Chandra Large, Very Large and X-ray Visionary Projects

CLUSTERS OF GALAXIES

Proposal Number	Subject Category	PI Name	Title
02800845	CLUSTERS OF GALAXIES	Stanford	A COMPLETE X-RAY CLUSTER SAMPLE AT Z > 0.8
03800272	CLUSTERS OF GALAXIES	Ebeling	MACS: THE X-RAY PROPERTIES OF THE MOST MASSIVE GALAXY CLUSTERS AT Z>0.3
04800280	CLUSTERS OF GALAXIES	Scharf	SURVEYING THE FORNAX CLUSTER OF GALAXIES
04800927	CLUSTERS OF GALAXIES	Hughes	CHANDRA OBSERVATIONS OF DLS SHEAR-SELECTED CLUSTERS
05800170	CLUSTERS OF GALAXIES	Fabian	A Megasecond Image of the Core of the Perseus Cluster
05800890	CLUSTERS OF GALAXIES	Markevitch	THE MOST INTERESTING CLUSTER IN THE UNIVERSE
06800101	CLUSTERS OF GALAXIES	Vikhlinin	DARK ENERGY WITH X-RAY CLUSTERS: CHANDRA OBSERVATIONS OF 41 HIGH-REDSHIFT CLUSTERS FROM THE 400 deg^2 ROSAT PSPC SURVEY
06800102	CLUSTERS OF GALAXIES	Vikhlinin	A CHANDRA TREASURY OBSERVATION OF THE BEST EXAMPLE OF A CLUSTER COLD FRONT
06800613	CLUSTERS OF GALAXIES	forman	The History of AGN Activity in M87 and the Interaction of Nuclear Outbursts with the Surrounding Atmosphere
07800432	CLUSTERS OF GALAXIES	BUOTE	The Cosmological Formation of Galaxy Groups
08800952	CLUSTERS OF GALAXIES	Mulchaey	A Complete Baryon Census in a Nearby Galaxy Group
09800310	CLUSTERS OF GALAXIES	Allen	Probing Dark Energy with Relaxed Galaxy Clusters
09800847	CLUSTERS OF GALAXIES	Markevitch	BOW SHOCK, ELECTRON-ION EQUILIBRIUM, BREAKUP OF COOL CORE, AND DARK SUBCLUSTER IN ABELL 520
10800641	CLUSTERS OF GALAXIES	McNamara	A Deep Image of the Most Powerful Cluster AGN Outburst
10800762	CLUSTERS OF GALAXIES	Stanford	The Role of AGN in Massive Galaxy Formation
10800779	CLUSTERS OF GALAXIES	Blanton	Shocks, Ripples, and Bubbles: A Very Deep Observation of Abell 2052
11800102	CLUSTERS OF GALAXIES	Fabian	Extending the Deep Image of the Perseus Cluster: The Outer Bubbles, Filaments and Ripples
11800471	CLUSTERS OF GALAXIES	Mohr	Chandra Observations of a Complete Sample of SZE Selected Galaxy Clusters
12800339	CLUSTERS OF GALAXIES	Russell	Revealing the ICM transport processes with the bow shock, upstream shock and turbulent wake in Abell 2146
12800433	CLUSTERS OF GALAXIES	Kraft	A Deep {\em Chandra} Study of NGC 4472 - Gas Dynamics in the Nearest Group-Cluster Merger
12800632	CLUSTERS OF GALAXIES	Hughes	Chandra Observations of the ACT Sample of SZE-Selected Galaxy Clusters
13800359	CLUSTERS OF GALAXIES	Sanders	Examining incredible structure in the core of the Coma cluster
13800509	CLUSTERS OF GALAXIES	Vikhlinin	CHANDRA EXPLORATION OF THE COSMIC MELTING POT IN THE VIRIALIZATION REGION OF A RICH GALAXY CLUSTER
13800581	CLUSTERS OF GALAXIES	forman	Abell 115: It Takes Two to Tango - The interaction of Relativistic and Thermal Plasma in a Merging Subcluster
13800764	CLUSTERS OF GALAXIES	Hughes	Chandra Observations of the Brightest Sunyaev-Zeldovich Effect Cluster
13800883	CLUSTERS OF GALAXIES	Benson	Cosmology and Cluster Evolution from the 80 Most Massive Clusters in 2000 deg^2 from the South Pole Telescope Survey
14800360	CLUSTERS OF GALAXIES	Tozzi	Extreme constraints on ICM physics and cosmology: a deep observation of XMMUJ0044, the most distant massive cluster
14800365	CLUSTERS OF GALAXIES	Jones	A Chandra-Planck Legacy Program for Massive Clusters of Galaxies
14800434	CLUSTERS OF GALAXIES	Randall	A Detailed Study of the Longest Known Ram Pressure Stripped Tail with Deep Chandra Observations of M86
14800815	CLUSTERS OF GALAXIES	Werner	Resolving the nearest cold front in the sky: the cleanest experimental tool to study detailed ICM physics

Subject Category: CLUSTERS OF GALAXIES

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
09:10:43.80	+54:22:04.00	RX J0910+5422	ACIS-I	NONE	190
13:17:21.40	+29:11:25.00	RX J1317.4+2911	ACIS-I	NONE	115
13:50:46.10	+60:07:09.00	RX J1350.0+6007	ACIS-I	NONE	60

