Chandra X-Ray Observatory
	(CXC)

Accepted Cycle 13 Large / X-Ray Visionary Project Proposals

Proposal NumberSubject CategoryPI NameTypeTime (Ms)Title
13200221STARS AND WDMicelaLP300Simultaneous Chandra - CoRoT - Spitzer Observation of the Star Forming Region NGC 2264
13200314STARS AND WDLeuteneggerLP300A systematic measurement of the mass-loss rate of Zeta Ori
13200852STARS AND WDAguerosLP450Deep Imaging of M37, A Better Hyades
13500124SN, SNR AND ISOLATED NSWinklerLP690SN1006: SHOCK PHYSICS, COSMIC-RAY ACCELERATION, AND SN IA EXPLOSIONS
13500316SN, SNR AND ISOLATED NSSlaneLP350Bowing to Pressure During the Reformation: A Study of the Composite SNR G327.1-1.1
13610752NORMAL GALAXIES: DIFFUSE EMISSIONKuntzLP750M51: Using the Kinematics of a Grand-Design Spiral to Understand the Physics of the Hot ISM, SNRs, and XRBs
13610808NORMAL GALAXIES: DIFFUSE EMISSIONIrwinXVP1000A Chandra Legacy Project to Resolve the Accretion Flow of Gas Captured by a Supermassive Black Hole
13620807NORMAL GALAXIES: X-RAY POPULATIONSBaganoffXVP3000Chandra HETG Ultra-deep Gratings Spectroscopy of Sgr A* (CHUGSS)
13700587ACTIVE GALAXIES AND QUASARSVeilleuxLP400Quasar Feedback in Action: The Wide-Angle Wind of Mrk 231
13700784ACTIVE GALAXIES AND QUASARSEvansLP350A DIRECT TEST OF AGN FEEDBACK IN LATE-TYPE GALAXIES: SPATIALLY RESOLVED HETG SPECTROSCOPY OF NGC 3393
13800359CLUSTERS OF GALAXIESSandersLP500Examining incredible structure in the core of the Coma cluster
13800509CLUSTERS OF GALAXIESVikhlininXVP2000CHANDRA EXPLORATION OF THE COSMIC MELTING POT IN THE VIRIALIZATION REGION OF A RICH GALAXY CLUSTER
13800581CLUSTERS OF GALAXIESFormanLP310Abell 115: It Takes Two to Tango - The interaction of Relativistic and Thermal Plasma in a Merging Subcluster
13800764CLUSTERS OF GALAXIESHughesLP300Chandra Observations of the Brightest Sunyaev-Zeldovich Effect Cluster
13800883CLUSTERS OF GALAXIESBensonXVP2070.68Cosmology and Cluster Evolution from the 80 Most Massive Clusters in 2000 deg^2 from the South Pole Telescope Survey

Subject Category: STARS AND WD

Proposal Number: 13200221

Title: Simultaneous Chandra - CoRoT - Spitzer Observation of the Star Forming Region NGC 2264

Type: LP Total Time: 300

PI Name: Giuseppina Micela

We propose a 300 ks observation of the star forming region NGC2264, to be performed in December 2011, during a 30 day Spitzer and CoRoT joint observation of the region. The program, also involving a series of ground observations, will be a unique experiment: using three space telescopes we will, for the first time, monitor hundreds of young stellar objects simultaneously over a broad wavelength range. We will thus obtain crucial insights on the physics of flares, the morphology of coronal emitting structures, and the physical processes responsible for the extreme variability of Classical T Tauri Stars at all wavelengths.

