Chandra X-Ray Observatory
	(CXC)

Accepted Cycle 11 Large / Very Large Proposals

Proposal NumberSubject CategoryPI NameTypeTime
(Ks)
Title
11200169STARS AND WDOskinovaLP300Cosmic archaeology with Chandra: from a supergiant shell to young stellar objects in NGC 602
11200420STARS AND WDGuedelLP360New Thrust for Jets: Understanding the Physics of Young Stellar Jets and Outflows
11200698STARS AND WDDrakeVLP1080The Chandra Cygnus OB2 Survey
11500272SN, SNR AND ISOLATED NSParkLP450A Detailed Study of the Aged O-Rich Supernova Remnant 0049-73.6
11500276SN, SNR AND ISOLATED NSParkLP640A Detailed Study of the Type Ia Supernova Remnant G299.2-2.9
11620601NORMAL GALAXIES: X-RAY POPULATIONSPrestwichLP192.127Ultra-Luminous x-Ray Sources in the Most Metal-Poor Galaxies
11620915NORMAL GALAXIES: X-RAY POPULATIONSGalloLP479.2Accretion onto nuclear black holes in early type galaxies: comparing field vs. clusters
11700501ACTIVE GALAXIES AND QUASARSKochanekLP584The Size of Quasar Non-Thermal/X-ray Emission Regions
11700510ACTIVE GALAXIES AND QUASARSCrostonLP400The environmental and epoch dependence of radio-loud AGN feedback
11700858ACTIVE GALAXIES AND QUASARSSiemiginowskaLP300Jet-ISM Interactions in a Restarting Radio Galaxy 4C 29.30
11800102CLUSTERS OF GALAXIESFabianLP500Extending the Deep Image of the Perseus Cluster: The Outer Bubbles, Filaments and Ripples
11800471CLUSTERS OF GALAXIESMohrLP342.1Chandra Observations of a Complete Sample of SZE Selected Galaxy Clusters
11900514EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYSGultekinLP360COMBH: Chandra Observations of M-sigma Black Holes

Subject Category: STARS AND WD

Proposal Number: 11200169

Title: Cosmic archaeology with Chandra: from a supergiant shell to young stellar objects in NGC 602

PI Name: Lidia Oskinova

The Wing of the SMC has low metalicity, and low content of gas and dust. It provides an ideal nearby laboratory to study star formation and feedback in an environment that resembles the early Universe. We propose a 300 ks Chandra observation of NGC602, a massive star cluster at the edge of a supergiant shell in the Wing. This cluster has a simple morphology and is located in a region of high transparency for X-rays. The Chandra data will help to answer the fundamental questions about the mechanisms that sculpture the largest structures in the ISM, and trigger the formation of stars. This observation will be complemented with data from other NASA Great Observatories HST and Spitzer, and will establish a template for studies of active star formation in external galaxies.

R.A. Dec. Target Name Det. Grating Exp.Time
01:29:38.60-73:34:25.10NGC 602ACIS-INONE300

Subject Category: STARS AND WD

Proposal Number: 11200420

Title: New Thrust for Jets: Understanding the Physics of Young Stellar Jets and Outflows

PI Name: Manuel Guedel

We propose a deep ACIS observation of the jet system of the classical T Tauri star DG Tau. DG Tau is so far unique because both its jet and counter-jet have been detected in X-rays. We will study jet structure, temperatures and proper motions of the sources and model the heating, propagation, and cooling physics of the hot plasma jets. The system orientation allows the counter-jet to be viewed through the circumstellar disk. X-ray absorption by the disk gas can thus be reliably determined and be used, together with optical information, to determine the gas-to-dust ratio in the disk. We will request radio (VLA) observations for complementary imaging, and near-IR (VLT) observing time for high-resolution spectroscopy to characterize the jet shocks and measure extinction along the jets.

