Abundance Stratification in Type Ia Supernovae -- VIII. The 03fg-like SN\,2012dn: a double-degenerate merger interpretation

Abstract

A detailed study using abundance tomography of SN 2012dn, a peculiar Type Ia supernova, is presented. Despite exhibiting a normal peak luminosity, it retains early-phase super-Chandrasekhar (03fg-like) characteristics: weak Fe III, narrow intermediate-mass element (IME), persistent carbon, and the absence of high-velocity Ca II features. Its nebular spectrum is unusually faint due to grey dimming beginning $\sim$60 days after maximum and shows [O I] emission, rare in SNe Ia. While a Chandrasekhar-mass density profile reproduces the photospheric phase, it fails at late times. The [O I] emission requires additional low-velocity mass, implying a total ejecta mass of $1.66$ $M_\odot$, including $0.33$ $M_\odot$ of oxygen (with $0.1$ $M_\odot$ in the core). The $^{56}$Ni mass is estimated to be $0.45$--$0.49$ $M_\odot$, a range set by uncertainties in the grey-extinction correction applied at the nebular phase, and is insufficient on its own to account for the peak luminosity. Stable iron is confined to intermediate layers and absent from both the core and outer ejecta, the latter indicating sub-solar progenitor metallicity. Silicon and sulfur span the full ejecta, while carbon extends down to $v \sim 6000$ ${\rm km,s^{-1}}$. These properties favour a double-degenerate CO--CO white dwarf merger scenario. The remaining luminosity deficit may be explained by additional energy input from a weak interaction with a low-mass, carbon-rich circumstellar shell.