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Near-ultraviolet signatures of environment-driven galaxy quenching in Sloan Digital Sky Survey groups

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  • Jacob P. Crossett
  • Kevin A. Pimbblet
  • D. Heath Jones
  • Michael J. I. Brown
  • John P. Stott
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<mark>Journal publication date</mark>01/2017
<mark>Journal</mark>Monthly Notices of the Royal Astronomical Society
Issue number1
Volume464
Number of pages11
Pages (from-to)480-490
Publication StatusPublished
Early online date7/09/16
<mark>Original language</mark>English

Abstract

We have investigated the effect of group environment on residual star formation in galaxies, using Galaxy Evolution Explorer near-ultraviolet (NUV) galaxy photometry with the Sloan Digital Sky Survey group catalogue of Yang et al. We compared the (NUV - r) colours of grouped and non-grouped galaxies, and find a significant increase in the fraction of red sequence galaxies with blue (NUV - r) colours outside of groups. When comparing galaxies in mass-matched samples of satellite (non-central), and non-grouped galaxies, we found a >4 sigma difference in the distribution of (NUV - r) colours, and an (NUV - r) blue fraction >3 sigma higher outside groups. A comparison of satellite and non-grouped samples has found the NUV fraction is a factor of similar to 2 lower for satellite galaxies between 10(10.5) and 10(10.7)M(circle dot), showing that higher mass galaxies are more likely to have residual star formation when not influenced by a group potential. There was a higher (NUV - r) blue fraction of galaxies with lower Sersic indices (n <3) outside of groups, not seen in the satellite sample. We have used stellar population models of Bruzual & Charlot with multiple burst, or exponentially declining star formation histories to find that many of the (NUV - r) blue non-grouped galaxies can be explained by a slow (similar to 2 Gyr) decay of star formation, compared to the satellite galaxies. We suggest that taken together, the difference in (NUV - r) colours between samples can be explained by a population of secularly evolving, non-grouped galaxies, where star formation declines slowly. This slow channel is less prevalent in group environments where more rapid quenching can occur.