Accepted Cycle 13 Observing Proposals

EXTRAGALACTIC DIFFUSE EMISSION & SURVEYS

Proposal Number	Subject Category	PI Name	Title
13900121	EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS	Randall	Measuring the Temperature Structure of the A3395/A3391 Large Scale Filament in the Horologium Supercluster
13900353	EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS	Lopez	Probing the Nature and Role of X-ray Emission in HII Regions with Chandra
13900549	EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS	Su	Joint Chandra/XMM-Newton Observation of NGC1407/1400 complex
13900823	EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS	ajello	BAT, Chandra, NuSTAR and The origin of the Cosmic X-ray Background
13900828	EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS	Levan	The demographics of dark gamma-ray bursts

Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS

Proposal Number: 13900121

Title: Measuring the Temperature Structure of the A3395/A3391 Large Scale Filament in the Horologium Supercluster

PI Name: Scott Randall

We propose to observe the large scale filament between the galaxy clusters A3395 and A3391 detected with ROSAT, with the goal of a direct imaging detection of, and mapping the thermal structure of, a filament for the first time. This filament is nearby (z~0.053) and oriented close to our line of sight (< 9 deg), such that the projected surface brightness favors X-ray detection. Chandra's low, stable background (for the ACIS-I array) and high angular resolution, which allows for the removal of contaminating sources, make it well-suited to this kind of study. We propose three 50 ks pointings to fully cover the filament, with highest priority given to the central pointing.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
06:26:24.50	-54:04:49.40	Abell 3395 Filament Center	ACIS-I	NONE	50
06:26:34.40	-54:17:57.30	Abell 3395 Filament South	ACIS-I	NONE	50
06:26:19.70	-53:52:04.20	Abell 3395 Filament North	ACIS-I	NONE	50

Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS

Proposal Number: 13900353

Title: Probing the Nature and Role of X-ray Emission in HII Regions with Chandra

PI Name: Laura Lopez

We propose four new ACIS-I observations totaling 105 ks of five HII regions in the Large Magellanic Cloud. With this data, we aim to undertake the first systematic study of HII regions with Chandra and to describe the nature and role of the X-ray emission in star-forming regions. In particular, our analyses will 1) probe the relative contribution of stellar winds and supernovae to the X-ray emission and test superbubble and wind models, 2) examine the role of hot gas in the dynamics of HII regions, and 3) search for and characterize the non-thermal X-rays in our sources. We will compare the sources of our sample to ascertain how the X-ray properties vary with age, size, and stellar content. Only Chandra has the spatial resolution and sensitivity necessary for our proposed analyses.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
05:39:26.00	-69:34:40.00	N158C	ACIS-I	NONE	15
05:21:40.00	-69:40:43.00	N127A	ACIS-I	NONE	30
05:18:33.00	-69:13:51.00	N119	ACIS-I	NONE	30
05:13:25.00	-69:22:46.00	N113	ACIS-I	NONE	30

Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS

Proposal Number: 13900549

Title: Joint Chandra/XMM-Newton Observation of NGC1407/1400 complex

PI Name: Yuanyuan Su

The nearby dark group centered on NGC 1407 is notable for a nearby bright galaxy (NGC 1400) with a velocity differing by at least 1200 km/s. This large velocity difference, plus controversy over these two galaxies' respective distances, has led to a wide range of mass estimates for this group. Our analysis of XMM-Newton data reveals an extended region of enhanced surface brightness near NGC 1400 which may be a cold front. We also find that the hottest regions lie between NGC 1400 and 1407, suggesting that their atmospheres are colliding. We propose a 55 ks Chandra ACIS-S pointing of NGC 1400 to reveal the nature of the enhanced region, and a 30 ks XMM-Newton pointing covering the east side of NGC 1407 to obtain a complete temperature map as well as a total group mass profile.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
03:39:41.00	-18:40:02.70	NGC1407/1400	ACIS-S	NONE	55

Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS

Proposal Number: 13900823

Title: BAT, Chandra, NuSTAR and The origin of the Cosmic X-ray Background

PI Name: marco ajello

We propose a quick snapshot program with Chandra to observe the remaining 18 AGN detected by BAT that do not have any X-ray observation in the 0.1-10 keV band. These AGN are expected to be absorbed by 23

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
01:32:00.00	-41:56:56.40	J0132.0-4156	ACIS-I	NONE	5
02:32:18.70	-36:39:32.40	J0232.3-3639	ACIS-I	NONE	5
02:33:24.70	+27:53:60.00	J0233.4+2754	ACIS-I	NONE	5
02:52:00.00	-16:41:60.00	J0252.0-1642	ACIS-I	NONE	5
02:59:00.20	-57:17:60.00	J0259.0-5717	ACIS-I	NONE	5
05:43:47.30	-27:39:03.60	J0543.7-2739	ACIS-I	NONE	5
06:40:47.80	-43:21:00.00	J0640.7-4321	ACIS-I	NONE	5
12:13:60.00	+29:32:56.40	J1214.0+2932	ACIS-I	NONE	5
13:39:48.70	+55:47:60.00	J1339.8+5548	ACIS-I	NONE	5
13:54:00.00	-11:24:00.00	J1354.0-1123	ACIS-I	NONE	5
13:54:25.20	-37:46:40.80	J1354.4-3746	ACIS-I	NONE	5
14:19:12.00	+07:56:52.80	J1419.2+0756	ACIS-I	NONE	5
18:57:55.40	-78:30:18.40	J1857.9-7830	ACIS-I	NONE	5
22:42:24.00	-37:06:00.00	J2242.4-3705	ACIS-I	NONE	5
11:39:12.00	+03:36:00.00	J1139.2+0336	ACIS-I	NONE	5
14:58:24.00	-24:48:00.00	J1458.4-2447	ACIS-I	NONE	5
16:23:36.00	-09:35:60.00	J1623.6-0935	ACIS-I	NONE	5

Subject Category: EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS

Proposal Number: 13900828

Title: The demographics of dark gamma-ray bursts

PI Name: Andrew Levan

Dark gamma-ray bursts (GRBs) -- where the optical emission is apparently suppressed -- can only be reliably localized by their X-ray afterglows. Here we propose to complete a survey using the sensitivity and point spread function of Chandra to precisely pinpoint the GRB locations, and HST to locate and study the host galaxies. Our results to date are suggestive of most dark GRBs originating in more luminous galaxies than "bright" GRBs. Our new observations will increase the statistical certainty of this result, while simultaneously allowing us to more precisely identify the minority of dark GRBs which most likely originate from the highest redshifts.

Target Name	Det.	Grating	Exp.Time
DARK-GRB1	ACIS-S	NONE	15
DARK-GRB2	ACIS-S	NONE	15
DARK-GRB3	ACIS-S	NONE	15

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