The critical property here is the ability of the telescope to resolve all sources with luminosities $L_{\rm x}>10^{35}$ erg s^-1, since at lower luminosities the contribution of LMXBs becomes small. For a distance of 1 Mpc Chandra needs $\sim$ 20 ks to achieve this sensitivity.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

http://hea-www.harvard.edu/saord/zhtools/

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

...(Nolthenius & Ford 1986)

Note that while this value of the total mass of the galaxy is slightly smaller than the stellar mass determined from the K-band luminosity of the galaxy ( $\sim$ $10^{9}~M_\odot$ ), it is consistent with it given the different uncertainties involved in the measurement of both values. On a general note, it was mentioned by Nolthenius & Ford (1986) that the mass to light ratio of M 32 is consistent with that of globular clusters, therefore it is likely that stars provide the dominant contribution to the total mass of M 32.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... stars

Inclusion of young stars would increase the local emissivity even further, up to $L_{\rm0.5{-}2~keV}/M \sim 27\times10^{27}$ erg s^-1 $M^{-1}_\odot$ .

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.