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    The growth of brightest cluster galaxies and intracluster light over the past 10 billion years

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    Author
    DeMaio, Tahlia
    Gonzalez, Anthony H
    Zabludoff, Ann
    Zaritsky, Dennis
    Aldering, Greg
    Brodwin, Mark
    Connor, Thomas
    Donahue, Megan
    Hayden, Brian
    Mulchaey, John S
    Perlmutter, Saul
    Stanford, S A
    Show allShow less
    Affiliation
    Univ Arizona, Dept Astron, Steward Observ
    Issue Date
    2019-11-23
    Keywords
    galaxies: clusters: general
    galaxies: evolution
    
    Metadata
    Show full item record
    Publisher
    OXFORD UNIV PRESS
    Citation
    Tahlia DeMaio, Anthony H Gonzalez, Ann Zabludoff, Dennis Zaritsky, Greg Aldering, Mark Brodwin, Thomas Connor, Megan Donahue, Brian Hayden, John S Mulchaey, Saul Perlmutter, S A Stanford, The growth of brightest cluster galaxies and intracluster light over the past 10 billion years, Monthly Notices of the Royal Astronomical Society, Volume 491, Issue 3, January 2020, Pages 3751–3759, https://doi.org/10.1093/mnras/stz3236
    Journal
    MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
    Rights
    © 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    We constrain the evolution of the brightest cluster galaxy plus intracluster light (BCG + ICL) using an ensemble of 42 galaxy groups and clusters that span redshifts of z = 0.05-1.75 and masses of M-500,M-c = 2 x 10(13)-10(15) M-circle dot. Specifically, we measure the relationship between the BCG + ICL stellar mass M-star and M-500,M-c at projected radii 10 < r < 100 kpc for three different epochs. At intermediate redshift ((z) over bar = 0.40), where we have the best data, we find M-star M-500,c(0.48 +/- 0.06). Fixing the exponent of this power law for all redshifts, we constrain the normalization of this relation to be 2.08 +/- 0.21 times higher at (z) over bar = 0.40 than at high redshift ((z) over bar = 1.55). We find no change in the relation from intermediate to low redshift ((z) over bar = 0.10). In other words, for fixed M-500,M-c, M-star at 10 < r < 100 kpc increases from (z) over bar = 1.55 to (z) over bar = 0.40 and not significantly thereafter. Theoretical models predict that the physical mass growth of the cluster from z = 1.5 to z = 0 within r(500,c) is 1.4x, excluding evolution due to definition of r(500,c). We find that M-star within the central 100 kpc increases by similar to 3.8x over the same period. Thus, the growth of M-star in this central region is more than a factor of 2 greater than the physical mass growth of the cluster as a whole. Furthermore, the concentration of the BCG + ICL stellar mass, defined by the ratio of stellar mass within 10 kpc to the total stellar mass within 100 kpc, decreases with increasing M-500,M-c at all z. We interpret this result as evidence for inside-out growth of the BCG + ICL over the past 10 Gyr, with stellar mass assembly occurring at larger radii at later times.
    ISSN
    0035-8711
    DOI
    10.1093/mnras/stz3236
    Version
    Final published version
    ae974a485f413a2113503eed53cd6c53
    10.1093/mnras/stz3236
    Scopus Count
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    UA Faculty Publications

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