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Spectroscopic constraints on the buildup of intracluster light in the Coma Cluster

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Date
01/05/2020
Author
Gu, Meng
Conroy, Charlie
Law, David
Van Dokkum, Pieter
Yan, Renbin
Wake, David
Bundy, Kevin
Villaume, Alexa
Abraham, Roberto
Merritt, Allison
Zhang, Jielai
Bershady, Matthew
Bizyaev, Dmitry
Drory, Niv
Pan, Kaike
Thomas, Daniel
Weijmans, Anne Marie
Keywords
Coma Cluster
Galaxy evolution
QB Astronomy
Astronomy and Astrophysics
Space and Planetary Science
3rd-DAS
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Abstract
The stellar content of the intracluster light (ICL) provides unique insight into the hierarchical assembly process of galaxy clusters. We present optical spectra of three ICL regions (μ g ≈ 25.3-26.2 mag arcsec-2) in the Coma cluster, located between 100 and 180 kpc from their nearest brightest cluster galaxies (BCGs): NGC 4889 and NGC 4874. Integral-field unit (IFU) spectroscopy with 13.5 hr on-source integration was acquired in an ancillary program within the Sloan Digital Sky Survey-IV MaNGA survey. We stacked the 127 individual fiber spectra in each IFU to achieve a 1σ limiting surface brightness of 27.9 mag arcsec-2, corresponding to a mean signal-to-noise ratio in the optical of 21.7, 9.0, and 11.7 Å-1, for each ICL region. We apply stellar population models to the stacked spectra. Our results show that the velocity dispersions of ICL regions are very high (σ ∼ 630 km s-1), indicating the stars in these regions are tracing the gravitational potential of the cluster, instead of any individual galaxy. The line-of-sight velocities are different from each other by ∼700 km s-1, while the velocity of each region is similar to the closest BCG. This suggests that the ICL regions are associated with two distinct subclusters centered on NGC 4889 and NGC 4874. The stellar populations of these regions are old and metal-poor, with ages of {equation presented}. From the derived age and metallicity, the buildup of ICL in Coma is likely to be through the accretion of low-mass galaxies or the tidal stripping of the outskirts of massive galaxies that have ended their star formation early on, instead of directly from major mergers of massive galaxies.
Citation
Gu , M , Conroy , C , Law , D , Van Dokkum , P , Yan , R , Wake , D , Bundy , K , Villaume , A , Abraham , R , Merritt , A , Zhang , J , Bershady , M , Bizyaev , D , Drory , N , Pan , K , Thomas , D & Weijmans , A M 2020 , ' Spectroscopic constraints on the buildup of intracluster light in the Coma Cluster ' , Astrophysical Journal , vol. 894 , no. 1 , 32 . https://doi.org/10.3847/1538-4357/ab845c
Publication
Astrophysical Journal
Status
Peer reviewed
DOI
https://doi.org/10.3847/1538-4357/ab845c
ISSN
0004-637X
Type
Journal article
Rights
Copyright © 2020. The American Astronomical Society. All rights reserved. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.3847/1538-4357/ab845c
Description
M.G. acknowledges support from the National Science Foundation Graduate Research Fellowship and the Henry Norris Russell Postdoctoral Fellowship. C.C. acknowledges support from NASA grant NNX15AK14G, NSF grant AST-1313280, and the Packard Foundation. M.A.B. acknowledges NSF Award AST-1517006. The computations in this paper were run on the Odyssey cluster supported by the FAS Division of Science, Research Computing Group at Harvard University. Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah.
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  • University of St Andrews Research
URI
http://hdl.handle.net/10023/20140

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