Exploring the diversity of groups at 0.1 <z <0.8 with X-ray and optically selected samples

J.L. Connelly, D.J. Wilman, A. Finoguenov, A. Hou, J.S. Mulchaey, S.L. McGee, M. Balogh, L.C. Parker, R. Saglia, R.D.E. Henderson, R.G. Bower

Research output: Contribution to journalArticlepeer-review

25 Citations (Scopus)

Abstract

We present the global group properties of two samples of galaxy groups containing 39 high-quality X-ray-selected systems and 38 optically (spectroscopically) selected systems in coincident spatial regions at 0.12 < z < 0.79. The total mass range of the combined sample is ~(1012-5) × 1014 M. Only nine optical systems are associable with X-ray systems. We discuss the confusion inherent in the matching of both galaxies to extended X-ray emission and of X-ray emission to already identified optical systems. Extensive spectroscopy has been obtained and the resultant redshift catalog and group membership are provided here. X-ray, dynamical, and total stellar masses of the groups are also derived and presented. We explore the effects of utilizing different centers and applying three different kinds of radial cut to our systems: a constant cut of 1 Mpc and two r200 cuts, one based on the velocity dispersion of the system and the other on the X-ray emission. We find that an X-ray-based r200 results in less scatter in scaling relations and less dynamical complexity as evidenced by results of the Anderson-Darling and Dressler-Schectman tests, indicating that this radius tends to isolate the virialized part of the system. The constant and velocity dispersion based cuts can overestimate membership and can work to inflate velocity dispersion and dynamical and stellar mass. We find L-σ and Mstellar-LX scaling relations for X-ray and optically selected systems are not dissimilar. The mean fraction of mass found in stars, excluding intracluster light, for our systems is ~0.014 with a logarithmic standard deviation of 0.398 dex. We also define and investigate a sample of groups which are X-ray underluminous given the total group stellar mass. For these systems the fraction of stellar mass contributed by the most massive galaxy is typically lower than that found for the total population of groups implying that there may be less intragroup medium contributed from the most massive member in these systems. Eighty percent of 15 underluminous groups have less than 40% of their stellar mass in the most massive galaxy which happens in less than 1% of cases with samples matched in stellar mass, taken from the combined group catalog.
Original languageEnglish
Article number139
Number of pages27
JournalThe Astrophysical Journal
Volume756
Issue number2
DOIs
Publication statusPublished - 10 Sep 2012

Bibliographical note

Export Date: 15 August 2017

Correspondence Address: Connelly, J.L.; Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, D-85748 Garching, Germany

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Keywords

  • galaxies: groups: general
  • X-rays: galaxies: clusters

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