TY - JOUR
T1 - HSC Year 1 cosmology results with the minimal bias method
T2 - HSC ×bOSS galaxy-galaxy weak lensing and BOSS galaxy clustering
AU - Sugiyama, Sunao
AU - Takada, Masahiro
AU - Miyatake, Hironao
AU - Nishimichi, Takahiro
AU - Shirasaki, Masato
AU - Kobayashi, Yosuke
AU - Mandelbaum, Rachel
AU - More, Surhud
AU - Takahashi, Ryuichi
AU - Osato, Ken
AU - Oguri, Masamune
AU - Coupon, Jean
AU - Hikage, Chiaki
AU - Hsieh, Bau Ching
AU - Komiyama, Yutaka
AU - Leauthaud, Alexie
AU - Li, Xiangchong
AU - Luo, Wentao
AU - Lupton, Robert H.
AU - Murayama, Hitoshi
AU - Nishizawa, Atsushi J.
AU - Park, Youngsoo
AU - Price, Paul A.
AU - Simet, Melanie
AU - Speagle, Joshua S.
AU - Strauss, Michael A.
AU - Tanaka, Masayuki
N1 - Funding Information:
This work was supported in part by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and JSPS KAKENHI Grants No. JP15H03654, No. JP15H05887, No. JP15H05893, No. JP15H05896, No. JP15K21733, No. JP17H01131, No. JP17K14273, No. JP18H04350, No. JP18H04358, No. JP19H00677, No. JP19K14767, No. JP20H00181, No. JP20H01932, No. JP20H04723, No. JP20H05850, No. JP20H05855, No. JP20H05861, No. JP21J00011, No. JP20H05856, No. JP21H01081 and No. JP21J10314 by Japan Science and Technology Agency (JST) CREST JPMHCR1414, by JST AIP Acceleration Research Grant No JP20317829, Japan, and by Basic Research Grant (Super AI) of Institute for AI and Beyond of the University of Tokyo. S. S. is supported by International Graduate Program for Excellence in Earth-Space Science (IGPEES), World-leading Innovative Graduate Study (WINGS) Program, the University of Tokyo. H. M. and M. Si. were supported by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. K. O. is supported by JSPS Research Fellowships for Young Scientists. Y. K. was supported by the Advanced Leading Graduate Course for Photon Science at the University of Tokyo. 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 Japanese Cabinet Office, the Ministry 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. This paper makes use of software developed for the Vera C. Rubin LSST. We thank the LSST Project for making their code available as free software at . 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’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. J. S. S. is a Banting & Dunlap Fellow.
Publisher Copyright:
© 2022 American Physical Society.
PY - 2022/6/15
Y1 - 2022/6/15
N2 - We present cosmological parameter constraints from a blinded joint analysis of galaxy-galaxy weak lensing, Δς(R), and the projected correlation function, wp(R), measured from the first-year HSC (HSC-Y1) data and SDSS spectroscopic galaxies over 0.150.75 for the Δς measurements, selected based on their photometric redshifts. As a theoretical template, we use the "minimal bias"model for the cosmological clustering observables for the flat ΛCDM cosmological model. We compare the model predictions with the measurements in each redshift bin on large scales, R>12 and 8h-1 Mpc for Δς(R) and wp(R), respectively, where the perturbation-theory-inspired model is valid. As part of our model, we account for the effect of lensing magnification bias on the Δς measurements. When we employ weak priors on cosmological parameters, without cosmic microwave background (CMB) information, we find S8=0.936-0.086+0.092, σ8=0.85-0.11+0.16, and ωm=0.283-0.035+0.12 (mode and 68% credible interval) for the flat ΛCDM model. Although the central value of S8 appears to be larger than those inferred from other cosmological experiments, we find that the difference is consistent with expected differences due to sample variance, and our results are consistent with the other results to within the statistical uncertainties. When combined with the Planck 2018 likelihood for the primary CMB anisotropy information (TT,TE,EE+lowE), we find S8=0.817-0.021+0.022, σ8=0.892-0.056+0.051, ωm=0.246-0.035+0.045, and the equation-of-state parameter of dark energy, wde=-1.28-0.19+0.20 for the flat wCDM model, which is consistent with the flat ΛCDM model to within the error bars.
AB - We present cosmological parameter constraints from a blinded joint analysis of galaxy-galaxy weak lensing, Δς(R), and the projected correlation function, wp(R), measured from the first-year HSC (HSC-Y1) data and SDSS spectroscopic galaxies over 0.150.75 for the Δς measurements, selected based on their photometric redshifts. As a theoretical template, we use the "minimal bias"model for the cosmological clustering observables for the flat ΛCDM cosmological model. We compare the model predictions with the measurements in each redshift bin on large scales, R>12 and 8h-1 Mpc for Δς(R) and wp(R), respectively, where the perturbation-theory-inspired model is valid. As part of our model, we account for the effect of lensing magnification bias on the Δς measurements. When we employ weak priors on cosmological parameters, without cosmic microwave background (CMB) information, we find S8=0.936-0.086+0.092, σ8=0.85-0.11+0.16, and ωm=0.283-0.035+0.12 (mode and 68% credible interval) for the flat ΛCDM model. Although the central value of S8 appears to be larger than those inferred from other cosmological experiments, we find that the difference is consistent with expected differences due to sample variance, and our results are consistent with the other results to within the statistical uncertainties. When combined with the Planck 2018 likelihood for the primary CMB anisotropy information (TT,TE,EE+lowE), we find S8=0.817-0.021+0.022, σ8=0.892-0.056+0.051, ωm=0.246-0.035+0.045, and the equation-of-state parameter of dark energy, wde=-1.28-0.19+0.20 for the flat wCDM model, which is consistent with the flat ΛCDM model to within the error bars.
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U2 - 10.1103/PhysRevD.105.123537
DO - 10.1103/PhysRevD.105.123537
M3 - Article
AN - SCOPUS:85134752303
SN - 2470-0010
VL - 105
JO - Physical Review D
JF - Physical Review D
IS - 12
M1 - 123537
ER -