  We report on $H$-band spectra of chemically peculiar Mercury-Manganese (HgMn)
stars obtained via the SDSS/APOGEE survey. As opposed to other varieties of
chemically peculiar stars such as classical Ap/Bp stars, HgMn stars lack strong
magnetic fields and are defined by extreme overabundances of Mn, Hg, and other
heavy elements. A satisfactory explanation for the abundance patterns remains
to be determined, but low rotational velocity is a requirement and involvement
in binary/multiple systems may be as well. The APOGEE HgMn sample currently
consists of 269 stars that were identified among the telluric standard stars as
those whose metallic absorption content is limited to or dominated by the
$H$-band Mn II lines. Due to the fainter magnitudes probed by the APOGEE survey
as compared to past studies, only 9/269 stars in the sample were previously
known as HgMn types. The 260 newly-identified HgMn stars represents a more than
doubling of the known sample. At least 32% of the APOGEE sample are found to be
binary or multiple systems, and from multi-epoch spectroscopy, we were able to
determine orbital solutions for at least one component in 32 binaries. Many of
the multi-lined systems include chemically peculiar companions, with noteworthy
examples being the HgMn+Ap/Bp binary HD 5429, the HgMn+HgMn binary HD 298641,
and the HgMn+BpMn+Am triple system HD 231263. As a further peculiarity, roughly
half of the sample produces narrow emission in the C I 16895 angstroms line,
with widths and radial velocities that match those of the Mn II lines.
