  The low surface brightness Universe holds clues to the first formation of
galaxies. Specifically, the shape and morphology of local stellar haloes have
encoded in them the early formation history of their parent galaxies. Early
progenitor galaxies were absorbed by the dark halo and scattered their stars in
a diffuse halo around the main galaxy. If the accretion event was relatively
recent, it may show as a coherent stream of stars within the halo. in addition,
the low-mass, low-surface brightness satellite galaxies, perhaps the
ultradiffuse galaxies recently reported would help solve the "Missing Dwarf
Problem", the apparent over-prediction of $\Lambda$CDM models of the number of
satellite galaxies around a Milky Way Halo.
  However low surface brightness is not what most telescopes are optimized for,
most are best for resolving point sources and not sensitivity for large-scale
low-light. To be sensitive to the low surface brightness Universe, a telescope
needs a simple, unobstructed light path (disfavoring mirrors), fast optics (low
f/D), and relatively coarse sampling (big pixels). Exceptions are the superb
Dragonfly and Huntsman telescopes which are purposely designed to be sensitive
to low surface brighnesses. Similarly designed, if not with low surface
brightness in mind is the successfully launched TESS satellite. We show in this
Research Note that the envisaged total exposure times and optical setup are
near-ideal for low surface brightness work in the local Universe.
  With combined TESS imaging, one can model the stellar halo surrounding a
galaxy. Technical challenges include the image quality, zodiacal and Galactic
cirrus background light, PSF characterization and subtraction. Once accounted
for with a processing pipeline, one can model the stellar halo for all nearby
galaxies and to search for substructure in these haloes.
