NONE	69
0:24:05.80	-72:04:51.20	47 TUCANAE	ACIS-S	NONE	69
0:24:05.80	-72:04:51.20	47 TUCANAE	ACIS-S	NONE	69
0:24:05.80	-72:04:51.20	47 TUCANAE	ACIS-S	NONE	69

Proposal Number: 07400594

Title: The lowest-luminosity quiescent neutron star transient: implications for strong field gravity and the neutron star EoS

PI Name: Peter Jonker

We propose to obtain a 300 ksec ACIS-S observation of the quiescent neutron star (NS) SXT 1H1905+000. Because of a non-detection during a previous 25 ksec Chandra ACIS-S observation, the NS quiescent luminosity is the lowest of all NS SXTs. It also has a low N_H, a well-known source distance, and an accurately known source position. These observations will eliminate the gap in the derived quiescent luminosities between NS and BH SXTs which is used as being evidence for a BH event horizon. Furthermore, this extremely low NS luminosity allows us to derive that 1H1905+000 harbors a cold, massive NS ruling out all equations of state (EoSs) except the stiffest EoSs for NSs with a nucleonic core. Constraining the NS EoS is one of the ultimate goals of NS studies.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
19:08:27.00	0:10:08.00	1H 1905+000	ACIS-S	NONE	10
19:08:27.00	0:10:08.00	1H 1905+000	ACIS-S	NONE	40
19:08:27.00	0:10:08.00	1H 1905+000	ACIS-S	NONE	42
19:08:27.00	0:10:08.00	1H 1905+000	ACIS-S	NONE	43
19:08:27.00	0:10:08.00	1H 1905+000	ACIS-S	NONE	165

Proposal Number: 06800102

Title: A CHANDRA TREASURY OBSERVATION OF THE BEST EXAMPLE OF A CLUSTER COLD FRONT

PI Name: Alexey Vikhlinin

We propose a 450 ksec observation of A3667, the best example of a cluster cold front. A deep image of the best cold front by the highest angular resolution X-ray telescope will push the study of the physics of the intracluster medium to the limit. Our main goals are 1) to observe the turbulence in the intracluster medium by direct imaging of any perturbations of the front surface; 2) to study transport processes in the ICM using the gas density and temperature profiles across the front with a spatial resolution of 1/5 of the Coulomb mean free path; 3) to characterize the magnetic field structure by mapping the onset of the Kelvin-Helmholtz instability. The proposed deep Chandra image of A3667 will be one of the treasury images of the X-ray astronomy.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
20:13:07.25	-56:53:24.00	Abell 3667	ACIS-I	NONE	46
20:13:07.25	-56:53:24.00	Abell 3667	ACIS-I	NONE	47
20:13:07.25	-56:53:24.00	Abell 3667	ACIS-I	NONE	50
20:13:07.25	-56:53:24.00	Abell 3667	ACIS-I	NONE	61
20:13:07.25	-56:53:24.00	Abell 3667	ACIS-I	NONE	115
20:13:07.25	-56:53:24.00	Abell 3667	ACIS-I	NONE	131

Proposal Number: 03800272

Title: MACS: THE X-RAY PROPERTIES OF THE MOST MASSIVE GALAXY CLUSTERS AT Z>0.3

PI Name: Harald Ebeling

We propose ACIS-I and HST observations of 30 distant and very X-ray luminous clusters (z>0.3, Lx>1e45) detected in the MAssive Cluster Survey (MACS). 22 of these 30 are new discoveries. Our targets are the high-z counterparts of the best-studied local systems and, combined with 4 others scheduled for observation, form a statistical sample >10 times larger than any previous one in this redshift and luminosity range. Chandra's unique capabilities will allow us to obtain spatially resolved gas temperature and density maps to constrain both the cosmological and physical parameters governing the evolution of the most massive clusters at z<0.5. The proposed observations are complemented by extensive groundbased follow-up studies of weak gravitational lensing, galaxy dynamics and the SZ effect.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
0:11:42.90	-15:23:22.00	MACSJ0011.7-1523	ACIS-I	NONE	22
0:35:26.10	-20:15:44.00	MACSJ0035.4-2015	ACIS-I	NONE	22
0:47:21.60	-8:09:21.00	MACSJ0047.3-0810	ACIS-I	NONE	14
1:52:32.60	-28:53:22.00	MACSJ0152.5-2852	ACIS-I	NONE	18
1:59:49.30	-8:49:59.00	MACSJ0159.8-0849	ACIS-I	NONE	18
2:42:35.90	-21:32:26.00	MACSJ0242.5-2132	ACIS-I	NONE	12
2:57:41.70	-22:09:11.99	MACSJ0257.6-2209	ACIS-I	NONE	20
3:08:56.00	26:45:37.00	MACSJ0308.9+2645	ACIS-I	NONE	25
4:04:33.20	11:07:58.00	MACSJ0404.6+1109	ACIS-I	NONE	24
4:17:34.70	-11:54:33.00	MACSJ0417.5-1154	ACIS-I	NONE	12
4:29:36.10	-2:53:07.00	MACSJ0429.6-0253	ACIS-I	NONE	24
5:20:42.00	-13:28:48.00	MACSJ0520.7-1328	ACIS-I	NONE	20
5:47:01.50	-39:04:28.00	MACSJ0547.0-3904	ACIS-I	NONE	22
9:49:51.80	17:07:09.00	MACSJ0949.8+1708	ACIS-I	NONE	15
11:15:51.90	1:29:54.00	MACSJ1115.8+0129	ACIS-I	NONE	16
11:31:54.20	-19:55:42.00	MACSJ1131.8-1955	ACIS-I	NONE	15
12:06:12.20	-8:48:04.00	MACSJ1206.2-0847	ACIS-I	NONE	24
13:20:08.50	70:04:39.00	MACSJ1319.9+7003	ACIS-I	NONE	20
14:27:39.50	-25:21:03.00	MACSJ1427.6-2521	ACIS-I	NONE	17
17:20:16.90	35:36:25.00	MACSJ1720.2+3536	ACIS-I	NONE	21
17:31:40.00	22:51:58.00	MACSJ1731.6+2252	ACIS-I	NONE	21
19:31:49.70	-26:34:34.00	MACSJ1931.8-2634	ACIS-I	NONE	14
20:49:55.90	-32:16:49.00	MACSJ2049.9-3217	ACIS-I	NONE	24
22:11:46.00	-3:49:45.00	MACSJ2211.7-0349	ACIS-I	NONE	18
22:28:33.90	20:37:16.00	MACSJ2228.5+2036	ACIS-I	NONE	21
22:29:45.40	-27:55:37.00	MACSJ2229.7-2755	ACIS-I	NONE	17
22:45:04.80	26:38:04.00	MACSJ2245.0+2637	ACIS-I	NONE	17
23:11:33.30	3:38:04.00	MACSJ2311.5+0338	ACIS-I	NONE	14

Proposal Number: 08800952

Title: A Complete Baryon Census in a Nearby Galaxy Group

PI Name: John Mulchaey

We propose an ACIS-I mosaic of the NGC2563 group to study the X-ray properties of the group galaxies out to the virial radius of the system. The proposed observations will provide important observational constraints on the mechanisms that drive galaxy evolution in groups by allowing us to study how the properties of galaxies vary with distance from the group center, IGM and galaxy density. The Chandra data will allow us to study the hot ISM halos of individual galaxies as well as the more extended intragroup medium component, which combined with our existing optical and HI data will provide a complete census of all of the major baryonic components in the group.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
8:18:00.00	20:49:42.20	NGC2563-P12	ACIS-I	NONE	30
8:18:50.80	21:42:31.10	NGC2563-P11	ACIS-I	NONE	30
8:19:15.00	21:20:56.80	NGC2563-P8	ACIS-I	NONE	30
8:19:15.10	21:04:59.40	NGC2563-P6	ACIS-I	NONE	30
8:19:15.30	20:49:00.40	NGC2563-P7	ACIS-I	NONE	30
8:19:17.70	20:33:33.70	NGC2563-P13	ACIS-I	NONE	30
8:20:23.70	20:49:01.60	NGC2563-P3	ACIS-I	NONE	30
8:20:23.70	21:05:00.50	NGC2563-P1	ACIS-I	NONE	50
8:20:23.70	21:20:57.90	NGC2563-P5	ACIS-I	NONE	30
8:21:32.10	20:49:01.00	NGC2563-P2	ACIS-I	NONE	30
8:21:32.20	21:05:00.00	NGC2563-P10	ACIS-I	NONE	30
8:21:32.30	21:20:57.40	NGC2563-P4	ACIS-I	NONE	30
8:22:40.20	21:02:03.90	NGC2563-P9	ACIS-I	NONE	30
8:23:16.40	21:23:09.90	NGC2563-P14	ACIS-I	NONE	30

