The baryon budget on the galaxy group/cluster boundary
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Colleges, School and Institutes
- UNIVERSITY OF SOUTH FLORIDA
- Harvard-Smithsonian Center for Astrophysics
- University of Toronto
- Embry-Riddle Aeronautical University, Prescott, Arizona 86301 USA
- School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
We present a study of the hot gas and stellar content of five optically selected poor galaxy clusters, including a full accounting of the contribution from intracluster light (ICL) and a combined hot gas and hydrostatic X-ray mass analysis with XMM-Newton observations. We find weighted mean stellar (including ICL), gas and total baryon mass fractions within r of 0.026 ± 0.003, 0.070 ± 0.005 and 0.096 ± 0.006, respectively, at a corresponding weighted mean M of (1.08) × 10 M. Even when accounting for the intracluster stars, four out of five clusters show evidence for a substantial baryon deficit within r, with baryon fractions (f) between 50 ± 6 and 59 ± 8 per cent of the universal mean level (i.e. Ω/Ω), the remaining cluster having f = 75±11 per cent. For the three clusters where we can trace the hot halo to r we find no evidence for a steepening of the gas density profile in the outskirts with respect to a power law, as seen in more massive clusters. We find that in all cases, the X-ray mass measurements are larger than those originally published on the basis of the galaxy velocity dispersion (σ) and an assumed σ-M relation, by a factor of 1.7-5.7. Despite these increased masses, the stellar fractions (in the range 0.016-0.034, within r) remain consistent with the trend with mass published by Gonzalez et al., from which our sample is drawn.
Copyright 2013 Elsevier B.V., All rights reserved.
|Number of pages||17|
|Journal||Royal Astronomical Society. Monthly Notices|
|Publication status||Published - 11 Mar 2013|