Halo Radius (Splashback Radius) of Groups and Clusters of Galaxies on Small Scales
Astrophysical Bulletin(2023)
摘要
We report the results of a study of the distribution of galaxies in the projection along the radius (
$$R \leqslant 3{{R}_{{200{\text{c}}}}}$$
) for 157 groups and clusters of galaxies in the local Universe (0.01 <
$$z$$
< 0.10) with line-of-sight velocity dispersions 200 <
$$\sigma $$
< 1100 km s–1. We introduce a new observed boundary for the halos of clusters of galaxies, which we identify with the splashback radius
$${{R}_{{{\text{sp}}}}}$$
. We also identified the core of groups/clusters of galaxies with the radius
$${{R}_{{\text{c}}}}$$
. These radii are determined by the observed integrated distribution of the number of galaxies as a function of squared angular radius from the center of the group/cluster, which (usually) coincides with the brightest galaxy. We found for the entire sample that the boundary of dark matter
$${{R}_{{{\text{sp}}}}}$$
for groups/clusters of galaxies is proportional to the radius
$${{R}_{{{\text{200}}}}}$$
of the virialized region. We measured the mean radius
$$\langle {{R}_{{{\text{sp}}}}}\rangle = 1.14 \pm 0.02$$
Mpc for groups of galaxies (
$$\sigma \leqslant 400$$
km s–1) and
$$\langle {{R}_{{{\text{sp}}}}}\rangle = 2.00 \pm 0.07$$
Mpc for clusters of galaxies (
$$\sigma > 400$$
km s–1). The mean ratio of radii is
$$\langle {{{{R}_{{{\text{sp}}}}}} \mathord{\left/ {\vphantom {{{{R}_{{{\text{sp}}}}}} {{{R}_{{{\text{200c}}}}}}}} \right. \kern-0em} {{{R}_{{{\text{200c}}}}}}}\rangle = 1.40 \pm 0.02$$
, or
$$\langle {{{{R}_{{{\text{sp}}}}}} \mathord{\left/ {\vphantom {{{{R}_{{{\text{sp}}}}}} {{{R}_{{{\text{200m}}}}}}}} \right. \kern-0em} {{{R}_{{{\text{200m}}}}}}}\rangle = 0.88 \pm 0.02$$
.
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关键词
galaxies: groups and clusters:, general—galaxies: evolution—cosmology: large-scale structure of the Universe
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