HSC Year 1 cosmology results with the minimal bias method: HSC$\times$BOSS galaxy-galaxy weak lensing and BOSS galaxy clustering

Autor: Sugiyama, Sunao, Takada, Masahiro, Miyatake, Hironao, Nishimichi, Takahiro, Shirasaki, Masato, Kobayashi, Yosuke, More, Surhud, Takahashi, Ryuichi, Osato, Ken, Oguri, Masamune, Coupon, Jean, Hikage, Chiaki, Hsieh, Bau-Ching, Komiyama, Yotaka, Leauthaud, Alexie, Li, Xiangchong, Luo, Wentao, Lupton, Robert H., Murayama, Hitoshi, Nishizawa, Atsushi J., Park, Youngsoo, Price, Paul A., Simet, Melanie, Speagle, Joshua S., Strauss, Michael A., Tanaka, Masayuki
Rok vydání: 2021
Předmět:
Druh dokumentu: Working Paper
DOI: 10.1103/PhysRevD.105.123537
Popis: We present cosmological parameter constraints from a blinded joint analysis of galaxy-galaxy weak lensing, $\Delta\!\Sigma(R)$, and projected correlation function, $w_\mathrm{p}(R)$, measured from the first-year HSC (HSC-Y1) data and SDSS spectroscopic galaxies over $0.150.75$ for the $\Delta\!\Sigma$ measurements, selected based on their photometric redshifts. For theoretical template, we use the "minimal bias" model for the cosmological clustering observables for the flat $\Lambda$CDM cosmological model. We compare the model predictions with the measurements in each redshift bin on large scales, $R>12$ and $8~h^{-1}\mathrm{Mpc}$ for $\Delta\!\Sigma(R)$ and $w_\mathrm{p}(R)$, respectively, where the perturbation theory-inspired model is valid. When we employ weak priors on cosmological parameters, without CMB information, we find $S_8=0.936^{+0.092}_{-0.086}$, $\sigma_8=0.85^{+0.16}_{-0.11}$, and $\Omega_\mathrm{m}=0.283^{+0.12}_{-0.035}$ for the flat $\Lambda$CDM model. Although the central value of $S_8$ 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. (abriged)
Comment: 24 pages, 19 figures, 4 tables, to be submitted to Phys. Rev. D
Databáze: arXiv
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