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tokens: The Pan-STARRS1 Surveys have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, the Max Planck Institute for Extraterrestrial Physics, Garching, Johns Hopkins University, Durham University, the University of Edinburgh, Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant no. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under grant no. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE). Some observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério da Ciência, Tecnologia e Inovação (Brazil), and Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina). This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. Based on observations obtained with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium. C.W.S. and G.N. thank the DOE Office of Science for their support under grant ER41843. Partial support for this work was provided by National Science Foundation grant AST-1009749. The ESSENCE/SuperMACHO data reduction pipeline photpipe was developed with support from National Science Foundation grant AST-0507574 and HST programs GO-10583 and GO-10903. R.P.K.’s supernova research is supported in part by NSF grant AST-1211196 and HST program GO-13046. Some of the computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. Much of the analysis was done using the Midway-RCC computing cluster at University of Chicago. This research has made use of the CfA Supernova Archive, which is funded in part by the National Science Foundation through grant AST 0907903. This research has made use of NASA’s Astrophysics Data System. This work was generated as part of NASA WFIRST Preparatory Science program 14-WPS14-0048 and is supported in part by the U.S. Department of Energy under contract DE-AC02-76CH03000. This work was supported in part by the Kavli Institute for Cosmological Physics at the University of Chicago through grant NSF PHY-1125897 and an endowment from the Kavli Foundation and its founder Fred Kavli. We gratefully acknowledge support from NASA grant 14-WPS14-0048. D.S. is supported by NASA through Hubble Fellowship grant HST -HF2-51383.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. D.O.J. is supported by the Gordon and Betty Moore Foundation postdoctoral fellowship at the University of California, Santa Cruz. R.C. thanks the Kavli Institute for Theoretical Physics for its hospitality while this work was in the final stages of preparation. This research was supported in part by the National Science Foundation under grant no. NSF PHY11-25915. R.K. is supported by DOE grant DEAC02-76CH03000. The computations in this paper used a combination of three computing clusters. The bulk of the final analysis was performed using the University of Chicago Research Computing Center, and the earlier analysis was done at the Odyssey cluster at Harvard University. The Odyssey cluster is supported by the FAS Division of Science, Research Computing Group at Harvard University. Supernova light-curve reprocessing would not have been possible without the Data-Scope project at the Institute for Data Intensive Engineering and Science at Johns Hopkins University. Facilities: PS1 (GPC1) , Gemini:South (GMOS) , Gemini:North (GMOS) , MMT (Blue Channel spectrograph) , MMT (Hectospec) , Magellan:Baade (IMACS) , Magellan:Clay (LDSS3) , APO (DIS) .