Faculty Profiles - MIYATAKE Hironao

Papers - MIYATAKE Hironao

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Hyper Suprime-Cam Year 3 results: Cosmology from cosmic shear power spectra Reviewed International coauthorship

Roohi Dalal, Xiangchong Li, Andrina Nicola, Joe Zuntz, Michael A. Strauss, Sunao Sugiyama, Tianqing Zhang, Markus M. Rau, Rachel Mandelbaum, Masahiro Takada, Surhud More, Hironao Miyatake, Arun Kannawadi, Masato Shirasaki, Takanori Taniguchi, Ryuichi Takahashi, Ken Osato, Takashi Hamana, Masamune Oguri, Atsushi J. Nishizawa, Andrés A.Plazas Malagón, Tomomi Sunayama, David Alonso, Anže Slosar, Wentao Luo, Robert Armstrong, James Bosch, Bau Ching Hsieh, Yutaka Komiyama, Robert H. Lupton, Nate B. Lust, Lauren A. Macarthur, Satoshi Miyazaki, Hitoshi Murayama, Takahiro Nishimichi, Yuki Okura, Paul A. Price, Philip J. Tait, Masayuki Tanaka, Shiang Yu Wang

Physical Review D Vol. 108 ( 12 ) 2023.12

Language：English Publishing type：Research paper (scientific journal)

We measure weak lensing cosmic shear power spectra from the 3-year galaxy shear catalog of the Hyper Suprime-Cam (HSC) Subaru Strategic Program imaging survey. The shear catalog covers 416 deg2 of the northern sky, with a mean i-band seeing of 0.59 arcsec and an effective galaxy number density of 15 arcmin-2 within our adopted redshift range. With an i-band magnitude limit of 24.5 mag, and four tomographic redshift bins spanning 0.3≤zph≤1.5 based on photometric redshifts, we obtain a high-significance measurement of the cosmic shear power spectra, with a signal-to-noise ratio of approximately 26.4 in the multipole range 300<ℓ<1800. The accuracy of our power spectrum measurement is tested against realistic mock shear catalogs, and we use these catalogs to get a reliable measurement of the covariance of the power spectrum measurements. We use a robust blinding procedure to avoid confirmation bias, and model various uncertainties and sources of bias in our analysis, including point spread function systematics, redshift distribution uncertainties, the intrinsic alignment of galaxies and the modeling of the matter power spectrum. For a flat ΛCDM model, we find S8σ8(ωm/0.3)0.5=0.776-0.033+0.032, which is in excellent agreement with the constraints from the other HSC Year 3 cosmology analyses, as well as those from a number of other cosmic shear experiments. This result implies a ∼2σ-level tension with the Planck 2018 cosmology. We study the effect that various systematic errors and modeling choices could have on this value, and find that they can shift the best-fit value of S8 by no more than ∼0.5σ, indicating that our result is robust to such systematics.

DOI： 10.1103/PhysRevD.108.123519

Hyper Suprime-Cam Year 3 results: Measurements of clustering of SDSS-BOSS galaxies, galaxy-galaxy lensing, and cosmic shear Reviewed International coauthorship

Surhud More, Sunao Sugiyama, Hironao Miyatake, Markus Michael Rau, Masato Shirasaki, Xiangchong Li, Atsushi J. Nishizawa, Ken Osato, Tianqing Zhang, Masahiro Takada, Takashi Hamana, Ryuichi Takahashi, Roohi Dalal, Rachel Mandelbaum, Michael A. Strauss, Yosuke Kobayashi, Takahiro Nishimichi, Masamune Oguri, Wentao Luo, Arun Kannawadi, Bau Ching Hsieh, Robert Armstrong, James Bosch, Yutaka Komiyama, Robert H. Lupton, Nate B. Lust, Lauren A. Macarthur, Satoshi Miyazaki, Hitoshi Murayama, Yuki Okura, Paul A. Price, Philip J. Tait, Masayuki Tanaka, Shiang Yu Wang

