HSC Year 1 cosmology results with the minimal bias method: <math display="inline"><mrow><mi>HSC</mi><mo stretchy="false">×</mo><mi>BOSS</mi><mrow/></mrow></math> galaxy-galaxy weak lensing and BOSS galaxy clustering - INSPIRE

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

Sunao Sugiyama
(
- Tokyo U., IPMU and
- Tokyo U.
)
,
Masahiro Takada
(
- Tokyo U., IPMU
)
,
Hironao Miyatake
(
- Tokyo U., IPMU and
- KMI, Nagoya and
- Nagoya U., IAR and
- Nagoya U. and
- Caltech, JPL
)
,
Takahiro Nishimichi
(
- Tokyo U., IPMU and
- Kyoto U., Yukawa Inst., Kyoto
)
,
Masato Shirasaki
(
- Natl. Astron. Observ. of Japan and
- Tokyo U.
)

Nov 21, 2021

23 pages

Published in:

Phys.Rev.D 105 (2022) 12, 123537

Published: Jun 15, 2022

e-Print:

2111.10966 [astro-ph.CO]

DOI:

10.1103/PhysRevD.105.123537 (publication)

Report number:

IPMU21-0078,
YITP-21-126

View in:

reference search17 citations

Citations per year

Abstract: (APS)

We present cosmological parameter constraints from a blinded joint analysis of galaxy-galaxy weak lensing,

Δ Σ (R)

, and the projected correlation function,

w_{p} (R)

, measured from the first-year HSC (HSC-Y1) data and SDSS spectroscopic galaxies over

0.15 < z < 0.7

. We use luminosity-limited samples as lens samples for

Δ Σ

and as large-scale structure tracers for

w_{p}

in three redshift bins, and use the HSC-Y1 galaxy catalog to define a secure sample of source galaxies at

z_{ph} > 0.75

for the

Δ Σ

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

Λ CDM

cosmological model. We compare the model predictions with the measurements in each redshift bin on large scales,

R > 12

and

8 h^{- 1} Mpc

for

Δ Σ (R)

and

w_{p} (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

Δ Σ

measurements. When we employ weak priors on cosmological parameters, without cosmic microwave background (CMB) information, we find

S_{8} = 0.93 6_{- 0.086}^{+ 0.092}

,

σ_{8} = 0.8 5_{- 0.11}^{+ 0.16}

, and

Ω_{m} = 0.28 3_{- 0.035}^{+ 0.12}

(mode and 68% credible interval) for the flat

Λ 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. When combined with the Planck 2018 likelihood for the primary CMB anisotropy information (

TT, TE, EE + lowE

), we find

S_{8} = 0.81 7_{- 0.021}^{+ 0.022}

,

σ_{8} = 0.89 2_{- 0.056}^{+ 0.051}

,

Ω_{m} = 0.24 6_{- 0.035}^{+ 0.045}

, and the equation-of-state parameter of dark energy,

w_{de} = - 1.2 8_{- 0.19}^{+ 0.20}

for the flat

w CDM

model, which is consistent with the flat

Λ CDM

model to within the error bars.

Note:

24 pages, 19 figures, 4 tables, to be submitted to Phys. Rev. D

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