Proposal Number: 07800432

Title: The Cosmological Formation of Galaxy Groups

PI Name: David Buote

One of the strongest, untested cosmological predictions is the scatter of the concentrations of dark matter halos on the group scale. To quantify this scatter of concentrations requires well-defined samples. We propose a novel systematic study of the core properties of 15 groups representing a complete, X-ray flux-limited sample. In addition to dark matter properties, we will address: (1) entropy and non-gravitational heating, (2) central iron abundances and stellar enrichment, (3) AGN heating and the cooling flow paradox, and (4) the formation of central galaxies. The implications of these measurements for cosmology, supernovae history, star formation and AGN heating will be assessed with numerical simulations. We request observations of 10 unobserved groups in our sample

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
10:22:04.70	38:30:43.00	RXC J1022.0+3830	ACIS-S	NONE	42
11:00:48.90	10:33:35.00	RXC J1100.8+1033	ACIS-S	NONE	27
11:09:43.10	21:45:43.00	RXC J1109.7+2145	ACIS-S	NONE	37
11:10:32.60	28:42:59.00	RXC J1110.5+2842	ACIS-S	NONE	27
11:30:01.80	36:37:49.00	RXC J1130.0+3637	ACIS-S	NONE	50
11:34:50.50	49:03:28.00	RXC J1134.8+4903	ACIS-S	NONE	52
11:47:20.70	55:44:36.00	RXC J1147.3+5544	ACIS-S	NONE	44
12:06:37.40	28:11:01.00	RXC J1206.6+2811	ACIS-S	NONE	36
13:20:15.40	33:08:30.00	RXC J1320.2+3308	ACIS-S	NONE	39
13:24:11.90	13:58:45.00	RXC J1324.1+1358	ACIS-S	NONE	21
13:24:11.90	13:58:45.00	RXC J1324.1+1358	ACIS-S	NONE	26

Proposal Number: 05800170

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

PI Name: Andrew Fabian

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.	Grating	Exp.Time
3:19:48.20	41:30:42.20	Abell 426	ACIS-S	NONE	29
3:19:48.20	41:30:42.20	Abell 426	ACIS-S	NONE	30
3:19:48.20	41:30:42.20	Abell 426	ACIS-S	NONE	30
3:19:48.20	41:30:42.20	Abell 426	ACIS-S	NONE	30
3:19:48.20	41:30:42.20	Abell 426	ACIS-S	NONE	50
3:19:48.20	41:30:42.20	Abell 426	ACIS-S	NONE	50
3:19:48.20	41:30:42.20	Abell 426	ACIS-S	NONE	91
3:19:48.20	41:30:42.20	Abell 426	ACIS-S	NONE	100
3:19:48.20	41:30:42.20	Abell 426	ACIS-S	NONE	100
3:19:48.20	41:30:42.20	Abell 426	ACIS-S	NONE	120
3:19:48.20	41:30:42.20	Abell 426	ACIS-S	NONE	170

Proposal Number: 02800845

Title: A COMPLETE X-RAY CLUSTER SAMPLE AT Z > 0.8

PI Name: Spencer Stanford

We propose to observe three X-ray selected clusters of galaxies from the RDCS, one at z = 1.1 and two at z ~ 0.8. In conjunction with other data already being obtained by Chandra and XMM, we would then have luminosity and temperature measurements for a complete sample of 8 clusters at z > 0.8. We will produce the first temperature function at these high redshifts. Using Chandra's high angular resolution, we can minimize the contamination from point sources, a serious problem at faint flux limits, as well as study the spatial properties of the intra-cluster medium. With this combination of temperatures, luminosities, and spatial profiles, we will both probe the cluster mass function of the universe at high redshift and study the thermal history of the intra-cluster medium.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
9:10:45.41	54:22:05.00	RX J0910+5422	ACIS-I	NONE	76
9:10:45.41	54:22:05.00	RX J0910+5422	ACIS-I	NONE	124
13:17:21.84	29:11:17.00	RX J1317.4+2911	ACIS-I	NONE	115
13:50:46.10	60:07:09.00	RX J1350.0+6007	ACIS-I	NONE	60

Proposal Number: 06800101

Title: DARK ENERGY WITH X-RAY CLUSTERS: CHANDRA OBSERVATIONS OF 41 HIGH-REDSHIFT CLUSTERS FROM THE 400 deg^2 ROSAT PSPC SURVEY

PI Name: Alexey Vikhlinin

We propose Chandra observations to measure temperature and gas mass in a sample of 41 high-z galaxy clusters from our 400 deg^2 ROSAT survey. This sample is comparable in number to all clusters in the local Universe (z<0.1) above a similar limiting mass, and covers a factor of 3 larger volume at z=0.4-1. Chandra observations will provide the total mass function estimates at =0.4, 0.5, and 0.65, which can be directly compared with the local measurements at =0.05. These data will provide a measurement of the dark energy equation of state via the cluster evolution test which is completely independent from SN Ia and CMB and has different degeneracies. Some targets in this proposal are in common with the HRC GTO proposal 06900018. These programs are not in conflict.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
0:30:33.60	26:18:16.00	cl0030+2618	ACIS-I	NONE	20
2:16:33.70	-17:47:27.00	cl0216-1747	ACIS-I	NONE	24.5
2:16:33.70	-17:47:27.00	cl0216-1747	ACIS-I	NONE	40.5
2:30:26.60	18:36:22.00	cl0230+1836	ACIS-I	NONE	70
3:28:36.10	-21:40:04.00	cl0328-2140	ACIS-I	NONE	12
3:28:36.10	-21:40:04.00	cl0328-2140	ACIS-I	NONE	48
3:33:10.30	-24:56:40.00	cl0333-2456	ACIS-I	NONE	40
3:55:59.30	-37:41:46.00	cl0355-3741	ACIS-I	NONE	30
4:05:24.30	-41:00:15.00	cl0405-4100	ACIS-I	NONE	8
4:05:24.30	-41:00:15.00	cl0405-4100	ACIS-I	NONE	72
5:21:10.50	-25:30:36.00	cl0521-2530	ACIS-I	NONE	15
8:53:13.40	57:59:44.00	cl0853+5759	ACIS-I	NONE	25
9:56:02.80	41:07:08.00	cl0956+4107	ACIS-I	NONE	40
12:02:13.70	57:51:53.00	cl1202+5751	ACIS-I	NONE	60
12:12:19.20	27:33:13.00	cl1212+2733	ACIS-I	NONE	15
12:22:01.90	27:09:19.00	cl1222+2709	ACIS-I	NONE	15
12:22:01.90	27:09:19.00	cl1222+2709	ACIS-I	NONE	50
13:57:19.40	62:32:42.00	cl1357+6232	ACIS-I	NONE	19
13:57:19.40	62:32:42.00	cl1357+6232	ACIS-I	NONE	26