Subject Category: CLUSTERS OF GALAXIES

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
04:17:33.70	-11:54:12.00	MACSJ0417.5-1154	ACIS-I	NONE	12
02:42:35.90	-21:32:15.00	MACSJ0242.5-2132	ACIS-I	NONE	12
19:31:50.10	-26:34:36.50	MACSJ1931.8-2634	ACIS-I	NONE	14
23:11:35.20	+03:38:24.50	MACSJ2311.5+0338	ACIS-I	NONE	14
00:47:20.90	-08:10:30.50	MACSJ0047.3-0810	ACIS-I	NONE	14
11:31:53.70	-19:55:43.50	MACSJ1131.8-1955	ACIS-I	NONE	15
09:49:53.80	+17:08:03.00	MACSJ0949.8+1708	ACIS-I	NONE	15
11:15:53.30	+01:29:47.00	MACSJ1115.8+0129	ACIS-I	NONE	16
22:45:05.20	+26:37:58.00	MACSJ2245.0+2637	ACIS-I	NONE	17
14:27:40.60	-25:21:06.00	MACSJ1427.6-2521	ACIS-I	NONE	17
22:11:44.60	-03:49:47.00	MACSJ2211.7-0349	ACIS-I	NONE	18
22:29:44.50	-27:55:38.50	MACSJ2229.7-2755	ACIS-I	NONE	17
01:52:35.50	-28:52:47.00	MACSJ0152.5-2852	ACIS-I	NONE	18
05:20:42.40	-13:28:55.00	MACSJ0520.7-1328	ACIS-I	NONE	20
01:59:49.90	-08:49:49.00	MACSJ0159.8-0849	ACIS-I	NONE	18
17:31:40.10	+22:52:39.00	MACSJ1731.6+2252	ACIS-I	NONE	21
13:19:59.60	+70:03:34.50	MACSJ1319.9+7003	ACIS-I	NONE	20
02:57:42.00	-22:09:01.50	MACSJ0257.6-2209	ACIS-I	NONE	20
04:04:38.50	+11:09:21.00	MACSJ0404.6+1109	ACIS-I	NONE	24
22:28:34.40	+20:36:47.00	MACSJ2228.5+2036	ACIS-I	NONE	21
17:20:15.50	+35:36:22.00	MACSJ1720.2+3536	ACIS-I	NONE	21
05:47:02.20	-39:04:25.00	MACSJ0547.0-3904	ACIS-I	NONE	22
03:08:55.40	+26:45:39.00	MACSJ0308.9+2645	ACIS-I	NONE	25
04:29:36.00	-02:53:01.50	MACSJ0429.6-0253	ACIS-I	NONE	24
00:35:26.80	-20:15:37.50	MACSJ0035.4-2015	ACIS-I	NONE	22
00:11:43.00	-15:23:12.00	MACSJ0011.7-1523	ACIS-I	NONE	22
20:49:55.90	-32:17:10.50	MACSJ2049.9-3217	ACIS-I	NONE	24
12:06:13.00	-08:47:43.00	MACSJ1206.2-0847	ACIS-I	NONE	24

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	-35:27:04.00	FORNAX CLUSTER	ACIS-I	NONE	50
03:38:58.30	-35:10:46.00	FORNAX CLUSTER	ACIS-I	NONE	50
03:39:53.30	-35:21:50.00	FORNAX CLUSTER	ACIS-I	NONE	50
03:36:40.50	-35:04:49.00	FORNAX CLUSTER	ACIS-I	NONE	50
03:37:35.10	-35:16:03.00	FORNAX CLUSTER	ACIS-I	NONE	50
03:39:24.60	-35:38:09.00	FORNAX CLUSTER	ACIS-I	NONE	50
03:35:45.90	-35:15:45.00	FORNAX CLUSTER	ACIS-I	NONE	50
03:36:40.50	-35:27:01.00	FORNAX CLUSTER	ACIS-I	NONE	50
03:37:35.30	-35:37:57.00	FORNAX CLUSTER	ACIS-I	NONE	50
03:38:30.00	-35:49:04.00	FORNAX CLUSTER	ACIS-I	NONE	50

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	-48:20:10.00	DLS J0522-4820	ACIS-I	NONE	20
10:49:41.00	-04:17:44.00	DLS J1049-0417	ACIS-I	NONE	20
10:54:08.00	-05:49:44.00	DLS J1054-0549	ACIS-I	NONE	20
10:55:12.00	-05:03:43.00	DLS J1055-0503	ACIS-I	NONE	20
14:02:12.00	-10:28:14.00	DLS J1402-1028	ACIS-I	NONE	20
09:16:00.00	+29:31:34.00	DLS J0916+2931	ACIS-I	NONE	20
14:02:03.00	-10:19:44.00	DLS J1402-1019	ACIS-I	NONE	20

Subject Category: CLUSTERS OF GALAXIES

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
03:19:48.20	+41:30:42.20	Abell 426	ACIS-S	NONE	200
03:19:48.20	+41:30:42.20	Abell 426	ACIS-S	NONE	200
03:19:48.20	+41:30:42.20	Abell 426	ACIS-S	NONE	200
03:19:48.20	+41:30:42.20	Abell 426	ACIS-S	NONE	200

Subject Category: CLUSTERS OF GALAXIES

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
06:58:19.70	-55:56:20.00	1E0657-56	ACIS-I	NONE	500

