Analyzing SN 2010ih

SN 2010ih is a type Ia supernova, which is thought to come from a binary star system in which at least one of the stars is a white dwarf. The white dwarf gains mass until it reaches the Chandrasekhar limit, where the pressure and temperature set off a runaway thermonuclear explosion. We plan to analyze the light curve of the supernova to characterize late-time behavior. We reduced images of Supernova 2010ih taken with the 4m Mayall Telescope using the software Image Reduction and Analysis Facility (IRAF). I removed bad pixels and crosstalk, subtracted the darks and the zeros, divided out the flats, fit the image to a world coordinate system, and then combined the images into a final image, for each filter; B, V, R, and I. After achieving the four final images, I then performed photometry to find the magnitude for the supernova and thirty field stars.