Alastair J. R. Sanderson, Ewan O'Sullivan, Trevor J. Ponman, Anthony H. Gonzalez, Suresh Sivanandam, Ann I. Zabludoff, Dennis Zaritsky
We present a study of the hot gas and stellar content of 5 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 observations. We find weighted mean stellar (including ICL), gas and total baryon mass fractions within r500 of 0.026+/-0.003, 0.070+/-0.005 and 0.096+/-0.006, respectively, at a corresponding weighted mean M500 of (1.08_{-0.18}^{+0.21}) x 10^14 Msun. Even when accounting for the intracluster stars, 4 out of 5 clusters show evidence for a substantial baryon deficit within r500, with baryon fractions (f_bary) between 50+/-6 to 59+/-8 per cent of the Universal mean level (i.e. Omega_b / Omega_m); the remaining cluster having f_bary = 75+/-11 per cent. For the 3 clusters where we can trace the hot halo to r500 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 (sigma) and an assumed sigma-M500 relation, by a factor of 1.7-5.7. Despite these increased masses, the stellar fractions (in the range 0.016-0.034, within r500) remain consistent with the trend with mass published by Gonzalez, Zaritsky & Zabludoff (2007), from which our sample is drawn.
View original:
http://arxiv.org/abs/1212.1613
No comments:
Post a Comment