@article{9a20e633cad344ef9bb5bb0a19956ede,
title = "SN 2016jhj at redshift 0.34: Extending the Type II supernova Hubble diagram using the standard candle method",
abstract = "Although Type Ia supernova cosmology has now reached a mature state, it is important to develop as many independent methods as possible to understand the true nature of dark energy. Recent studies have shown that Type II supernovae (SNe II) offer such a path and could be used as alternative distance indicators. However, the majority of these studies were unable to extend the Hubble diagram above redshift z=0.3 because of observational limitations. Here, we show that we are now ready to move beyond low redshifts and attempt high-redshift (z ≳ 0.3) SN II cosmology as a result of new-generation deep surveys such as the Subaru/Hyper Suprime-Cam survey. Applying the 'standard candle method' toSN2016jhj (z=0.3398±0.0002; discovered by HSC) together with a low-redshift sample, we are able to construct the highest-redshift SN II Hubble diagram to date with an observed dispersion of 0.27 mag (i.e. 12-13 per cent in distance). This work demonstrates the bright future of SN II cosmology in the coming era of large, wide-field surveys like that of the Large Synoptic Survey Telescope.",
keywords = "Distance scale, Galaxies: distances and redshifts, Supernovae: general",
author = "{de Jaeger}, T. and L. Galbany and Filippenko, {A. V.} and S. Gonz{\'a}lez-Gait{\'a}n and N. Yasuda and K. Maeda and M. Tanaka and T. Morokuma and Moriya, {T. J.} and N. Tominaga and K. Nomoto and Y. Komiyama and Anderson, {J. P.} and Brink, {T. G.} and Carlberg, {R. G.} and G. Folatelli and M. Hamuy and G. Pignata and W. Zheng",
note = "Funding Information: We thank the referee for their thorough reading of the manuscript, which helped clarify and improve it. T.d. J. also thanks P. Nugent and M. Sullivan for helpful comments on this manuscript. Support for A.V.F.'s supernova research group at U.C. Berkeley has been provided by US NSF grant AST-1211916, the TABASGO Foundation, Gary and Cynthia Bengier (T.d. J. is a Bengier Postdoctoral Fellow), the Christopher R. Redlich Fund, and the Miller Institute for Basic Research in Science (U.C. Berkeley). The work of A.V.F. was completed in part at the Aspen Center for Physics, which is supported by NSF grant PHY-1607611; he thanks the Center for its hospitality during the neutron stars workshop in 2017 June and July. L.G. was supported in part by the NSF under grant AST-1311862. S.G.G, M.H. and G.P acknowledge support from the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics (MAS). This work has been supported by Japan Society for the Promotion of Science (JSPS) KAKENHI Grant JP15H02075 (M.T.), JP25800103 (M.T.), JP26400222, JP16H02168 and JP17K05382 (K.N.). K.M acknowledges the JSPS Open Partnership Bilateral Joint Research Project between Japan and Chile, the YITP workshop YITP-T-16-05 supported by the Yukawa Institute for Theoretical Physics at Kyoto University, and JSPS KAKENHI Grant 17H02864. The work of the CSP-I has been supported by the NSF under grants AST-0306969, AST-0607438 and AST-1008343. This paper is based on the data collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by the Subaru Telescope and Astronomy Data Center at National Astronomical Observatory of Japan (NAOJ). The HSC collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the NAOJ, the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), theUniversity of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from Japanese Cabinet Office, theMinistry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, theMax-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, 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 (NASA) under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the NSF under grant AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE). This paper makes use of software developed for the Large Synoptic Survey Telescope. We thank the LSST Project for making their code available as free software at http://dm.lsst.org. 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 NASA; the observatory was made possible by the generous financial support of theW.M. Keck Foundation. Thiswork is based in part on data produced at the Canadian Astronomy Data Centre as part of the CFHT Legacy Survey, a collaborative project of the National Research Council of Canada and the French Centre National de la Recherche Scientifique. The work is also 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 NSF, the STFC (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil) and CONICET (Argentina). This research used observations from Gemini program number: GN-2005A-Q-11, GN-2005B-Q-7, GN-2006A-Q-7, GS-2005A-Q-11 and GS-2005B-Q-6, and GS-2008B-Q-56. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA and of data provided by the Central Bureau forAstronomical Telegrams. Publisher Copyright: {\textcopyright} 2017 The Authors.",
year = "2017",
month = dec,
day = "21",
doi = "10.1093/mnras/stx2300",
language = "English",
volume = "472",
pages = "4233--4243",
journal = "Monthly Notices of the Royal Astronomical Society: Letters",
issn = "1745-3925",
publisher = "Oxford University Press",
number = "4",
}