Cosmological inference from an emulator based halo model. II. Joint analysis of galaxy-galaxy weak lensing and galaxy clustering from HSC-Y1 and SDSS
Abstract
Here, we present high-fidelity cosmology results from a blinded joint analysis of galaxy-galaxy weak lensing (ΔΣ) and projected galaxy clustering (wp) measured from the Hyper Suprime-Cam Year-1 (HSC-Y1) data and spectroscopic Sloan Digital Sky Survey (SDSS) galaxy catalogs in the redshift range 0.15 < z < 0.7. We define luminosity-limited samples of SDSS galaxies to serve as the tracers of wp in three spectroscopic redshift bins, and as the lens samples for ΔΣ. For the ΔΣ measurements, we select a single sample of 4×106 source galaxies over 140 deg2 from HSC-Y1 with photometric redshifts (photo z) greater than 0.75, enabling a better handle of photo- z errors by comparing the ΔΣ amplitudes for the three lens redshift bins. The deep, high-quality HSC-Y1 data enable significant detections of the ΔΣ signals, with integrated signal-to-noise ratio S/N ~ 15 in the range 3 ≤ R/[h–1 Mpc] ≤ 30 for the three lens samples, despite the small area coverage. For cosmological parameter inference, we use an input galaxy-halo connection model built on the dark emulator package (which uses an ensemble set of high-resolution N-body simulations and enables fast, accurate computation of the clustering observables) with a halo occupation distribution that includes nuisance parameters to marginalize over modeling uncertainties. We model the ΔΣ and wp measurements on scales from R≃3 and 2h–1 Mpc , respectively, up to 30 h–1 Mpc (therefore excluding the baryon acoustic oscillations information) assuming a flat Λ CDM cosmology, marginalizing over about 20 nuisance parameters and demonstrating the robustness of our results to them. With various tests using mock catalogs described in Miyatake et al. [preceding paper, Phys. Rev. D 106, 083519 (2022)], we show that any bias in the clustering amplitude S8 ≡ σ8(Ωm/0.3)0.5 due to uncertainties in the galaxy-halo connection is less than ~ 50 % of the statistical uncertainty of S8, unless the assembly biaseffect is unexpectedly large. Our best-fit models have S8 = 0.795$$_{-0.042}^{+0.049}$$ (mode and 68% credible interval) for the flat Λ CDM model; we find tighter constraints on the quantity S8(α = 0.17)≡σ8(Ωm/0.3)0.17 = 0.745$$_{-0.031}^{+0.039}$$.
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[2];
[3];
[4];
[5];
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- Nagoya Univ. (Japan); Univ. of Tokyo (Japan). Kavli Institute for the Physics and Mathematics of the Universe (WPI); California Institute of Technology (CalTech), Pasadena, CA (United States)
- Univ. of Tokyo (Japan). Kavli Institute for the Physics and Mathematics of the Universe (WPI); Univ. of Tokyo (Japan). Dept. of Physics
- Univ. of Tokyo (Japan). Kavli Institute for the Physics and Mathematics of the Universe (WPI)
- Kyoto Univ. (Japan); Univ. of Tokyo (Japan). Kavli Institute for the Physics and Mathematics of the Universe (WPI)
- National Astronomical Observatory of Japan (Japan); Institute of Statistical Mathematics (Japan)
- Univ. of Arizona, Tucson, AZ (United States); Univ. of Tokyo (Japan). Kavli Institute for the Physics and Mathematics of the Universe (WPI)
- Carnegie Mellon Univ., Pittsburgh, PA (United States)
- Inter-University Centre for Astronomy and Astrophysics (IUCAA), Pune (India); Univ. of Tokyo (Japan). Kavli Institute for the Physics and Mathematics of the Universe (WPI)
- Chiba University (Japan); Univ. of Tokyo (Japan)
- Kyoto Univ. (Japan); Centre National de la Recherche Scientifique (CNRS) (France); Paris Sciences et Lettres University; Sorbonne Univ., Paris (France); Univ. of Paris (France)
- Hirosaki Univ. (Japan)
- Univ. of Geneva (Switzerland)
- Academia Sinica, Taipei (Taiwan)
- National Astronomical Observatory of Japan (Japan)
- Univ. of California, Santa Cruz, CA (United States)
- Carnegie Mellon Univ., Pittsburgh, PA (United States); Univ. of Tokyo (Japan). Kavli Institute for the Physics and Mathematics of the Universe (WPI)
- Univ. of Science and Technology of China, Hefei (China)
- Princeton Univ., NJ (United States)
- Univ. of California, Berkeley, CA (United States); Univ. of Tokyo (Japan). Kavli Institute for the Physics and Mathematics of the Universe (WPI); Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)
- Gifu Shotoku Gakuen University (Japan); Nagoya Univ. (Japan)
- Univ. of California, Riverside, CA (United States); California Institute of Technology (CalTech), Pasadena, CA (United States)
- Univ. of Toronto, ON (Canada)
- Univ. of Tokyo (Japan). Dept. of Physics; Univ. of Tokyo (Japan). Kavli Institute for the Physics and Mathematics of the Universe (WPI)
- Publication Date:
- Research Org.:
- Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), High Energy Physics (HEP)
- OSTI Identifier:
- 1992466
- Grant/Contract Number:
- AC02-05CH11231; SC0019301
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Physical Review. D.
