Progenitor constraints on the Type Ia supernova SN 2014J from Hubble Space Telescope H$\beta$ and [O III] observations

Abstract

Type Ia supernovae are understood to arise from the thermonuclear explosion of a carbon-oxygen white dwarf, yet the evolutionary mechanisms leading to such events remain unknown. Many proposed channels, including the classical single-degenerate scenario, invoke a hot, luminous evolutionary phase for the progenitor, in which it is a prodigious source of photoionizing emission. Here, we examine the environment of SN 2014J for evidence of a photoionized nebula in pre- and post-explosion [O III] $\lambda 5007$ Å and H$\beta$ images taken with the Hubble Space Telescope. From the absence of any extended emission, we exclude a stable nuclear-burning white dwarf at the location of SN 2014J in the last ~100,000 years, assuming a typical warm interstellar medium (ISM) particle density of 1 cm${}^{-3}$. These limits greatly exceed existing X-ray constraints at temperatures typical of known supersoft sources. Significant extreme-UV/soft X-ray emission prior to explosion remains plausible for lower ISM densities (e.g., $n_{\mathrm{ISM}}\sim 0.1{\mathrm{cm}}^{-3}$). In this case, however, any putative nebula would be even more extended, allowing deeper follow-up observations to resolve this ambiguity in the near future.

6 pages, 3 figures. Accepted by MNRAS Letters with minor revisions