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THE CARNEGIE SUPERNOVA PROJECT: LIGHT-CURVE FITTING WITH SNooPy

Chris R. BurnsObservatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena CA 91101, USAM. StritzingerThe Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, 10691 Stockholm, SwedenM. M. PhillipsLas Campanas ObservatoryShiAnne KattnerAstronomy Department, San Diego State University, 5500 Campanile Drive, San Diego, CA 92182, USAS. E. PerssonObservatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena CA 91101, USABarry F. MadoreCarnegie ObservatoriesWendy L. FreedmanCarnegie ObservatoriesLuis BoldtCarnegie Institution of Washington, Las Campanas Observatory, Colina El Pino, Casilla 601, ChileA. CampillayLas Campanas ObservatoryC. ContrerasCentre for Astrophysics & Supercomputing, Swinburne University of Technology, P.O. Box 218, Victoria 3122, AustraliaG. FolatelliLas Campanas ObservatoryS. GonzalezLas Campanas ObservatoryW. KrzemińskiLas Campanas ObservatoryN. MorrellCarnegie ObservatoriesF. SalgadoCarnegie Institution of Washington, Las Campanas Observatory, Colina El Pino, Casilla 601, ChileN. B. SuntzeffTexas A&M University

2010en

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ABI

Annotatsiya

In providing an independent measure of the expansion history of the Universe, the Carnegie Supernova Project (CSP) has observed 71 high-z Type Ia supernovae (SNe Ia) in the near-infrared bands Y and J. These can be used to construct rest-frame i-band light curves which, when compared to a low-z sample, yield distance moduli that are less sensitive to extinction and/or decline-rate corrections than in the optical. However, working with NIR observed and i-band rest frame photometry presents unique challenges and has necessitated the development of a new set of observational tools in order to reduce and analyze both the low-z and high-z CSP sample. We present in this paper the methods used to generate uBVgriYJH light-curve templates based on a sample of 24 high-quality low-z CSP SNe. We also present two methods for determining the distances to the hosts of SN Ia events. A larger sample of 30 low-z SNe Ia in the Hubble Flow are used to calibrate these methods. We then apply the method and derive distances to seven galaxies that are so nearby that their motions are not dominated by the Hubble flow.

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DOI: 10.1088/0004-6256/141/1/19

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