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We present results from the first robust investigation of galaxy morphologyas a function of environment at z>1.5. Our study is motivated by the fact thatstar-forming galaxies contained within a protocluster at z=2.3 in the HS1700+64field have significantly older ages and larger stellar masses on average thanthose at similar redshifts but more typical environmental densities. In theanalysis of HST/ACS images, we apply non-parametric statistics to characterizethe rest-frame UV morphologies of a sample of 85 UV-selected star-forminggalaxies at z=1.7-2.9, 22 of which are contained in the protocluster. Theremaining 63 control-sample galaxies are not in the protocluster but have asimilar mean redshift of <z>~2.3. We find no environmental dependence for thedistributions of morphological properties. Combining the measured morphologieswith the results of population synthesis modeling, we find only weakcorrelations, if any, between morphological and stellar population propertiessuch as stellar mass, age, extinction and star-formation rate. Given theincomplete census of the protocluster galaxy population, and the lack ofcorrelation between rest-frame UV morphology and star-formation history at z~2within our sample, the absence of environmental trends in the distribution ofmorphological properties is not surprising. Additionally, using a larger sampleof photometric candidates, we compare morphological distributions for 282UV-selected and 43 near-IR-selected galaxies. While the difference in thedegree of nebulosity between the two samples appears to be a byproduct of thefainter average rest-frame UV surface brightness of the near-IR-selectedgalaxies, we find that, among the lowest surface brightness galaxies, thenear-IR-selected objects have significantly smaller angular sizes (abridged).

Morphologies of Galaxies in and around a Protocluster at z=2.300