The HectoMAP Cluster Survey: Spectroscopically Identified Clusters and their Brightest Cluster Galaxies (BCGs)

Sohn, Jubee; Geller, Margaret J.; Hwang, Ho Seong; Diaferio, Antonaldo; Rines, Kenneth J.; Utsumi, Yousuke

doi:10.3847/1538-4357/ac29c3

Title: The HectoMAP Cluster Survey: Spectroscopically Identified Clusters and their Brightest Cluster Galaxies (BCGs)

Journal Article · Thu Dec 16 00:00:00 EST 2021 · The Astrophysical Journal

DOI:https://doi.org/10.3847/1538-4357/ac29c3· OSTI ID:1867892

^[1];

^[2];

^[3]; Rines, Kenneth J. ^[4];

^[5]

Smithsonian Astrophysical Observatory, Cambridge, MA (United States)
Seoul National Univ. (South Korea); Seoul National Univ. (South Korea). SNU Astronomy Research Center
Univ. di Torino (Italy); Istituto Nazionale di Fisica Nucleare (INFN), Torino (Italy)
Western Washington Univ., Bellingham, WA (United States)
Stanford Univ., CA (United States). Kavli Institute for Particle Astrophysics & Cosmology; SLAC National Accelerator Lab., Menlo Park, CA (United States)

We apply a friends-of-friends (FoF) algorithm to identify galaxy clusters and we use the catalog to explore the evolutionary synergy between brightest cluster galaxies (BCGs) and their host clusters. We base the cluster catalog on the dense HectoMAP redshift survey (2000 redshifts deg^-2). The HectoMAP FoF catalog includes 346 clusters with 10 or more spectroscopic members within the range 0.05 < z < 0.55 and with a median z = 0.29. We list these clusters and their members. We also include central velocity dispersions (σ*,_BCG) for the FoF cluster BCGs, a distinctive feature of the HectoMAP FoF catalog. HectoMAP clusters with higher galaxy number density (80 systems) are all genuine clusters with a strong concentration and a prominent BCG in Subaru/Hyper Suprime-Cam images. The phase-space diagrams show the expected elongation along the line of sight. Lower-density systems include some low reliability systems. We establish a connection between BCGs and their host clusters by demonstrating that σ*,_BCG/σ_cl decreases as a function of cluster velocity dispersion (σ_cl), in contrast, numerical simulations predict a constant σ*,_BCG/σ_cl. Sets of clusters at two different redshifts show that BCG evolution in massive systems is slow over the redshift range z < 0.4. The data strongly suggest that minor mergers may play an important role in BCG evolution in clusters with σ_cl ≳ 300 km s^-1. For lower mass systems (σ_cl< 300 km s^-1), major mergers may play a significant role. The coordinated evolution of BCGs and their host clusters provides an interesting test of simulations in high-density regions of the universe.

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Research Organization:: SLAC National Accelerator Lab., Menlo Park, CA (United States)

Sponsoring Organization:: USDOE Office of Science (SC), Basic Energy Sciences (BES); Italian Ministry of Education, University and Research (MIUR)

Grant/Contract Number:: AC02-76SF00515; L.232/2016

OSTI ID:: 1867892

Journal Information:: The Astrophysical Journal, Vol. 923, Issue 2; ISSN 0004-637X

Publisher:: IOP PublishingCopyright Statement

Country of Publication:: United States

Language:: English

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