  I identify a point-symmetric morphology of the supernova remnant (SNR)
G352.7-0.1 and propose that the outer axially-symmetric structure is the
remnant of a common envelope evolution (CEE) of the progenitor system, while
the inner structure is the ejecta of a thermonuclear explosion triggered by the
merger 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 symmetry
axis inclined to the symmetry axis of the large radio ellipse. The high
abundance 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 progenitor
system. I propose a scenario with progenitors of initial masses of M1=5-7Mo and
M2=4-5 Mo. At a later phase, the WD remnant of the primary star and the AGB
secondary star experience a CEE that ejects the circumstellar material that
swept up more ISM to form the large elliptical radio structure. An explosion
during the merger of the WD with the core of the AGB star triggered a
super-Chandrasekhar thermonuclear explosion that formed the inner structure
that is bright in X-ray. A tertiary star in the system caused the misalignment
of the two symmetry axes. This study adds to the wide variety of evolutionary
routes within the scenarios of normal and peculiar SNe Ia.