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
3:36:59.85	-35:29:39.84	FORNAX CLUSTER	ACIS-I	NONE	50
3:37:09.50	-35:44:00.06	FORNAX CLUSTER	ACIS-I	NONE	50
3:37:14.40	-35:13:27.84	FORNAX CLUSTER	ACIS-I	NONE	50
3:38:11.20	-35:41:54.20	FORNAX CLUSTER	ACIS-I	NONE	50
3:38:25.56	-35:25:42.60	FORNAX CLUSTER	ACIS-I	NONE	50
3:38:37.01	-35:09:27.72	FORNAX CLUSTER	ACIS-I	NONE	50
3:38:49.58	-35:34:36.34	FORNAX CLUSTER	ACIS-I	NONE	50
3:39:30.51	-35:45:22.03	FORNAX CLUSTER	ACIS-I	NONE	50
3:39:44.60	-35:29:08.92	FORNAX CLUSTER	ACIS-I	NONE	50
3:39:55.80	-35:12:56.16	FORNAX CLUSTER	ACIS-I	NONE	50

Proposal Number: 09800310

Title: Probing Dark Energy with Relaxed Galaxy Clusters

PI Name: Steven Allen

We seek to constrain dark energy using studies of the apparent evolution of the X-ray gas mass fraction in the most X-ray luminous, dynamically relaxed galaxy clusters. The proposed observations will improve the detection of the effects of dark energy from the X-ray data alone to > 5 sigma. More importantly, they will allow us to measure the level of intrinsic (systematic) scatter in distance measurements from this technique and establish whether this is smaller than from type Ia supernovae measurements. Used in combination with supernovae and CMB data, the new Chandra observations will allow the most precise search to date for evolution in the dark energy equation of state - our best approach in trying to understand the origin of cosmic acceleration.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
1:59:49.30	8:49:59.20	MACS0159	ACIS-I	NONE	20
4:39:02.30	5:20:43.60	RXJ0439-0520	ACIS-I	NONE	30
10:23:39.40	4:11:14.30	Zwicky 3146	ACIS-I	NONE	40
11:15:52.10	1:29:52.90	MACS1115	ACIS-I	NONE	40
13:11:01.60	-3:10:40.00	MACS1311	ACIS-I	NONE	30
13:59:10.30	-19:29:24.40	MACS1359	ACIS-I	NONE	50
14:27:16.20	44:07:31.00	MACS1427+44	ACIS-I	NONE	40
14:27:39.40	-25:21:02.00	MACS1427-25	ACIS-I	NONE	30
16:21:24.80	38:10:09.00	MACS1621	ACIS-I	NONE	60
20:46:00.60	-34:30:17.00	MACS2046	ACIS-I	NONE	40
21:29:39.90	0:05:20.00	RXJ2129+0005	ACIS-I	NONE	30
22:29:45.30	-27:55:36.90	MACS2229	ACIS-I	NONE	15
23:08:22.10	-2:11:29.10	Abell 2537	ACIS-I	NONE	40

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
5:22:17.00	-48:20:10.00	DLS J0522-4820	ACIS-I	NONE	20
9:16:00.00	29:31:34.00	DLS J0916+2931	ACIS-I	NONE	20
10:49:41.00	-4:17:44.00	DLS J1049-0417	ACIS-I	NONE	20
10:54:08.00	-5:49:44.00	DLS J1054-0549	ACIS-I	NONE	20
10:55:12.00	-5:03:43.00	DLS J1055-0503	ACIS-I	NONE	20
14:02:01.70	-10:19:44.00	DLS J1402-1019	ACIS-I	NONE	20
14:02:12.00	-10:28:14.00	DLS J1402-1028	ACIS-I	NONE	20

Proposal Number: 09800847

Title: BOW SHOCK, ELECTRON-ION EQUILIBRIUM, BREAKUP OF COOL CORE, AND DARK SUBCLUSTER IN ABELL 520

PI Name: Maxim Markevitch

Shock fronts provide a unique tool to study the cluster plasma. Only two have been found, those in 1E0657 and A520. Using a long observation of 1E0657, we have determined, for the first time in any astrophysical plasma, that electron-proton equilibration time is shorter than Coulomb - a tantalizing result but based on one object. A520 gives the only chance to confirm it. Its shock also coincides with an edge of the radio halo, enabling tests of the origin of the intracluster relativistic electrons. A520 also exhibits a remnant of a cool core broken up by merger-induced instabilities, providing data on plasma viscosity. Finally, weak lensing map of A520 reveals an intriguing dark subcluster almost devoid of galaxies. We propose a long observation of this exceptionally interesting cluster.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
4:54:05.40	2:53:35.00	A520_OFF1	ACIS-I	NONE	115
4:54:05.40	2:53:35.00	A520_OFF2	ACIS-I	NONE	115
4:54:05.40	2:53:35.00	A520_OFF3	ACIS-I	NONE	115
4:54:05.40	2:53:35.00	A520_OFF4	ACIS-I	NONE	115

Proposal Number: 06800613

Title: The History of AGN Activity in M87 and the Interaction of Nuclear Outbursts with the Surrounding Atmosphere

PI Name: William Forman

We propose a 500 ksec ACIS-I observation to study the interaction between energy outbursts from the supermassive black hole (SMBH) in M87 and its surrounding gaseous atmosphere. We will inventory the plasma bubbles inflated by the SMBH, search for weak shocks, study the interaction of relativistic plasma in bubbles with the surrounding hot gas, measure turbulence in the cluster gas, study the microphysics of the interaction between the plasma in the bubbles and the surrounding gas, and estimate the gas viscosity by measuring the width of shock fronts. By determining the energy associated with bubbles and shocks, we can chronicle the mechanical power output of the SMBH. Finally we will study particle acceleration and cooling models by measuring inter-knot spectra along the jet.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
12:30:49.50	12:23:28.00	M87	ACIS-I	NONE	4
12:30:49.50	12:23:28.00	M87	ACIS-I	NONE	4
12:30:49.50	12:23:28.00	M87	ACIS-I	NONE	4
12:30:49.50	12:23:28.00	M87	ACIS-I	NONE	17
12:30:49.50	12:23:28.00	M87	ACIS-I	NONE	32
12:30:49.50	12:23:28.00	M87	ACIS-I	NONE	33
12:30:49.50	12:23:28.00	M87	ACIS-I	NONE	48
12:30:49.50	12:23:28.00	M87	ACIS-I	NONE	70
12:30:49.50	12:23:28.00	M87	ACIS-I	NONE	140
12:30:49.50	12:23:28.00	M87	ACIS-I	NONE	160

Proposal Number: 05800890

Title: THE MOST INTERESTING CLUSTER IN THE UNIVERSE

PI Name: Maxim Markevitch

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.	Grating	Exp.Time
6:58:19.85	-55:56:29.40	1E0657-56	ACIS-I	NONE	28
6:58:19.85	-55:56:29.40	1E0657-56	ACIS-I	NONE	30
6:58:19.85	-55:56:29.40	1E0657-56	ACIS-I	NONE	40
6:58:19.85	-55:56:29.40	1E0657-56	ACIS-I	NONE	41
6:58:19.85	-55:56:29.40	1E0657-56	ACIS-I	NONE	79
6:58:19.85	-55:56:29.40	1E0657-56	ACIS-I	NONE	85
6:58:19.85	-55:56:29.40	1E0657-56	ACIS-I	NONE	96
6:58:19.85	-55:56:29.40	1E0657-56	ACIS-I	NONE	101

