  TESS has proven to be a powerful resource for finding planets, including
those that orbit the most prevalent stars in our galaxy: the M dwarfs.
Identification of stellar companions (both bound and unbound) has become a
standard component of the transiting planet confirmation process in order to
assess the level of light curve dilution and the possibility of the target
being a false positive. Studies of stellar companions have also enabled
investigations into stellar multiplicity in planet-hosting systems, which has
wide-ranging implications for both exoplanet detection and characterization, as
well as for the formation and evolution of planetary systems. Speckle and AO
imaging are some of the most efficient and effective tools for revealing
close-in stellar companions; we therefore present observations of 58 M-dwarf
TOIs obtained using a suite of speckle imagers at the 3.5-m WIYN telescope, the
4.3-m Lowell Discovery Telescope, and the 8.1-m Gemini North and South
telescopes. These observations, as well as near-infrared adaptive optics images
obtained for a subset (14) of these TOIs, revealed only two close-in stellar
companions. Upon surveying the literature, and cross-matching our sample with
Gaia, SUPERWIDE, and the catalog from El-Badry et al. (2021), we reveal an
additional 15 widely-separated common proper motion companions. We also
evaluate the potential for undetected close-in companions. Taking into
consideration the sensitivity of the observations, our findings suggest that
the orbital period distribution of stellar companions to planet-hosting M
dwarfs is shifted to longer periods compared to the expected distribution for
field M dwarfs.
