0
Assigned ID: 380
----- Attempting Submission 1 (Fri Apr 11 06:35:36 GMT 2014) -----
HST Phase I Proposal 380 (cycle22_CTAGN.apt) successfully submitted.
----- Attempting Submission 2 (Fri Apr 11 22:26:39 GMT 2014) -----
HST Phase I Proposal 380 (cycle22_CTAGN.apt) successfully submitted.
----- Attempting Submission 3 (Fri Apr 11 23:12:51 GMT 2014) -----
HST Phase I Proposal 380 (cycle22_CTAGN.apt) successfully submitted.
----- Attempting Submission 4 (Fri Apr 11 23:14:30 GMT 2014) -----
HST Phase I Proposal 380 (cycle22_CTAGN.apt) successfully submitted.
----- Attempting Submission 5 (Fri Apr 11 23:55:45 GMT 2014) -----
HST Phase I Proposal 380 (cycle22_CTAGN.apt) successfully submitted.
Shifted Visit 19 south to help locate guide stars. Duplicate targets 26-29 are now deleted.
use fgs3, visit 19
change dec target 19, back to 1 59 57
887554485
----- Attempting Submission 2 (Fri Aug 22 04:12:36 GMT 2014) -----
HST Phase II Proposal 13868 (cycle22_CTAGN.phaseII.apt) successfully submitted.
----- Attempting Submission 3 (Fri Aug 29 01:04:10 GMT 2014) -----
----- Attempting Submission 4 (Fri Aug 29 12:34:21 GMT 2014) -----
----- Attempting Submission 5 (Fri Aug 29 13:53:39 GMT 2014) -----
----- Attempting Submission 6 (Fri Aug 29 18:08:24 GMT 2014) -----
HST Phase II Proposal 13868 (13868.apt) successfully submitted.
----- Attempting Submission 7 (Fri Aug 29 18:39:51 GMT 2014) -----
HST Phase II Proposal 13868 (13868.apt) successfully submitted.
----- Attempting Submission 8 (Fri Aug 29 19:20:09 GMT 2014) -----
Shifted Visit 19 south to helo locate guide stars.
Are Compton-Thick AGN the Missing Link Between Mergers and Black Hole Growth?
Galaxy mergers have long been proposed as a possible triggering mechanism for AGN activity, but surveys of AGN out to z~2 have consistently failed to find morphological signatures of recent merger activity. A major caveat to these results is that past studies have not been sensitive to heavily obscured, Compton-thick AGN. Hydrodynamical merger simulations predict that this obscured phase should coincide with the most morphologically disturbed phase of a galaxy interaction. To address this potential bias, we propose WFC3 F160W observations of 25 Compton-thick AGN at z~2. The majority of these AGN are newly discovered and have been found by their reflection dominated X-ray spectra and Fe Kalpha emission. We will use the F160W imaging to examine the rest-frame optical morphologies of their host galaxies to determine if obscured SMBH growth is preferentially associated with merger activity at z~2. The F160W imaging is vital as it provides high-resolution imaging beyond the 4000A break at z~2, revealing bulges, disks, and even interaction signatures for the first time. Our proposed observations will increase by a factor of three our current sample of Compton-thick AGN with rest-frame optical imaging at z>1.5. X-ray spectroscopy is arguably the most reliable technique for identifying Compton-thick AGN and our current sample is the largest ever compiled with this method at z~2. As such, the observations requested here will enable the first large-scale study of the host morphologies of bona fide Compton-thick AGN at this redshift and will help reveal if the long predicted AGN-merger connection has been missed in the past due to the effects of obscuration.
We propose to image 25 newly identified Compton-thick AGN (CT-AGN) at z~2 with WFC3/IR in F160W. These AGN are located in the COSMOS, EGS and CDFS fields, although they fall outside the existing CANDELS F160W imaging in these regions. We request the F160W filter as it samples redward of the Balmer/4000A break at z~2. We anticipate that 1-orbit per target is sufficient to assess the morphologies of the CT-AGN host galaxies, based on extensive testing done by the CANDELS collaboration. Our targets are sufficiently spaced on the sky that we require a unique WFC3/IR observation for each source, necessitating a total of 25 orbits to image the complete sample. We will split our total exposure into four sub-exposures using the default WFC3/IR 4-point box dither pattern in order to sufficiently characterize the PSF. Taking into account WFC3 overheads (guide-star acquisition and exposure overheads), we expect 43-46 min of on-source exposure, split into 4 sub-exposures of 650-700 sec each. Most (20/25) visits will be centered on the target CT-AGN, however a handful (5/25) have offsets in place to image multiple CT-AGN. In order to maximize schedulability, we do not place any a priori restrictions on the orientation of the detector for 24/25 of the visits. The only visit which has an orient constraint has plenty of visibility in the specified orient range.
AGN/QUASARS
Default
false
false
false
false
false
SUPPORTED
GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
J2000
J2000
GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
J2000
J2000
GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
J2000
J2000
GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
J2000
J2000
GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
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J2000
GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
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GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
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GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
J2000
J2000
GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
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J2000
GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
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GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
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GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
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GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
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GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
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GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
J2000
J2000
GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
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GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
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GALAXY
HIGH REDSHIFT GALAXY
SEYFERT
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GALAXY
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SEYFERT
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WFC3/IR
Imaging
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F160W
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F160W
WFC3/IR
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F160W
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F160W
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Imaging
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F160W
WFC3/IR
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F160W
WFC3/IR
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F160W
WFC3/IR
Imaging
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F160W
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Imaging
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F160W
WFC3/IR
Imaging
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No
F160W
WFC3/IR
Imaging
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No
F160W
WFC3/IR
Imaging
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No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
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No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F160W
POS-TARG
DITHER
0.572
LINE
0.365
false
false
74.653
4
18.528
WFC3-IR-DITHER-BOX-MIN
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false
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false
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false
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