The Massive and Distant Clusters of WISE Survey XI: Stellar Mass Fractions and Luminosity Functions of MaDCoWS Clusters at $z sim 1$. (arXiv:2112.12239v1 [astro-ph.GA])

The Massive and Distant Clusters of WISE Survey XI: Stellar Mass Fractions and Luminosity Functions of MaDCoWS Clusters at $z sim 1$. (arXiv:2112.12239v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Decker_B/0/1/0/all/0/1">Bandon Decker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brodwin_M/0/1/0/all/0/1">Mark Brodwin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Saha_R/0/1/0/all/0/1">Ripon Saha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Connor_T/0/1/0/all/0/1">Thomas Connor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eisenhardt_P/0/1/0/all/0/1">Peter R. M. Eisenhardt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_A/0/1/0/all/0/1">Anthony H. Gonzalez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moravec_E/0/1/0/all/0/1">Emily Moravec</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muhibullah_M/0/1/0/all/0/1">Mustafa Muhibullah</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stanford_S/0/1/0/all/0/1">S. Adam Stanford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stern_D/0/1/0/all/0/1">Daniel Stern</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thongkham_K/0/1/0/all/0/1">Khunanon Thongkham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wylezalek_D/0/1/0/all/0/1">Dominika Wylezalek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dicker_S/0/1/0/all/0/1">Simon R. Dicker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mason_B/0/1/0/all/0/1">Brian Mason</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mroczkowski_T/0/1/0/all/0/1">Tony Mroczkowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romero_C/0/1/0/all/0/1">Charles E. Romero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruppin_F/0/1/0/all/0/1">Florian Ruppin</a>

We present stellar mass fractions and composite luminosity functions (LFs)
for a sample of Ncl clusters from the Massive and Distant Clusters of WISE
Survey (MaDCoWS) at a redshift range of $0.951 leq z leq 1.43$. Using SED
fitting of optical and deep mid-infrared photometry, we establish the
membership of objects along the lines-of-sight to these clusters and calculate
the stellar masses of member galaxies. We find stellar mass fractions for these
clusters largely consistent with previous works, including appearing to display
a negative correlation with total cluster mass. We measure a composite
$3.6~mathrm{mu m}$ LF down to $m^*+2.5$ for all 12 clusters. Fitting a
Schechter function to the LF, we find a characteristic $3.6~mathrm{mu m}$
magnitude of $m^*=19.83pm0.12$ and faint-end slope of $alpha=-0.81pm0.10$
for the full sample at a mean redshift of $bar{z} = 1.18$. We also divide the
clusters into high- and low-redshift bins at $bar{z}=1.29$ and $bar{z}=1.06$
respectively and measure a composite LF for each bin. We see a small, but
statistically significant evolution in $m^*$ and $alpha$ — consistent with
passive evolution — when we study the joint fit to the two parameters, which
is probing the evolution of faint cluster galaxies at $zsim1$. This highlights
the importance of deep IR data in studying the evolution of cluster galaxy
populations at high-redshift.

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