TY - JOUR
T1 - The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139
AU - Sengupta, Aparajita
AU - Keel, William C.
AU - Morrison, Glenn
AU - Windhorst, Rogier A.
AU - Miller, Neal
AU - Smith, Brent
N1 - Funding Information:
Funding for SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/ .
Funding Information:
We acknowledge the support from NASA James Webb Space Telescope (JWST) Interdisciplinary Scientist grants NAG5−12460, NNX14AN10G, and 80NSSC18K0200 from Goddard Space Flight Center (GSFC).
Funding Information:
IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. α β
Funding Information:
The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max Planck Institute for Astronomy, the Max Planck Institute for Astrophysics, New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalog is based on data taken from the SDSS and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programs, including GALEX Medium Imaging Surveys (MIS), VLT Survey Telescope Kilo-Degree Survey (VST KiDS), VISTA Kilo-Degree Infrared Galaxy Survey (VIKING), Wide-field Infrared Survey Explorer (WISE) Herschel-Asteroid Terrestrial-impact Last Alert System (ATLAS), Giant Metrewave Radio Telescope (GMRT), and Australian Square Kilometre Array Pathfinder (ASKAP), providing UV-to-radio coverage. GAMA is funded by the Science and Technology Facilities Council (STFC) (UK), the Australian Research Council (ARC) (Australia), the Australian Astronomical Optics (AAO), and the participating institutions. The GAMA website is http://www.gama-survey.org/ .
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022
Y1 - 2022
N2 - 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 >1010.5 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 < 1010.5 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.
AB - 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 >1010.5 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 < 1010.5 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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U2 - 10.3847/1538-4365/ac3761
DO - 10.3847/1538-4365/ac3761
M3 - Article
AN - SCOPUS:85125434766
SN - 0067-0049
VL - 258
JO - Astrophysical Journal, Supplement Series
JF - Astrophysical Journal, Supplement Series
IS - 2
M1 - 32
ER -