Subject Category: CLUSTERS OF GALAXIES

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
02:30:26.60	+18:36:22.00	cl0230+1836	ACIS-I	NONE	70
03:28:36.10	-21:40:04.00	cl0328-2140	ACIS-I	NONE	60
04:05:24.30	-41:00:15.00	cl0405-4100	ACIS-I	NONE	80
05:21:10.50	-25:30:36.00	cl0521-2530	ACIS-I	NONE	15
09:56:02.80	+41:07:08.00	cl0956+4107	ACIS-I	NONE	40
02:16:33.70	-17:47:27.00	cl0216-1747	ACIS-I	NONE	65
03:55:59.30	-37:41:46.00	cl0355-3741	ACIS-I	NONE	30
00:30:33.60	+26:18:16.00	cl0030+2618	ACIS-I	NONE	20
13:57:19.40	+62:32:42.00	cl1357+6232	ACIS-I	NONE	45
08:53:13.40	+57:59:44.00	cl0853+5759	ACIS-I	NONE	25
12:22:01.90	+27:09:19.00	cl1222+2709	ACIS-I	NONE	50
12:12:19.20	+27:33:13.00	cl1212+2733	ACIS-I	NONE	15
12:02:13.70	+57:51:53.00	cl1202+5751	ACIS-I	NONE	60
03:33:10.30	-24:56:40.00	cl0333-2456	ACIS-I	NONE	40

Subject Category: CLUSTERS OF GALAXIES

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
20:12:50.80	-56:50:53.90	Abell 3667	ACIS-I	NONE	450

Subject Category: CLUSTERS OF GALAXIES

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	500
12:30:49.50	+12:23:28.00	M87	ACIS-I	NONE	12

Subject Category: CLUSTERS OF GALAXIES

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
11:10:32.60	+28:42:59.00	RXC J1110.5+2842	ACIS-S	NONE	27
11:00:48.90	+10:33:35.00	RXC J1100.8+1033	ACIS-S	NONE	27
12:06:37.40	+28:11:01.00	RXC J1206.6+2811	ACIS-S	NONE	36
11:09:43.10	+21:45:43.00	RXC J1109.7+2145	ACIS-S	NONE	37
13:20:15.40	+33:08:30.00	RXC J1320.2+3308	ACIS-S	NONE	39
10:22:04.70	+38:30:43.00	RXC J1022.0+3830	ACIS-S	NONE	42
11:47:20.70	+55:44:36.00	RXC J1147.3+5544	ACIS-S	NONE	44
13:24:11.90	+13:58:45.00	RXC J1324.1+1358	ACIS-S	NONE	47
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

Subject Category: CLUSTERS OF GALAXIES

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
08:20:23.70	+21:05:00.50	NGC2563-P1	ACIS-I	NONE	50
08:21:32.10	+20:49:01.00	NGC2563-P2	ACIS-I	NONE	30
08:20:23.70	+20:49:01.60	NGC2563-P3	ACIS-I	NONE	30
08:20:23.70	+21:20:57.90	NGC2563-P5	ACIS-I	NONE	30
08:19:15.10	+21:04:59.40	NGC2563-P6	ACIS-I	NONE	30
08:19:15.30	+20:49:00.40	NGC2563-P7	ACIS-I	NONE	30
08:19:15.00	+21:20:56.80	NGC2563-P8	ACIS-I	NONE	30
08:22:40.20	+21:02:03.90	NGC2563-P9	ACIS-I	NONE	30
08:21:32.20	+21:04:60.00	NGC2563-P10	ACIS-I	NONE	30
08:18:50.80	+21:42:31.10	NGC2563-P11	ACIS-I	NONE	30
08:18:00.00	+20:49:42.20	NGC2563-P12	ACIS-I	NONE	30
08:19:17.70	+20:33:33.70	NGC2563-P13	ACIS-I	NONE	30
08:23:16.40	+21:23:09.90	NGC2563-P14	ACIS-I	NONE	30
08:21:32.30	+21:20:57.40	NGC2563-P4	ACIS-I	NONE	30

Subject Category: CLUSTERS OF GALAXIES

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
04:39:02.30	+05:20:43.60	RXJ0439-0520	ACIS-I	NONE	30
21:29:39.90	+00:05:20.00	RXJ2129+0005	ACIS-I	NONE	30
10:23:39.40	+04:11:14.30	Zwicky 3146	ACIS-I	NONE	40
23:08:22.10	-02:11:29.10	Abell 2537	ACIS-I	NONE	40
14:27:39.40	-25:21:02.00	MACS1427-25	ACIS-I	NONE	30
22:29:45.30	-27:55:36.90	MACS2229	ACIS-I	NONE	15
11:15:52.10	+01:29:52.90	MACS1115	ACIS-I	NONE	40
01:59:49.30	+08:49:59.20	MACS0159	ACIS-I	NONE	20
20:46:00.60	-34:30:17.00	MACS2046	ACIS-I	NONE	40
13:59:10.30	-19:29:24.40	MACS1359	ACIS-I	NONE	50
16:21:24.80	+38:10:09.00	MACS1621	ACIS-I	NONE	60
14:27:16.20	+44:07:31.00	MACS1427+44	ACIS-I	NONE	40
13:11:01.60	-03:10:40.00	MACS1311	ACIS-I	NONE	30

Subject Category: CLUSTERS OF GALAXIES

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
04:54:05.40	+02:53:35.00	A520_OFF1	ACIS-I	NONE	115
04:54:05.40	+02:53:35.00	A520_OFF3	ACIS-I	NONE	115
04:54:05.40	+02:53:35.00	A520_OFF4	ACIS-I	NONE	115
04:54:05.40	+02:53:35.00	A520_OFF2	ACIS-I	NONE	115

