0 Assigned ID: 1840 ----- Attempting Submission 1 (Fri Mar 01 22:09:00 GMT 2013) ----- HST Phase I Proposal 1840 (hst_dfall.pdf.apt) successfully submitted. ----- Attempting Submission 2 (Fri Mar 01 22:20:48 GMT 2013) ----- HST Phase I Proposal 1840 (hst_dfall_subm.pdf.apt) successfully submitted. ----- Attempting Submission 3 (Fri Mar 01 22:36:52 GMT 2013) ----- HST Phase I Proposal 1840 (hst_dfall_subm.pdf.apt) successfully submitted. ----- Attempting Submission 4 (Fri Mar 01 22:41:24 GMT 2013) ----- 0 ----- Attempting Submission 1 (Wed Jun 26 22:16:56 GMT 2013) ----- We have recently initiated a study that has the potential to fundamentally change our picture of galaxy evolution. Using the Jansky Very Large Array, we target a "Molecular Deep Field" to measure, for the first time, the unbiased cosmic evolution of the gas content of galaxies ("Cold Gas History of the Universe") at high redshift. We here request HST ACS and WFC3/IR observations to determine the rest-frame optical morphologies and spatially resolved star formation and stellar mass properties of the galaxies in this region to simultaneously measure the cold gas, star formation rate and stellar mass histories of the universe in a common legacy field. The high resolution and sensitivity of the HST data will allow us to directly tie the gas content, gas fractions, and star formation rates to the structural properties of galaxies. This will provide a deeper understanding of the drivers of star formation and stellar bulge/disk growth based and their connection to the gas supply and dynamics in galaxies, as well as the relative importance of mergers vs. passively evolving galaxies. The proposed inexpensive study will also enable us to study the star formation properties of the most distant spectroscopically confirmed galaxy protocluster at z=5.3. With ALMA, we have serendipitously discovered a new population of [CII]-luminous, otherwise undetected galaxies at the redshift of this protocluster. The proposed WFC3/IR data will likely be deep enough to detect the rest-frame UV emission from these enigmatic galaxies, enabling us to investigate their true nature. Program uses 4 orbits, 3 with WFC3/IR in the F125W and F160W filters, and 1 with ACS/WFC and the F606W filter. It is broken up into two visits, one consisting of the single ACS orbit, and the other consisting of the three WFC3 IR orbits (concatenated to ensure similar rotation angles between orbits, and thus, coverage of the same galaxies in both filters - this is not an issue for ACS, given the much larger field of view relative to WFC3, it will cover the full area of interest at any orientation angle). There is no restriction on the orientation angle. All observations are of the same target field (CODEEPFIELD). 4-point position/readout dither patterns are employed, primarily to improve the PSF through subpixel sampling, i.e., to mitigate the effects of the large detector pixel sizes (especially for WFC3/IR), as well as to offset by a sufficiently large amount to move persistent pixels to different locations on the sky in each exposure, and to provide good cosmic ray rejection. For ACS/WFC, this is also important to cover the 50 pixel gap in y direction between the two detector chips. The ACS/WFC dither pattern consists of 2 positions with offset large enough to cover the inter-chip gap, and 2 subpositions each to dither on subpixel scales. The WFC3/IR dither patterns consist of 2 postions large enough to cover the "death star" feature, and 2 subpositions each to dither on subpixel scales. For the one F125W orbit, 4 positions are targeted. For the two F160W orbits, each orbit contains two subpixel dither positions, and the larger re-positioning is done between orbits. UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTURE Default false false false false false SUPPORTED GALAXY HIGH REDSHIFT GALAXY PROTOGALAXY J2000 J2000 ACS/WFC Imaging No No F606W WFC3/IR Imaging No No F125W WFC3/IR Imaging No No F160W POS-TARG DITHER BACKGROUND 2 3.011 LINE false false 0.149 2 85.28 POS-TARG ACS-WFC-DITHER-LINE 34.25 1 true 1372200190177 /Users/dr/proposals/HST_2013/OP-cache/phase2_3-v01.xml The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. 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