Journal
ASTROPHYSICAL JOURNAL
Volume 898, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/ab9cb8
Keywords
Galaxy evolution; Galaxy quenching; Infrared galaxies; Late-type galaxies; Galaxy groups; Star formation
Categories
Funding
- Australian Research Council Future Fellowship - Australian Government [FT170100273]
- National Research Foundation (South Africa)
- STFC (UK)
- ARC (Australia)
- AAO
- ESO Telescopes at the La Silla Paranal Observatory [177.A-3016]
- National Aeronautics and Space Administration
- Australian Research Council [FT170100273] Funding Source: Australian Research Council
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Combining high-fidelity group characterization from the Galaxy and Mass Assembly survey and source-tailoredz < 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 10(10) M less than or similar to M-stellar less than or similar to 10(11)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 (M-stellar > 10(10.5)M), consistent with mass quenching. Group galaxies with massesM(stellar) Mshow 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.
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