Physical Review D Vol. 108 ( 12 ) 2023.12

Language：English Publishing type：Research paper (scientific journal)

We utilize the Sloan Digital Sky Survey Baryon Oscillation Spectroscopic Survey (SDSS-BOSS) galaxies and its overlap with approximately 416 sq degrees of deep grizy-band imaging from the Subaru Hyper Suprime-Cam Survey (HSC). We perform measurements of three two-point correlations which form the basis of the cosmological inference presented in our companion papers, Miyatake et al. and Sugiyama et al. We use three approximately volume limited subsamples of spectroscopic galaxies by their i-band magnitude from the SDSS-BOSS: LOWZ (0.1<z<0.35), CMASS1 (0.43<z<0.55) and CMASS2 (0.55<z<0.7), respectively. We present high signal-to-noise ratio measurements of the projected correlation functions of these galaxies, which is expected to be proportional to the projected matter correlation function on large scales with a proportionality constant dependent on the bias of galaxies. In order to help break the degeneracy between the amplitude of the matter correlation and the bias of these spectroscopic galaxies, we use the distortions of the shapes of fainter galaxies in HSC due to weak gravitational lensing, to measure the galaxy-galaxy lensing signal, which probes the projected galaxy-matter cross-correlation function of the SDSS-BOSS galaxies. We also measure the cosmic shear correlation functions from HSC galaxies which is related to the projected matter correlation function. We demonstrate the robustness of our measurements by subjecting each of them to a variety of systematic tests. Our use of a single sample of HSC source galaxies is crucial to calibrate any residual systematic biases in the inferred redshifts of our galaxies. We also describe the construction of a suite of mocks: (i) spectroscopic galaxy catalogs which obey the clustering and abundance of each of the three SDSS-BOSS subsamples, and (ii) galaxy shape catalogs which obey the footprint of the HSC survey and have been appropriately sheared by the large-scale structure expected in a Λ Cold Dark Matter model. We use these mock catalogs to compute the covariance of each of our observables.

DOI： 10.1103/PhysRevD.108.123520

Hyper Suprime-Cam Year 3 results: Cosmology from galaxy clustering and weak lensing with HSC and SDSS using the minimal bias model Reviewed International coauthorship

Sunao Sugiyama, Hironao Miyatake, Surhud More, Xiangchong Li, Masato Shirasaki, Masahiro Takada, Yosuke Kobayashi, Ryuichi Takahashi, Takahiro Nishimichi, Atsushi J. Nishizawa, Markus M. Rau, Tianqing Zhang, Roohi Dalal, Rachel Mandelbaum, Michael A. Strauss, Takashi Hamana, Masamune Oguri, Ken Osato, Arun Kannawadi, Bau Ching Hsieh, Wentao Luo, Robert Armstrong, James Bosch, Yutaka Komiyama, Robert H. Lupton, Nate B. Lust, Satoshi Miyazaki, Hitoshi Murayama, Yuki Okura, Paul A. Price, Philip J. Tait, Masayuki Tanaka, Shiang Yu Wang

Physical Review D Vol. 108 ( 12 ) 2023.12

Language：English Publishing type：Research paper (scientific journal)

