0
Assigned ID: 210
----- Attempting Submission 1 (Thu Apr 09 16:11:59 GMT 2015) -----
HST Phase I Proposal 210 (DLA_HSTimaging.apt) successfully submitted.
Receipt: # 210-1
----- Attempting Submission 2 (Fri Apr 10 13:12:55 GMT 2015) -----
0
----- Attempting Submission 1 (Wed Jul 22 13:44:06 GMT 2015) -----
Unveiling stellar populations in absorption-selected galaxies
Metal absorption lines in Damped Ly-alpha systems (DLAs) allow us to trace the metallicity of galaxies back to redshifts z>5. Therefore, understanding the galaxies that host the DLAs is our best strategy for understanding the physics of galaxy formation and evolution in the early universe. The average DLA arise in low-mass galaxies and detecting these in emission has been difficult. Metal-rich absorbers have proven to arise in brighter galaxies, and we have a growing number of emission line detections from DLA galaxies with ground-based VLT spectra. Combining spectral information of the DLA system with imaging of the host galaxy continuum emission gives unparalleled information of the nature of absorption-selected galaxies and their gaseous halos.
We propose to obtain multi-band images in 3 filters covering the optical to near-IR for seven z>2 DLA systems where we already have a spectroscopic confirmation of the host galaxy. High spatial resolution imaging allows us to accurately measure the impact parameters, morphologies, derive stellar masses, stellar population ages and dust reddening from SED fits, and allow us to investigate several scaling relations such as the mass-metallicity relation. This program will more than double the number of high-z DLA galaxies for which we have detected the stellar continuum. This is science that is impossible to do from the ground due to the glare of the background QSOs and hence the data will be an important part of the legacy of HST. We can now finally begin to investigate absorption selected galaxies on the same footing as luminosity selected ones and probe the build-up of metals in the outskirts of galaxies in the early universe.
This program aims to image galaxies that cause strong absorption lines in spectra of background QSOs. There are 7 targets and each target is imaged in 3 filters (UVIS/F606W, IR/F105W and IR/F160W), with 1 orbit per filter. One target only uses two filters and 2 orbits. All the orbits can be run independently of each other.
Previous spectra of the QSO have revealed emission lines arising from these galaxies at some position angle. We will use orientations to avoid diffraction spikes falling on the galaxies. The QSOs are bright (mag 16-19), while the nearby galaxies are faint (expected magnitudes around 25) and offset by 0.7-3 arcsec from the QSO positions.
Six of the targets will only reach minor degrees of saturation in the central pixels so here we use a simple 4 point dither strategy with exposures of equal lengths. One target, He2243-60 is brighter V=16.3, and will saturate the detector. For this target we use a sequence with a short exposure followed by a series of longer exposure in the UVIS. The IR exposures will saturate within a 2 pixel radius, but since the impact parameter for the galaxy is large, this saturation is acceptable.
Orientations:
The primary targets have to avoid the diffraction spikes. Table 7.4 in P2PI specifies that to place the target along rows in UVIS,the orientation is target_angle +221 deg. For the IR aperture the angle is target_angle +224 deg. Also ORIENT angles -/+180 will place the target along columns. In cases of fainter QSOs, where bleeding will be minor and offsets between the QSO and the target is sufficiently large, ORIENT angles +/- 90 degrees can be used too. Only the UVIS CCD has bleeding.
The specified orient angles are flexible within +/-10 (or 15) degrees depending on the impact parameter.
Following information give the orient angles for each target and each visit:
....
Q0124+0044: Target PA =-50, impact parameter =1.3 arcsec. No strong bleeding of QSO emission.
UVIS ORIENT: -50 +221 = 171. Allow a +90 and -180 ORIENT and a +/-10 deg range.
To add visibility target can be placed near the direction of CCD bleeding (-90 deg)
Allowed ORIENT ranges: 341 - 1 , 161 - 181 , 251 - 271, 113 - 123, 66 - 76
IR ORIENT: -50 +224 = 174. Allow a +/-90 and -180 ORIENT and a +/-10 deg range.
Allowed ORIENT ranges: 344 - 4 , 164 - 184 , 74 - 94 , 254 - 274
....
Q0139-0824: Target PA =-98, impact parameter = 1.6 arcsec. No strong bleeding of QSO emission.