Proposal Number: 08900073

Title: THE CHANDRA-COSMOS SURVEY

PI Name: Martin Elvis

We propose the Chandra-COSMOS survey which will provide an unprecedented combination of contiguous area, depth and resolution. 36 densely tiled observations will cover the central 0.7 sq.deg. COSMOS field to a uniform 200ksec depth. COSMOS explores the coupled evolution of galaxies, dark matter halos and AGNs (massive black holes) largely free of cosmic variance. COSMOS is a comprehensive survey including: HST, Spitzer, Subaru, VLT, Magellan, VLA, MAMBO, GALEX, & potentially EVLA & ALMA. Chandra resolution & sensitivity enables the study of large scale phenomena: (1) influence of the surrounding environment; (2) interaction between galaxies; (3) influence of groups and clusters: (4) BH growth and census; (5) star formation and stellar populations; (6) feedback from starbursts and AGNs.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
9:58:36.96	1:58:41.53	C-COSMOS6-6	ACIS-I	NONE	50
9:58:47.90	2:06:12.48	C-COSMOS5-6	ACIS-I	NONE	50
9:58:58.85	2:13:43.42	C-COSMOS4-6	ACIS-I	NONE	50
9:59:07.03	1:55:57.49	C-COSMOS6-5	ACIS-I	NONE	50
9:59:09.81	2:21:14.70	C-COSMOS3-6	ACIS-I	NONE	50
9:59:17.97	2:03:28.44	C-COSMOS5-5	ACIS-I	NONE	50
9:59:20.76	2:28:45.64	C-COSMOS2-6	ACIS-I	NONE	11
9:59:20.76	2:28:45.64	C-COSMOS2-6	ACIS-I	NONE	17
9:59:20.76	2:28:45.64	C-COSMOS2-6	ACIS-I	NONE	22
9:59:28.92	2:10:59.38	C-COSMOS4-5	ACIS-I	NONE	50
9:59:31.72	2:36:16.58	C-COSMOS1-6	ACIS-I	NONE	20
9:59:31.72	2:36:16.58	C-COSMOS1-6	ACIS-I	NONE	30
9:59:37.10	1:53:13.47	C-COSMOS6-4	ACIS-I	NONE	50
9:59:39.88	2:18:30.67	C-COSMOS3-5	ACIS-I	NONE	50
9:59:48.04	2:00:44.41	C-COSMOS5-4	ACIS-I	NONE	50
9:59:50.83	2:26:01.61	C-COSMOS2-5	ACIS-I	NONE	50
9:59:58.99	2:08:15.36	C-COSMOS4-4	ACIS-I	NONE	50
10:00:01.79	2:33:32.55	C-COSMOS1-5	ACIS-I	NONE	22
10:00:01.79	2:33:32.55	C-COSMOS1-5	ACIS-I	NONE	28
10:00:07.17	1:50:29.44	C-COSMOS6-3	ACIS-I	NONE	50
10:00:09.95	2:15:46.64	C-COSMOS3-4	ACIS-I	NONE	22
10:00:09.95	2:15:46.64	C-COSMOS3-4	ACIS-I	NONE	28
10:00:18.11	1:58:00.38	C-COSMOS5-3	ACIS-I	NONE	50
10:00:20.90	2:23:17.58	C-COSMOS2-4	ACIS-I	NONE	20
10:00:20.90	2:23:17.58	C-COSMOS2-4	ACIS-I	NONE	30
10:00:29.06	2:05:31.33	C-COSMOS4-3	ACIS-I	NONE	50
10:00:31.85	2:30:48.52	C-COSMOS1-4	ACIS-I	NONE	21
10:00:31.85	2:30:48.52	C-COSMOS1-4	ACIS-I	NONE	29
10:00:37.24	1:47:45.41	C-COSMOS6-2	ACIS-I	NONE	50
10:00:40.02	2:13:02.61	C-COSMOS3-3	ACIS-I	NONE	22
10:00:40.02	2:13:02.61	C-COSMOS3-3	ACIS-I	NONE	28
10:00:48.18	1:55:16.35	C-COSMOS5-2	ACIS-I	NONE	50
10:00:50.97	2:20:33.55	C-COSMOS2-3	ACIS-I	NONE	50
10:00:59.13	2:02:47.30	C-COSMOS4-2	ACIS-I	NONE	50
10:01:01.92	2:28:04.50	C-COSMOS1-3	ACIS-I	NONE	50
10:01:07.30	1:45:01.39	C-COSMOS6-1	ACIS-I	NONE	17
10:01:07.30	1:45:01.39	C-COSMOS6-1	ACIS-I	NONE	33
10:01:10.08	2:10:18.59	C-COSMOS3-2	ACIS-I	NONE	18
10:01:10.08	2:10:18.59	C-COSMOS3-2	ACIS-I	NONE	32
10:01:18.25	1:52:32.34	C-COSMOS5-1	ACIS-I	NONE	24
10:01:18.25	1:52:32.34	C-COSMOS5-1	ACIS-I	NONE	26
10:01:21.03	2:17:49.54	C-COSMOS2-2	ACIS-I	NONE	50
10:01:29.19	2:00:03.29	C-COSMOS4-1	ACIS-I	NONE	15
10:01:29.19	2:00:03.29	C-COSMOS4-1	ACIS-I	NONE	35
10:01:31.99	2:25:20.48	C-COSMOS1-2	ACIS-I	NONE	50
10:01:40.15	2:07:34.57	C-COSMOS3-1	ACIS-I	NONE	15
10:01:40.15	2:07:34.57	C-COSMOS3-1	ACIS-I	NONE	35
10:01:51.10	2:15:05.52	C-COSMOS2-1	ACIS-I	NONE	50
10:02:02.05	2:22:36.46	C-COSMOS1-1	ACIS-I	NONE	50

Proposal Number: 05900547

Title: The Balance of Power between Starbursts and AGN: a Chandra/SIRTF Survey.

PI Name: Belinda Wilkes

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.	Grating	Exp.Time
10:43:27.23	59:10:15.07	SWIRE LOCKMAN 7	ACIS-I	NONE	70
10:44:06.67	58:56:05.28	SWIRE LOCKMAN 4	ACIS-I	NONE	70
10:44:46.15	58:41:55.45	SWIRE LOCKMAN 1	ACIS-I	NONE	70
10:45:20.56	59:15:11.16	SWIRE LOCKMAN 8	ACIS-I	NONE	70
10:46:00.00	59:01:00.00	SWIRE LOCKMAN 5 (center)	ACIS-I	NONE	70
10:46:39.44	58:46:51.24	SWIRE LOCKMAN 2	ACIS-I	NONE	70
10:47:13.85	59:20:06.95	SWIRE LOCKMAN 9	ACIS-I	NONE	70
10:47:53.44	59:05:57.00	SWIRE LOCKMAN 6	ACIS-I	NONE	70
10:48:32.77	58:51:47.33	SWIRE LOCKMAN 3	ACIS-I	NONE	70

Proposal Number: 09900660

Title: The Evolution of Faint AGN at High Redshift

PI Name: Kirpal Nandra

We propose a very deep (total 800ks/field) Chandra survey of 0.25 deg2 covering 3 contiguous fields in the Extended Groth Strip, which have exceptional multiwaveband coverage obtained by the AEGIS project. These data, in combination with the CDF North and South, will provide a definitive measurement of the evolution of faint, X-ray selected AGN from z=3-4, where the optical number counts start to drop dramatically. In combination with ultradeep Spitzer data in the same region, this survey will also provide a crucial step forward towards a more complete census of AGN activity and the importance of Compton thick AGN at high z, with associated implications for the total accretion budget of the universe.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
14:18:09.00	52:37:04.40	AEGIS-3	ACIS-I	NONE	120
14:18:09.00	52:37:04.40	AEGIS-3	ACIS-I	NONE	160
14:18:09.00	52:37:04.40	AEGIS-3	ACIS-I	NONE	160
14:18:09.00	52:37:04.40	AEGIS-3	ACIS-I	NONE	160
14:19:12.00	52:48:38.20	AEGIS-2	ACIS-I	NONE	120
14:19:12.00	52:48:38.20	AEGIS-2	ACIS-I	NONE	160
14:19:12.00	52:48:38.20	AEGIS-2	ACIS-I	NONE	160
14:19:12.00	52:48:38.20	AEGIS-2	ACIS-I	NONE	160
14:20:15.50	53:00:09.70	AEGIS-1	ACIS-I	NONE	120
14:20:15.50	53:00:09.70	AEGIS-1	ACIS-I	NONE	160
14:20:15.50	53:00:09.70	AEGIS-1	ACIS-I	NONE	160
14:20:15.50	53:00:09.70	AEGIS-1	ACIS-I	NONE	160

