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I identify a point-symmetric morphology of the supernova remnant (SNR)G352.7-0.1 and propose that the outer axially-symmetric structure is theremnant of a common envelope evolution (CEE) of the progenitor system, whilethe inner structure is the ejecta of a thermonuclear explosion triggered by themerger of a white dwarf (WD) and the core of an asymptotic giant branch (AGB)star. The main radio structure of SNR G352.7-0.1 forms an outer (large)ellipse. The bright X-ray emitting gas forms a smaller ellipse with a symmetryaxis inclined to the symmetry axis of the large radio ellipse. The highabundance of iron and the energy of its X-ray lines suggest a type Ia supernova(SN Ia). The massive swept-up gas suggests a relatively massive progenitorsystem. I propose a scenario with progenitors of initial masses of M1=5-7Mo andM2=4-5 Mo. At a later phase, the WD remnant of the primary star and the AGBsecondary star experience a CEE that ejects the circumstellar material thatswept up more ISM to form the large elliptical radio structure. An explosionduring the merger of the WD with the core of the AGB star triggered asuper-Chandrasekhar thermonuclear explosion that formed the inner structurethat is bright in X-ray. A tertiary star in the system caused the misalignmentof the two symmetry axes. This study adds to the rich variety of evolutionaryroutes within the different scenarios of normal and peculiar SNe Ia.

Explaining supernova remnant G352.7-0.1 as a peculiar type Ia supernova inside a planetary nebula