UVIS ORIENT: -98 +221 = 123. Allow a +90 and -180 ORIENT and a +/-10 deg range.
To add visibility target can be placed near the direction of CCD bleeding (-90 deg)
Allowed ORIENT ranges: 113 - 133, 293 -313, 203 - 223, 65 - 75, 18 - 28
IR ORIENT: -98 +224 = 126. Allow a +/-90 and -180 ORIENT and a +/-10 deg range.
Allowed ORIENT ranges: 116 - 136 , 296-316 , 26 - 46 , 206 - 226
....
Q0310+0055: Target PA = 77 deg. Imparct param ~< 3.8 arcsec. Only IR observations.
IR ORIENT: 77 +224 = 301. Allow a +/-90 and -180 ORIENT and a +/-10 deg range.
Allowed ORIENT ranges: 291 - 311 , 111 - 131 , 21 - 41 , 201 - 221
....
Q1313+1441: Target PA =60. Impact parameter = 0.7 arcsec. Some bleeding in the UVIS CCD.
UVIS ORIENT: 60 +221 = 281. Allow a -180 ORIENT and a +/-10 deg range.
Allowed ORIENT ranges: 271 - 291 , 91 - 111
IR ORIENT: 60 +224 = 284. Allow a +/-90 and-180 ORIENT and a +/-10 deg range.
Allowed ORIENT ranges: 274 - 294 , 94 - 114, 4 - 24, 184 - 204
....
Q2059-0528: Target PA = 60, impact parameter = 0.7 arcsec. No strong bleeding of QSO emission.
UVIS ORIENT: 60 +221 = 281. Allow a -180 ORIENT and a +/-10 deg range.
Allowed ORIENT ranges: 271 - 291 , 91 - 111
IR ORIENT: 60 +224 = 284. Allow a +/-90 and -180 ORIENT and a +/-10 deg range.
Allowed ORIENT ranges: 274 - 294 , 94 - 114 , 184 - 204 , 4 - 24
....
Q2239-2949: Target PA =-10, impact parameter = 2.4 arcsec. No strong bleeding of QSO emission.
UVIS ORIENT: -10 +221 = 211. Allow a -180 ORIENT and a +/-10 deg range.
Allowed ORIENT ranges: 21 - 41 , 201 - 221
IR ORIENT: -10 +224 = 214. Allow a +/-90 and -180 ORIENT and a +/-10 deg range.
Allowed ORIENT ranges: 24 - 44 , 204 - 224 , 294 - 314 , 114 - 134
.....
Q2243-60: Target PA = -135. Impact parameter = 3.0 arcsec. Strong bleeding in the UVIS CCD.
UVIS ORIENT: -135 +221 = 86. Allow a -180 ORIENT and a +/-15 deg range.
Allowed ORIENT ranges: 251 - 281 , 71 - 101
IR ORIENT: -135 +224 = 89. Allow a +/-90 and -180 ORIENT and a +/-15 deg range.
Allowed ORIENT ranges: 254 - 284 , 74 - 104, 344 - 14 , 164 - 194
-------------------
QUASAR ABSORPTION LINES AND IGM
12
false
false
false
false
SUPPORTED
GALAXY
QUASAR
Q0124+0044
J2000
J2000
I: 18.0 +/-0.01
GALAXY
QSO
Q0139-0824
J2000
J2000
GALAXY
QSO
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GALAXY
QUASAR
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J2000
i: 17.98 +/-0.02
GALAXY
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GALAXY
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GALAXY
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Q2247-6015
J2000
J2000
R=16.1, J=15.0, H=14.7 (2MASS)
WFC3/IR
Imaging
No
No
F105W
WFC3/IR
Imaging
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No
F105W
WFC3/IR
Imaging
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No
F105W
WFC3/IR
Imaging
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F105W
WFC3/IR
Imaging
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F105W
WFC3/IR
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F105W
WFC3/IR
Imaging
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F105W
WFC3/IR
Imaging
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F160W
WFC3/IR
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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/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F606W
POS-TARG
DITHER
0.173
LINE
0.112
false
false
81.785
4
23.884
WFC3-UVIS-DITHER-BOX
1
false
POS-TARG
DITHER
0.572
LINE
0.365
false
false
74.653
4
18.528
WFC3-IR-DITHER-BOX-MIN
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true
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true
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true
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true
1
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true
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true
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true
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