We simulate the phase-space distribution of stellar mass in 9 massive
Lambda-CDM galaxy clusters by applying the semi-analytic particle tagging
method of Cooper et al. to the Phoenix suite of high-resolution N-body
simulations (M200 = 7.5 to 33 x 10^14 Msol). The resulting surface brightness
(SB) profiles of brightest cluster galaxies (BCGs) match well to observations.
On average, stars formed in galaxies accreted by the BCG account for ~90 per
cent of its total mass (the remainder is formed in situ). In circular
BCG-centred apertures, the superposition of multiple debris clouds (each ~10
per cent of the total BCG mass) from different progenitors can result in an
extensive outer diffuse component, qualitatively similar to a 'cD envelope'.
These clouds typically originate from tidal stripping at z < 1 and comprise
both streams and the extended envelopes of other massive galaxies in the
cluster. The faint regions of the BCG contribute a significant part of the
total cluster stellar mass budget: in the central 1 Mpc^2 of a z ~ 0.15 cluster
imaged at SDSS-like resolution, our fiducial model predicts 80-95 per cent of
stellar mass below a SB of mu_V = 26.5 mag arcsec^2 is associated with accreted
stars in the envelope of the BCG.The ratio of BCG stellar mass to total cluster
stellar mass is ~30 per cent.
Описание
[1407.5627] Surface photometry of BCGs and intracluster stars in Lambda-CDM
%0 Generic
%1 cooper2014surface
%A Cooper, Andrew P.
%A Gao, Liang
%A Guo, Qi
%A Frenk, Carlos S.
%A Jenkins, Adrian
%A Springel, Volker
%A White, Simon D. M.
%D 2014
%K central cluster galaxy
%T Surface photometry of BCGs and intracluster stars in Lambda-CDM
%U http://arxiv.org/abs/1407.5627
%X We simulate the phase-space distribution of stellar mass in 9 massive
Lambda-CDM galaxy clusters by applying the semi-analytic particle tagging
method of Cooper et al. to the Phoenix suite of high-resolution N-body
simulations (M200 = 7.5 to 33 x 10^14 Msol). The resulting surface brightness
(SB) profiles of brightest cluster galaxies (BCGs) match well to observations.
On average, stars formed in galaxies accreted by the BCG account for ~90 per
cent of its total mass (the remainder is formed in situ). In circular
BCG-centred apertures, the superposition of multiple debris clouds (each ~10
per cent of the total BCG mass) from different progenitors can result in an
extensive outer diffuse component, qualitatively similar to a 'cD envelope'.
These clouds typically originate from tidal stripping at z < 1 and comprise
both streams and the extended envelopes of other massive galaxies in the
cluster. The faint regions of the BCG contribute a significant part of the
total cluster stellar mass budget: in the central 1 Mpc^2 of a z ~ 0.15 cluster
imaged at SDSS-like resolution, our fiducial model predicts 80-95 per cent of
stellar mass below a SB of mu_V = 26.5 mag arcsec^2 is associated with accreted
stars in the envelope of the BCG.The ratio of BCG stellar mass to total cluster
stellar mass is ~30 per cent.
@misc{cooper2014surface,
abstract = {We simulate the phase-space distribution of stellar mass in 9 massive
Lambda-CDM galaxy clusters by applying the semi-analytic particle tagging
method of Cooper et al. to the Phoenix suite of high-resolution N-body
simulations (M200 = 7.5 to 33 x 10^14 Msol). The resulting surface brightness
(SB) profiles of brightest cluster galaxies (BCGs) match well to observations.
On average, stars formed in galaxies accreted by the BCG account for ~90 per
cent of its total mass (the remainder is formed in situ). In circular
BCG-centred apertures, the superposition of multiple debris clouds (each ~10
per cent of the total BCG mass) from different progenitors can result in an
extensive outer diffuse component, qualitatively similar to a 'cD envelope'.
These clouds typically originate from tidal stripping at z < 1 and comprise
both streams and the extended envelopes of other massive galaxies in the
cluster. The faint regions of the BCG contribute a significant part of the
total cluster stellar mass budget: in the central 1 Mpc^2 of a z ~ 0.15 cluster
imaged at SDSS-like resolution, our fiducial model predicts 80-95 per cent of
stellar mass below a SB of mu_V = 26.5 mag arcsec^2 is associated with accreted
stars in the envelope of the BCG.The ratio of BCG stellar mass to total cluster
stellar mass is ~30 per cent.},
added-at = {2014-07-23T09:39:00.000+0200},
author = {Cooper, Andrew P. and Gao, Liang and Guo, Qi and Frenk, Carlos S. and Jenkins, Adrian and Springel, Volker and White, Simon D. M.},
biburl = {https://www.bibsonomy.org/bibtex/245dcb75913150f5bf3aa8e8c85233a8d/miki},
description = {[1407.5627] Surface photometry of BCGs and intracluster stars in Lambda-CDM},
interhash = {911ad6ef0a73fd700f7ecb9583a7a125},
intrahash = {45dcb75913150f5bf3aa8e8c85233a8d},
keywords = {central cluster galaxy},
note = {cite arxiv:1407.5627Comment: Submitted to MNRAS; 17 pages, 16 figures (appendix 2 pages, 3 figures)},
timestamp = {2014-07-23T09:39:00.000+0200},
title = {Surface photometry of BCGs and intracluster stars in Lambda-CDM},
url = {http://arxiv.org/abs/1407.5627},
year = 2014
}