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SN 2007od exhibits characteristics that have rarely been seen in a Type IIPsupernova (SN). Optical V band photometry reveals a very steep brightnessdecline between the plateau and nebular phases of ~4.5 mag, likely due to SN2007od containing a low mass of 56Ni. The optical spectra show an evolutionfrom normal Type IIP with broad Halpha emission, to a complex, four componentHalpha emission profile exhibiting asymmetries caused by dust extinction afterday 232. This is similar to the spectral evolution of the Type IIn SN 1998S,although no early-time narrow (~200 km s-1) Halpha component was present in SN2007od. In both SNe, the intermediate-width Halpha emission components arethought to arise in the interaction between the ejecta and its circumstellarmedium (CSM). SN 2007od also shows a mid-IR excess due to new dust. Theevolution of the Halpha profile and the presence of the mid-IR excess providestrong evidence that SN 2007od formed new dust before day 232. Late-timeobservations reveal a flattening of the visible lightcurve. This flattening isa strong indication of the presence of a light echo, which likely accounts formuch of the broad, underlying Halpha component seen at late-times. We believethe multi-peaked Halpha emission is consistent with the interaction of theejecta with a circumstellar ring or torus (for the inner components at \pm1500km s-1), and a single blob or cloud of circumstellar material out of the planeof the CSM ring (for the outer component at -5000 km s-1). The most probablelocation for the formation of new dust is in the cool dense shell created bythe interaction between the expanding ejecta and its CSM. Monte Carlo radiativetransfer modeling of the dust emission from SN 2007od implies that up to 4x10-4Msun of new dust has formed. This is similar to the amounts of dust formedin other CCSNe such as SNe 1999em, 2004et, and 2006jc.

SN 2007od: A Type IIP SN with Circumstellar Interaction