TY - JOUR
T1 - First Results on the Cluster Galaxy Population from the Subaru Hyper Suprime-Cam Survey. III. Brightest Cluster Galaxies, Stellar Mass Distribution, and Active Galaxies
AU - Lin, Yen Ting
AU - Hsieh, Bau Ching
AU - Lin, Sheng Chieh
AU - Oguri, Masamune
AU - Chen, Kai Feng
AU - Tanaka, Masayuki
AU - Chiu, I. Non
AU - Huang, Song
AU - Kodama, Tadayuki
AU - Leauthaud, Alexie
AU - More, Surhud
AU - Nishizawa, Atsushi J.
AU - Bundy, Kevin
AU - Lin, Lihwai
AU - Miyazaki, Satoshi
N1 - Funding Information:
The Hyper Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University.
Funding Information:
The PanSTARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under grant No.AST-1238877, the University of Maryland, and Eötvös Loránd University (ELTE), and the Los Alamos National Laboratory.
Funding Information:
We thank an anonymous referee for comments that helped improve the clarity of the paper. Y.T.L. thanks the Sesto Center for Astrophysics for the stimulating workshop “The remarkable life of a BCG” and Observatório Nacional in Rio de Janeiro for hospitality. Y.T.L. is grateful to Andrey Kravtsov, Roderik Overzier, Robert Lupton, Yi-Kuan Chiang, and Greg Rudnick for helpful comments. Y.T.L. acknowledges support from the Ministry of Science and Technology grants MOST104-2112-M-001-047 and MOST105-2112-M-001-028-MY3, and a Career Development Award (2017–2021) from Academia Sinica. This project received financial support from the Conselho Nacional de Desenvolvimento Científico e Tecnoló-gico (CNPq) through grant 400738/2014-7. Y.T.L. thanks I.H. and L.Y. for constant support and encouragement. This work was supported in part by the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and JSPS KAKENHI grant numbers 26800093 and 15H05892.
Funding Information:
Y.T.L. acknowledges support from the Ministry of Science and Technology grants MOST 104-2112-M-001-047 and MOST 105-2112-M-001-028-MY3, and a Career Development Award (2017-2021) from Academia Sinica. This project received financial support from the Conselho Nacional de Desenvolvimento Cientofico e Tecnologico (CNPq) through grant 400738/2014-7. Y.T.L. thanks I.H. and L.Y. for constant support and encouragement. This work was supported in part by the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and JSPS KAKENHI grant numbers 26800093 and 15H05892
Publisher Copyright:
© 2017. The American Astronomical Society. All rights reserved.
PY - 2017/12/20
Y1 - 2017/12/20
N2 - The unprecedented depth and area surveyed by the Subaru Strategic Program with the Hyper Suprime-Cam (HSCSSP) have enabled us to construct and publish the largest distant cluster sample out to z ∼ 1 to date. In this exploratory study of cluster galaxy evolution from z = 1 to z = 0.3, we investigate the stellar mass assembly history of brightest cluster galaxies (BCGs), the evolution of stellar mass and luminosity distributions, the stellar mass surface density profile, as well as the population of radio galaxies. Our analysis is the first high-redshift application of the top N richest cluster selection, which is shown to allow us to trace the cluster galaxy evolution faithfully. Over the 230 deg2 area of the current HSC-SSP footprint, selecting the top 100 clusters in each of the four redshift bins allows us to observe the buildup of galaxy population in descendants of clusters whose z ≈ 1 mass is about 2 × 1014 M⊙. Our stellar mass is derived from a machine-learning algorithm, which is found to be unbiased and accurate with respect to the COSMOS data. We find very mild stellar mass growth in BCGs (about 35% between z = 1 and 0.3), and no evidence for evolution in both the total stellar mass-cluster mass correlation and the shape of the stellar mass surface density profile. We also present the first measurement of the radio luminosity distribution in clusters out to z ∼ 1, and show hints of changes in the dominant accretion mode powering the cluster radio galaxies at z ∼ 0.8.
AB - The unprecedented depth and area surveyed by the Subaru Strategic Program with the Hyper Suprime-Cam (HSCSSP) have enabled us to construct and publish the largest distant cluster sample out to z ∼ 1 to date. In this exploratory study of cluster galaxy evolution from z = 1 to z = 0.3, we investigate the stellar mass assembly history of brightest cluster galaxies (BCGs), the evolution of stellar mass and luminosity distributions, the stellar mass surface density profile, as well as the population of radio galaxies. Our analysis is the first high-redshift application of the top N richest cluster selection, which is shown to allow us to trace the cluster galaxy evolution faithfully. Over the 230 deg2 area of the current HSC-SSP footprint, selecting the top 100 clusters in each of the four redshift bins allows us to observe the buildup of galaxy population in descendants of clusters whose z ≈ 1 mass is about 2 × 1014 M⊙. Our stellar mass is derived from a machine-learning algorithm, which is found to be unbiased and accurate with respect to the COSMOS data. We find very mild stellar mass growth in BCGs (about 35% between z = 1 and 0.3), and no evidence for evolution in both the total stellar mass-cluster mass correlation and the shape of the stellar mass surface density profile. We also present the first measurement of the radio luminosity distribution in clusters out to z ∼ 1, and show hints of changes in the dominant accretion mode powering the cluster radio galaxies at z ∼ 0.8.
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U2 - 10.3847/1538-4357/aa9bf5
DO - 10.3847/1538-4357/aa9bf5
M3 - Article
AN - SCOPUS:85039694766
VL - 851
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 139
ER -