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 10800641

Title: A Deep Image of the Most Powerful Cluster AGN Outburst

PI Name: Brian McNamara

Powerful AGN outbursts in galaxy clusters can release upward of 1E61 erg into the intracluster medium. Events of this magnitude are able to quench cooling flows and drive large-scale outflows that redistribute and heat the gas on cluster-wide scales. The most potent example of this is seen in the z=0.22 cluster MS0735.6+7421, whose powerful shock and cavity system have injected an estimated 6E61 erg of energy into the ICM. We propose to obtain a 500 ksec ACIS image of the cluster to examine in detail the relationships between the shock, cavity, and radio systems, and to investigate the impact of powerful AGN outbursts on the structure of the cluster.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
07:41:44.00	+74:14:38.30	MS0735.6+7421	ACIS-S	NONE	500

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 10800762

Title: The Role of AGN in Massive Galaxy Formation

PI Name: Spencer Stanford

There is increasing evidence that high rates of star formation in massive galaxies was common in rich environments at z > 1. The leading candidate for quenching the star formation and transforming cluster galaxies into red sequence galaxies is AGN. Therefore we expect to see an increase in AGN incidence in dense environments at z > 1. We propose to systematically determine the incidence of AGN in galaxy clusters at 1 < z < 1.5 using moderately deep ACIS imaging of IR-selected clusters in the Bootes field. In conjunction with extensive data from Spitzer, HST, and Keck, we will test the AGN quenching paradigm for the origin of the stars in massive galaxies.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
14:29:14.30	+33:57:20.70	ISCS1051	ACIS-I	NONE	24
14:26:09.50	+34:03:41.10	ISCS1034	ACIS-I	NONE	12
14:32:29.20	+33:32:48.30	ISCS1017	ACIS-I	NONE	33
14:26:30.40	+33:39:33.20	ISCS1014	ACIS-I	NONE	35
14:29:18.50	+34:37:25.80	ISCS1030	ACIS-I	NONE	32
14:34:30.40	+34:27:12.30	ISCS1034	ACIS-I	NONE	35
14:32:38.40	+34:36:49.00	ISCS1029	ACIS-I	NONE	32
14:32:24.20	+32:50:03.70	ISCS1036+1088	ACIS-I	NONE	36
14:25:19.30	+34:28:38.20	ISCS0890	ACIS-I	NONE	36
14:34:46.30	+35:19:45.80	ISCS1025	ACIS-I	NONE	34

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 10800779

Title: Shocks, Ripples, and Bubbles: A Very Deep Observation of Abell 2052

PI Name: Elizabeth Blanton

The cooling flow cluster A2052 has, arguably, the morphology most similar to the Perseus cluster as seen with Chandra. Two clear bubbles to the N and S of the center of A2052 are filled with the radio lobes associated with 3C 317. Surface brightness discontinuities consistent with shocks with Mach numbers of 1.8 and 1.2 are seen near the cluster center. These may be isothermal shocks. We propose to observe Abell 2052 much more deeply to study these shock features, ripple features due to sound waves that may be found at larger radii, possible ghost bubbles, cooling gas in the bright shells around the radio source that may link the X-ray and H-alpha emission, and possible hot gas within the X-ray holes. We will directly compare the star formation and cooling rates in the cluster center.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
15:16:44.50	+07:01:16.60	Abell 2052	ACIS-S	NONE	500

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 11800102

Title: Extending the Deep Image of the Perseus Cluster: The Outer Bubbles, Filaments and Ripples

PI Name: Andrew Fabian

Our existing 900ks image of the core of the Perseus cluster has revealed a wealth of detail on the bubbles, shocks and ripples caused by the action of the central AGN on the surrounding ICM. Most of the advances are directly due to the high surface brightness of the Perseus cluster (higher than any other cluster) and to the high spatial resolution of Chandra. This resolution is degraded significantly 4 arcmin or more off-axis, meaning that the region studied at the highest resolution is quite small. Here we propose three further exposures totalling 700ks to extend the highest resolution region, covering areas to the N and S of the nucleus where the current data suggest the presence of further intriguing and important structures due to the AGN activity.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
03:19:44.20	+41:25:18.00	Perseus cluster, Abell 426	ACIS-I	NONE	300
03:19:39.50	+41:36:01.41	Perseus cluster, Abell 426	ACIS-I	NONE	200

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 11800471

Title: Chandra Observations of a Complete Sample of SZE Selected Galaxy Clusters

PI Name: Joseph Mohr

We propose to obtain X-ray observations of a complete sample of 16 SZE selected galaxy clusters from the South Pole Telescope (SPT) survey. The SZE selection produces an approximately mass limited sample (at all redshifts) over the existing 200 deg^2 SPT survey. The Chandra observations provide X-ray mass estimates and morphologies, allowing (1) an initial calibration of the SZE flux-mass relation and (2) early tests of cosmology and the evolution of structure. Our 346ks request leverages 625ks of GTO time in AO10/11; these X-ray data are crucial to developing an understanding of the new window on the universe that SPT has opened and in laying the foundation for future studies using the full SPT survey (~1400deg^2 by 2010).

