@article{e4406c88af024c2cb6cc8523423b94ee,
title = "Cosmology from cosmic shear power spectra with Subaru Hyper Suprime-Cam first-year data",
abstract = "We measure cosmic weak lensing shear power spectra with the Subaru Hyper Suprime- Cam (HSC) survey first-year shear catalog covering 137 deg2 of the sky. Thanks to the high effective galaxy number density of ∼17 arcmin-2, even after conservative cuts such as a magnitude cut of i < 24.5 and photometric redshift cut of 0.3 ≤ z ≤ 1.5, we obtain a high-significance measurement of the cosmic shear power spectra in four tomographic redshift bins, achieving a total signal-to-noise ratio of 16 in the multipole range 300 ≤ ℓ ≤ 1900. We carefully account for various uncertainties in our analysis including the intrinsic alignment of galaxies, scatters and biases in photometric redshifts, residual uncertainties in the shear measurement, and modeling of the matter power spectrum. The accuracy of our power spectrummeasurement method as well as our analytic model of the covariance matrix are tested against realistic mock shear catalogs. For a flat ∧ cold dark matter model, we find S8 ≡ σ8(Ωm/0.3)α = 0.800+0.029-0.028 for α = 0.45 (S8 = 0.780+0.030-0.033 for α = 0.5) from our HSC tomographic cosmic shear analysis alone. In comparison with Planck cosmic microwave background constraints, our results prefer slightly lower values of S8, although metrics such as the Bayesian evidence ratio test do not show significant evidence for discordance between these results. We study the effect of possible additional systematic errors that are unaccounted for in our fiducial cosmic shear analysis, and find that they can shift the best-fit values of S8 by up to ∼0.6 σ in both directions. The full HSC survey data will contain several times more area, and will lead to significantly improved cosmological constraints.",
keywords = "Dark matter, Gravitational lensing: weak, Large-scale structure of universe",
author = "Chiaki Hikage and Masamune Oguri and Takashi Hamana and Surhud More and Rachel Mandelbaum and Masahiro Takada and Fabian K{\"o}hlinger and Hironao Miyatake and Nishizawa, {Atsushi J.} and Hiroaki Aihara and Robert Armstrong and James Bosch and Jean Coupon and Anne Ducout and Paul Ho and Hsieh, {Bau Ching} and Yutaka Komiyama and Fran{\c c}ois Lanusse and Alexie Leauthaud and Lupton, {Robert H.} and Elinor Medezinski and Sogo Mineo and Shoken Miyama and Satoshi Miyazaki and Ryoma Murata and Hitoshi Murayama and Masato Shirasaki and Crist{\'o}bal Sif{\'o}n and Melanie Simet and Joshua Speagle and Spergel, {David N.} and Strauss, {Michael A.} and Naoshi Sugiyama and Masayuki Tanaka and Yousuke Utsumi and Wang, {Shiang Yu} and Yoshihiko Yamada",
note = "Funding Information: This work was supported in part by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, JSPS KAKENHI Grant Numbers JP15H03654, JP16K17684, JP16H01089, JP17H06599, JP18H04348, JP18K03693, and JP18H04350, MEXT Grants-in-Aid for Scientific Research on Innovative Areas (JP15H05887, JP15H05892, JP15H05893, and JP15K21733), and JST CREST Grant Number JPMJCR1414. HMi Funding Information: The Hyper Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University 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 the Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), the Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. 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>. Funding Information: and MSi are supported by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. RMa is supported by the Department of Energy Cosmic Frontier program, grant DE-SC0010118. Funding Information: We thank the referee, Catherine Heymans, for very useful comments and suggestions. We thank Michael Troxel for kindly providing the outputs of nested sampling with DES Y1 likelihoods. We also thank Ryuichi Takahashi, Chihway Chang, and David Alonso for their feedback that improved the quality of the paper. Our likelihood code is partly based on the likelihood code from K?hlinger et al. (2017), which is publicly available at https://bitbucket.org/fkoehlin/kids450-qe-likelihood-public. This work was supported in part by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, JSPS KAKENHI Grant Numbers JP15H03654, JP16K17684, JP16H01089, JP17H06599, JP18H04348, JP18K03693, and JP18H04350, MEXT Grants-in-Aid for Scientific Research on Innovative Areas (JP15H05887, JP15H05892, JP15H05893, and JP15K21733), and JST CREST Grant Number JPMJCR1414. HMi and MSi are supported by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with theNational Aeronautics and Space Administration. RMa is supported by the Department of Energy Cosmic Frontier program, grant DE-SC0010118. Data analysis was in part carried out on a PC cluster at the Center for Computational Astrophysics, National Astronomical Observatory of Japan. Numerical computations were in part carried out on a Cray XC30 at the Center for Computational Astrophysics, National Astronomical Observatory of Japan. Funding Information: 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, 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, Queen{\textquoteright}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) and the Los Alamos National Laboratory. Publisher Copyright: {\textcopyright} The Author(s) 2019.",
year = "2019",
month = apr,
day = "1",
doi = "10.1093/pasj/psz010",
language = "English (US)",
volume = "71",
journal = "Publication of the Astronomical Society of Japan",
issn = "0004-6264",
publisher = "Astronomical Society of Japan",
number = "2",
}