R.A. Dec. Target Name Det. Grating Exp.Time
04:27:04.70+26:06:16.20DG TauACIS-SNONE360

Subject Category: STARS AND WD

Proposal Number: 11200698

Title: The Chandra Cygnus OB2 Survey

PI Name: Jeremy Drake

Understanding massive "starburst" clusters is crucial for the first stars, starburst galaxies, galactic and ISM evolution, and star and planet formation on universal and galactic scales. But Galactic superclusters are generally too distant for detailed study. Recent awareness that Cygnus OB2 (1.5kpc; ~2Myr old) has supercluster characteristics has sparked a multiwavelength legacy effort exploiting its proximity to study starburst astrophysics. This Chandra Legacy project will provide an exquisite vision of the anatomy of a massive "collapse" mode of star formation, allowing detailed archeology of its history and content. 8000-10000 detections down to 0.1Msun will incisively test theories of giant molecular cloud collapse, massive star formation and protoplanetary disk evolution.

R.A. Dec. Target Name Det. Grating Exp.Time
20:33:12.00+41:19:00.00Cygnus OB2ACIS-INONE1080

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 11500272

Title: A Detailed Study of the Aged O-Rich Supernova Remnant 0049-73.6

PI Name: Sangwook Park

O-rich supernova remnants (SNRs) provide an excellent opportunity for the study of core-collapse (CC) nucleosynthesis and the late-stage evolution of a massive star. While young O-rich SNRs (e.g., Cas A and G292.0+1.8) are being extensively studied, such studies are intrinsically limited because the early-stage of the blast wave and reverse shock may not reveal the full nature of metal-rich ejecta and the surroundings. Studies of relatively old O-rich SNRs are essential for a comprehensive understanding of CC SNRs, complementing those of young SNRs. The old O-rich SNR 0049-73.6 is a perfect example for such a study, revealing both high- and low-Z ejecta and well-evolved blast wave. Thus, we propose a deep 450 ks ACIS observation of 0049-73.6 for a detailed X-ray imaging spectroscopy.

R.A. Dec. Target Name Det. Grating Exp.Time
00:51:07.00-73:21:30.00SNR 0049-73.6ACIS-SNONE450

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 11500276

Title: A Detailed Study of the Type Ia Supernova Remnant G299.2-2.9

PI Name: Sangwook Park

Supernova remnant (SNR) G299.2-2.9 is a unique example of the Type Ia SNR which allows us a detailed 2-D spectral study for both of the metal-rich ejecta and ambient structures. Such studies of the ejecta and ambient medium are essential to reveal the detailed SNe Ia explosion mechanisms and their specific environments, which would critically impact their utility in cosmology. The proposed studies of both of the Type Ia SN ejecta and ambient structures cannot be performed with young historical Type Ia SNRs, and the mid-aged Type Ia SNR G299.2-2.9 provides a unique opportunity. Thus, we propose a 640 ks Chandra observation of G299.2-2.9. The proposed observation will serve a legacy which will be an essential basis for a high resolution spectroscopy of Type Ia SNRs with IXO and Astro-H.

R.A. Dec. Target Name Det. Grating Exp.Time
12:14:50.00-65:28:25.00G299.2-2.9ACIS-INONE640

Subject Category: NORMAL GALAXIES: X-RAY POPULATIONS

Proposal Number: 11620601

Title: Ultra-Luminous x-Ray Sources in the Most Metal-Poor Galaxies

PI Name: Andrea Prestwich

There is growing observational and theoretical evidence to suggest that Ultra-Luminous X-ray sources (ULX) form preferentially in low metallicity environments. Here we propose a survey of 27 nearby (< 30Mpc) star-forming Extremely Metal Poor Galaxies (Z<5% solar). There are almost no X-ray observations of such low abundance galaxies (3 in the Chandra archive). These are the most metal-deficient galaxies known, and a logical place to find ULX if they favor metal-poor systems. We plan to test recent population synthesis models which predict that ULX should be very numerous in metal-poor galaxies. We will also test the hypothesis that ULX form in massive young star clusters, and ask for HST time to obtain the necessay imaging data.