We present cosmological parameter constraints from a blind joint analysis of three two-point correlation functions measured from the Year 3 Hyper Suprime-Cam (HSC-Y3) imaging data, covering about 416 deg2, and the SDSS DR11 spectroscopic galaxies spanning the redshift range [0.15, 0.70]. We subdivide the SDSS galaxies into three luminosity-cut, and therefore nearly volume-limited samples separated in redshift, each of which acts as a large-scale structure tracer characterized by the measurement of the projected correlation function, wp(R). We also use the measurements of the galaxy-galaxy weak-lensing signal Δς(R) for each of these SDSS samples which act as lenses for a secure sample of source galaxies selected from the HSC-Y3 shape catalog based on their photometric redshifts. We combine these measurements with the cosmic shear correlation functions, ζ± measured for our HSC source sample. We model these observables with the minimal bias model of the galaxy clustering observables in the context of a flat ΛCDM cosmology. We use conservative scale cuts, R>12 and 8h-1 Mpc for Δς and wp, respectively, where the minimal bias model is valid, in addition to conservative prior on the residual bias in the mean redshift of the HSC photometric source galaxies. We present various validation tests of our model as well as analysis methods. Our baseline analysis yields S8=0.775-0.038+0.043 (68% C.I.) for the ΛCDM model, after marginalizing over uncertainties in other parameters. Our value of S8 is consistent with that from the Planck 2018 data, but the credible interval of our result is still relatively large. We show that various internal consistency tests based on different splits of the data are passed. Our results are statistically consistent with those of a companion paper, which extends this analysis to smaller scales with an emulator-based halo model, using Δς(R) and wp(R) down to R>3 and 2h-1 Mpc, respectively.

DOI： 10.1103/PhysRevD.108.123521

Hyper Suprime-Cam Year 3 results: Cosmology from cosmic shear two-point correlation functions Reviewed International coauthorship

Xiangchong Li, Tianqing Zhang, Sunao Sugiyama, Roohi Dalal, Ryo Terasawa, Markus M. Rau, Rachel Mandelbaum, Masahiro Takada, Surhud More, Michael A. Strauss, Hironao Miyatake, Masato Shirasaki, Takashi Hamana, Masamune Oguri, Wentao Luo, Atsushi J. Nishizawa, Ryuichi Takahashi, Andrina Nicola, Ken Osato, Arun Kannawadi, Tomomi Sunayama, Robert Armstrong, James Bosch, Yutaka Komiyama, Robert H. Lupton, Nate B. Lust, Lauren A. Macarthur, Satoshi Miyazaki, Hitoshi Murayama, Takahiro Nishimichi, Yuki Okura, Paul A. Price, Philip J. Tait, Masayuki Tanaka, Shiang Yu Wang

Physical Review D Vol. 108 ( 12 ) 2023.12

Language：English Publishing type：Research paper (scientific journal)

We perform a blinded cosmology analysis with cosmic shear two-point correlation functions measured from more than 25 million galaxies in the Hyper Suprime-Cam three-year shear catalog in four tomographic redshift bins ranging from 0.3 to 1.5. After conservative masking and galaxy selection, the survey covers 416 deg2 of the northern sky with an effective galaxy number density of 15 arcmin-2 over the four redshift bins. The 2PCFs adopted for cosmology analysis are measured in the angular range; 7.1<θ/arcmin<56.6 for ζ+ and 31.2<θ/arcmin<248 for ζ-, with a total signal-to-noise ratio of 26.6. We apply a conservative, wide, flat prior on the photometric redshift errors on the last two tomographic bins, and the relative magnitudes of the cosmic shear amplitude across four redshift bins allow us to calibrate the photometric redshift errors. With this flat prior on redshift errors, we find ωm=0.256-0.044+0.056 and S8σ8ωm/0.3=0.769-0.034+0.031 (both 68% C.I.) for a flat Λ cold dark matter cosmology. We find, after unblinding, that our constraint on S8 is consistent with the Fourier space cosmic shear and the 3×2 pt analyses on the same HSC dataset. We carefully study the potential systematics from astrophysical and systematic model uncertainties in our fiducial analysis using synthetic data, and report no biases (including projection bias in the posterior space) greater than 0.5σ in the estimation of S8. Our analysis hints that the mean redshifts of the two highest tomographic bins are higher than initially estimated. In addition, a number of consistency tests are conducted to assess the robustness of our analysis. Comparing our result with Planck-2018 cosmic microwave background observations, we find a ∼2σ tension for the ΛCDM model.

