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We analyze 166 spheroid subdwarfs $(6.5<M_V<14.5)$ found in 53 fieldsobserved with the Wide Field Camera on the {\it Hubble Space Telescope}. Thefields cover 221 square arcmin over a wide range of directions. The spheroidluminosity function (LF) is inconsistent at about the 3 sigma level with thelocal spheroid LF of Dahn et al. even when the normalization of the latter iscorrected to take account of the latest data on spheroid kinematics. Thedifference may reflect systematic errors in one of the two studies or featuresof the spheroid spatial distribution that are not included in the simplestmodels. The mass function, which shows no obvious structure, can be representedby a power law, d N/d ln M ~ M^\alpha, with \alpha=0.25 +/- 0.32 over the massrange 0.71 Msun > M >0.09 Msun. The spheroid therefore does not contributesignificantly to microlensing unless the mass function changes slopedramatically in the substellar range. The total local mass density of spheroidstars (including remnants and unseen binary companions) is \rho ~ 6.4E-5Msun/pc^3, with an uncertainty of about 50%. The power-law indices \alpha=0.25for the spheroid and \alpha=0.44 for the disk (both uncorrected for binaries)are similar to those of globular clusters of moderate to high metallicity.Comment: Clarifications and improvements made in response to referee repor

Spheroid Luminosity and Mass Functions fromHubble Space TelescopeStar Counts