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
23:31:50.20	-50:51:50.40	SPT-CL 2332-5052	ACIS-I	NONE	5.9
05:46:36.00	-53:45:21.60	SPT-CL 0547-5345	ACIS-I	NONE	23.9
00:00:59.30	-57:48:28.80	SPT-CL 0001-5749	ACIS-I	NONE	7.3
23:42:45.10	-54:11:20.40	SPT-CL 2343-5411	ACIS-I	NONE	64.1
23:59:40.60	-50:09:39.60	SPT-CL 0000-5010	ACIS-I	NONE	22.7
05:51:35.30	-57:09:21.60	SPT-CL 0552-5709	ACIS-I	NONE	16.5
23:43:00.70	-55:21:46.80	SPT-CL 2343-5522	ACIS-I	NONE	75
05:09:19.90	-53:42:07.20	SPT-CL 0509-5342	ACIS-I	NONE	5.9
23:55:49.70	-50:56:09.60	SPT-CL 2356-5056	ACIS-I	NONE	11.5
05:28:02.60	-52:59:52.80	SPT-CL 0528-5300	ACIS-I	NONE	38.5
05:33:35.50	-50:05:24.00	SPT-CL 0534-5005	ACIS-I	NONE	75

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 12800339

Title: Revealing the ICM transport processes with the bow shock, upstream shock and turbulent wake in Abell 2146

PI Name: Helen Russell

Shock fronts generated by galaxy cluster mergers provide a key tool for studying the cluster gas. However, unambiguous detections of shock fronts are rare and only two have previously been found, those in the Bullet cluster and Abell 520. Our recent Chandra observation of Abell 2146 has revealed that this cluster has two Mach 2 merger shock fronts and a gas structure remarkably similar to the Bullet cluster (eg. Markevitch et al. 2002). We propose a deep observation of Abell 2146 to test electron-ion equilibrium, which was found to be shorter than the Coulomb time in the Bullet cluster, and investigate the ICM transport processes by studying the complex substructures and shocks in the subcluster tail.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
15:56:14.70	+66:20:48.90	Abell 2146	ACIS-I	NONE	400

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 12800433

Title: A Deep {\em Chandra} Study of NGC 4472 - Gas Dynamics in the Nearest Group-Cluster Merger

PI Name: Ralph Kraft

We propose a deep, 300 ks, Chandra/ACIS-S observation of the nearby galaxy NGC 4472. NGC 4472 is the most optically luminous galaxy of the Virgo cluster, and is the dominant member of a group falling into M87. It is the nearest, brightest example of a group being ram-pressure stripped as it falls into a cluster, and this deep observation will elucidate microphysics of the stripping process unobservable in any other object. We will measure temperature and elemental abundance variations of 4% and 15% (90% confidence), respectively, on scales as small as 250pcx250pc. We will also make a deep study of the LMXB population, and probe the dynamics of the gas flow near the Bondi radius of the central SMBH.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
12:29:46.70	+08:00:02.00	NGC 4472	ACIS-S	NONE	300

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 12800632

Title: Chandra Observations of the ACT Sample of SZE-Selected Galaxy Clusters

PI Name: John Hughes

We propose to obtain Chandra observations of a complete sample of galaxy clusters detected by the Atacama Cosmology Telescope (ACT) using the Sunyaev-Zeldovich effect (SZE). The proposed ACIS-I observations of 14 massive, newly-discovered SZE clusters will provide a precision calibration of the SZE signal versus mass correlation out to redshifts of 1. This effort is part of an intensive multi-wavelength campaign to produce an unbiased, well-observed sample of massive galaxy clusters out to high redshifts for cosmological investigations. These proposed observations will allow us to link directly the X-ray and SZE properties of massive clusters, so that cosmologists can reliably utilize the new large cluster samples that are being accumulated from both Chandra and the new SZ experiments.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
01:02:53.00	-49:15:16.90	ACT J0102-4915	ACIS-I	NONE	60
04:38:21.00	-54:19:48.10	ACT J0438-5419	ACIS-I	NONE	20
02:45:28.50	-53:02:05.00	ACT J0245-5302	ACIS-I	NONE	20
06:16:37.30	-52:27:37.10	ACT J0616-5227	ACIS-I	NONE	39
02:35:50.70	-51:21:55.40	ACT J0235-5121	ACIS-I	NONE	20
02:32:50.30	-52:57:50.00	ACT J0232-5257	ACIS-I	NONE	20
05:59:46.00	-52:50:21.40	ACT J0559-5249	ACIS-I	NONE	115
03:04:19.10	-49:21:53.50	ACT J0304-4921	ACIS-I	NONE	23
02:37:04.70	-49:38:39.30	ACT J0237-4939	ACIS-I	NONE	42
06:41:37.80	-49:46:54.70	ACT J0641-4948	ACIS-I	NONE	20
02:15:15.10	-52:12:53.90	ACT J0215-5212	ACIS-I	NONE	21
02:17:10.70	-52:44:32.00	ACT J0217-5245	ACIS-I	NONE	20
03:46:58.60	-54:39:31.00	ACT J0346-5438	ACIS-I	NONE	37
07:07:08.00	-55:23:37.00	ACT J0707-5522	ACIS-I	NONE	20

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 13800359

Title: Examining incredible structure in the core of the Coma cluster

PI Name: Jeremy Sanders

We propose to make Chandra observations of the core of the Coma cluster that are an order of magnitude deeper than currently exist. With this substantial increase in detail we will study the quasi-linear structures that we have discovered from existing XMM data, which do not look like conventional hydrodynamical turbulence. The new observations will tell us much about the intracluster medium, including the degree of turbulence, the viscosity and the mixing of metals. We will look for shocks, sound waves and other features associated with the merger. We plan to also examine gas clumping and the coronae around the central galaxies. The Coma cluster is the best multiwavelength studied cluster and the 3rd X-ray brightest. This new observation will provide an excellent legacy resource.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
12:59:49.00	+27:57:48.00	Coma cluster	ACIS-I	NONE	125
12:59:49.00	+27:57:48.00	Coma cluster	ACIS-I	NONE	125
12:59:49.00	+27:57:48.00	Coma cluster	ACIS-I	NONE	125
12:59:49.00	+27:57:48.00	Coma cluster	ACIS-I	NONE	125