DOI： 10.1103/PhysRevD.108.123518

Robustness of baryon acoustic oscillations measurements with photometric redshift uncertainties Reviewed

Ishikawa, K; Sunayama, T; Nishizawa, AJ; Miyatake, H; Nishimichi, T

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 526 ( 4 ) page： 5374 - 5385 2023.10

Language：English Publishing type：Research paper (scientific journal) Publisher：Monthly Notices of the Royal Astronomical Society

We investigate the robustness of baryon acoustic oscillations (BAO) measurements with a photometric galaxy sample using mock galaxy catalogues with various sizes of photometric redshift (photo-z) uncertainties. We first conduct the robustness of BAO measurements, assuming we have a perfect knowledge of photo-z uncertainties. We find that the BAO shift parameter α can be constrained in an unbiased manner even for 3 per cent photometric redshift uncertainties up to z ∼ 1. For instance, α = 1.006 ± 0.078 with 95 per cent confidence level is obtained from 3 per cent photo-z uncertainty data at z = 1.03 using the sample of M∗ ≥ 1010.25 M☉ h−2. We also find that a sparse galaxy sample, e.g. <2 × 10−4 [h Mpc−1]3, causes additional noise in the covariance matrix calculation and can bias the constraint on α. Following this, we look into the scenario where incorrect photometric redshift uncertainties are assumed in the fitting model. We find that underestimating the photo-z uncertainty leads to a degradation in the constraining power on α. However, the constrained value of α is not biased. We also quantify the constraining power on Ωm0 assuming the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST)-like covariance and find that the 95 per cent confidence level is σ(Ωm0) ∼ 0.03–0.05 corresponding to the photo-z uncertainties of 1–3 per cent, respectively. Finally, we examine whether the skewness in the photometric redshift can bias the constraint on α and confirm that the constraint on α is unbiased, even assuming a Gaussian photo-z uncertainty in our model.

DOI： 10.1093/mnras/stad3078

A general framework for removing point-spread function additive systematics in cosmological weak lensing analysis Reviewed International coauthorship

Zhang, TQ; Li, XC; Dalal, R; Mandelbaum, R; Strauss, MA; Kannawadi, A; Miyatake, H; Nicola, A; Malagón, AAP; Shirasaki, M; Sugiyama, S; Takada, M; More, S

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 525 ( 2 ) page： 2441 - 2471 2023.10

Language：English Publishing type：Research paper (scientific journal) Publisher：Monthly Notices of the Royal Astronomical Society

Cosmological weak lensing measurements rely on a precise measurement of the shear two-point correlation function (2PCF) along with a deep understanding of systematics that affect it. In this work, we demonstrate a general framework for detecting and modelling the impact of PSF systematics on the cosmic shear 2PCF and mitigating its impact on cosmological analysis. Our framework can detect PSF leakage and modelling error from all spin-2 quantities contributed by the PSF second and higher moments, rather than just the second moments, using the cross-correlations between galaxy shapes and PSF moments. We interpret null tests using the HSC Year 3 (Y3) catalogs with this formalism and find that leakage from the spin-2 combination of PSF fourth moments is the leading contributor to additive shear systematics, with total contamination that is an order-of-magnitude higher than that contributed by PSF second moments alone. We conducted a mock cosmic shear analysis for HSC Y3 and find that, if uncorrected, PSF systematics can bias the cosmological parameters m and S8 by ∼0.3σ. The traditional second moment-based model can only correct for a 0.1σ bias, leaving the contamination largely uncorrected. We conclude it is necessary to model both PSF second and fourth moment contaminations for HSC Y3 cosmic shear analysis. We also reanalyse the HSC Y1 cosmic shear analysis with our updated systematics model and identify a 0.07σ bias on m when using the more restricted second moment model from the original analysis. We demonstrate how to self-consistently use the method in both real space and Fourier space, assess shear systematics in tomographic bins, and test for PSF model overfitting.