R.A. Dec. Target Name Det. Grating Exp.Time
01:13:39.40+00:52:27.80UGC 772ACIS-SNONE5
21:04:55.30-00:35:22.00SDSS J210455.31-003522.2ACIS-SNONE5
11:32:02.50+57:22:45.70SBS 1129+576ACIS-SNONE15.03
08:25:55.50+35:32:32.00HS 0822+3542ACIS-SNONE5
11:05:53.70+60:22:28.70SBS 1102+606ACIS-SNONE10.261
12:01:22.30+02:11:08.30SDSS J120122.32+021108.5ACIS-SNONE8.072
11:19:34.40+51:30:12.10[RC2] A1116+51ACIS-SNONE10.901
09:44:16.60+54:11:34.30SBS 0940+544ACIS-SNONE16.93
10:16:24.50+37:54:46.00KUG 1013+381ACIS-SNONE9.411
12:30:48.50+12:02:42.10[RC2] A1228+12ACIS-SNONE12.124
14:17:01.40+43:30:05.50SBS 1415+437ACIS-SNONE5
04:05:20.40-36:49:00.706dF J0405204-364859ACIS-SNONE5
14:14:54.20-02:08:22.90SDSS J141454.13-020822.9ACIS-SNONE16.75
22:30:36.80-00:06:37.00SDSS J223036.79-000636.9ACIS-SNONE7.657
12:38:40.10+32:46:00.50UGCA 292ACIS-SNONE5
14:44:12.80+42:37:44.00HS 1442+4250ACIS-SNONE5
02:04:25.60-10:09:35.00KUG 0201-103ACIS-SNONE13.596
08:12:39.50+48:36:45.40SDSS J081239.52+483645.3ACIS-SNONE5
08:59:46.90+39:23:05.60SDSS J085946.92+392305.6ACIS-SNONE5
07:47:32.10+51:11:28.20KUG 0743+513ACIS-SNONE5
09:40:12.80+29:35:30.30KUG 0937+298ACIS-SNONE5
09:46:22.80+54:52:08.30KUG 0942+551ACIS-SNONE16.395

Subject Category: NORMAL GALAXIES: X-RAY POPULATIONS

Proposal Number: 11620915

Title: Accretion onto nuclear black holes in early type galaxies: comparing field vs. clusters

PI Name: Elena Gallo

IF black holes are indeed ubiquitous in galactic nuclei, little is known about the frequency and intensity of their activity, the more so at the low-mass/low-luminosity end. Our cycle 8 observations of the Virgo clusters have delivered the most comprehensive measurement of the duty cycle, showing that although black holes are present even in low mass spheroids, activity is a strong function of mass. However, nuclear activity is also expected to be a strong function of environment, which regulates the gas supply through processes such as ram pressure stripping and merging. We propose the first systematic study of the effects of the environment on low level accretion, by combining our Virgo study with new observations and archival data of a volume limited sample of 100 field spheroids.