R.A. Dec. Target Name Det. Grating Exp.Time
06:40:58.70+09:34:14.00NGC 2264ACIS-INONE300

Subject Category: STARS AND WD

Proposal Number: 13200314

Title: A systematic measurement of the mass-loss rate of Zeta Ori

Type: LP Total Time: 300

PI Name: Maurice Leutenegger

We propose a 300 ks HETGS observation of the O supergiant Zeta Orionis. In combination with 74 ks archival data, we will make very high signal-to-noise measurements of emission line profile shapes, which sensitively measure the wind optical depth as a function of wavelength. We will use the wavelength dependence of wind optical depth from all usable lines to make a precise measurement of the mass-loss rate. The wavelength dependence of wind optical depth will also test the importance of porosity. We will use XCMFGEN, our powerful new radiative transfer code, to construct global models which will be fit to X-ray, UV, and optical data, providing the strongest possible constraints on stellar and wind properties.

R.A. Dec. Target Name Det. Grating Exp.Time
05:40:45.50-01:56:33.20Zeta OrionisACIS-SHETG300

Subject Category: STARS AND WD

Proposal Number: 13200852

Title: Deep Imaging of M37, A Better Hyades

Type: LP Total Time: 450

PI Name: Marcel Agueros

Recent studies suggest that the picture of stellar LX decaying from 10 Myr to 5 Gyr as a single power-law is overly simplistic. M37, a Hyades analog, has been carefully surveyed in the optical, and we propose complementary deep (450 ksec) ACIS-I imaging of this open cluster. M37's rich membership, good match to Chandra's FOV, and large number of measured periods (~700) make it ideal for examining the evolution of coronal X-ray emission. Together, our X-ray and optical data will provide independent determinations of LX and v_rot; map out M37's X-ray luminosity function, with stacking of optically similar sources extending our flux limits by ~10x; test whether magnetic effects produce anomalous optical colors/luminosities for high LX sources; and characterize M37's interacting binaries.

R.A. Dec. Target Name Det. Grating Exp.Time
05:52:18.80+32:33:34.10M37ACIS-INONE450

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 13500124

Title: SN1006: SHOCK PHYSICS, COSMIC-RAY ACCELERATION, AND SN IA EXPLOSIONS

Type: LP Total Time: 690

PI Name: P. Winkler

Remnant of the brightest SN in recorded history, SN1006 is the object where the connection between SNR shocks and cosmic rays was first confirmed observationally. It is the closest and least absorbed of all the historical SNRs--yet it has been the least observed by Chandra. We propose deep ACIS observations to: 1) measure proper motions (through comparison with earlier data) to give the shock velocity around most of the shell; 2) elucidate the physics of nonthermal shocks and diffusive acceleration in unprecedented detail; and 3) study small-scale ejecta knots within SN1006 to obtain abundances and constrain the explosion properties. The new data will complete deep coverage for the entire SN1006 remnant, so deep studies of all the historical SNIa remnants will at last be in the archive.

R.A. Dec. Target Name Det. Grating Exp.Time
15:02:20.30-41:46:38.00SN1006 NWACIS-SNONE90
15:01:37.00-41:59:00.00SN1006 WACIS-INONE100
15:02:08.50-42:07:00.00SN1006 SWACIS-INONE100
15:03:05.00-42:08:60.00SN1006 SACIS-INONE100
15:02:52.20-41:56:16.00SN1006 CTRACIS-INONE100
15:03:14.80-41:42:45.00SN1006 NACIS-INONE100
15:03:51.00-42:03:30.00SN1006 SEACIS-INONE100

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 13500316

Title: Bowing to Pressure During the Reformation: A Study of the Composite SNR G327.1-1.1

Type: LP Total Time: 350

PI Name: Patrick Slane

G327.1-1.1 is a composite supernova remnant whose pulsar wind nebula is defined by an offset radio nebula and a cometary X-ray nebula surrounding a neutron star that appears to be moving rapidly through the remnant. Complex structures indicate that the PWN has been disrupted by the reverse shock of the SNR, and that the nebula is re-forming while being swept back into a bowshock-like morphology by the pressure associated with its rapid motion. The manner in which a PWN evolves through such a stage determines the ultimate spectrum of its relativistic particles, and the process by which they eventually escape into the ISM. We propose a deep Chandra observation of G327.1-1.1 in order to study its complex spectral and spatial structure during this crucial phase of evolution.