DOI： 10.1093/mnras/stad1801

Weak lensing tomographic redshift distribution inference for the Hyper Suprime-Cam Subaru Strategic Program three-year shape catalogue Reviewed International coauthorship

Rau, MM; Dalal, R; Zhang, TQ; Li, XC; Nishizawa, AJ; More, S; Mandelbaum, R; Miyatake, H; Strauss, MA; Takada, M

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 524 ( 4 ) page： 5109 - 5131 2023.7

Language：English Publishing type：Research paper (scientific journal) Publisher：Monthly Notices of the Royal Astronomical Society

We present posterior sample redshift distributions for the Hyper Suprime-Cam Subaru Strategic Program Weak Lensing three-year (HSC Y3) analysis. Using the galaxies' photometry and spatial cross-correlations, we conduct a combined Bayesian Hierarchical Inference of the sample redshift distributions. The spatial cross-correlations are derived using a subsample of Luminous Red Galaxies (LRGs) with accurate redshift information available up to a photometric redshift of z < 1.2. We derive the photometry-based constraints using a combination of two empirical techniques calibrated on spectroscopic and multiband photometric data that cover a spatial subset of the shear catalogue. The limited spatial coverage induces a cosmic variance error budget that we include in the inference. Our cross-correlation analysis models the photometric redshift error of the LRGs to correct for systematic biases and statistical uncertainties. We demonstrate consistency between the sample redshift distributions derived using the spatial cross-correlations, the photometry, and the posterior of the combined analysis. Based on this assessment, we recommend conservative priors for sample redshift distributions of tomographic bins used in the three-year cosmological Weak Lensing analyses.

DOI： 10.1093/mnras/stad1962

KiDS-1000: Combined halo-model cosmology constraints from galaxy abundance, galaxy clustering and galaxy-galaxy lensing Reviewed International coauthorship

Andrej Dvornik, Catherine Heymans, Marika Asgari, Constance Mahony, Benjamin Joachimi, Maciej Bilicki, Elisa Chisari, Hendrik Hildebrandt, Henk Hoekstra, Harry Johnston, Konrad Kuijken, Alexander Mead, Hironao Miyatake, Takahiro Nishimichi, Robert Reischke, Sandra Unruh, Angus H. Wright

Astronomy & Astrophysics Vol. 675 page： A189 2023.7

Language：English Publishing type：Research paper (scientific journal)

We present constraints on the flat $\Lambda$CDM cosmological model through a
joint analysis of galaxy abundance, galaxy clustering and galaxy-galaxy lensing
observables with the Kilo-Degree Survey. Our theoretical model combines a
flexible conditional stellar mass function, to describe the galaxy-halo
connection, with a cosmological N-body simulation-calibrated halo model to
describe the non-linear matter field. Our magnitude-limited bright galaxy
sample combines 9-band optical-to-near-infrared photometry with an extensive
and complete spectroscopic training sample to provide accurate redshift and
stellar mass estimates. Our faint galaxy sample provides a background of
accurately calibrated lensing measurements. We constrain the structure growth
parameter $S_8=\sigma_8\sqrt{\Omega_{\mathrm{m } }/0.3}=0.773^{+0.028}_{-0.030}$,
and the matter density parameter $\Omega_{\mathrm{m } }=0.290^{+0.021}_{-0.017}$.
The galaxy-halo connection model adopted in the work is shown to be in
agreement with previous studies. Our constraints on cosmological parameters are
comparable to, and consistent with, joint $3\times2{\mathrm{pt } }$
clustering-lensing analyses that additionally include a cosmic shear
observable. This analysis therefore brings attention to the significant
constraining power in the often-excluded non-linear scales for galaxy
clustering and galaxy-galaxy lensing observables. By adopting a theoretical
model that accounts for non-linear halo bias, halo exclusion, scale-dependent
galaxy bias and the impact of baryon feedback, this work demonstrates the
potential and a way forward to include non-linear scales in cosmological
analyses. Varying the width of the satellite galaxy distribution with an
additional parameter yields a strong preference for sub-Poissonian variance,
improving the goodness of fit by 0.18 in reduced $\chi^{2}$ value compared to a
fixed Poisson distribution.