R.A. Dec. Target Name Det. Grating Exp.Time
14:21:03.60+03:16:15.71NGC5576ACIS-SNONE8.5
14:29:40.56+03:14:00.67NGC5638ACIS-SNONE10.2
15:04:06.96+01:13:11.68NGC5831ACIS-SNONE10.3
12:51:48.00-10:27:17.21NGC4742ACIS-SNONE5.3
13:30:42.96-22:25:15.92ESO576-076ACIS-SNONE8.8
12:51:06.72+10:54:43.49NGC4733ACIS-SNONE3.5
12:42:56.40+03:40:35.54PGC042748ACIS-SNONE3.5
13:21:19.44-13:02:31.56NGC5099ACIS-SNONE5.7
12:37:48.24-01:20:41.35PGC042173ACIS-SNONE8.2
15:03:50.40+01:07:36.62PGC1185375ACIS-SNONE9.2
12:42:50.88+12:18:31.50PGC042737ACIS-SNONE11
12:43:51.12+11:28:01.31PGC042846ACIS-SNONE3.5
15:00:33.12+02:13:49.30SDSSJ150033.02+021349.1ACIS-SNONE6.3
14:58:28.56+01:32:34.91SDSSJ145828.64+013234.6ACIS-SNONE8.4
12:45:15.36+07:36:56.45PGC042982ACIS-SNONE6.4
15:01:00.96+01:00:49.68SDSSJ150100.85+010049.8ACIS-SNONE11.4
12:54:05.28-00:06:04.54PGC135814ACIS-SNONE4.5
15:02:33.12+01:56:08.95SDSSJ150233.03+015608.3ACIS-SNONE10.1
15:04:24.00+00:55:06.20PGC1179083ACIS-SNONE10.2
12:42:45.36+03:25:50.12PGC042724ACIS-SNONE1.7
15:01:16.08+01:46:24.49PGC1205406ACIS-SNONE8.5
13:31:33.84+02:11:17.16PGC135829ACIS-SNONE6.7
13:03:44.16+02:02:23.86PGC135818ACIS-SNONE3.5
12:41:45.12+04:00:23.62PGC042596ACIS-SNONE2.5
14:59:44.88+02:07:51.82SDSSJ145944.77+020752.1ACIS-SNONE8
14:58:41.04+02:20:23.50PGC1223766ACIS-SNONE9.5
12:50:07.44+02:14:52.87PGC043421ACIS-SNONE4.2
15:02:28.32+01:21:51.19PGC1192611ACIS-SNONE8.6
12:40:25.92+04:03:01.01PGC042454ACIS-SNONE2.4
22:32:13.44-41:10:09.52PGC085239ACIS-SNONE6.8
20:27:34.08-55:05:23.82PGC064718ACIS-SNONE2
02:08:21.12+10:59:47.04NGC0821ACIS-SNONE10.4
23:12:07.44-28:32:26.20NGC7507ACIS-SNONE7.3
03:28:19.63-31:04:05.09NGC1340ACIS-SNONE3.2
03:44:49.99-21:55:15.60NGC1439ACIS-SNONE7.5
03:42:49.10-22:06:30.10NGC1426ACIS-SNONE5.4
03:01:36.05-14:50:11.80NGC1172ACIS-SNONE6.5
01:47:55.30-26:53:31.88IC1729ACIS-SNONE6
03:35:14.62-20:22:25.28NGC1370ACIS-SNONE2.6
02:26:28.30+01:09:37.73IC0225ACIS-SNONE7.4
00:41:11.76-21:07:53.11ESO540-014ACIS-SNONE7.9
23:37:39.60+30:07:45.88PGC071938ACIS-SNONE7.8
00:23:04.20-27:55:37.31PGC132768ACIS-SNONE6.5
02:41:25.51-08:07:36.88PGC3097911ACIS-SNONE5.7
23:11:46.80-28:31:45.12PGC740586ACIS-SNONE5.7
20:49:40.08-32:41:53.026dFJ2049400-324154ACIS-SNONE9
02:43:10.61-00:15:45.72PGC135659ACIS-SNONE2.7
12:20:17.76+75:22:15.38NGC4291ACIS-SNONE13.7
10:18:24.96+21:53:38.29NGC3193ACIS-SNONE7.2
14:20:43.20+39:41:36.89NGC5582ACIS-SNONE9.5
12:41:44.40+74:25:15.10NGC4648ACIS-SNONE11
15:57:15.60+05:59:54.10NGC6017ACIS-SNONE12.3
10:54:48.72+17:37:13.40NGC3457ACIS-SNONE5.2
11:51:47.76+48:40:59.20NGC3457ACIS-SNONE4.5
12:07:56.64+65:06:50.40NGC4121ACIS-SNONE9.5
12:35:32.64+73:40:29.39UGC07767ACIS-SNONE8.9
10:31:06.72+28:47:47.65NGC3265ACIS-SNONE8.3
09:43:31.20+31:58:36.84NGC2970ACIS-SNONE10.6
10:52:04.32+71:46:22.91UGC05955ACIS-SNONE7.8
11:06:40.56+20:05:08.38NGC3522ACIS-SNONE5.9
12:41:60.00+32:34:25.00NGC4627ACIS-SNONE2
16:02:47.52+19:47:14.75PGC056821ACIS-SNONE11.4
15:06:34.32+01:33:31.79PGC3119319ACIS-SNONE8.7
14:58:46.08+02:58:08.36PGC1242097ACIS-SNONE11.9
09:50:10.80+28:00:47.59PGC028305ACIS-SNONE8.2
15:09:14.88+01:55:17.08PGC1210284ACIS-SNONE11.3
10:19:01.44+21:17:01.57PGC030133ACIS-SNONE4.6
15:05:50.64+01:54:30.10PGC1209872ACIS-SNONE11.2
15:11:01.44+01:40:50.20PGC1202458ACIS-SNONE11
15:04:24.72+02:06:52.67PGC1216386ACIS-SNONE11.5
15:03:44.16+02:33:08.68PGC1230503ACIS-SNONE11.7
15:09:07.92+00:43:29.17SDSSJ150907.83+004329.7ACIS-SNONE10.4
15:08:12.48+01:29:59.24rACIS-SNONE9.9
15:08:22.80+01:47:54.31PGC1206166ACIS-SNONE10.5
15:08:01.44+02:09:03.67PGC1217593ACIS-SNONE4.5

