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16 April 2024
 
  » arxiv » 2001.2465

 Article overview


Galaxy And Mass Assembly (GAMA): Defining Passive Galaxy Samples and Searching for the UV Upturn
S. Phillipps ; S.S. Ali ; M.N. Bremer ; R. De Propris ; A.E. Sansom ; M.E. Cluver ; M. Alpaslan ; S. Brough ; M.J.I. Brown ; L.J.M. Davies ; S.P. Driver ; . M.W. Grootes ; B.W. Holwerda ; A.M. Hopkins ; P.A. James ; K. Pimbblet ; A.S.G. Robotham ; E.N. Taylor ; L. Wang ;
Date 8 Jan 2020
AbstractWe use data from the GAMA and GALEX surveys to demonstrate that the UV upturn, an unexpected excess of ultraviolet flux from a hot stellar component, seen in the spectra of many early-type galaxies, arises from processes internal to individual galaxies with no measurable influence from the galaxies’ larger environment. We first define a clean sample of passive galaxies without a significant contribution to their UV flux from low-level star formation. We confirm that galaxies with the optical colours of red sequence galaxies often have signs of residual star formation, which, without other information, would prevent a convincing demonstration of the presence of UV upturns. However, by including (NUV$-u$) and {it WISE} (W2-W3) colours, and FUV data where it exists, we can convincingly constrain samples to be composed of non-star-forming objects. Using such a sample, we examine GALEX photometry of low redshift GAMA galaxies in a range of low-density environments, from groups to the general field, searching for UV upturns. We find a wide range of (NUV$-r$) colours, entirely consistent with the range seen -- and attributed to the UV upturn -- in low-redshift red sequence cluster galaxies. The range of colours is independent of group multiplicity or velocity dispersion, with isolated passive galaxies just as likely to have blue UV-to-optical colours, implying significant upturn components, as those in richer groups and in the previous data on clusters. This is supported by equivalent results for (FUV$-r$) colours which are clear indicators of upturn components.
Source arXiv, 2001.2465
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