Proposal Number: 07900865

Title: Searching for WHIM in Large-Scale Structures

PI Name: Luca Zappacosta

Simulations and observations indicate that galaxy overdensities are good tracers of the dark matter large-scale structures and therefore of the diffuse warm-hot phase (WHIM) that should be associated with them. The WHIM in these large-scale structures should have large column densities, and therefore should be much easier to detect than the low column density WHIM which has been targeted so far. However, this efficient method of investigating WHIM has yet to be exploited. We have identified 5 bright blazars just in the background of known large-scale structures. We propose to probe and study the WHIM in these structures by identifying the associated absorption lines in the spectrum of these AGNs during their outburst phases, through TOO observations for a total of 300ks with HRC-S/LETG.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
1:23:08.75	34:20:49.54	1ES 0120+340	HRC-S	LETG	1
2:32:48.60	20:17:17.00	1ES 0229+200	HRC-S	LETG	98
16:53:52.20	39:45:36.60	Mkn 501	HRC-S	LETG	99
22:02:43.30	42:16:40.00	BL Lac	HRC-S	LETG	1
23:23:52.14	42:10:58.88	1ES 2321+419	HRC-S	LETG	1

Proposal Number: 02900378

Title: AN ULTRADEEP SURVEY IN THE CHANDRA DEEP FIELD SOUTH

PI Name: RICCARDO GIACCONI

We propose to exploit the unique combination of angular resolution, sensitivity and field-of-view of the Chandra ACIS imager to perform the deepest X-ray survey ever in the well-studied "Chandra Deep Field South" (CDFS). With a total integration time of 1.5 Msec (request for this AO: 1 Msec) we reach a 0.5-2 keV flux limit of 2E-17 cgs. We aim to detect >500 sources, i.e. AGN to z=10, clusters to z=3 and starburst galaxies to z~1. Simulations based on the existing 130 ksec observation in the CDFS and realistic source counts and correlation function models show, that Chandra exposures will not be background or confusion limited up to 3Msec. We propose to make the Chandra data public immediately.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
3:32:27.50	-27:48:23.00	CDFS	ACIS-I	NONE	31
3:32:27.50	-27:48:23.00	CDFS	ACIS-I	NONE	69
3:32:27.50	-27:48:23.00	CDFS	ACIS-I	NONE	132
3:32:27.50	-27:48:23.00	CDFS	ACIS-I	NONE	132
3:32:27.50	-27:48:23.00	CDFS	ACIS-I	NONE	136

Proposal Number: 05900888

Title: X-Raying the Intergalactic Medium with Blazars in Outburst

PI Name: Fabrizio Nicastro

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.	Grating	Exp.Time
5:07:56.20	67:37:24.00	BL 0502+675	HRC-S	LETG	130
6:50:46.50	25:03:00.30	1ES 0647+250	HRC-S	LETG	80
10:31:18.40	50:53:36.00	1ES 1028+511	HRC-S	LETG	170

Proposal Number: 06900444

Title: Deep Chandra Imaging of the Extended Groth Strip: The Co-evolution of Black Holes and Galaxies

PI Name: Kirpal Nandra

The Extended Groth Strip (EGS) is a half square degree region that has been targeted intensively for galaxy evolution studies. A remarkable array of ultra-deep data have been or will be accumulated, to include radio, near/mid/far IR, optical and UV data of depth comparable to or better than any part of the sky. It is also the subject of the massive DEEP2 redshift survey, giving high quality Keck spectra for 16-17,000 galaxies. The clear gap in the coverage of the EGS is in the X-ray, and we therefore propose to augment the single deep Chandra pointing with 7 more, to image the whole strip. Our goal is to study the co-evolution of galaxies and black holes, by examining in detail the astrophysics of AGN activity, and its relationship to the host galaxy and surrounding large scale structure.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
14:15:22.50	52:08:26.40	EGS-7	ACIS-I	NONE	9
14:15:22.50	52:08:26.40	EGS-7	ACIS-I	NONE	15
14:15:22.50	52:08:26.40	EGS-7	ACIS-I	NONE	35
14:15:22.50	52:08:26.40	EGS-7	ACIS-I	NONE	41
14:15:22.50	52:08:26.40	EGS-7	ACIS-I	NONE	50
14:15:22.50	52:08:26.40	EGS-7	ACIS-I	NONE	50
14:16:24.50	52:20:02.59	EGS-6	ACIS-I	NONE	16.1
14:16:24.50	52:20:02.59	EGS-6	ACIS-I	NONE	16.1
14:16:24.50	52:20:02.59	EGS-6	ACIS-I	NONE	3.8
14:16:24.50	52:20:02.59	EGS-6	ACIS-I	NONE	4.5
14:16:24.50	52:20:02.59	EGS-6	ACIS-I	NONE	9
14:16:24.50	52:20:02.59	EGS-6	ACIS-I	NONE	10
14:16:24.50	52:20:02.59	EGS-6	ACIS-I	NONE	11.5
14:16:24.50	52:20:02.59	EGS-6	ACIS-I	NONE	17
14:16:24.50	52:20:02.59	EGS-6	ACIS-I	NONE	17.5
14:16:24.50	52:20:02.59	EGS-6	ACIS-I	NONE	20.5
14:16:24.50	52:20:02.59	EGS-6	ACIS-I	NONE	36
14:16:24.50	52:20:02.59	EGS-6	ACIS-I	NONE	38
14:18:20.38	52:39:01.87	EGS-5	ACIS-I	NONE	50
14:18:20.38	52:39:01.87	EGS-5	ACIS-I	NONE	50
14:18:20.38	52:39:01.87	EGS-5	ACIS-I	NONE	50
14:18:20.38	52:39:01.87	EGS-5	ACIS-I	NONE	50
14:19:23.90	52:50:32.69	EGS-4	ACIS-I	NONE	50
14:19:23.90	52:50:32.69	EGS-4	ACIS-I	NONE	50
14:19:23.90	52:50:32.69	EGS-4	ACIS-I	NONE	50
14:19:23.90	52:50:32.69	EGS-4	ACIS-I	NONE	50
14:20:28.00	53:02:01.30	EGS-3	ACIS-I	NONE	50
14:20:28.00	53:02:01.30	EGS-3	ACIS-I	NONE	50
14:20:28.00	53:02:01.30	EGS-3	ACIS-I	NONE	50
14:20:28.00	53:02:01.30	EGS-3	ACIS-I	NONE	50
14:21:32.70	53:13:27.70	EGS-2	ACIS-I	NONE	50
14:21:32.70	53:13:27.70	EGS-2	ACIS-I	NONE	50
14:21:32.70	53:13:27.70	EGS-2	ACIS-I	NONE	50
14:21:32.70	53:13:27.70	EGS-2	ACIS-I	NONE	50
14:22:42.30	53:25:37.51	EGS-1	ACIS-I	NONE	20
14:22:42.30	53:25:37.51	EGS-1	ACIS-I	NONE	30
14:22:42.30	53:25:37.51	EGS-1	ACIS-I	NONE	50
14:22:42.30	53:25:37.51	EGS-1	ACIS-I	NONE	50
14:22:42.30	53:25:37.51	EGS-1	ACIS-I	NONE	50

