The Development and Scientific Application of the Dragonfly Telephoto
  Array
  The low surface brightness visible wavelength Universe below 29 mag
arcsec$^{-2}$ is teeming with unexplored astrophysical phenomena. Structures
fainter than this surface brightness are extremely difficult to image due to
systematic errors of sky subtraction and scattered light in the atmosphere and
in the telescope. In Chapter 1, I show how The Dragonfly Telephoto Array
(Dragonfly for short) addresses these systematics via a combination of hardware
and software and is able to image at a level of 30 mag arcsec$^{-2}$ or
fainter. In Chapter 2, I describe the Dragonfly Pipeline and how it is
optimized for low surface brightness imaging, how it automatically rejects
problematic exposures, and its cloud-orchestration. In Chapter 3, I present a
study of the outer disk of the nearby spiral galaxy NGC 2841 using Dragonfly as
well as archival data in UV from the Galaxy Evolution Explorer Satellite and
rest frame 21 cm data using the Very Large Array. While it is commonly accepted
that gas dominates over stars in galaxy outer disks, I find that in NGC 2841,
this is not the case. The stellar disk extends to five times R25, and there is
more stellar than gas mass at all radii. Surprisingly there is a constant ratio
of stellar to gas mass beyond 30 kpc, where the disk is also warped. I propose
the most likely formation mechanism for this outer disk is co-planar satellite
accretion. In Chapter 4, I present a study of thermally emitted and scattered
light from dust in the optically thin regions of the Spider HI Cloud, using
Dragonfly and Herschel Space Observatory data. In closing the thesis (Chapter
5), I look forward to further improvements in the Dragonfly Pipeline, a
population study of the formation mechanisms of galaxy disks and to carrying
out tests of dust models.