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 13800509

Title: CHANDRA EXPLORATION OF THE COSMIC MELTING POT IN THE VIRIALIZATION REGION OF A RICH GALAXY CLUSTER

PI Name: Alexey Vikhlinin

The virialization zone of rich galaxy clusters, R500

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
01:01:59.80	-21:32:20.70	A133-1	ACIS-I	NONE	250
01:01:13.90	-22:02:30.80	A133-3	ACIS-I	NONE	250
01:03:04.80	-21:37:39.50	A133-4	ACIS-I	NONE	250
01:02:19.00	-22:07:50.70	A133-5	ACIS-I	NONE	250
01:04:09.80	-21:42:56.70	A133-6	ACIS-I	NONE	250
01:03:24.20	-22:13:09.00	A133-8	ACIS-I	NONE	250
01:01:36.90	-21:47:25.90	A133-2	ACIS-I	NONE	250
01:03:47.00	-21:58:02.90	A133-7	ACIS-I	NONE	250

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 13800581

Title: Abell 115: It Takes Two to Tango - The interaction of Relativistic and Thermal Plasma in a Merging Subcluster

PI Name: william forman

We propose a 310 ks ACIS-I observation of the merging cluster A115 whose northern subcluster, A115-N, hosts 3C28 which shows two wispy "tails" pointing in the direction of subcluster motion! With 360 ks (310 ks new, plus 50 ks archival), we can study the hydrodynamics of the gas flow in and around A115-N to determine flow velocities that are traced by the radio plasma. We will measure and compare the circulation time of the gas to the aging time of the radio emitting electrons, understand the structure of the relativistic plasma (i.e., thin sheath or filled cavity) by measuring distortions in the X-ray surface brightness, investigate magnetic draping, and develop a 3D model for the merger using extensive optical spectroscopy with the velocity of A115-N measured from the X-ray analysis.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
00:55:56.50	+26:22:10.00	Abell 115	ACIS-I	NONE	310

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 13800764

Title: Chandra Observations of the Brightest Sunyaev-Zeldovich Effect Cluster

PI Name: John Hughes

We propose deep Chandra observations of ACT-CL J0102-4915, the brightest Sunyaev-Zeldovich effect cluster discovered by the Atacama Cosmology Telescope and South Pole Telescope surveys. These surveys covered approximately 3000 square degrees and are essentially complete to high redshift. Our recent Chandra and VLT optical data reveal ACL-CL J0102-4915 to be undergoing a major merger. It is likely a high redshift (z=0.870) counterpart to the famous ``bullet'' cluster. New Chandra data will determine the properties of the merger shock and the HST/ACS data will provide a weak lensing mass map.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
01:02:53.00	-49:15:16.90	ACT J0102-4915	ACIS-I	NONE	300

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 13800883

Title: Cosmology and Cluster Evolution from the 80 Most Massive Clusters in 2000 deg^2 from the South Pole Telescope Survey

