Assigned ID: 866
----- Attempting Submission 1 (Sat Feb 27 00:13:26 GMT 2010) -----
HST Phase I Proposal 866 (lyc_a1689.apt) successfully submitted.
----- Attempting Submission 2 (Sat Feb 27 00:40:34 GMT 2010) -----
HST Phase I Proposal 866 (lyc_a1689.apt) successfully submitted.
----- Attempting Submission 3 (Sat Feb 27 00:51:10 GMT 2010) -----
HST Phase I Proposal 866 (lyc_a1689.apt) successfully submitted.
----- Attempting Submission 4 (Sat Feb 27 00:58:10 GMT 2010) -----
----- Attempting Submission 1 (Fri Jul 09 07:40:57 GMT 2010) -----
There is one remaining warning because I've only used 34 orbits. The original
allotment was for 36 orbits but two were taken away due to duplication with a
cycle-17 program (11802 PI, Holland Ford).
Ionizing Emission from the Faint Galaxies Responsible for Reionization
The epoch of formation of the first galaxies, and the subsequent reionization of the universe is the final frontier in galaxy evolution studies. In order to reionize the intergalactic medium by z=6, large fractions of ionizing photons must be escaping from the numerous feeble galaxies which we are now just beginning to detect at 6<z<10. Semi-analytic models and numerical simulations have suggested several different mechanisms to explain the required high escape fractions in these systems. Unfortunately, these feeble galaxies are far too faint to actually measure the escape fraction of Lyman continuum photons. Given their importance to the global star formation rate in the early universe and to reionization, our team has been identifying and characterizing large numbers of intrinsically very faint (-15<M_UV<-19) galaxies at 1.5<z<4 that are highly magnified by foreground massive clusters. Here we propose a single deep (34 orbit) near-UV (F275W) image of the restframe HI-ionizing continuum of 13 of these galaxies with 2.52<z<2.66 lying behind the cluster Abell 1689. The increased sensitivity and spatial resolution provided by the strong gravitational lensing allows an unprecedented measurement of the escape fraction of ionizing radiation from the types of galaxies deeemed responsible for reionization. When combining these data with existing HST optical/IR imaging and our own very deep Keck/Subaru near-IR/optical spectra, we will be able to determine the mechanisms that allow for large escape fractions, and better understand the process of reionization.
We were initially allocated 36 orbits for WFC3 imaging of Abell 1689. Due to duplication with a cycle-17 program, we lost two orbits and now have a total of 34. All orbits will be used for imaging of Abell 1689 in one single pointing: 30 orbits in F275W and 4 orbits in F336W. In both filters, the default four point dither WFC3-UVIS-DITHER-BOX will be used with half-orbit (~1310s) exposures. There will be a total of 10,480 s of exposure in F336W (8x1310s) and 78,600 s of exposure in F275W (60x1310s). Each 2-orbit dither pattern will be offset by ~1.5" to cover the gap in the UVIS chips. The ORIENT is required to be the same for all visits.
Though we can theoretically get about 5% more exposure time, we've chosen to use 1310s exposures because this allows the largest visibility window and easiest scheduling.
UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTURE
12
false
0.0
0.0
false
false
false
false
false
false
SUPPORTED
CLUSTER OF GALAXIES
EINSTEIN RING
GRAVITATIONAL LENS
RICH CLUSTER
J2000
00 00 0.0000
+00 00 0.00
J2000
WFC3/UVIS
Imaging
No
No
F275W
WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Imaging
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F160W
POS-TARG
DITHER
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LINE
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false
false
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WFC3-UVIS-DITHER-BOX
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(Tic-Orbit
:proposal-id 12201
:visit-id "09"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2756
:al-overhead-at-end 116
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3234
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 12201
:visit-id "09"
:orbit-number 2
:pcs-time 222
:si-vis-utilization 2756
:al-overhead-at-end 116
:internal-dur-at-end 670
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3234
:pcs-gap 0
)
true
2
0