This is a resubmission with a new grouping of orbits and visits to facilitate data reduction.
All the rest is the same (except "GS Acq Scenario" for WFC3 orbits).
Now WFC3 has 4 orbits per visit (4 exposures per visit) and ACS has 2 orbits per visit (4 exposure per visit).
Checked with HST support that planned window is the same with the new grouping.317129827----- Attempting Submission 2 (Thu Jul 31 18:34:23 GMT 2014) -----Illuminating the Dark Phases of Galaxy-Formation with the Help of a z=2.4 QuasarGalaxy formation occurs along the densest regions of the Intergalactic Medium (IGM) where the gas can collapse and form stars. However, despite their importance, the phases preceding substantial star formation are usually unobservable and thus poorly constrained. How is the IGM converted into stars at high-z and what is the efficiency of this process? The aim of this project is to answer these questions taking advantage of a new and, so far, unique dataset: "dark" galaxies fluorescently illuminated by a bright quasar at z=2.4, recently discovered by Cantalupo et al. with deep Ly-alpha imaging on the VLT. Differently from any previous Ly-alpha survey, fluorescent emission provides a direct constraint on the gas distribution independent of any associated star formation. We have discovered a large number of high Equivalent Width (>240A) objects for which the emission is likely powered by fluorescence. These are the best candidates for "dark" galaxies currently known. Unfortunately they are spatially unresolved in our ground-based observations: the study of this new category of objects requires space-based imaging for any major advancement. A direct measurement of the star formation efficiency (SFE) of these clouds would represent a major breakthrough in the study of galaxy-formation. HST imaging will provide the key elements to achieve this goal: i) resolved Ly-alpha imaging with WFC3, providing the source sizes and gas mass; ii) ACS imaging at rest-frame 1500A, providing a measurement of recent SFR. Combined together, these observations will provide the first direct constraint on the size, gas mass and SFE of the lowest mass haloes at high-z.The program consists of 12 WFC3/UVIS (filter F410M) and 10 ACS/WFC (filter F606W) orbits on a single pointing with orientation optimized to obtain Ly-alpha and continuum imaging of a sample of 8 of the 12 dark galaxies discovered in our ground-based survey (Cantalupo et al. 2012).
We will use full-orbit exposures for F410M and half-orbit exposures for F606W. The long exposure allow us to reach a 12e background and therefore avoiding post-flashing for CTE. The large number of expsoures, 12 for F410M and 20 for F606W, will allow to efficiently remove cosmic rays during image combination. Full-orbit exposures have been already used with success in the past cycle by other groups.
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