PI Name: Bradford Benson

We propose Chandra X-ray observations to complete a mass-limited sample of 80 clusters of galaxies between 0.4 < z < 1.2, uniformly selected by the Sunyaev-Zeldovich effect from 2000 deg^2 surveyed by the South Pole Telescope. This sample increases the number of clusters at a similar mass threshold with X-ray observations by factors of 4 and 8 at z>0.6, 0.8, respectively, thereby providing a unique legacy sample for Chandra. These observations will significantly improve cluster-based dark energy constraints, are coordinated to overlap with several current and future cluster surveys, and will be uniquely valuable for the study of the formation and evolution of massive clusters.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
00:13:19.10	-49:06:50.40	SPT-CLJ0013-4906	ACIS-I	NONE	15.4
21:35:38.60	-57:26:27.20	SPT-CLJ2135-5726	ACIS-I	NONE	18.7
02:12:26.40	-46:57:00.70	SPT-CLJ0212-4656	ACIS-I	NONE	30.7
03:48:17.70	-45:14:59.30	SPT-CLJ0348-4514	ACIS-I	NONE	14.2
20:35:12.20	-52:51:05.40	SPT-CLJ2035-5251	ACIS-I	NONE	20.4
01:42:11.90	-50:32:36.20	SPT-CLJ0142-5032	ACIS-I	NONE	31.9
01:06:25.80	-59:43:17.00	SPT-CLJ0106-5943	ACIS-I	NONE	19.3
21:46:34.80	-46:32:57.80	SPT-CLJ2146-4632	ACIS-I	NONE	80.8
03:34:10.20	-46:59:22.90	SPT-CLJ0334-4659	ACIS-I	NONE	29
00:14:46.70	-49:52:37.60	SPT-CLJ0014-4952	ACIS-I	NONE	60.7
04:49:06.80	-49:01:17.00	SPT-CLJ0449-4901	ACIS-I	NONE	61.3
04:56:26.80	-51:16:25.00	SPT-CLJ0456-5116	ACIS-I	NONE	55.2
04:41:47.30	-48:54:45.00	SPT-CLJ0441-4854	ACIS-I	NONE	76.3
03:07:46.70	-50:42:22.30	SPT-CLJ0307-5042	ACIS-I	NONE	47.2
20:43:18.00	-50:35:26.50	SPT-CLJ2043-5035	ACIS-I	NONE	81.4
00:58:17.50	-61:45:36.40	SPT-CLJ0058-6145	ACIS-I	NONE	61
01:51:23.90	-59:54:07.60	SPT-CLJ0151-5954	ACIS-I	NONE	89
02:56:23.20	-56:17:46.30	SPT-CLJ0256-5617	ACIS-I	NONE	52
04:46:02.60	-58:49:17.40	SPT-CLJ0446-5849	ACIS-I	NONE	58.8
02:43:25.80	-59:30:43.60	SPT-CLJ0243-5930	ACIS-I	NONE	51.5
01:02:40.70	-46:03:53.60	SPT-CLJ0102-4603	ACIS-I	NONE	66.8
06:55:50.60	-52:34:02.60	SPT-CLJ0655-5234	ACIS-I	NONE	22.1
02:00:35.20	-48:52:37.60	SPT-CLJ0200-4852	ACIS-I	NONE	25.7
01:56:08.40	-55:41:37.30	SPT-CLJ0156-5541	ACIS-I	NONE	85.3
03:52:55.70	-56:47:53.20	SPT-CLJ0352-5647	ACIS-I	NONE	49.5
01:23:09.60	-48:21:19.40	SPT-CLJ0123-4821	ACIS-I	NONE	79.8
03:10:29.20	-46:46:52.30	SPT-CLJ0310-4646	ACIS-I	NONE	40.3
00:37:45.20	-50:47:37.70	SPT-CLJ0037-5047	ACIS-I	NONE	82.6
		SPT-CLJ0000-0000	ACIS-I	NONE	38.46
		SPT-CLJ0000-0000	ACIS-I	NONE	38.46
		SPT-CLJ0000-0000	ACIS-I	NONE	38.46
		SPT-CLJ0000-0000	ACIS-I	NONE	38.46
		SPT-CLJ0000-0000	ACIS-I	NONE	38.46
		SPT-CLJ0000-0000	ACIS-I	NONE	38.46
		SPT-CLJ0000-0000	ACIS-I	NONE	38.46
		SPT-CLJ0000-0000	ACIS-I	NONE	38.46
		SPT-CLJ0000-0000	ACIS-I	NONE	38.46
		SPT-CLJ0000-0000	ACIS-I	NONE	38.46
		SPT-CLJ0000-0000	ACIS-I	NONE	38.46
		SPT-CLJ0000-0000	ACIS-I	NONE	38.46
04:26:03.90	-54:55:16.30	SPT-CLJ0426-5455	ACIS-I	NONE	38.5
04:06:53.60	-48:04:52.30	SPT-CLJ0406-4804	ACIS-I	NONE	28.6
00:33:54.20	-63:26:37.70	SPT-CLJ0033-6326	ACIS-I	NONE	23.1
21:48:42.00	-61:16:42.60	SPT-CLJ2148-6116	ACIS-I	NONE	39.8
02:52:44.90	-48:24:45.40	SPT-CLJ0252-4824	ACIS-I	NONE	33.8
		SPT-CLJ0000-0000	ACIS-I	NONE	38.46

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 14800360

Title: Extreme constraints on ICM physics and cosmology: a deep observation of XMMUJ0044, the most distant massive cluster

PI Name: Paolo Tozzi

We propose a deep (380 ks) Chandra observation of the distant galaxy cluster XMMUJ0044 at z=1.58. With this observation we will push detailed studies of X-ray clusters to the edge of the current discovery limit, by measuring global temperature and Fe abundance, gas and total mass, putting strong constraints on the time formation of cool core, on the chemical enrichment time scale, on the relation between ICM and galaxy population, and deriving the best constraint to the standard Lambda-CDM model attainable at present. These results, achievable only with Chandra, are secured by a first X-ray characterization of XMMUJ0044 based on XMM data, and will constitute an unrivaled reference for distant cluster studies until the next generation of high-angular resolution X-ray satellites.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
00:44:05.20	-20:33:59.70	XMMUJ0044.0-2033	ACIS-S	NONE	380

