Shifted pointing for UDS118604 by 25 arcsec to move a very bright (H=7.8) star out of the detector field.
----- Attempting Submission 2 (Sat Aug 04 03:13:51 GMT 2012) -----
Monsters at the Dawn of the Thermal Era: Probing the extremes of galactic mass at z>2.5
There can now be little doubt that a significant population of massive early-type galaxies exists at z~2. Revealed by a combination of wide-field, deep near-IR photometric surveys and medium-resolution near-IR spectroscopy, they look like nothing in the local universe: despite having stellar masses comparable to nearby ellipticals, their average effective radii are 5 times smaller, implying enormous stellar densities. Their formation remains a mystery, as all their stellar mass must have been assembled within the first 1-2 Gyr after the Big Bang. Using new ultradeep, wide-field near-IR imaging, we have now uncovered a population of rare and extremely massive (log M/Msun>11.2) quiescent galaxies at even higher redshifts (2.5<z<3.5). Interestingly, these galaxies do not seem to follow the same size evolution trends as less-extreme galaxies; however, since their sizes are estimated from ground-based imaging, details of their structure (clumps, extended envelopes, and/or multiplicity) cannot be ascertained. These "monster" galaxies are so rare that essentially none will be covered in the infrared by existing large HST surveys. Here we propose WFC3/IR imaging of the 12 most massive quiescent galaxies in our z>2.5 sample to determine their sizes and structural parameters. By combining targeted near-IR imaging of these rare objects with robust sizes of less-massive galaxies from the complementary CANDELS MCT program, we will place the first strong constraints on the structural evolution of the extreme tail of the galaxy population at z~2.7.
The purpose of this program is to obtain imaging of twelve z>2.5, massive, compact early-type galaxies (ten for one orbit each, two for two orbits each) in order to place precise limits on their sizes, structures, and morphologies. At these redshifts the most robust band to measure such quantities is the near-IR, which traces rest-frame optical light; we thus employ the F160W filter on WFC3/IR. A well-sampled PSF is critical to perform these measurements, so we will use the standard four-point WFC3-IR-DITHER-BOX pattern; since the targets are all small in extent (<0.5 arcsec), there is no need to step over IR blobs or the death star.
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