DLT17u turned out to be a very interesting thermonuclear explosion that show a blue bump in the first few days after explosion. Our best-fit model suggests the presence of a subgiant star 56 solar radii from the exploding white dwarf.
Read about it at this link: Press Release
Read about it at this link: Article
What are the progenitors of different kinds of supernovae?
How do these stars explode? One of the best ways to gain
insight into SN progenitors and their explosion physics is
with early data in the hours to days after they explode.
The early emission from SNe is generally dominated by the
explosion itself rather than radioactive decay and can be
used to measure the radius of the exploding star (Piro & Nakar 2013),
a fundamental property of the explosion. The early light curve can
also measure properties of a companion star (Kasen 2010), the presence
of which is still an outstanding question for SNe Ia and thought to be
critical for generating many stripped-envelope SNe. The rise of the
early light curve can measure the outer 56Ni distribution (Piro 2012),
an important constraint for explosion models. Furthermore, observations
on these timescales can even help us study entirely new classes of
transients, including the radioactively powered kilonovae that are
expected from neutron star mergers (Metzger et al. 2010) and will be
crucial for gravitational wave detections, and the shock breakout
expected during black hole formation (Piro 2013), the birth of which
have never been observed.
Motivated by the early-time science opportunities described above, we have begun a one-day cadence SN search in nearby galaxies with a rented PROMPT 0.4m telescope (located at CTIO, Chile) which will uncover ~10 SNe per year within a day of explosion. Named the DLT40 survey, the general strategy is to observe galaxies within D < 40 Mpc every night down to a survey depth of ~19