  Preliminary trigonometric parallaxes and BVI photometry are presented for two
dwarf carbon stars, LP765-18 (= LHS1075) and LP328-57 (= CLS96). The data are
combined with the literature values for a third dwarf carbon star, G77-61 (=
LHS1555). All three stars have very similar luminosities (9.6<M_V<10.0) and
very similar broadband colors across the entire visual-to-near IR (BVIJHK)
wavelength range. Their visual (BVI) colors differ from all known red dwarfs,
subdwarfs, and white dwarfs. In the M_V versus V-I color-magnitude diagram they
are approximately 2 magnitudes subluminous compared with normal disk dwarfs
with solar-like metallicities, occupying a region also populated by O-rich
subdwarfs with -1.5<[m/H]<-1.0. The kinematics indicate that they are members
of the Galactic spheroid population. The subluminosity of all three stars is
due to an as-yet-unknown combination of (undoubtedly low) metallicity, possibly
enhanced helium abundance, and unusual line-blanketing in the bandpasses
considered. The properties of the stars are compared with models for the
production of dwarf carbon stars.