- Additional Journal Information:
- Journal Volume: 106; Journal Issue: 8; Journal ID: ISSN 2470-0010
- Publisher:
- American Physical Society (APS)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; cosmology; dark energy; gravitational lenses
Citation Formats
Miyatake, Hironao, Sugiyama, Sunao, Takada, Masahiro, Nishimichi, Takahiro, Shirasaki, Masato, Kobayashi, Yosuke, Mandelbaum, Rachel, More, Surhud, Oguri, Masamune, Osato, Ken, Park, Youngsoo, Takahashi, Ryuichi, Coupon, Jean, Hikage, Chiaki, Hsieh, Bau-Ching, Komiyama, Yutaka, Leauthaud, Alexie, Li, Xiangchong, Luo, Wentao, Lupton, Robert H., Miyazaki, Satoshi, Murayama, Hitoshi, Nishizawa, Atsushi J., Price, Paul A., Simet, Melanie, Speagle, Joshua S., Strauss, Michael A., Tanaka, Masayuki, and Yoshida, Naoki. Cosmological inference from an emulator based halo model. II. Joint analysis of galaxy-galaxy weak lensing and galaxy clustering from HSC-Y1 and SDSS. United States: N. p., 2022.
Web. doi:10.1103/physrevd.106.083520.
Miyatake, Hironao, Sugiyama, Sunao, Takada, Masahiro, Nishimichi, Takahiro, Shirasaki, Masato, Kobayashi, Yosuke, Mandelbaum, Rachel, More, Surhud, Oguri, Masamune, Osato, Ken, Park, Youngsoo, Takahashi, Ryuichi, Coupon, Jean, Hikage, Chiaki, Hsieh, Bau-Ching, Komiyama, Yutaka, Leauthaud, Alexie, Li, Xiangchong, Luo, Wentao, Lupton, Robert H., Miyazaki, Satoshi, Murayama, Hitoshi, Nishizawa, Atsushi J., Price, Paul A., Simet, Melanie, Speagle, Joshua S., Strauss, Michael A., Tanaka, Masayuki, & Yoshida, Naoki. Cosmological inference from an emulator based halo model. II. Joint analysis of galaxy-galaxy weak lensing and galaxy clustering from HSC-Y1 and SDSS. United States. https://doi.org/10.1103/physrevd.106.083520
Miyatake, Hironao, Sugiyama, Sunao, Takada, Masahiro, Nishimichi, Takahiro, Shirasaki, Masato, Kobayashi, Yosuke, Mandelbaum, Rachel, More, Surhud, Oguri, Masamune, Osato, Ken, Park, Youngsoo, Takahashi, Ryuichi, Coupon, Jean, Hikage, Chiaki, Hsieh, Bau-Ching, Komiyama, Yutaka, Leauthaud, Alexie, Li, Xiangchong, Luo, Wentao, Lupton, Robert H., Miyazaki, Satoshi, Murayama, Hitoshi, Nishizawa, Atsushi J., Price, Paul A., Simet, Melanie, Speagle, Joshua S., Strauss, Michael A., Tanaka, Masayuki, and Yoshida, Naoki. Fri .
