Halo mass-observable proxy scaling relations and their dependencies on galaxy and group properties. (arXiv:2305.06803v1 [astro-ph.GA])

Halo mass-observable proxy scaling relations and their dependencies on galaxy and group properties. (arXiv:2305.06803v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_Z/0/1/0/all/0/1">Ziwen Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_H/0/1/0/all/0/1">Huiyuan Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Luo_W/0/1/0/all/0/1">Wentao Luo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mo_H/0/1/0/all/0/1">Houjun Mo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_J/0/1/0/all/0/1">Jun Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_X/0/1/0/all/0/1">Xiaohu Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_H/0/1/0/all/0/1">Hao Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_Q/0/1/0/all/0/1">Qinxun Li</a>

Based on the DECaLS shear catalog, we study the scaling relations between
halo mass($M_{rm h}$) and various proxies for SDSS central galaxies, including
stellar mass($M_*$), stellar velocity dispersion($sigma_*$), abundance
matching halo mass($M_{rm AM}$) and satellite velocity dispersion($sigma_{rm
s}$), and their dependencies on galaxy and group properties. In general, they
are all good proxies of $M_{rm h}$, and their scaling relations are consistent
with previous studies. We find that the $M_{rm h}$-$M_*$ and $M_{rm
h}$-$sigma_*$ relations depend strongly on group richness($N_{rm sat}$),
while the $M_{rm h}$-$M_{rm AM}$ and $M_{rm h}$-$sigma_{rm s}$ relations
are independent of it. Moreover, the dependence on star formation rate(SFR) is
rather weak in the $M_{rm h}$-$sigma_*$ and $M_{rm h}$-$sigma_{rm s}$
relations, but very prominent in the other two. $sigma_{rm s}$ is thus the
best proxy among them, and its scaling relation is in good agreement with
hydro-dynamical simulations. However, estimating $sigma_{rm s}$ accurately
for individual groups/clusters is challenging because of interlopers and the
requirement for sufficient satellites. We construct new proxies by combining
$M_*$, $sigma_*$, and $M_{rm AM}$, and find the proxy with 30% contribution
from $M_{rm AM}$ and 70% from $sigma_*$ can minimize the dependence on
$N_{rm sat}$ and SFR. We obtain the $M_{rm h}$-supermassive black hole(SMBH)
mass relation via the SMBH scaling relation and find indications for rapid and
linear growth phases for SMBH. We also find that correlations among $M_{rm
h}$, $M_*$ and $sigma_*$ change with $M_*$, indicating that different
processes drive the growth of galaxies and SMBH at different stages.

Based on the DECaLS shear catalog, we study the scaling relations between
halo mass($M_{rm h}$) and various proxies for SDSS central galaxies, including
stellar mass($M_*$), stellar velocity dispersion($sigma_*$), abundance
matching halo mass($M_{rm AM}$) and satellite velocity dispersion($sigma_{rm
s}$), and their dependencies on galaxy and group properties. In general, they
are all good proxies of $M_{rm h}$, and their scaling relations are consistent
with previous studies. We find that the $M_{rm h}$-$M_*$ and $M_{rm
h}$-$sigma_*$ relations depend strongly on group richness($N_{rm sat}$),
while the $M_{rm h}$-$M_{rm AM}$ and $M_{rm h}$-$sigma_{rm s}$ relations
are independent of it. Moreover, the dependence on star formation rate(SFR) is
rather weak in the $M_{rm h}$-$sigma_*$ and $M_{rm h}$-$sigma_{rm s}$
relations, but very prominent in the other two. $sigma_{rm s}$ is thus the
best proxy among them, and its scaling relation is in good agreement with
hydro-dynamical simulations. However, estimating $sigma_{rm s}$ accurately
for individual groups/clusters is challenging because of interlopers and the
requirement for sufficient satellites. We construct new proxies by combining
$M_*$, $sigma_*$, and $M_{rm AM}$, and find the proxy with 30% contribution
from $M_{rm AM}$ and 70% from $sigma_*$ can minimize the dependence on
$N_{rm sat}$ and SFR. We obtain the $M_{rm h}$-supermassive black hole(SMBH)
mass relation via the SMBH scaling relation and find indications for rapid and
linear growth phases for SMBH. We also find that correlations among $M_{rm
h}$, $M_*$ and $sigma_*$ change with $M_*$, indicating that different
processes drive the growth of galaxies and SMBH at different stages.

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