DOI： 10.1051/0004-6361/202245158

Other Link： http://arxiv.org/pdf/2210.03110v2

Cosmological gravity probes: connecting recent theoretical developments to forthcoming observations Reviewed

Shun Arai, Katsuki Aoki, Yuji Chinone, Rampei Kimura, Tsutomu Kobayashi, Hironao Miyatake, Daisuke Yamauchi, Shuichiro Yokoyama, Kazuyuki Akitsu, Takashi Hiramatsu, Shin’ichi Hirano, Ryotaro Kase, Taishi Katsuragawa, Yosuke Kobayashi, Toshiya Namikawa, Takahiro Nishimichi, Teppei Okumura, Maresuke Shiraishi, Masato Shirasaki, Tomomi Sunayama, Kazufumi Takahashi, Atsushi Taruya, Junsei Tokuda

Progress of Theoretical and Experimental Physics Vol. 2023 ( 7 ) 2023.7

Language：English Publishing type：Research paper (scientific journal) Publisher：Oxford University Press (OUP)

Abstract

Since the discovery of the accelerated expansion of the present Universe, significant theoretical developments have been made in the area of modified gravity. In the meantime, cosmological observations have been providing more high-quality data, allowing us to explore gravity on cosmological scales. To bridge the recent theoretical developments and observations, we present an overview of a variety of modified theories of gravity and the cosmological observables in the cosmic microwave background and large-scale structure, supplemented with a summary of predictions for cosmological observables derived from cosmological perturbations and sophisticated numerical studies. We specifically consider scalar-tensor theories in the Horndeski and DHOST family, massive gravity/bigravity, vector-tensor theories, metric-affine gravity, and cuscuton/minimally-modified gravity, and discuss the current status of those theories with emphasis on their physical motivations, validity, appealing features, the level of maturity, and calculability. We conclude that the Horndeski theory is one of the most well-developed theories of modified gravity, although several remaining issues are left for future observations. The paper aims to help to develop strategies for testing gravity with ongoing and forthcoming cosmological observations.

DOI： 10.1093/ptep/ptad052

Galaxy clustering from the bottom up: a streaming model emulator I Reviewed International coauthorship

Cuesta-Lazaro, C; Nishimichi, T; Kobayashi, Y; Ruan, CZ; Eggemeier, A; Miyatake, H; Takada, M; Yoshida, N; Zarrouk, P; Baugh, CM; Bose, S; Li, BJ

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 523 ( 3 ) page： 3219 - 3238 2023.6

Language：English Publishing type：Research paper (scientific journal) Publisher：Monthly Notices of the Royal Astronomical Society

In this series of papers, we present a simulation-based model for the non-linear clustering of galaxies based on separate modelling of clustering in real space and velocity statistics. In the first paper, we present an emulator for the real-space correlation function of galaxies, whereas the emulator of the real-to-redshift space mapping based on velocity statistics is presented in the second paper. Here, we show that a neural network emulator for real-space galaxy clustering trained on data extracted from the dark quest suite of N-body simulations achieves sub-per cent accuracies on scales 1 < r < 30 h-1 Mpc, and better than 3 per cent on scales r < 1 h-1 Mpc in predicting the clustering of dark-matter haloes with number density 10-3.5 (h-1 Mpc)-3, close to that of SDSS LOWZ-like galaxies. The halo emulator can be combined with a galaxy-halo connection model to predict the galaxy correlation function through the halo model. We demonstrate that we accurately recover the cosmological and galaxy-halo connection parameters when galaxy clustering depends only on the mass of the galaxies' host halos. Furthermore, the constraining power in σ8 increases by about a factor of 2 when including scales smaller than 5h-1 Mpc. However, when mass is not the only property responsible for galaxy clustering, as observed in hydrodynamical or semi-analytic models of galaxy formation, our emulator gives biased constraints on σ8. This bias disappears when small scales (r < 10 h-1 Mpc) are excluded from the analysis. This shows that a vanilla halo model could introduce biases into the analysis of future data sets.

