The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139

Sengupta, Aparajita; Keel, William C.; Morrison, Glenn; Windhorst, Rogier A.; Miller, Neal; Smith, Brent

doi:10.3847/1538-4365/ac3761

Title: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139

Journal Article · 31 January 2022 · The Astrophysical Journal. Supplement Series

DOI: https://doi.org/10.3847/1538-4365/ac3761 · OSTI ID:1983303

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Indiana Univ.-Purdue Univ. Indianapolis (IUPUI), Indianapolis, IN (United States)
Univ. of Alabama, Tuscaloosa, AL (United States)
Univ. of Hawaii, Honolulu, HI (United States); Canada-France-Hawaii Telescope, Kamuela, HI (United States)
Arizona State Univ., Tempe, AZ (United States)
Stevenson University, Owings Mills, MD (United States)

A rare opportunity to distinguish between internal and environmental effects on galaxy evolution is afforded by "SuperGroups," systems that are rich and massive, but include several comparably rich substructures, surrounded by filaments. We present here a multiwavelength photometric and spectroscopic study of the galaxy population in the SuperGroup Abell 1882 (A1882) at z = 0.139, combining new data from the MMT and Hectospec with archival results from the Galaxy And Mass Assembly survey, the Sloan Digital Sky Survey, the Nasa/IPAC Extragalactic Database, the Gemini Multi-Object Spectrograph, and the Galaxy Evolution Explorer. These provide spectroscopic classifications for 526 member galaxies, across wide ranges of local density and velocity dispersion. We identify three prominent filaments along which galaxies seem to be entering the SuperGroup (mostly in E–W directions). A1882 has a well-populated red sequence, containing most galaxies with stellar mass >10^10.5 M_Sun, and a pronounced color–density relation even within its substructures. Thus, galaxy evolution responds to the external environment as strongly in these unrelaxed systems as we find in rich and relaxed clusters. From these data, local density remains the primary factor, with a secondary role for distance from the inferred center of the entire structure's potential well. The effects on star formation, as traced by optical and near-UV colors, depend on galaxy mass. We see changes in lower-mass galaxies (M < 10^10.5 M_Sun) at four times the virial radius of major substructures, while the more massive near-UV Green Valley galaxies show low levels of star formation within two virial radii. The suppression of star formation ("quenching") occurs in the infall regions of these structures even before the galaxies enter the denser group environment.

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Research Organization:: US Department of Energy (USDOE), Washington, DC (United States). Office of Science, Sloan Digital Sky Survey (SDSS)

Sponsoring Organization:: Alfred P. Sloan Foundation; National Aeronautics and Space Administration (NASA); National Science Foundation (NSF); USDOE Office of Science (SC)

OSTI ID:: 1983303

Journal Information:: The Astrophysical Journal. Supplement Series, Journal Name: The Astrophysical Journal. Supplement Series Journal Issue: 2 Vol. 258; ISSN 0067-0049

Publisher:: IOP PublishingCopyright Statement

Country of Publication:: United States

Language:: English

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Title: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139

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