Paper: 2018MNRAS.475..193F (acknowledgments)
Acknowledgements We thank the SN community, both professional and amateur, for its tireless efforts discovering and classifying SNe. We especially thank those who make discoveries, classifications, and data immediately public. Timely, public access to this information was both critical for this work and a significant benefit for all of science. We especially thank A. Castro-Tirado, R. Chornock, A. Gal-Yam, B. Shappee, I. Shivvers, J. Strader, and O. Yaron for providing additional information about their observations. We thank S. Downing, A. Duarte, M. Garcia, R. Hounsell, A. Kniazev, M. Kotze, B. Miszalski, B. Patel, E. Romero Colmenero, R. Skelton, and J. Tonry for assisting in some of the observations presented here. We thank C. Stubbs for his continued support of this project and other intellectual contributions. This manuscript is based upon work supported by the National Aeronautics and Space Administration under Contract No. NNG16PJ34C issued through the WFIRST Science Investigation Teams Programme. RJF and DS were supported in part by NASA grant 14-WPS14-0048. The UCSC group is supported in part by NSF grant AST-1518052, the Gordon Betty Moore Foundation, and from fellowships from the Alfred P. Sloan Foundation and the David and Lucile Packard Foundation to RJF. DS acknowledges support from 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 and 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. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement no. [291222] (PI: SJS). Pan-STARRS is supported in part by the National Aeronautics and Space Administration under Grants NNX12AT65G and NNX14AM74G. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by 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 and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the 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 Grant No. AST–1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. This paper is based on observations (NOAO Prop. IDs: 2015A-0253 and 2015B-0313; PI: RJF) obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia, e Inovação (MCTI) da República Federativa do Brasil; the U.S. National Optical Astronomy Observatory (NOAO); the University of North Carolina at Chapel Hill (UNC); and Michigan State University (MSU), and at Kitt Peak National Observatory, NOAO, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. The authors are honoured to be permitted to conduct astronomical research on Iolkam Du'ag (Kitt Peak), a mountain with particular significance to the Tohono O'odham. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Research at Lick Observatory is partially supported by a generous gift from Google. Some of the observations reported in this paper were obtained with the Southern African Large Telescope (SALT), and we thank the SALT Astronomers for assistance. Based on observations obtained with the Apache Point Observatory 3.5-m telescope, which is owned and operated by the Astrophysical Research Consortium. We acknowledge use of some data collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile as part of PESSTO, (the Public ESO Spectroscopic Survey for Transient Objects Survey) ESO programme 188.D-3003, 191.D-0935. This manuscript was initiated during the ‘Dynamic Universe: Understanding ExaScale Astronomical Synoptic Surveys’ workshop at the Aspen Center for Physics, which is supported in part by the NSF under grant No. PHYS-1066293. RJF and DS thank the Aspen Center for Physics for its hospitality during the ‘Dynamic Universe’ workshop in 2015 June. Facility: Pan-STARRS-1 (GPC1); SOAR (Goodman spectrograph); Mayall (KOSMOS spectrograph); FLWO:1.5m (FAST); ARC (DIS); SALT (RSS); Keck:I (LRIS); Keck:II (DEIMOS) Shane (Kast)