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SN 2007it is a bright, Type IIP supernova which shows indications of bothpre-existing and newly formed dust. The visible photometry shows a brightlate-time luminosity, powered by the 0.09 M$_{\sun}$ of $^{56}$Ni present inthe ejecta. There is also a sudden drop in optical brightness after day 339,and a corresponding brightening in the IR due to new dust forming in theejecta. CO and SiO emission, generally thought to be precursors to dustformation, may have been detected in the mid-IR photometry of SN 2007it. Theoptical spectra show stronger than average [O I] emission lines and weaker thanaverage [Ca II] lines, which may indicate a 16 - 27 M$_{\sun}$ progenitor, onthe higher end of expected Type IIP masses. Multi-component [O I] lines arealso seen in the optical spectra, most likely caused by an asymmetric blob or atorus of oxygen core material being ejected during the SN explosion.Interaction with circumstellar material prior to day 540 may have created acool dense shell between the forward and reverse shocks where new dust iscondensing. At late times there is also a flattening of the visible lightcurveas the ejecta luminosity fades and a surrounding light echo becomes visible.Radiative transfer models of SN 2007it SEDs indicate that up to 10$^{-4}$M$_{\sun}$ of new dust has formed in the ejecta, which is consistent with theamount of dust formed in other core collapse supernovae.

Photometric and Spectroscopic Evolution of the Type IIP SN 2007it to Day 944