R.A. Dec. Target Name Det. Grating Exp.Time
15:54:37.60-55:05:49.70G327.1-1.1ACIS-INONE350

Subject Category: NORMAL GALAXIES: DIFFUSE EMISSION

Proposal Number: 13610752

Title: M51: Using the Kinematics of a Grand-Design Spiral to Understand the Physics of the Hot ISM, SNRs, and XRBs

Type: LP Total Time: 750

PI Name: K.D. Kuntz

M51 is an iconic grand design spiral galaxy with a strong arm/inter-arm density contrast and a high star-formation rate, but with very little star-formation between its arms. As a result, one can age-date the hot gas and high-mass binaries produced in the arms that have moved into the inter-arm regions. We propose a 750 ks observation with ACIS-S3 to employ this technique to measure gas cooling times, search for non-radiative cooling, and constrain time scales for HMXB evolution. We also propose 10 orbits of HST WFC3 observations in [SII], which with existing HST data, will allow the first comprehensive survey of the rich population of SNR expected in M51. Given the strong density contrast, we will better characterize SNR properties as a function of environment.

R.A. Dec. Target Name Det. Grating Exp.Time
13:30:00.00+47:12:00.00M51ACIS-SNONE750

Subject Category: NORMAL GALAXIES: DIFFUSE EMISSION

Proposal Number: 13610808

Title: A Chandra Legacy Project to Resolve the Accretion Flow of Gas Captured by a Supermassive Black Hole

Type: XVP Total Time: 1000

PI Name: Jimmy Irwin

We propose a 1 Msec observation of the hot gas around the supermassive black hole at the center of the nearby S0 galaxy NGC3115 in order to place the first direct observational constraints on the temperature and density structure of an accretion flow inside the Bondi radius of a black hole. These temperature/density constraints will provide a critical test for competing inefficient accretion flow theories. The large angular Bondi radius of this black hole provides the *only* opportunity to perform such a test of inefficient accretion flow theory in the Chandra era and the foreseeable future. An additional benefit of this long observation is that it will also provide the deepest look of the X-ray binary population of a normal early-type galaxy to date.

R.A. Dec. Target Name Det. Grating Exp.Time
10:05:14.00-07:43:06.90NGC3115ACIS-SNONE1000

Subject Category: NORMAL GALAXIES: X-RAY POPULATIONS

Proposal Number: 13620807

Title: Chandra HETG Ultra-deep Gratings Spectroscopy of Sgr A* (CHUGSS)

Type: XVP Total Time: 3000

PI Name: Frederick Baganoff

We propose a 3-Msec HETG exposure to spatially and spectrally resolve the Bondi flow of Sgr A*. This would provide the first high spectral resolution data on Sgr A* and diffuse emission from the central pc of the galaxy. The spectrum will measure the energy and velocity width of the known Fe line from accreting matter within the Bondi radius. It will also detect plasma line emission (e.g., Si & S), if present at levels predicted by RIAF models. Polarization measurements suggest most of the matter crossing the Bondi radius does not reach the event horizon. Understanding the dynamics and thermal structure of this plasma will tell us how this matter flows in and how much and where some of it flows back out. This exposure will also permit extensive multiwavelength monitoring of Sgr A* flares.

