We present characteristics of the X-ray point source population in the M84 galaxy , observed by Chandra ACIS-S. We find an excess in the number of sources centered on M84 , with a spatial distribution closely corresponding to the M84 stellar light .
Given an absence of recent star-formation , accreting binaries are the only candidates for the M84 X-ray sources .
The majority of M84 sources ( with luminosities exceeding 10 ^ { 38 } ergs/s ) exhibit hardness ratios expected from multi-temperature black-body disk emission .
The most luminous sources , which we attribute to accreting black holes exhibit X-ray colors typical of a black body spectrum .
We also identify the sources whose X-ray colors match the expectations for constituents of the Cosmic X-ray Background .
The number of such sources agrees with that expected to be background sources .
After correcting for incompleteness in the source detection , we find a log ( N ) - log ( S ) for M84 similar to that of the elliptical galaxy NGC4697 , i.e .
having a break at a luminosity of L _ { b } = 2.4 ^ { +0.6 } _ { -0.3 } \times 10 ^ { 38 } ergs/s , approximately the Eddington limit on the isotropic luminosity for accretion onto a neutron star .
The slope of the luminosity function above the break provides evidence for a mass distribution in the M84 accreting black holes .