----- Attempting Submission 3 (Wed Aug 08 21:07:29 GMT 2012) -----
the only errors are due to post-flash in UVIS while also using ACS in parallel. I think this is fine.
Resolving Lyman Continuum Emission from Lya-Emitters
Escaping Lyman-continuum (LyC) radiation from star-forming galaxies is likely responsible for the reionization of the universe. The direct measurement of escaping LyC radiation has proven exceptionally challenging. Using deep, ground-based, near-UV imaging, we have obtained direct LyC detections of both Lyman Break Galaxies (LBGs) and Lyman-Alpha Emitters (LAEs) at z=3.1. These observations have revealed high values for the escape fraction of LyC photons, based on the observed ratio of ionizing to non-ionizing UV radiation. In particular, the LyC escape fractions for some LAEs challenge models of stellar populations. While representing progress, the interpretation of these detections is ambiguous due to the seeing-limited resolution. Our Cycle 17 WFC3/UVIS program mapping the LyC emission for a pilot sample of 6 objects (3 LBGs, 3 LAEs) has revealed a diversity of mechanisms for the escape of ionizing radiation, and highlighted the need for a larger sample of resolved LyC observations. With two additional WFC3/UVIS+F336W pointings, we will target 9 faint z=3.1 LAEs and 2 LBGs - all spectroscopically confirmed at z~3.1 and all with LyC detections in ground-based data. Our observations will quadruple the sample of LAEs with resolved LyC observations, and almost double the sample of LBGs. Based on an efficient observing strategy, we require 24 orbits of WFC3/UVIS+F336W imaging of ionizing radiation and 3 orbits of ACS+F814W imaging of the non-ionizing UV continuum. With these deep, high-resolution maps of ionizing and non-ionizing UV radiation, we will constrain the mechanisms responsible for large escape fractions, and gain insight into the process of reionization.
The program has two primary WFC3/UVIS pointings (with ACS/WFC F814W parallels). For one of these two pointings, we also have a primary ACS/WFC F814W image. Each pointing uses a number of 4-point box dither patterns, with POSTARGS of a few arceconds between each pattern. In order to get all of our objects within the field-of-view, we are constraning the orientations significantly.
To minimize CTE losses, we are using the post-flash mode to deposit ~8 electrons throughout each UVIS F336W exposure. With background and dark current, this should result in ~12 e- per pixel background, where the CTE white paper says the CTE losses are significantly reduced.
COSMOLOGY
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SUPPORTED
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HIGH REDSHIFT GALAXY
LYMAN ALPHA CLOUD
PROTOGALAXY
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