Journal article

The Young Supernova Experiment: Survey Goals, Overview, and Operations

DO Jones, RJ Foley, G Narayan, J Hjorth, ME Huber, PD Aleo, KD Alexander, CR Angus, K Auchettl, VF Baldassare, SH Bruun, KC Chambers, D Chatterjee, DL Coppejans, DA Coulter, L DeMarchi, G Dimitriadis, MR Drout, A Engel, KD French Show all

The Astrophysical Journal | IOP PUBLISHING LTD | Published : 2021

Abstract

Time-domain science has undergone a revolution over the past decade, with tens of thousands of new supernovae (SNe) discovered each year. However, several observational domains, including SNe within days or hours of explosion and faint, red transients, are just beginning to be explored. Here we present the Young Supernova Experiment (YSE), a novel optical time-domain survey on the Pan-STARRS telescopes. Our survey is designed to obtain well-sampled griz light curves for thousands of transient events up to z ≈ 0.2. This large sample of transients with four-band light curves will lay the foundation for the Vera C. Rubin Observatory and the Nancy Grace Roman Space Telescope, providing a critica..

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University of Melbourne Researchers

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Awarded by NASA by the Space Telescope Science Institute


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Awarded by National Science Foundation


Awarded by Danish National Research Foundation


Awarded by Hong Kong government (GRF)


Awarded by Heising-Simons Foundation


Awarded by VILLUM FONDEN


Awarded by Villum Young Investor Grants


Awarded by Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D)


Awarded by STFC


Awarded by Future Investigators in NASA Earth and Space Science and Technology (FINESST)


Awarded by NSERC


Awarded by European Union


Awarded by Independent Research Fund Denmark


Awarded by National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate


Funding Acknowledgements

D.O.J. acknowledges support from a Gordon and Betty Moore Foundation postdoctoral fellowship at the University of California, Santa Cruz. D.O.J., K.D.A., and K.D.F. also acknowledge support provided by NASA Hubble Fellowship grants HST-HF2-51462.001, HST-HF2-51403.001, and HST-HF2-51391.001-A, respectively, which are awarded by the Space Telescope Science Institute, operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. The UCSC team is supported in part by NASA grants NNG17PX03C, 80NSSC19K1386, and 80NSSC20K0953; NSF grants AST-1518052, AST-1815935, and AST-1911206; the Gordon & Betty Moore Foundation; the Heising-Simons Foundation; and a fellowship from the David and Lucile Packard Foundation to R.J.F. D.A.C. and M.R.S. are supported by the National Science Foundation Graduate Research Fellowship Program Under grant Nos. DGE-1339067 and DGE-1842400, respectively. E.R.-R. is supported by the Heising-Simons Foundation and NSF (AST-1852393 and AST-1911206). E.R.-R. and H.P. are supported by the Danish National Research Foundation (DNRF132). H.P. is also indebted to the Hong Kong government (GRF grant HKU27305119) for support.W.J.-G. is supported by the National Science Foundation Graduate Research Fellowship Program under grant No. DGE-1842165 and the IDEAS Fellowship Program at Northwestern University. C.D.K. acknowledges support through NASA grants in support of Hubble Space Telescope program AR-16136. The computations in this paper were aided by the University of Chicago Research Computing Center. R.M. acknowledges partial support by the National Science Foundation under award Nos. AST-1909796 and AST-1944985 and by the Heising-Simons Foundation under grant No. 2018-0911. R.M. is a CIFAR Azrieli Global Scholar in the Gravity & the Extreme Universe Program (2019) and an Alfred P. Sloan Fellow in Physics (2019).This work was supported by a VILLUM FONDEN Investigator grant to J.H. (project No. 16599) and two Villum Young Investor Grants to C.G. and C.G. (10123 and 25501).G.N. and K.D.F are grateful for support from the University of Illinois at Urbana-Champaign. D.C. is supported by the Center for Astrophysical Surveys at NCSA through the Illinois Survey Science Postdoctoral Fellowship. A.G. is supported by the National Science Foundation Graduate Research Fellowship Program under grant No. DGE1746047. A.G. and P.D.A. are supported by the Center for Astrophysical Surveys as Illinois Survey Science Graduate Fellows. A.G. additionally acknowledges support from the Illinois Distinguished Fellowship. A.E.'s work was supported by a 2019 Physics & Astronomy Student Travel Grant from the Council for Undergraduate Research. The computations in this paper made extensive use of the Illinois Campus Cluster and facilities at the National Center for Supercomputing Applications at UIUC. Parts of this research were supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project No. CE170100013.S.J.S. and K.W.S. are supported by STFC grants ST/P000312/1, ST/S006109/1 and ST/T000198/1.A.H. is supported by Future Investigators in NASA Earth and Space Science and Technology (FINESST) award No. 80NSSC19K1422.M.R.D. acknowledges support from the NSERC through grant RGPIN-2019-06186, the Canada Research Chairs Program, the Canadian Institute for Advanced Research (CIFAR), and the Dunlap Institute at the University of Toronto.This project has received funding from the European Union's Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 891744 to S.I.R. Additionally, S.I.R. gratefully acknowledges support from the Independent Research Fund Denmark via grant Nos. DFF 4002-00275 and 8021-00130.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, 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.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.Based on observations obtained with the Samuel Oschin 48-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW.