Mass accretion rate of clusters of galaxies: CIRS and HeCS. (arXiv:2005.11562v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Pizzardo_M/0/1/0/all/0/1">M. Pizzardo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gioia_S/0/1/0/all/0/1">S. Di Gioia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diaferio_A/0/1/0/all/0/1">A. Diaferio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boni_C/0/1/0/all/0/1">C. De Boni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Serra_A/0/1/0/all/0/1">A. L. Serra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Geller_M/0/1/0/all/0/1">M. J. Geller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sohn_J/0/1/0/all/0/1">J. Sohn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rines_K/0/1/0/all/0/1">K. Rines</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baldi_M/0/1/0/all/0/1">M. Baldi</a>
We use a new spherical accretion recipe tested on N-body simulations to
measure the observed mass accretion rate (MAR) of 129 clusters in the Cluster
Infall Regions in the Sloan Digital Sky Survey (CIRS) and in the Hectospec
Cluster Survey (HeCS). The observed clusters cover the redshift range of
$0.01<z<0.30$ and the mass range of $sim 10^{14}-10^{15}h^{-1}$~M$_odot$.
Based on three-dimensional mass profiles of simulated clusters reaching beyond
the virial radius, our recipe returns MARs that agree with MARs based on merger
trees. We adopt this recipe to estimate the MAR of real clusters based on
measurements of the mass profile out to $sim 3R_{200}$. We use the caustic
method to measure the mass profiles to these large radii. We demonstrate the
validity of our estimates by applying the same approach to a set of mock
redshift surveys of a sample of 2000 simulated clusters with a median mass of
$M_{200}= 10^{14} {h^{-1}~rm{M_{odot}}}$ as well as a sample of 50 simulated
clusters with a median mass of $M_{200}= 10^{15} {h^{-1}~rm{M_{odot}}}$: the
median MARs based on the caustic mass profiles of the simulated clusters are
unbiased and agree within 19% with the median MARs based on the real mass
profile of the clusters. The MAR of the CIRS and HeCS clusters increases with
the mass and the redshift of the accreting cluster, which is in excellent
agreement with the growth of clusters in the $Lambda$CDM model.
We use a new spherical accretion recipe tested on N-body simulations to
measure the observed mass accretion rate (MAR) of 129 clusters in the Cluster
Infall Regions in the Sloan Digital Sky Survey (CIRS) and in the Hectospec
Cluster Survey (HeCS). The observed clusters cover the redshift range of
$0.01<z<0.30$ and the mass range of $sim 10^{14}-10^{15}h^{-1}$~M$_odot$.
Based on three-dimensional mass profiles of simulated clusters reaching beyond
the virial radius, our recipe returns MARs that agree with MARs based on merger
trees. We adopt this recipe to estimate the MAR of real clusters based on
measurements of the mass profile out to $sim 3R_{200}$. We use the caustic
method to measure the mass profiles to these large radii. We demonstrate the
validity of our estimates by applying the same approach to a set of mock
redshift surveys of a sample of 2000 simulated clusters with a median mass of
$M_{200}= 10^{14} {h^{-1}~rm{M_{odot}}}$ as well as a sample of 50 simulated
clusters with a median mass of $M_{200}= 10^{15} {h^{-1}~rm{M_{odot}}}$: the
median MARs based on the caustic mass profiles of the simulated clusters are
unbiased and agree within 19% with the median MARs based on the real mass
profile of the clusters. The MAR of the CIRS and HeCS clusters increases with
the mass and the redshift of the accreting cluster, which is in excellent
agreement with the growth of clusters in the $Lambda$CDM model.
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