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
14:25:15.44	32:50:45.01	SS11	ACIS-I	NONE	5
14:25:15.44	33:15:11.61	SD41	ACIS-I	NONE	5
14:25:15.44	33:39:38.20	SD16	ACIS-I	NONE	5
14:25:15.44	34:04:04.80	SS24	ACIS-I	NONE	5
14:26:06.54	32:38:31.71	SS22	ACIS-I	NONE	5
14:26:06.54	33:02:58.31	SD52	ACIS-I	NONE	5
14:26:06.54	33:27:24.90	SS5	ACIS-I	NONE	5
14:26:06.54	33:51:51.50	SS13	ACIS-I	NONE	5
14:26:58.62	32:50:45.01	SS54	ACIS-I	NONE	5
14:26:58.62	33:15:11.61	SD30	ACIS-I	NONE	5
14:26:58.62	33:39:38.20	SD27	ACIS-I	NONE	5
14:26:58.62	34:04:04.80	SS35	ACIS-I	NONE	5
14:27:49.72	32:38:31.71	SS33	ACIS-I	NONE	5
14:27:49.72	33:02:58.31	SS9	ACIS-I	NONE	5
14:27:49.72	33:27:24.90	SS6	ACIS-I	NONE	5
14:27:49.72	33:51:51.50	SS2	ACIS-I	NONE	5
14:28:41.80	32:50:45.01	SS43	ACIS-I	NONE	5
14:28:41.80	33:15:11.61	SS19	ACIS-I	NONE	5
14:28:41.80	33:39:38.20	SD38	ACIS-I	NONE	5
14:28:41.80	34:04:04.80	SS46	ACIS-I	NONE	5
14:29:32.90	32:38:31.71	SS44	ACIS-I	NONE	5
14:29:32.90	33:02:58.31	SS20	ACIS-I	NONE	5
14:29:32.90	33:27:24.90	SD17	ACIS-I	NONE	5
14:29:32.90	33:51:51.50	SS47	ACIS-I	NONE	5
14:30:24.98	32:50:45.01	SS32	ACIS-I	NONE	5
14:30:24.98	33:15:11.61	SS8	ACIS-I	NONE	5
14:30:24.98	33:39:38.20	SD49	ACIS-I	NONE	5
14:30:24.98	34:04:04.80	SS1	ACIS-I	NONE	5
14:31:16.08	32:38:31.71	SS55	ACIS-I	NONE	5
14:31:16.08	33:02:58.31	SS31	ACIS-I	NONE	5
14:31:16.08	33:27:24.90	SD28	ACIS-I	NONE	5
14:31:16.08	33:51:51.50	SS36	ACIS-I	NONE	5
14:32:08.16	32:50:45.01	SS21	ACIS-I	NONE	5
14:32:08.16	33:15:11.61	SD51	ACIS-I	NONE	5
14:32:08.16	33:39:38.20	SS4	ACIS-I	NONE	5
14:32:08.16	34:04:04.80	SS12	ACIS-I	NONE	5
14:32:59.26	33:02:58.31	SS42	ACIS-I	NONE	5
14:32:59.26	33:27:24.90	SD39	ACIS-I	NONE	5
14:32:59.26	33:51:51.50	SS25	ACIS-I	NONE	5
14:33:51.34	32:50:45.01	SS10	ACIS-I	NONE	5
14:33:51.34	33:15:11.61	SD40	ACIS-I	NONE	5
14:33:51.34	33:39:38.20	SS15	ACIS-I	NONE	5
14:33:51.34	34:04:04.80	SS23	ACIS-I	NONE	5
14:34:42.44	33:02:58.31	SS53	ACIS-I	NONE	5
14:34:42.44	33:27:24.90	SD50	ACIS-I	NONE	5
14:34:42.44	33:51:51.50	SS14	ACIS-I	NONE	5
14:35:34.52	33:15:11.61	SD29	ACIS-I	NONE	5
14:35:34.52	33:39:38.20	SS26	ACIS-I	NONE	5
14:35:34.52	34:04:04.80	SS34	ACIS-I	NONE	5
14:36:25.62	33:27:24.90	SS7	ACIS-I	NONE	5
14:36:25.62	33:51:51.50	SS3	ACIS-I	NONE	5
14:37:17.70	33:39:38.20	SS37	ACIS-I	NONE	5
14:37:17.70	34:04:04.80	SS45	ACIS-I	NONE	5
14:38:08.80	33:27:24.90	SD18	ACIS-I	NONE	5
14:38:08.80	33:51:51.50	SS48	ACIS-I	NONE	5

Proposal Number: 03900164

Title: THE CHANDRA SURVEY OF THE HUBBLE DEEP FIELD NORTH AREA: A PUBLIC RESOURCE FOR THE PRESENT AND FUTURE OF X-RAY ASTRONOMY

PI Name: William Brandt

We propose to extend the Chandra deep survey of the HDF-N and its vicinity. The ultimate goal is to obtain 5 Ms of coverage over the next 5 years; currently we have 1 Ms coverage. Here we propose two public 500 ks observations. This project will fulfill one of Chandra's central design goals and will be a long-lasting legacy of Chandra, laying the groundwork for the next generation of X-ray observatories. We should remain nearly photon limited for point-sources near the aim point. We will study obscured and high-redshift AGN, starbursts, normal galaxies, clusters, groups, and diffuse X-ray emission. The HDF-N field is the ideal region for multiwavelength follow-up studies due to the enormous database already in place. Our ACIS team expertise will be extensively utilized.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
12:36:49.40	62:12:58.00	HDF-N	ACIS-I	NONE	50
12:36:49.40	62:12:58.00	HDF-N	ACIS-I	NONE	67
12:36:49.40	62:12:58.00	HDF-N	ACIS-I	NONE	90
12:36:49.40	62:12:58.00	HDF-N	ACIS-I	NONE	126.7
12:36:49.40	62:12:58.00	HDF-N	ACIS-I	NONE	166.7
12:36:49.40	62:12:58.00	HDF-N	ACIS-I	NONE	166.7
12:36:49.40	62:12:58.00	HDF-N	ACIS-I	NONE	166.7
12:36:49.40	62:12:58.00	HDF-N	ACIS-I	NONE	166.7

