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Assigned ID: 355
----- Attempting Submission 1 (Fri Feb 24 09:59:34 GMT 2012) -----
HST Phase I Proposal 355 (cluster_uvis.apt) successfully submitted.
----- Attempting Submission 2 (Fri Feb 24 16:35:20 GMT 2012) -----
HST Phase I Proposal 355 (cluster_uvis.apt) successfully submitted.
----- Attempting Submission 3 (Fri Feb 24 23:53:06 GMT 2012) -----
I am resubmitting the phase-II to replace two of the F336W orbits with F275W imaging with post -flash.
This is to test the CTE in previous observations. I have been allowed to make this change.
-280352421
----- Attempting Submission 1 (Mon Jul 09 21:28:55 GMT 2012) -----
----- Attempting Submission 2 (Thu Mar 14 21:31:27 GMT 2013) -----
----- Attempting Submission 3 (Mon May 06 15:07:47 GMT 2013) -----
Ultra-Faint Galaxies at the Peak Epoch of Star Formation
There has been much recent interest in the ultra-faint galaxies that are near or beyond our current detection limits at z>1. These galaxies are likely responsible for reionizing the intergalactic medium and make up a significant fraction of the global star formation rate density. Unfortunately, we can not study them in detail as they are too faint (27 < V < 30) for morphological studies or follow-up spectroscopy. With previous UVIS F275W imaging, we have demonstrated that we can efficiently select ultra-faint galaxies at z~2 by using magnification from strong gravitational lensing by the massive cluster Abell 1689. This unique cluster offers the largest area with high magnifications (1.5-4 magnitudes). We selected 81 galaxies at 1.7<z<2.3 behind Abell 1689, extending the previous luminosity function a factor of 100x fainter.
We propose to extend this study to a much broader redshift range. 10 orbits of F225W and 16 orbits of F336W imaging will allow identification of 50-100 ultra-faint star-forming (SFR < 0.1 M_sol/yr) galaxies at each of the two target redshifts, 1<z<1.7 and 2.3<z<3.0, respectively. The high magnification of these samples enables ultra-high resolution (<100 pc) morphologies as well as rest-frame UV and optical spectroscopy from the ground.
We will extend the measurement of the faint-end of the UV luminosity function 30-100x fainter than before and measure the evolution of the faint-end slope from 1<z<3, allowing the ultimate determination of the global star formation rate density at the epoch of peak star formation. Finally, we will measure the Lyman continuum escape fraction in these galaxies that are analogous to those that reionized the universe.
The program will obtain 16 orbits of UVIS F336W and 10 orbits of F225W imaging of a single pointing centered on the lensing cluster Abell 1689. We will use half-orbit exposures to reduce read noise. There are plenty of exposures to remove the significant number of cosmic rays in half-orbit exposures.
We will use the WFC3-UVIS-DITHER-BOX pattern with sub-pixel dithering to allow us to reconstruct the PSF at higher resolution. Because of recent degradation in the CTE, we will be using the post-flash LED to add background to each image to get us to an average background of 13 e-, including dark and background. This requires 8 and 11 e- flashes in F336W and F225W, respectively.
For each filter, we obtain images with orientation rotations of approximately 90 degrees. This will allow us to assess the magnitude of CTE issues at the faint end, as many objects will lie near the readout edge at one orientation and far from the readout edge at the other orientation.
COSMOLOGY
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false
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SUPPORTED
CLUSTER OF GALAXIES
GRAVITATIONAL LENS
RICH CLUSTER
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
WFC3/UVIS
Imaging
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F225W
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WFC3-UVIS-DITHER-BOX
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POS-TARG
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