HSC-XXL: Baryon budget of the 136 XXL groups and clusters

被引:37
作者
Akino, Daichi [1 ]
Eckert, Dominique [2 ]
Okabe, Nobuhiro [1 ,3 ,4 ]
Sereno, Mauro [5 ,6 ]
Umetsu, Keiichi [7 ]
Oguri, Masamune [8 ,9 ,10 ]
Gastaldello, Fabio [11 ]
Chiu, I-Non [7 ]
Ettori, Stefano [5 ,6 ]
Evrard, August E. [12 ,13 ,14 ]
Farahi, Arya [12 ,13 ,14 ]
Maughan, Ben [15 ]
Pierre, Marguerite [16 ]
Ricci, Marina [17 ]
Valtchanov, Ivan [18 ]
McCarthy, Ian [19 ]
McGee, Sean [20 ]
Miyazaki, Satoshi [21 ]
Nishizawa, Atsushi J. [22 ]
Tanaka, Masayuki [21 ]
机构
[1] Hiroshima Univ, Grad Sch Adv Sci & Engn, Phys Program, 1-3-1 Kagamiyama, Higashihiroshima, Hiroshima 7398526, Japan
[2] Univ Geneva, Dept Astron, Ch dEcogia 16, CH-1290 Versoix, Switzerland
[3] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, 1-3-1 Kagamiyama, Higashihiroshima, Hiroshima 7398526, Japan
[4] Hiroshima Univ, Core Res Energet Universe, 1-3-1 Kagamiyama, Higashihiroshima, Hiroshima 7398526, Japan
[5] INAF, Osservatorio Astrofis & Sci Spazio Bologna, Via Piero Gobetti 93-3, I-40129 Bologna, Italy
[6] Ist Nazl Fis Nucl, Sez Bologna, Viale Berti Pichat 6-2, I-40127 Bologna, Italy
[7] Acad Sinica, Inst Astron & Astrophys ASIAA, 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan
[8] Univ Tokyo, Res Ctr Early Universe, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan
[9] Univ Tokyo, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan
[10] Univ Tokyo, Kavli Inst Phys & Math Universe Kavli IPMU, WPI, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan
[11] INAF IASF Milano, Via Bassini 15, I-20133 Milan, Italy
[12] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA
[13] Univ Michigan, Michigan Ctr Theoret Phys, Ann Arbor, MI 48109 USA
[14] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Dept Phys, Pittsburgh, PA 15213 USA
[15] Univ Bristol, HH Wills Phys Lab, Tyndall Ave, Bristol BS8 1TL, Avon, England
[16] Univ Paris Diderot, Univ Paris Saclay, Sorbonne Paris Cite, CNRS,CEA,AIM, F-91191 Gif Sur Yvette, France
[17] Univ Savoie Mt Blanc, Lab Annecy Phys Particules, CNRS IN2P3, F-74941 Annecy, France
[18] European Space Astron Ctr, Operat Dept, Telespazio UK ESA, E-28691 Villanueva De La Canada, Spain
[19] Liverpool John Moores Univ, Astrophys Res Inst, 146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England
[20] Univ Birmingham, Sch Astron & Phys, Birmingham B15 2TT, W Midlands, England
[21] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan
[22] Nagoya Univ, Inst Adv Res, Chikusa Ku, Furocho, Nagoya, Aichi 4648602, Japan
基金
美国国家科学基金会; 日本学术振兴会; 日本科学技术振兴机构; 美国国家航空航天局;
关键词
galaxies: clusters: intracluster medium; galaxies: stellar content; gravitational lensing: weak; X-rays: galaxies: clusters; MASSIVE GALAXY CLUSTERS; SHEAR-SELECTED CLUSTERS; RAY-SELECTED CLUSTERS; SURVEYS 1ST RELEASE; X-RAY; STELLAR MASS; SCALING RELATIONS; HYDRODYNAMICAL SIMULATIONS; LUMINOSITY FUNCTION; LINEAR-REGRESSION;
D O I
10.1093/pasj/psab115
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present our determination of the baryon budget for an X-ray-selected XXL sample of 136 galaxy groups and clusters spanning nearly two orders of magnitude in mass (M-500 similar to 10(13)-10(15) M-circle dot) and the redshift range 0 less than or similar to z less than or similar to 1. Our joint analysis is based on the combination of Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) weak-lensing mass measurements, XXL X-ray gas mass measurements, and HSC and Sloan Digital Sky Survey multiband photometry. We carry out a Bayesian analysis of multivariate mass-scaling relations of gas mass, galaxy stellar mass, stellar mass of brightest cluster galaxies (BCGs), and soft-band X-ray luminosity, by taking into account the intrinsic covariance between cluster properties, selection effect, weak-lensing mass calibration, and observational error covariance matrix. The mass-dependent slope of the gas mass-total mass (M-500) relation is found to be 1.29(-0.10)(+0.16), which is steeper than the self-similar prediction of unity, whereas the slope of the stellar mass-total mass relation is shallower than unity; 0.85(-0.09)(+0.12). The BCG stellar mass weakly depends on cluster mass with a slope of 0.49(-0.10)(+0.11). The baryon, gas mass, and stellar mass fractions as a function of M-500 agree with the results from numerical simulations and previous observations. We successfully constrain the full intrinsic covariance of the baryonic contents. The BCG stellar mass shows the larger intrinsic scatter at a given halo total mass, followed in order by stellar mass and gas mass. We find a significant positive intrinsic correlation coefficient between total (and satellite) stellar mass and BCG stellar mass and no evidence for intrinsic correlation between gas mass and stellar mass. All the baryonic components show no redshift evolution.
引用
收藏
页码:175 / 208
页数:34
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