Proposal Number: 08900784

Title: The Duty Cycle of Supermassive Black Holes: X-raying Virgo

PI Name: Tommaso Treu

Nuclear accretion on to super-massive black holes (SMBHs) plays a key role in the evolution of their host galaxies, as inferred from the ubiquity of SMBHs and the correlations between BH mass, and host mass and velocity dispersion. A fundamental unadressed issue is the actual distribution of accretion rates; we propose snapshot observations of an unbiased sample of 84 early-type galaxies in the Virgo cluster. Together with joint Spitzer 24 um observations, and publicly available HST-ACS and UV data, this survey will probe low-level nuclear activity over four orders of magnitude in black hole mass, thereby delivering the first unbiased census of the duty cycle of local SMBHs.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
12:09:22.30	13:59:33.10	9	ACIS-S	NONE	5.4
12:10:23.20	10:11:17.60	21	ACIS-S	NONE	5.4
12:11:07.80	14:16:29.80	33	ACIS-S	NONE	5.4
12:15:12.60	14:25:59.10	140	ACIS-S	NONE	5.4
12:16:33.70	13:01:53.10	200	ACIS-S	NONE	5.4
12:17:19.60	11:56:36.20	230	ACIS-S	NONE	5.4
12:19:30.60	14:52:41.40	355	ACIS-S	NONE	5.4
12:19:45.40	12:47:54.30	369	ACIS-S	NONE	5.4
12:20:48.80	17:29:13.40	437	ACIS-S	NONE	5.4
12:22:14.80	7:10:00.80	538	ACIS-S	NONE	5.4
12:22:19.50	14:45:38.60	543	ACIS-S	NONE	5.4
12:22:41.10	7:57:01.10	571	ACIS-S	NONE	5.4
12:22:43.30	8:11:53.70	575	ACIS-S	NONE	5.4
12:23:35.30	16:43:22.30	654	ACIS-S	NONE	5.4
12:24:05.00	11:13:06.00	698	ACIS-S	NONE	5.4
12:24:48.30	18:11:42.00	751	ACIS-S	NONE	5.4
12:24:55.50	11:42:15.00	759	ACIS-S	NONE	5.4
12:25:12.30	14:45:43.80	778	ACIS-S	NONE	5.4
12:25:14.70	15:36:27.20	784	ACIS-S	NONE	5.4
12:25:41.70	12:48:38.00	828	ACIS-S	NONE	5.4
12:25:57.80	10:03:12.80	856	ACIS-S	NONE	5.4
12:26:50.50	9:35:02.00	944	ACIS-S	NONE	5.4
12:27:36.70	8:09:14.80	1025	ACIS-S	NONE	5.4
12:27:40.50	13:04:44.20	1030	ACIS-S	NONE	5.4
12:27:54.90	8:05:25.20	1049	ACIS-S	NONE	5.4
12:28:03.90	9:48:14.00	1062	ACIS-S	NONE	5.4
12:28:12.30	10:17:51.00	1075	ACIS-S	NONE	5.4
12:28:14.90	11:47:24.00	1087	ACIS-S	NONE	5.4
12:28:43.40	11:45:21.00	1125	ACIS-S	NONE	5.4
12:28:57.60	13:14:30.80	1146	ACIS-S	NONE	5.4
12:29:21.30	8:09:23.00	1178	ACIS-S	NONE	5.4
12:29:23.40	12:27:02.40	1185	ACIS-S	NONE	5.4
12:29:30.20	7:59:34.00	1192	ACIS-S	NONE	5.4
12:29:35.00	8:03:31.40	1199	ACIS-S	NONE	5.4
12:29:53.50	14:04:07.00	1242	ACIS-S	NONE	5.4
12:29:59.10	12:20:55.00	1250	ACIS-S	NONE	5.4
12:30:10.40	10:46:46.10	1261	ACIS-S	NONE	5.4
12:30:17.40	12:19:43.90	1279	ACIS-S	NONE	5.4
12:30:18.40	13:34:40.90	1283	ACIS-S	NONE	5.4
12:30:40.60	9:00:55.90	1303	ACIS-S	NONE	5.4
12:30:52.20	16:45:32.60	1321	ACIS-S	NONE	5.4
12:30:57.60	12:16:17.20	1327	ACIS-S	NONE	5.4
12:31:20.00	14:06:53.50	1355	ACIS-S	NONE	5.4
12:32:02.70	11:53:24.80	1407	ACIS-S	NONE	5.4
12:32:14.20	10:15:05.00	1422	ACIS-S	NONE	5.4
12:32:23.40	11:15:46.20	1431	ACIS-S	NONE	5.4
12:32:33.40	15:24:55.20	1440	ACIS-S	NONE	5.4
12:33:05.00	16:15:55.90	1475	ACIS-S	NONE	5.4
12:33:13.40	9:23:49.80	1488	ACIS-S	NONE	5.4
12:33:13.80	10:55:43.60	1489	ACIS-S	NONE	5.4
12:33:19.80	12:51:12.80	1499	ACIS-S	NONE	5.4
12:33:34.60	11:15:42.80	1512	ACIS-S	NONE	5.4
12:33:51.60	13:19:21.30	1528	ACIS-S	NONE	5.4
12:34:06.10	11:19:17.00	1537	ACIS-S	NONE	5.4
12:34:06.80	12:44:30.10	1539	ACIS-S	NONE	5.4
12:34:11.50	12:02:55.90	1545	ACIS-S	NONE	5.4
12:35:30.60	12:13:15.40	1619	ACIS-S	NONE	5.4
12:35:37.30	12:22:54.90	1627	ACIS-S	NONE	5.4
12:35:38.00	12:15:50.50	1630	ACIS-S	NONE	5.4
12:36:24.80	10:23:04.60	1661	ACIS-S	NONE	5.4
12:36:53.40	7:14:47.00	1692	ACIS-S	NONE	5.4
12:36:54.90	12:31:12.50	1695	ACIS-S	NONE	5.4
12:37:30.60	9:33:18.80	1720	ACIS-S	NONE	5.4
12:38:06.80	10:04:56.60	1743	ACIS-S	NONE	5.4
12:39:04.70	14:43:51.50	1779	ACIS-S	NONE	5.4
12:40:11.20	9:53:45.90	1826	ACIS-S	NONE	5.4
12:40:13.40	12:52:29.00	1828	ACIS-S	NONE	5.4
12:40:19.60	15:56:07.20	1833	ACIS-S	NONE	5.4
12:40:53.10	10:28:34.00	1857	ACIS-S	NONE	5.4
12:40:58.50	11:11:04.40	1861	ACIS-S	NONE	5.4
12:41:15.70	11:23:13.50	1871	ACIS-S	NONE	5.4
12:41:32.70	7:18:53.00	1883	ACIS-S	NONE	5.4
12:41:39.40	12:14:52.40	1886	ACIS-S	NONE	5.4
12:41:52.00	9:24:10.30	1895	ACIS-S	NONE	5.4
12:42:08.70	11:45:14.90	1910	ACIS-S	NONE	5.4
12:42:10.70	7:40:37.00	1913	ACIS-S	NONE	5.4
12:42:47.40	11:26:33.00	1938	ACIS-S	NONE	5.4
12:42:58.00	10:40:54.50	1948	ACIS-S	NONE	5.4
12:44:12.00	12:56:30.10	1993	ACIS-S	NONE	5.4
12:44:31.90	11:11:25.10	2000	ACIS-S	NONE	5.4
12:45:20.40	13:41:33.00	2019	ACIS-S	NONE	5.4
12:47:15.30	10:12:13.00	2048	ACIS-S	NONE	5.4
12:47:20.70	12:09:58.70	2050	ACIS-S	NONE	5.4
12:52:17.50	11:18:50.00	2092	ACIS-S	NONE	5.4

Proposal Number: 02900196

Title: THE CHANDRA DEEP SURVEY OF THE HUBBLE DEEP FIELD NORTH (HDF-N) AREA

PI Name: William Brandt

We propose to extend the Chandra X-ray survey of the HDF-N and its vicinity with a 475 ks exposure; this will give 1 Ms of total coverage on this field and will fulfill one of Chandra's central design goals. We should remain photon limited to 1 Ms and will probe the X-ray Universe more than four times deeper than any observation to date. We should resolve essentially all of the X-ray background from 0.5-8 keV and will study obscured and high-redshift active galaxies, advection dominated sources, starbursts, X-ray binaries, clusters and groups, and diffuse X-ray emission. The HDF-N field is an ideal one for multiwavelength follow-up studies due to the enormous database already in place. All data are to be placed in the public archive immediately and we will request no GO science funding.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
12:36:49.40	62:12:58.00	HDF-N	ACIS-I	NONE	62.4
12:36:49.40	62:12:58.00	HDF-N	ACIS-I	NONE	64.6
12:36:49.40	62:12:58.00	HDF-N	ACIS-I	NONE	69.2
12:36:49.40	62:12:58.00	HDF-N	ACIS-I	NONE	130.8
12:36:49.40	62:12:58.00	HDF-N	ACIS-I	NONE	168

Proposal Number: 05900218

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

PI Name: William Brandt

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.	Grating	Exp.Time
3:31:48.79	-27:57:08.10	Extended CDF-S #3	ACIS-I	NONE	80
3:31:48.79	-27:57:08.10	Extended CDF-S #3	ACIS-I	NONE	170
3:31:52.60	-27:41:44.92	Extended CDF-S #2	ACIS-I	NONE	80
3:31:52.60	-27:41:44.92	Extended CDF-S #2	ACIS-I	NONE	170
3:33:01.78	-27:57:09.61	Extended CDF-S #4	ACIS-I	NONE	70
3:33:01.78	-27:57:09.61	Extended CDF-S #4	ACIS-I	NONE	80
3:33:01.78	-27:57:09.61	Extended CDF-S #4	ACIS-I	NONE	100
3:33:06.10	-27:40:53.50	Extended CDF-S #1	ACIS-I	NONE	80
3:33:06.10	-27:40:53.50	Extended CDF-S #1	ACIS-I	NONE	170

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
14:25:15.44	32:26:18.41	SS60	ACIS-I	NONE	5
14:26:58.62	32:26:18.41	SS59	ACIS-I	NONE	5
14:28:41.80	32:26:18.41	SS58	ACIS-I	NONE	5
14:30:24.98	32:26:18.41	SS57	ACIS-I	NONE	5
14:32:08.16	32:26:18.41	SS56	ACIS-I	NONE	5

Proposal Number: 06900144

Title: Continuing X-Raying the Intergalactic Medium with Blazars in Outburst: Deeper in Redshift and Wider in Area.

