Chandra centres for COSMOS X-ray galaxy groups : differences in stellar properties between central dominant and offset brightest group galaxies

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Gozaliasl , G , Finoguenov , A , Tanaka , M , Dolag , K , Montanari , F , Kirkpatrick , C C , Vardoulaki , E , Khosroshahi , H G , Salvato , M , Laigle , C , McCracken , H J , Ilbert , O , Cappelluti , N , Daddi , E , Hasinger , G , Capak , P , Scoville , N Z , Toft , S , Civano , F , Griffiths , R E , Balogh , M , Li , Y , Ahoranta , J , Mei , S , Iovino , A , Henriques , B M B & Erfanianfar , G 2019 , ' Chandra centres for COSMOS X-ray galaxy groups : differences in stellar properties between central dominant and offset brightest group galaxies ' , Monthly Notices of the Royal Astronomical Society , vol. 483 , no. 3 , pp. 3545-3565 . https://doi.org/10.1093/mnras/sty3203

Title: Chandra centres for COSMOS X-ray galaxy groups : differences in stellar properties between central dominant and offset brightest group galaxies
Author: Gozaliasl, Ghassem; Finoguenov, Alexis; Tanaka, Masayuki; Dolag, Klaus; Montanari, Francesco; Kirkpatrick, Charles C.; Vardoulaki, Eleni; Khosroshahi, Habib G.; Salvato, Mara; Laigle, Clotilde; McCracken, Henry J.; Ilbert, Olivier; Cappelluti, Nico; Daddi, Emanuele; Hasinger, Guenther; Capak, Peter; Scoville, Nick Z.; Toft, Sune; Civano, Francesca; Griffiths, Richard E.; Balogh, Michael; Li, Yanxia; Ahoranta, Jussi; Mei, Simona; Iovino, Angela; Henriques, Bruno M. B.; Erfanianfar, Ghazaleh
Contributor organization: Department of Physics
Helsinki Institute of Physics
Particle Physics and Astrophysics
Date: 2019-03
Language: eng
Number of pages: 21
Belongs to series: Monthly Notices of the Royal Astronomical Society
ISSN: 0035-8711
DOI: https://doi.org/10.1093/mnras/sty3203
URI: http://hdl.handle.net/10138/300793
Abstract: We present the results of a search for galaxy clusters and groups in the ∼2 deg2 of the COSMOS field using all available X-ray observations from the XMM-Newton and Chandra observatories.We reach an X-ray flux limit of 3 × 10−16 erg cm−2 s−1 in the 0.5-2 keV range, and identify 247 X-ray groups with M200c = 8 × 1012-3 × 1014M at a redshift range of 0.08 ≤ z < 1.53, using the multiband photometric redshift and the master spectroscopic redshift catalogues of the COSMOS. The X-ray centres of groups are determined using high-resolution Chandra imaging. We investigate the relations between the offset of the brightest group galaxies (BGGs) from halo X-ray centre and group properties and compare with predictions from semi-analytic models and hydrodynamical simulations. We find that BGG offset decreases with both increasing halo mass and decreasing redshift with no strong dependence on the X-ray flux and SNR. We show that the BGG offset decreases as a function of increasing magnitude gap with no considerable redshift-dependent trend. The stellar mass of BGGs in observations extends over a wider dynamic range compared to model predictions. At z < 0.5, the central dominant BGGs become more massive than those with large offsets by up to 0.3 dex, in agreement with model prediction. The observed and predicted log-normal scatter in the stellar mass of both low- and large-offset BGGs at fixed halo mass is ∼0.3 dex.
Subject: galaxies: clusters: general
galaxies: evolution
galaxies: groups: general
galaxies: statistics
galaxies: stellar content
X-rays: galaxies: clusters
STAR-FORMATION RATES
HALO MASS RELATION
CLUSTER GALAXIES
DARK-MATTER
PHOTOMETRIC REDSHIFTS
PLANCK COSMOLOGY
FOSSIL GROUPS
EVOLUTION
SIMULATIONS
I.
115 Astronomy, Space science
Peer reviewed: Yes
Rights: unspecified
Usage restriction: openAccess
Self-archived version: publishedVersion


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