The different growth pathways of brightest cluster galaxies and intracluster light

E. Contini, S. K. Yi, X. Kang

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18 Citations (Scopus)

Abstract

We study the growth pathways of brightest central galaxies (BCGs) and intracluster light (ICL) by means of a semi-analytic model. We assume that ICL forms by stellar stripping of satellite galaxies and violent processes during mergers, and implement two independent models: One considers bothmergers and stellar stripping (named STANDARDmodel), and the other considers only mergers (named MERGERS model). We find that BCGs and ICL form, grow, and overall evolve at different times and with different time-scales, but they show a clear coevolution after redshift z ~ 0.7-0.8. Around 90 per cent of the ICL from stellar stripping is built up in the innermost 150 kpc from the halo centre and the dominant contribution comes from disc-like galaxies (B/T < 0.4) through a large number of small/intermediate stripping events (Mstrip/Msat < 0.3). The fractions of stellar mass in BCGs and in the ICL over the total stellar mass within the virial radius of the halo evolve differently with time. At high redshift, the BCG accounts for the bulk of the mass, but its contribution gradually decreases with time and stays constant after z ~ 0.4-0.5. The ICL, instead, grows very fast and its contribution keeps increasing down to the present time. The STANDARD and MERGERS models make very similar predictions in most of the cases, but predict different amounts of ICL associated with galaxies within the virial radius of the group/cluster other than the BCG, at z =0.We then suggest that this quantity is a valid observable that can shed light on the relative importance of mergers and stellar stripping for the formation of ICL.

Original languageEnglish
Pages (from-to)932-944
Number of pages13
JournalMonthly Notices of the Royal Astronomical Society
Volume479
Issue number1
DOIs
Publication statusPublished - 2018 Sep 1

Bibliographical note

Funding Information:
We thank the anonymous referee for comments and suggestions that improved the manuscript. S.K.Y. and E.C. acknowledge support from the Korean National Research Foundation (NRF-2017R1A2A1A05001116) and from the Brain Korea 21 Plus Program (21A20131500002). This study was performed under the umbrella of the joint collaboration between Yonsei University Observatory and the Korean Astronomy and Space Science Institute. X.K. acknowledges financial support by the 973 Program (2015CB857003) and the NSFC (No.11333008).

Publisher Copyright:
© 2018 The Author(s). Published by Oxford University Press on behalf of The Royal Astronomical Society.

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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