The ACIS instrument on board the Chandra X-ray Observatory has been used to carry out the first systematic study of low-mass X-ray binaries (LMXBs) in M87, the giant elliptical galaxy near the dynamical center of the Virgo Cluster. These images — having a total exposure time of 154 ks — are the deepest X-ray observations yet obtained of M87. We identify 174 X-ray point-sources, of which ∼ 150 are likely LMXBs. This LMXB catalog is combined with deep F475W and F850LP images taken with ACS on HST (as part of the ACS Virgo Cluster Survey) to examine the connection between LMXBs and globular clusters in M87. Of the 1688 globular clusters in our catalog, fX = 3.6±0.5% contain a LMXB. Dividing the globular cluster sample by metallicity, we find that the metal-rich clusters are 3±1 times more likely to harbor a LMXB than their metal-poor counterparts. In agreement with previous findings for other galaxies based on smaller LMXB samples, we find the efficiency of LMXB formation to scale with both cluster metallicity, Z, and luminosity, in the sense that brighter, more metal-rich clusters are more likely to contain a LMXB. For the first time, however, we are able to demonstrate that the probability, pX, that a given cluster will contain a LMXB depends sensitively on the dynamical properties of the host cluster. Specifically, we use the HST images to measure the half-light radius, concentration index and central density, ρ0, for each globular, and define a parameter, which is related to the tidal capture and binary-neutron star exchange rate. Our preferred form for pX is then pX ∝ρ−0.42±0.11 0 (Z/Z⊙)0.33±0.1. We argue that if the form of pX is determined by dynamical processes, then the observed metallicity dependence is a consequence of an increased number of neutron stars per unit mass in metal-rich globular clusters. Finally, we present a critical examination of the LMXB luminosity function in M87 and re-examine the published LMXB luminosity functions for M49 and NGC 4697. We find no compelling evidence for a break in the luminosity distribution of resolved X-ray point sources in any of these galaxies. Instead, the LMXB luminosity function in all three galaxies is well described by a power law with an upper cutoff at LX ∼ 1039 erg s−1 [for exact px and Lx forms, see attached document].

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Also archived in: arXiv: astro-ph/0405188 v2 6 Jun 2004 The authors thank Jack Hughes for illuminating discussions and Craig Heinke for useful comments. AJ extends his thanks to the UCSC Department of Astronomy & Astrophysics, and especially to Mike Bolte and Jean Brodie, for their hospitality while this paper was be- ing prepared. PC acknowledges support for this research provided by NASA LTSA grant NAG5-11714, funding for Chandra program CXC03400562, and funding for HST program GO-9401, through a grant from the Space Tele- scope Science Institute which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Additional support for AJ was provided by the National Science Foundation through a grant from the Association of Universities for Research in Astronomy, Inc., under NSF cooperative agreement AST-9613615, and by Fundacion Andes under project No.C-13442. DM acknowledges support from NSF grants AST 00-71099 and AST 02-0631 and from NASA grants NAG5-6037 and NAG5-9046.ISSN:1538-4357 Note: imported from RIT’s Digital Media Library running on DSpace to RIT Scholar Works in February 2014.

Document Type


Department, Program, or Center

School of Physics and Astronomy (COS)


RIT – Main Campus