Galaxy Structure in the Ultraviolet: Case studies for Galaxy Evolution

Details Galaxy Structure in the Ultraviolet: Case studies for Galaxy Evolution Galaxy Structure in the Ultraviolet: Case studies for Galaxy Evolution

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21944117m&link_type=abstract

American Astronomical Society, AAS Meeting #219, #441.17

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The majority of high redshift galaxies appear similar to a relatively rare subset of low redshift irregular and peculiar galaxies whose morphologies are pathological due to mergers or interactions. The observed increase in the percentage of merging/interacting galaxies with redshift supports models of hierarchical galaxy formation. Detailed comparisons of galaxies as a function of redshift are essential to learn how galaxies assemble and evolve over time. These comparison studies are complicated by the fact that galaxies can look substantially different at shorter wavelengths than at longer ones. This leads to a "morphological k-correction” for a given galaxy between different rest-frame wavelengths. This is particularly important in studies of high redshift galaxies, as band-pass shifting will cause light originally emitted in the UV to be shifted as far as the IR. This raises questions about how much of the irregular/peculiar morphologies seen in high redshift studies are simply due to band-pass shifting, and not real differences in galaxy type. This is particularly important when comparing the UV to the optical or IR, as galaxy stellar energy distributions change drastically short-ward of the Balmer Break (< 360 nm), and UV-bright star-forming regions dominate morphologies that appear smoother at redder wavelengths. We thus calculate a morphological k-correction by quantifying the galaxy structure of several thousand nearby galaxies observed with GALEX (Galaxy Evolution Explorer) in the UV, via their "CAS parameters” (Concentration, Asymmetry, Clumpiness). Funded by a grant through NASA.

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