Galaxy and Mass Assembly (GAMA)

demonstrating the power of WISE in the study of galaxy groups to z < 0.1

M. E. Cluver, T. H. Jarrett, E. N. Taylor, A. M. Hopkins, S. Brough, S. Casura, B. W. Holwerda, J. Liske, K. A. Pimbblet, A. H. Wright

Research output: Contribution to journalArticle

Abstract

Combining high-fidelity group characterization from the Galaxy and Mass Assembly survey and source-tailored z < 0.1 photometry from the Wide-Field Infrared Survey Explorer (WISE) survey, we present a comprehensive study of the properties of ungrouped galaxies, compared to 497 galaxy groups (4 ≤ N FoF ≤ 20) as a function of stellar and halo mass. Ungrouped galaxies are largely unimodal in WISE color, the result of being dominated by star-forming, late-type galaxies. Grouped galaxies, however, show a clear bimodality in WISE color, which correlates strongly with stellar mass and morphology. We find evidence for an increasing early-type fraction, in stellar mass bins between 1010 M⊙ ≲ Mstellar ≲ 1011 M, with increasing halo mass. Using ungrouped, late-type galaxies with star-forming colors (W2-W3 > 3), we define a star-forming main sequence (SFMS), which we use to delineate systems that have moved below the sequence ("quenched"for the purposes of this work). We find that with increasing halo mass, the relative number of late-type systems on the SFMS decreases, with a corresponding increase in early-type, quenched systems at high stellar mass (Mstellar > 1010.5 M), consistent with mass quenching. Group galaxies with masses M stellar < 1010.5 M show evidence of quenching consistent with environmentally driven processes. The stellar mass distribution of late-type, quenched galaxies suggests that it may be an intermediate population as systems transition from being star-forming and late-type to the "red sequence."Finally, we use the projected area of groups on the sky to extract groups that are (relatively) compact for their halo mass. Although these show a marginal increase in their proportion of high-mass and early-type galaxies compared to nominal groups, a clear increase in quenched fraction is not evident.

Original languageEnglish
Article number20
Pages (from-to)1-27
Number of pages27
JournalAstrophysical Journal
Volume898
Issue number1
DOIs
Publication statusPublished - 20 Jul 2020

Bibliographical note

Copyright 2020 The American Astronomical Society. First published in the Astrophysical Journal, 898(1), 20, 2020, published by IOP Publishing. The original publication is available at https://doi.org/10.3847/1538-4357/ab9cb8. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.

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