PI Name: Fabrizio Nicastro

We propose to extend our highly succesful Chandra-AO4 and -AO5 TOO programs to the 6th 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 {\bf 340 ks} (2 orbits). We shall dramatically reduce the uncertainty on the cosmological baryon mass density $\Omega_b$ in the local Universe studying the ``warm'', low-redshift, phase of the intergalactic medium (WHIM), where most of the baryonic matter of the $z \ls 1$ Universe is believed to hide.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
0:00:00.00	0:00:00.00	moderate-z blazar in outburst	HRC-S	LETG	170
22:53:57.70	16:08:54.00	high-z blazar in outburst	HRC-S	LETG	112

Proposal Number: 08900745

Title: The Chandra Deep Proto-cluster Field: Black-Hole Growth and Feedback in Dense Environments

PI Name: DAVID ALEXANDER

Deep X-ray surveys have revolutionized our understanding of the growth of black holes (SMBH). But these surveys only sample low-density regions at high-z due to their limited solid angle. There is no comparably sensitive X-ray census of AGN in high-density regions at high-z. Such environments evolve into the most massive clusters at z=0, regions which exhibit remarkable trends in galaxy properties - which may reflect early interactions between SMBHs and their host galaxies. A survey of a proto-cluster at high-z would provide a unique view of the interplay of the growth of galaxies and their SMBHs. Here we propose a 400ks survey of the best-studied proto-cluster at high-z, to enable the first definitive study of the growth of SMBHs and their host galaxies in a dense, young, environment.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
22:17:35.90	0:15:58.90	SSA22 Protocluster	ACIS-I	NONE	68
22:17:35.90	0:15:58.90	SSA22 Protocluster	ACIS-I	NONE	110
22:17:35.90	0:15:58.90	SSA22 Protocluster	ACIS-I	NONE	110
22:17:35.90	0:15:58.90	SSA22 Protocluster	ACIS-I	NONE	112

Proposal Number: 07910613

Title: A Legacy Study of Stellar Life Cycles at the Galactic Center

PI Name: Michael Muno

We propose a set of 27 40 ks Chandra observations of the central 300x80 pc of the Galaxy, as part of a multiwavelength project to study stellar life cycles in the region. Our observations will increase the number of accreting compact objects detected there by a factor of 10, to 12,000. This sample will: (1) increase the known number of HMXBs with IR counterparts several-fold, providing stringent tests of population synthesis models, (2) provide spectral and timing data on a new class of faint X-ray transients, (3) identify the sites of recent star formation by detecting their X-ray luminous WR/O stars, (4) identify elusive young pulsars near the Galactic Center, and (5) constrain the physics of particle acceleration in the mysterious radio filaments.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
17:42:55.00	-29:31:11.30	Deep GCS 13	ACIS-I	NONE	40
17:43:23.70	-29:21:05.00	Deep GCS 10	ACIS-I	NONE	19
17:43:23.70	-29:21:05.00	Deep GCS 10	ACIS-I	NONE	21
17:43:41.50	-29:37:25.70	Deep GCS 12	ACIS-I	NONE	9.9
17:43:41.50	-29:37:25.70	Deep GCS 12	ACIS-I	NONE	14.7
17:43:41.50	-29:37:25.70	Deep GCS 12	ACIS-I	NONE	15.4
17:43:52.20	-29:10:58.10	Deep GCS 7	ACIS-I	NONE	40
17:44:20.70	-29:00:51.10	Deep GCS 4	ACIS-I	NONE	20
17:44:20.70	-29:00:51.10	Deep GCS 4	ACIS-I	NONE	20
17:44:38.60	-29:17:11.40	Deep GCS 6	ACIS-I	NONE	20
17:44:38.60	-29:17:11.40	Deep GCS 6	ACIS-I	NONE	20
17:44:49.10	-28:50:43.40	Deep GCS 1	ACIS-I	NONE	40
17:45:07.10	-29:07:03.70	Deep GCS 3	ACIS-I	NONE	40
17:45:17.40	-28:40:35.80	Deep GCS 26	ACIS-I	NONE	40
17:45:25.10	-29:23:23.60	Deep GCS 8	ACIS-I	NONE	40
17:45:45.60	-28:30:27.40	Deep GCS 24	ACIS-I	NONE	40
17:45:53.50	-29:13:15.20	Deep GCS 5	ACIS-I	NONE	40
17:46:31.80	-28:36:38.20	Deep GCS 23	ACIS-I	NONE	40
17:46:50.00	-28:52:57.40	Deep GCS 27	ACIS-I	NONE	40
17:47:18.10	-28:42:47.90	Deep GCS 25	ACIS-I	NONE	40

Proposal Number: 06910168

Title: Massive Star Life, Death, and Rebirth in the Perseus Arm

PI Name: Leisa Townsley

This joint Chandra/XMM mosaic of W4/W3/HB3 allows us to chronicle the X-ray output of the entire life cycle of high-mass stars, from their intrinsic and wind-collision emission, through their SN phase, and back to the embedded, protostellar X-rays heralding the next generation of massive star formation. In addition we see the feedback of these massive stars on the interstellar medium in the Perseus Arm: the stellar winds from a massive young cluster (IC 1805) have blown the W4 superbubble and chimney; perhaps an older superbubble is over 100 times brighter in X-rays due to supernovae in its interior (HB3), and the expansion of these bubbles is compressing the W3 molecular cloud and triggering a new generation of stars to form.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
2:25:40.60	62:05:52.40	W3 Main IRS5	ACIS-I	NONE	40
2:26:50.80	62:15:52.00	W3 North	ACIS-I	NONE	12
2:26:50.80	62:15:52.00	W3 North	ACIS-I	NONE	21
2:26:50.80	62:15:52.00	W3 North	ACIS-I	NONE	47
2:27:04.10	61:52:22.00	W3(OH)	ACIS-I	NONE	80

Proposal Number: 09910161

Title: The Great Nebula in Carina: Protoplanetary Disks to Starburst Galaxies

PI Name: Leisa Townsley

The Great Nebula in Carina is a superb site to study the violent massive star formation and feedback that typifies giant HII regions and starburst galaxies. We propose to map the Carina star-forming complex with a mosaic of 20 new 60-ks ACIS-I pointings as a testbed for understanding recent and ongoing star formation and to probe its regions of bright diffuse X-ray emission. We will provide a catalog of multiwavelength properties of ~12,000 X-ray-selected stars. We will explore superbubble confinement, shocks, cloud evaporation, mass-loading of winds, ISM enrichment, and HII region energetics. We will also examine Carina as a surrogate environment for our Solar System's formation, where protoplanetary disks are bathed in harsh winds and radiation from nearby massive stars.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
10:40:34.20	-59:49:30.70	Carina Superbubble Ptg 2	ACIS-I	NONE	60
10:41:31.80	-59:35:34.80	Carina Superbubble Ptg 1	ACIS-I	NONE	60
10:41:52.10	-60:01:43.70	Carina Superbubbl