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 14800365

Title: A Chandra-Planck Legacy Program for Massive Clusters of Galaxies

PI Name: Christine Jones

ESA's Planck Mission has provided a large, statistically representative sample of very massive clusters, detected over the full sky through their SZ effect. The Planck clusters are sufficiently X-ray bright that for all 165 z<0.35 clusters, Chandra will collect 10,000 source counts to characterize each cluster's dynamical state, including merger properties, measure cluster masses and mass proxies and define local cluster mass and temperature functions. Chandra observations will provide a benchmark at low redshifts for comparison to high redshift clusters and to cosmological N-body simulations. Our team is expert in the analysis of X-ray and SZ data and in theory, simulations, lensing, and radio studies of clusters. We plan to make our cluster analysis products available to the community.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
10:43:24.80	-20:37:18.00	G106.73-83.22	ACIS-I	NONE	12
21:35:19.90	+01:23:14.50	G055.97-34.88	ACIS-I	NONE	20
18:04:29.70	+18:04:29.70	G036.72+14.92	ACIS-I	NONE	10
05:16:37.50	-54:31:31.80	G262.25-35.36	ACIS-I	NONE	22
06:16:19.80	-21:57:35.00	G229.21-17.24	ACIS-I	NONE	24
22:18:41.30	-38:54:16.80	G002.74-56.18	ACIS-I	NONE	11
19:47:09.30	-76:23:52.00	G318.13-29.57	ACIS-I	NONE	20
21:27:03.50	-12:09:19.00	G039.85-39.98	ACIS-I	NONE	15
19:38:19.70	+54:09:26.30	G086.45+15.29	ACIS-I	NONE	15
10:22:27.30	+50:06:16.30	G163.72+53.53	ACIS-I	NONE	14
22:23:49.30	-01:37:13.20	G062.42-46.41	ACIS-I	NONE	9
20:23:24.30	-55:34:26.50	G342.31-34.90	ACIS-I	NONE	21
09:45:26.20	-08:40:06.00	G244.69+32.49	ACIS-I	NONE	16
02:25:56.00	-41:54:53.00	G256.45-65.71	ACIS-I	NONE	15
05:32:59.40	-37:01:39.60	G241.74-30.88	ACIS-I	NONE	25
03:03:53.10	-77:52:14.40	G294.66-37.02	ACIS-I	NONE	34
10:23:44.10	+49:08:17.00	G165.08+54.11	ACIS-I	NONE	10
22:17:46.10	-35:43:22.20	G008.44-56.35	ACIS-I	NONE	12
10:39:28.10	+05:10:06.00	G241.85+51.53	ACIS-I	NONE	14
17:47:18.00	+45:13:30.70	G071.61+29.79	ACIS-I	NONE	21
11:59:23.00	+49:47:39.00	G143.24+65.21	ACIS-I	NONE	22
19:34:54.00	-50:53:18.80	G347.18-27.35	ACIS-I	NONE	25
05:25:50.00	-47:14:38.30	G253.47-33.72	ACIS-I	NONE	18
13:15:06.60	+51:49:27.20	G114.33+64.87	ACIS-I	NONE	31
23:39:44.00	-85:10:33.00	G304.67-31.66	ACIS-I	NONE	23
06:16:29.50	-39:48:28.80	G247.17-23.32	ACIS-I	NONE	17
12:36:57.40	+63:11:08.00	G125.70+53.85	ACIS-I	NONE	29
09:20:24.80	+30:30:09.20	G195.62+44.05	ACIS-I	NONE	38
14:14:05.30	+71:17:36.50	G113.82+44.35	ACIS-I	NONE	19
18:19:55.30	+57:09:57.30	G085.99+26.71	ACIS-I	NONE	35
10:00:02.10	-30:15:55.80	G264.41+19.48	ACIS-I	NONE	31
20:51:50.20	-58:45:23.00	G345.40-39.34	ACIS-I	NONE	30
12:01:04.00	-39:52:11.00	G292.51+21.98	ACIS-I	NONE	45
19:14:36.90	-59:28:19.90	G337.09-25.97	ACIS-I	NONE	25
09:38:21.40	+52:02:38.40	G164.61+46.39	ACIS-I	NONE	42
12:59:37.60	+60:04:41.90	G121.11+57.01	ACIS-I	NONE	44
06:21:55.00	+74:41:38.40	G139.59+24.18	ACIS-I	NONE	18
11:11:37.10	+40:50:01.90	G172.88+65.32	ACIS-I	NONE	12
05:10:13.00	-45:19:29.00	G250.90-36.25	ACIS-I	NONE	16
05:31:34.70	-75:11:26.40	G286.58-31.25	ACIS-I	NONE	24
18:54:06.00	+68:22:15.00	G098.95+24.86	ACIS-I	NONE	17
06:37:19.50	-48:28:50.40	G257.34-22.18	ACIS-I	NONE	25
21:04:22.90	-41:21:46.00	G000.44-41.83	ACIS-I	NONE	14
11:42:37.40	+58:32:14.30	G139.19+56.35	ACIS-I	NONE	33
12:15:28.80	-39:01:47.00	G295.33+23.33	ACIS-I	NONE	15

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 14800434

Title: A Detailed Study of the Longest Known Ram Pressure Stripped Tail with Deep Chandra Observations of M86

PI Name: Scott Randall

We propose deep Chandra observations of the ram pressure stripped tail in M86, the longest ram pressure stripped tail known. M86 is nearby, in the Virgo cluster (~17 Mpc), and is X-ray bright. With Chandra's high spatial resolution we will image fine detail in the tail, and map the temperature and abundance structure along the tail. We will determine the origin of the stripped gas, place limits on gas mixing in the tail with the ICM, and ultimately place constrains on ICM microphysics through comparisons with detailed hydrodynamical simulations.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
12:25:45.90	+13:04:52.00	M86 Inner Tail	ACIS-I	NONE	150
12:25:02.30	+13:16:54.60	M86 Outer Tail	ACIS-I	NONE	200

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 14800815

Title: Resolving the nearest cold front in the sky: the cleanest experimental tool to study detailed ICM physics

PI Name: Norbert Werner

We propose a very deep legacy-class observation of the nearest, best resolved cold front in the sky which lies 90 kpc to the North of M87. Cold fronts are known to be remarkably sharp, with gas density and temperature discontinuities several times sharper than the Coulomb mean free path. The proposed observation will provide an extraordinary improvement in resolution (resolving ~80 pc scales), allowing to study the cold front interface in unprecedented detail. Cold fronts provide a relatively simple experimental setup - a unique tool to study ICM physics. The proposed observation will place crucial constraints on fundamental physical processes shaping cold fronts, such as: growth of instabilities in the ICM, intra-cluster magnetic fields, gas velocities, conduction and viscous stresses.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
12:29:56.30	+12:38:39.60	Virgo cold front	ACIS-I	NONE	500

The Chandra X-Ray Center (CXC) is operated for NASA by the Smithsonian Astrophysical Observatory. 60 Garden Street, Cambridge, MA 02138 USA. Email: cxcweb@head.cfa.harvard.edu Smithsonian Institution, Copyright © 1998-2012. All rights reserved.