  We present results based on observations of SN 2015H which belongs to the
small group of objects similar to SN 2002cx, otherwise known as type Iax
supernovae. The availability of deep pre-explosion imaging allowed us to place
tight constraints on the explosion epoch. Our observational campaign began
approximately one day post-explosion, and extended over a period of about 150
days post maximum light, making it one of the best observed objects of this
class to date. We find a peak magnitude of M$_r$ = -17.27 $\pm$ 0.07, and a
($\Delta m_{15})_r$ = 0.69 $\pm$ 0.04. Comparing our observations to synthetic
spectra generated from simulations of deflagrations of Chandrasekhar mass
carbon-oxygen white dwarfs, we find reasonable agreement with models of weak
deflagrations that result in the ejection of ~0.2 M$_{\odot}$ of material
containing ~0.07 M$_{\odot}$ of 56Ni. The model light curve however, evolves
more rapidly than observations, suggesting that a higher ejecta mass is to be
favoured. Nevertheless, empirical modelling of the pseudo-bolometric light
curve suggests that $\lesssim$0.6 M_sun of material was ejected, implying that
the white dwarf is not completely disrupted, and that a bound remnant is a
likely outcome.

High Energy Astrophysical Phenomena;Solar and Stellar Astrophysics