The baryon budget on the galaxy group/cluster boundary
  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.