R.A. Dec. Target Name Det. Grating Exp.Time
17:45:40.00-29:00:28.10Sgr A*ACIS-SHETG2680
17:45:40.00-29:00:28.10Sgr A*ACIS-SHETG160
17:45:40.00-29:00:28.10Sgr A*ACIS-SHETG40
17:45:40.00-29:00:28.10Sgr A*ACIS-SHETG40
17:45:40.00-29:00:28.10Sgr A*ACIS-SHETG40
17:45:40.00-29:00:28.10Sgr A*ACIS-SHETG40

Subject Category: ACTIVE GALAXIES AND QUASARS

Proposal Number: 13700587

Title: Quasar Feedback in Action: The Wide-Angle Wind of Mrk 231

Type: LP Total Time: 400

PI Name: Sylvain Veilleux

In recent months, our group has discovered a ~1000-km/s outflow in the nearest post-merger quasar Mrk 231 with mass outflow rate about 3x the star formation rate. This outflow extends over several kpc and is wide-angle, thus driven by a QSO wind rather than a jet. This powerful outflow may be the long-sought "smoking gun" of quasar mechanical feedback purported to transform gas-rich mergers into red and dead galaxies. We propose a 400-ksec ACIS-S observation of Mrk 231 to permit 2D spectral mapping of this QSO wind in the X-rays. The obscuring material in Mrk 231 will act as a natural coronagraph to help us study the faint X-ray nebula around the quasar. These data will also be used to monitor the central energy source and constrain the location of the obscuring / scattering material.

R.A. Dec. Target Name Det. Grating Exp.Time
12:56:14.20+56:52:25.00Mrk 231ACIS-SNONE400

Subject Category: ACTIVE GALAXIES AND QUASARS

Proposal Number: 13700784

Title: A DIRECT TEST OF AGN FEEDBACK IN LATE-TYPE GALAXIES: SPATIALLY RESOLVED HETG SPECTROSCOPY OF NGC 3393

Type: LP Total Time: 350

PI Name: Daniel Evans

We propose a 350-ks Chandra/HETG observation of the prototypical massive late-type galaxy NGC 3393, in order to (1) map the kinematics of the NLR, and (2) directly measure the mass outflow rate from the AGN. We will use extract, compare, and model the photoionized emission-line spectra at multiple off-nuclear points along the NLR and ENLR, constructing a picture of how the AGN imparts its energy into its environment. We will also use a novel technique to map the velocity field of the kpc-scale gas, directly constraining the spatial extent and impact of any AGN outflow. Our observations will provide the key test of whether or not outflows in such late-type galaxies expel significant quantities of material during their hosts' transition from the blue cloud to the red sequence.

R.A. Dec. Target Name Det. Grating Exp.Time
10:48:23.50-25:09:43.50NGC 3393ACIS-SHETG350

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 13800359

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

Type: LP Total Time: 500

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+27:57:48.00Coma clusterACIS-INONE125
12:59:49.00+27:57:48.00Coma clusterACIS-INONE125
12:59:49.00+27:57:48.00Coma clusterACIS-INONE125
12:59:49.00+27:57:48.00Coma clusterACIS-INONE125

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

Type: XVP Total Time: 2000

PI Name: Alexey Vikhlinin

The virialization zone of rich galaxy clusters, R500 < r < 3R500 is a ``cosmic melting pot''. Recent observations indicate that it is much more complicated than previously realized. Its study is a new territory for physics of clusters and intergalactic medium. Building upon our pathfinder Chandra GTO exploration of a rich cluster A133, we propose a 2.0 Msec observation of its outskirts, which will provide a detailed picture of the clumpy gas at these radii and of transition from the clumpy to smooth and relaxed state near R500.

R.A. Dec. Target Name Det. Grating Exp.Time
01:01:59.80-21:32:20.70A133-1ACIS-INONE250
01:01:13.90-22:02:30.80A133-3ACIS-INONE250
01:03:04.80-21:37:39.50A133-4ACIS-INONE250
01:02:19.00-22:07:50.70A133-5ACIS-INONE250
01:04:09.80-21:42:56.70A133-6ACIS-INONE250
01:03:24.20-22:13:09.00A133-8ACIS-INONE250
01:01:36.90-21:47:25.90A133-2ACIS-INONE250
01:03:47.00-21:58:02.90A133-7ACIS-INONE250

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

Type: LP Total Time: 310

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+26:22:10.00Abell 115ACIS-INONE310