"Cosmological inference from an emulator based halo model. II. Joint analysis of galaxy-galaxy weak lensing and galaxy clustering from HSC-Y1 and SDSS". United States. https://doi.org/10.1103/physrevd.106.083520. https://www.osti.gov/servlets/purl/1992466.
@article{osti_1992466,
title = {Cosmological inference from an emulator based halo model. II. Joint analysis of galaxy-galaxy weak lensing and galaxy clustering from HSC-Y1 and SDSS},
author = {Miyatake, Hironao and Sugiyama, Sunao and Takada, Masahiro and Nishimichi, Takahiro and Shirasaki, Masato and Kobayashi, Yosuke and Mandelbaum, Rachel and More, Surhud and Oguri, Masamune and Osato, Ken and Park, Youngsoo and Takahashi, Ryuichi and Coupon, Jean and Hikage, Chiaki and Hsieh, Bau-Ching and Komiyama, Yutaka and Leauthaud, Alexie and Li, Xiangchong and Luo, Wentao and Lupton, Robert H. and Miyazaki, Satoshi and Murayama, Hitoshi and Nishizawa, Atsushi J. and Price, Paul A. and Simet, Melanie and Speagle, Joshua S. and Strauss, Michael A. and Tanaka, Masayuki and Yoshida, Naoki},
abstractNote = {Here, we present high-fidelity cosmology results from a blinded joint analysis of galaxy-galaxy weak lensing (ΔΣ) and projected galaxy clustering (wp) measured from the Hyper Suprime-Cam Year-1 (HSC-Y1) data and spectroscopic Sloan Digital Sky Survey (SDSS) galaxy catalogs in the redshift range 0.15 < z < 0.7. We define luminosity-limited samples of SDSS galaxies to serve as the tracers of wp in three spectroscopic redshift bins, and as the lens samples for ΔΣ. For the ΔΣ measurements, we select a single sample of 4×106 source galaxies over 140 deg2 from HSC-Y1 with photometric redshifts (photo z) greater than 0.75, enabling a better handle of photo- z errors by comparing the ΔΣ amplitudes for the three lens redshift bins. The deep, high-quality HSC-Y1 data enable significant detections of the ΔΣ signals, with integrated signal-to-noise ratio S/N ~ 15 in the range 3 ≤ R/[h–1 Mpc] ≤ 30 for the three lens samples, despite the small area coverage. For cosmological parameter inference, we use an input galaxy-halo connection model built on the dark emulator package (which uses an ensemble set of high-resolution N-body simulations and enables fast, accurate computation of the clustering observables) with a halo occupation distribution that includes nuisance parameters to marginalize over modeling uncertainties. We model the ΔΣ and wp measurements on scales from R≃3 and 2h–1 Mpc , respectively, up to 30 h–1 Mpc (therefore excluding the baryon acoustic oscillations information) assuming a flat Λ CDM cosmology, marginalizing over about 20 nuisance parameters and demonstrating the robustness of our results to them. With various tests using mock catalogs described in Miyatake et al. [preceding paper, Phys. Rev. D 106, 083519 (2022)], we show that any bias in the clustering amplitude S8 ≡ σ8(Ωm/0.3)0.5 due to uncertainties in the galaxy-halo connection is less than ~ 50 % of the statistical uncertainty of S8, unless the assembly biaseffect is unexpectedly large. Our best-fit models have S8 = 0.795$_{-0.042}^{+0.049}$ (mode and 68% credible interval) for the flat Λ CDM model; we find tighter constraints on the quantity S8(α = 0.17)≡σ8(Ωm/0.3)0.17 = 0.745$_{-0.031}^{+0.039}$.},
doi = {10.1103/physrevd.106.083520},
journal = {Physical Review. D.},
number = 8,
volume = 106,
place = {United States},
year = {Fri Oct 21 00:00:00 EDT 2022},
month = {Fri Oct 21 00:00:00 EDT 2022}
}
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Cosmological parameter constraints from galaxy–galaxy lensing and galaxy clustering with the SDSS DR7
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Full-shape cosmology analysis of the SDSS-III BOSS galaxy power spectrum using an emulator-based halo model: A 5% determination of
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