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Type Ia supernovae are understood to arise from the thermonuclear explosionof a carbon-oxygen white dwarf, yet the evolutionary mechanisms leading to suchevents remain unknown. Many proposed channels, including the classicalsingle-degenerate scenario, invoke a hot, luminous evolutionary phase for theprogenitor, in which it is a prodigious source of photoionizing emission. Here,we examine the environment of SN 2014J for evidence of a photoionized nebula inpre- and post-explosion [O III] $\lambda5007$ \AA\ and H$\beta$ images takenwith the Hubble Space Telescope. From the absence of any extended emission, weexclude a stable nuclear-burning white dwarf at the location of SN 2014J in thelast ~100,000 years, assuming a typical warm interstellar medium (ISM) particledensity of 1 cm$^{-3}$. These limits greatly exceed existing X-ray constraintsat temperatures typical of known supersoft sources. Significant extreme-UV/softX-ray emission prior to explosion remains plausible for lower ISM densities(e.g., $n_{\rm ISM}\sim 0.1~\rm{cm}^{-3}$). In this case, however, any putativenebula would be even more extended, allowing deeper follow-up observations toresolve this ambiguity in the near future.

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