Subject Category: CLUSTERS OF GALAXIES

Proposal Number: 13800764

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

Type: LP Total Time: 300

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
01:02:53.00-49:15:16.90ACT J0102-4915ACIS-INONE300

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

Type: XVP Total Time: 2070.68

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
00:13:19.10-49:06:50.40SPT-CLJ0013-4906ACIS-INONE15.4
21:35:38.60-57:26:27.20SPT-CLJ2135-5726ACIS-INONE18.7
02:12:26.40-46:57:00.70SPT-CLJ0212-4656ACIS-INONE30.7
03:48:17.70-45:14:59.30SPT-CLJ0348-4514ACIS-INONE14.2
20:35:12.20-52:51:05.40SPT-CLJ2035-5251ACIS-INONE20.4
01:42:11.90-50:32:36.20SPT-CLJ0142-5032ACIS-INONE31.9
01:06:25.80-59:43:17.00SPT-CLJ0106-5943ACIS-INONE19.3
21:46:34.80-46:32:57.80SPT-CLJ2146-4632ACIS-INONE80.8
03:34:10.20-46:59:22.90SPT-CLJ0334-4659ACIS-INONE29
00:14:46.70-49:52:37.60SPT-CLJ0014-4952ACIS-INONE60.7
04:49:06.80-49:01:17.00SPT-CLJ0449-4901ACIS-INONE61.3
04:56:26.80-51:16:25.00SPT-CLJ0456-5116ACIS-INONE55.2
04:41:47.30-48:54:45.00SPT-CLJ0441-4854ACIS-INONE76.3
03:07:46.70-50:42:22.30SPT-CLJ0307-5042ACIS-INONE47.2
20:43:18.00-50:35:26.50SPT-CLJ2043-5035ACIS-INONE81.4
00:58:17.50-61:45:36.40SPT-CLJ0058-6145ACIS-INONE61
01:51:23.90-59:54:07.60SPT-CLJ0151-5954ACIS-INONE89
02:56:23.20-56:17:46.30SPT-CLJ0256-5617ACIS-INONE52
04:46:02.60-58:49:17.40SPT-CLJ0446-5849ACIS-INONE58.8
02:43:25.80-59:30:43.60SPT-CLJ0243-5930ACIS-INONE51.5
01:02:40.70-46:03:53.60SPT-CLJ0102-4603ACIS-INONE66.8
06:55:50.60-52:34:02.60SPT-CLJ0655-5234ACIS-INONE22.1
02:00:35.20-48:52:37.60SPT-CLJ0200-4852ACIS-INONE25.7
01:56:08.40-55:41:37.30SPT-CLJ0156-5541ACIS-INONE85.3
03:52:55.70-56:47:53.20SPT-CLJ0352-5647ACIS-INONE49.5
01:23:09.60-48:21:19.40SPT-CLJ0123-4821ACIS-INONE79.8
03:10:29.20-46:46:52.30SPT-CLJ0310-4646ACIS-INONE40.3
00:37:45.20-50:47:37.70SPT-CLJ0037-5047ACIS-INONE82.6
04:26:03.90-54:55:16.30SPT-CLJ0426-5455ACIS-INONE38.5
04:06:53.60-48:04:52.30SPT-CLJ0406-4804ACIS-INONE28.6
00:33:54.20-63:26:37.70SPT-CLJ0033-6326ACIS-INONE23.1
21:48:42.00-61:16:42.60SPT-CLJ2148-6116ACIS-INONE39.8
02:52:44.90-48:24:45.40SPT-CLJ0252-4824ACIS-INONE33.8
Smithsonian Institute Smithsonian Institute

The Chandra X-Ray Center (CXC) is operated for NASA by the Smithsonian Astrophysical Observatory. 60 Garden Street, Cambridge, MA 02138 USA.   Email:   cxchelp@head.cfa.harvard.edu Smithsonian Institution, Copyright © 1998-2017. All rights reserved.