Subject Category: ACTIVE GALAXIES AND QUASARS

Proposal Number: 11700501

Title: The Size of Quasar Non-Thermal/X-ray Emission Regions

PI Name: Christopher Kochanek

We will use microlensing, where the stars in a lens galaxy magnify the accretion disk of a gravitationally lensed quasar, to measure the sizes of the X-ray emission regions of 7 gravitationally lensed quasars with well-sampled optical light curves and accretion disk size measurements. We will use these to determine the scaling of the non-thermal emission regions with black hole mass. For two ``active'' systems, RXJ1131-1231 and Q2237+0305, we will use longer observations in order to measure the X-ray energy dependence of the size. We have HST time to monitor the 6 with UV flux to probe thermal emission from near the inner edge of the disk. These observations can only be done with Chandra because future X-ray observatories will lack the necessary angular resolution.

R.A. Dec. Target Name Det. Grating Exp.Time
22:40:30.30+03:21:28.80Q2237+0305ACIS-SNONE180
11:31:51.60-12:31:57.00RXJ1131-1231ACIS-SNONE162
10:04:34.20+41:12:44.00SDSS1004+4112ACIS-SNONE24
04:38:14.90-12:17:14.40HE0435-1223ACIS-SNONE39
11:06:33.50-18:21:24.20HE1104-1805ACIS-SNONE39
01:58:41.40-43:25:04.20QJ0158-4325ACIS-SNONE30
09:24:55.90+02:19:24.90SDSS0924+0219ACIS-SNONE110

Subject Category: ACTIVE GALAXIES AND QUASARS

Proposal Number: 11700510

Title: The environmental and epoch dependence of radio-loud AGN feedback

PI Name: Judith Croston

Feedback from radio-loud AGN outbursts is now thought to be an important ingredient in galaxy formation models, potentially solving the `cooling flow' problem in cluster centres and helping to resolve long-standing problems in reconciling CDM models with observed properties of groups and clusters. Now that the role of radio-loud AGN feedback is established, the next step is to understand the relationship between radio-loud AGN energy input, environment and epoch, which appears complex and is currently poorly understood. This Chandra Large Project aims to address this question by characterizing the environments of a unique sample of radio galaxies spanning three orders of magnitude in radio luminosity at a single, cosmologically interesting redshift.

R.A. Dec. Target Name Det. Grating Exp.Time
13:01:25.00+36:58:09.40TOOT 1301+3658ACIS-SNONE40
12:55:55.80+35:56:35.80TOOT 1255+3556ACIS-SNONE40
16:26:48.50+45:23:42.60TOOT 1626+4523ACIS-SNONE40
16:30:32.80+45:34:26.00TOOT 1630+4534ACIS-SNONE40
13:07:27.10+36:39:16.40TOOT 1307+3639ACIS-SNONE40
17:31:43.80+66:38:56.707C 1731+6638ACIS-SNONE40
13:03:10.30+33:34:07.00TOOT 1303+3334ACIS-SNONE40
02:19:37.80+34:23:11.207C 0219+3423ACIS-SNONE40
08:50:24.80+37:47:09.106C 0850+3747ACIS-SNONE40
11:32:45.70+34:39:36.206C 1132+3439ACIS-SNONE40

Subject Category: ACTIVE GALAXIES AND QUASARS

Proposal Number: 11700858

Title: Jet-ISM Interactions in a Restarting Radio Galaxy 4C 29.30

PI Name: Aneta Siemiginowska

We propose to study interactions between radio plasma and ISM with a deep 300ksec Chandra ACIS-S observation of a low redshift radio galaxy, 4C 29.30 where the complexity of such interactions is uniquely displayed allowing a direct mapping of the initial stage of the radio source growth. The high resolution Chandra image will match the resolution of optical and radio structures observed in this source. The X-ray morphology will provide the critical information needed for studying physical conditions and understanding the impact of the evolving radio source onto the host galaxy environment. Our target presents a great laboratory to study the physical mechanisms of AGN feedback, and so provide strong constraints on models of galaxy evolution.

