Ultraviolet ( UV ) , optical , and near infrared ( NIR ) observations of the Type IIP supernova ( SN ) 2007od , covering from maximum light to late phases , allow detailed investigation of different physical phenomena in the expanding ejecta .
These data turn this object into one of the most peculiar SNe IIP ever studied .
The early light curve of SNÂ 2007od is similar to that of a bright IIP , with a short plateau , a bright peak ( M _ { V } = - 18 mag ) , but a very faint late–time optical light curve .
However , with the inclusion of mid infrared ( MIR ) observations during the radioactive tail , we derive an ejected mass of ^ { 56 } Ni of M ( ^ { 56 } Ni ) \sim 2 \times 10 ^ { -2 } M _ { \odot } .
By modeling the bolometric light curve , ejecta expansion velocities , and blackbody temperature , we estimate a total ejected mass of 5 – 7.5 M _ { \odot } with a kinetic energy of at least 0.5 \times 10 ^ { 51 } erg .
The early spectra reveal a boxy H \alpha profile and high velocity features of the Balmer series that suggest the possible interaction of the ejecta with a close circumstellar matter ( CSM ) .
The interaction with the CSM and the presence of dust formed inside the ejecta are evident in the late-time spectra .
The episodes of mass loss shortly before explosion , the bright plateau , the relatively small amount of ^ { 56 } Ni , and the faint [ O I ] emission observed in the nebular spectra are consistent with a super-asymptotic giant branch ( super-AGB ) progenitor ( M \sim 9.7 - 11 M _ { \odot } ) .