  Hubble Space Telescope (HST) Fine Guidance Sensor (FGS) trigonometric
parallax observations were obtained to directly determine distances to five
nearby M-dwarf / M-dwarf eclipsing binary systems. These systems are
intrinsically interesting as benchmark systems for establishing basic physical
parameters for low-mass stars, such as luminosity L, and radius R. HST/FGS
distances are also one of the few direct checks on Gaia trigonometric
parallaxes, given the comparable sensitivity in both magnitude limit and
determination of parallactic angles. A spectral energy distribution (SED) fit
of each system's blended flux output was carried out, allowing for estimation
of the bolometric flux from the primary and secondary components of each
system. From the stellar M, L, and R values, the low-mass star relationships
between L and M, and R and M, are compared against idealized expectations for
such stars. An examination on the inclusion of these close M-dwarf/M-dwarf
pairs in higher-order common proper motion (CPM) pairs is analysed; each of the
5 systems has indications of being part of a CPM system. Unexpected distances
on interesting objects found within the grid of parallactic reference stars are
also presented, including a nearby M dwarf and a white dwarf.