R.A. Dec. Target Name Det. Grating Exp.Time
08:40:02.40+29:49:02.604c+29.30ACIS-SNONE300

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+41:25:18.00Perseus cluster, Abell 426ACIS-INONE300
03:19:39.50+41:36:01.41Perseus cluster, Abell 426ACIS-INONE200

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
23:31:50.20-50:51:50.40SPT-CL 2332-5052ACIS-INONE5.9
05:46:36.00-53:45:21.60SPT-CL 0547-5345ACIS-INONE23.9
00:00:59.30-57:48:28.80SPT-CL 0001-5749ACIS-INONE7.3
23:42:45.10-54:11:20.40SPT-CL 2343-5411ACIS-INONE64.1
23:59:40.60-50:09:39.60SPT-CL 0000-5010ACIS-INONE22.7
05:51:35.30-57:09:21.60SPT-CL 0552-5709ACIS-INONE16.5
23:43:00.70-55:21:46.80SPT-CL 2343-5522ACIS-INONE75
05:09:19.90-53:42:07.20SPT-CL 0509-5342ACIS-INONE5.9
23:55:49.70-50:56:09.60SPT-CL 2356-5056ACIS-INONE11.5
05:28:02.60-52:59:52.80SPT-CL 0528-5300ACIS-INONE38.5
05:33:35.50-50:05:24.00SPT-CL 0534-5005ACIS-INONE75

Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS

Proposal Number: 11900514

Title: COMBH: Chandra Observations of M-sigma Black Holes

PI Name: Kayhan Gultekin

Galaxies with dynamically-measured central BH masses allow us to understand BH accretion, jets, and interactions between BHs and host galaxies with a clarity not possible in random surveys. By measuring true Eddington fractions, we can calculate the energy in radiation vs mechanical jet energy and the efficacy of BHs in heating nuclear regions and affecting star formation. Remarkably, 1/3 of SMBHs making up the M-sigma relation have been poorly observed or totally unobserved with Chandra. We propose a survey of 15 M-sigma galaxies to complete the sample of reliable M-sigma SMBHs. For each galaxy we propose to obtain 30-60 ks exposures and an hour-long VLA observation. This survey will test and extend the fundamental plane of BH activity and facilitate studies of the origin of M-sigma.

R.A. Dec. Target Name Det. Grating Exp.Time
03:19:41.10-19:24:40.90NGC1300ACIS-SNONE30
09:13:43.00+76:28:31.20NGC 2748ACIS-SNONE30
09:12:24.40+35:01:39.10NGC2778ACIS-SNONE30
12:20:17.80+75:22:15.20NGC4291ACIS-SNONE30
12:51:48.00-10:27:17.00NGC4742ACIS-SNONE30
13:19:31.70-12:39:25.10NGC5077ACIS-SNONE30
14:21:03.70+03:16:15.60NGC5576ACIS-SNONE30
10:48:16.90+12:37:45.40NGC3384ACIS-SNONE30
12:30:57.70+12:16:13.30NGC4486AACIS-SNONE30
12:28:60.00+13:58:42.80NGC4459ACIS-SNONE30
12:39:55.90+10:10:33.90NGC4596ACIS-SNONE30
23:00:59.90+30:08:41.60NGC7457ACIS-SNONE30
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The Chandra X-Ray Center (CXC) is operated for NASA by the Smithsonian Astrophysical Observatory. 60 Garden Street, Cambridge, MA 02138 USA.   Email:   cxchelp@head.cfa.harvard.edu Smithsonian Institution, Copyright © 1998-2017. All rights reserved.