Observing the Next Galactic Supernova
  We model the distance, extinction, and magnitude probability distributions of
a successful Galactic core-collapse supernova (ccSN), its shock breakout
radiation, and its massive star progenitor. We find, at very high probability
(~100%), that the next Galactic SN will easily be detectable in the near-IR and
that near-IR photometry of the progenitor star very likely (~92%) already
exists in the 2MASS survey. Most ccSNe (~98%) will be easily observed in the
optical, but a significant fraction (~43%) will lack observations of the
progenitor due to a combination of survey sensitivity and confusion. If
neutrino detection experiments can quickly disseminate a likely position (~3
deg), we show that a modestly priced IR camera system can probably detect the
shock breakout radiation pulse even in daytime (~64% for the cheapest design).
Neutrino experiments should seriously consider adding such systems, both for
their scientific return and as an added and internal layer of protection
against false triggers. We find that shock breakouts from failed ccSNe of red
supergiants may be more observable than those of successful SNe. We review the
process by which neutrinos from a Galactic ccSN would be detected and
announced. We provide new information on the EGADS system and its potential for
providing instant neutrino alerts. We also discuss the distance, extinction,
and magnitude probability distributions for the next Galactic Type Ia SN. Based
on our modeled observability, we find a Galactic ccSN rate of 3.2 (+7.3/-2.6)
per century and a Galactic Type Ia SN rate of 1.4 (+1.4/-0.8) per century for a
total Galactic SN rate of 4.6 (+7.4/-2.7) per century is needed to account for
the SNe observed over the last millennium.
