2018MNRAS.481.4123K

We present deep X-ray limits on the presence of a pre-explosion counterpart to the low-luminosity Type Ia supernova (SN Ia) 2017ejb. SN 2017ejb was discovered in NGC 4696, a well-studied elliptical galaxy in the Centaurus cluster with 894 ks of Chandra imaging between 14 and 3 yr before SN 2017ejb was discovered. Using post-explosion photometry and spectroscopy of SN 2017ejb, we demonstrate that SN 2017ejb is most consistent with low-luminosity SNe Ia such as SN 1986G and SN 1991bg. Analysing the location of SN 2017ejb in pre-explosion images, we do not detect a pre-explosion X-ray source. We use these data to place upper limits on the presence of any unobscured supersoft X-ray source (SSS). SSS systems are known to consist of white dwarfs (WDs) accreting from a non-degenerate companion star. We rule out any source similar to known SSS systems with kT_eff > 85 eV and L_ bol_ > 4 ×10³⁸ erg s^–1 as well as models of stably accreting Chandrasekhar-mass WDs with accretion rates {dot}M> 3×10^–7 M_☉ yr^–1. These findings suggest that low-luminosity SNe Ia similar to SN 2017ejb explode from WDs that are low-mass, have low pre-explosion accretion rates, or accrete very soon before explosion. Based on the limits from SN 2017ejb and other nearby SNe Ia, we infer that <47 per cent of SNe Ia explode in stably accreting Chandrasekhar-mass SSS systems.