Logo Logo
Switch Language to German

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. and Erfanianfar, Ghazaleh (2019): Chandra centres for COSMOS X-ray galaxy groups: differences in stellar properties between central dominant and offset brightest group galaxies. In: Monthly Notices of the Royal Astronomical Society, Vol. 483, No. 3: pp. 3545-3565

Full text not available from 'Open Access LMU'.


We present the results of a search for galaxy clusters and groups in the similar to 2 deg(2) 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 x 10(-16) erg cm(-2) s(-1) in the 0.5-2 keV range, and identify 247 X-ray groups with M-200c = 8 x 10(12)-3 x 10(14)M(circle dot) 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 similar to 0.3 dex.

Actions (login required)

View Item View Item