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We present results based on observations of SN 2015H which belongs to thesmall group of objects similar to SN 2002cx, otherwise known as type Iaxsupernovae. The availability of deep pre-explosion imaging allowed us to placetight constraints on the explosion epoch. Our observational campaign beganapproximately one day post-explosion, and extended over a period of about 150days post maximum light, making it one of the best observed objects of thisclass 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 syntheticspectra generated from simulations of deflagrations of Chandrasekhar masscarbon-oxygen white dwarfs, we find reasonable agreement with models of weakdeflagrations that result in the ejection of ~0.2 M$_{\odot}$ of materialcontaining ~0.07 M$_{\odot}$ of 56Ni. The model light curve however, evolvesmore rapidly than observations, suggesting that a higher ejecta mass is to befavoured. Nevertheless, empirical modelling of the pseudo-bolometric lightcurve suggests that $\lesssim$0.6 M_sun of material was ejected, implying thatthe white dwarf is not completely disrupted, and that a bound remnant is alikely outcome.

The type Iax supernova, SN 2015H: a white dwarf deflagration candidate