DOI： 10.1093/mnras/stad1207

The eROSITA Final Equatorial-Depth Survey (eFEDS) - Splashback radius of X-ray galaxy clusters using galaxies from HSC survey Reviewed International coauthorship

Rana, D; More, S; Miyatake, H; Grandis, S; Klein, M; Bulbul, E; Chiu, IN; Miyazaki, S; Bahcall, N

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 522 ( 3 ) page： 4181 - 4195 2023.5

Language：English Publishing type：Research paper (scientific journal) Publisher：Monthly Notices of the Royal Astronomical Society

We present the splashback radius measurements around the SRG/eROSITA eFEDS X-ray selected galaxy clusters by cross-correlating them with HSC S19A photometric galaxies. The X-ray selection is expected to be less affected by systematics related to projection that affects optical cluster finder algorithms. We use a nearly volume-limited sample of 109 galaxy clusters selected in 0.5-2.0 keV band having luminosity LX > 1043.5 erg s−1 h−2 within the redshift z < 0.75 and obtain measurements of the projected cross-correlation with a signal to noise of 17.43. We model our measurements to infer a 3D profile and find that the steepest slope is sharper than −3 and associate the location with the splashback radius. We infer the value of the 3D splashback radius rsp = 1.45+−002630 h−1 Mpc. We also measure the weak-lensing signal of the galaxy clusters and obtain halo mass log[M200m/h−1 M☉] = 14.52 ± 0.06 using the HSC-S16A shape catalogue data at the median redshift z = 0.46 of our cluster sample. We compare our rsp values with the spherical overdensity boundary r200m = 1.75 ± 0.08 h−1 Mpc based on the halo mass, which is consistent within 1.2σ with the ЛCDM predictions. Our constraints on the splashback radius, although broad, are the best measurements thus far obtained for an X-ray selected galaxy cluster sample.

DOI： 10.1093/mnras/stad1239

Galaxy clusters at z ∼ 1 imaged by ALMA with the Sunyaev–Zel’dovich effect Reviewed International coauthorship

Tetsu Kitayama, Shutaro Ueda, Nobuhiro Okabe, Takuya Akahori, Matt Hilton, John P. Hughes, Yuto Ichinohe, Kotaro Kohno, Eiichiro Komatsu, Yen Ting Lin, Hironao Miyatake, Masamune Oguri, Cristóbal Sifón, Shigehisa Takakuwa, Motokazu Takizawa, Takahiro Tsutsumi, Joshiwa van Marrewijk, Edward J. Wollack

Publications of the Astronomical Society of Japan Vol. 75 ( 2 ) page： 311 - 337 2023.4

Language：English Publishing type：Research paper (scientific journal)

We present high angular resolution measurements of the thermal Sunyaev–Zel’dovich effect (SZE) toward two galaxy clusters, RCS J2319+0038 at z = 0.9 and HSC J0947−0119 at z = 1.1, by the Atacama Large Millimeter/submillimeter Array (ALMA) in Band 3. They are supplemented with available Chandra X-ray data, optical data taken by Hyper Suprime-Cam on Subaru, and millimeter-wave SZE data from the Atacama Cosmology Telescope. Taking into account departures from spherical symmetry, we have reconstructed non-parametrically the inner pressure profile of two clusters as well as electron temperature and density profiles for RCS J2319+0038. This is one of the first such measurements for an individual cluster at z ≳ 0.9. We find that the inner pressure profile of both clusters is much shallower than that of local cool-core clusters. Our results consistently suggest that RCS J2319+0038 hosts a weak cool core, where radiative cooling is less significant than in local cool cores. On the other hand, HSC J0947−0119 exhibits an even shallower pressure profile than RCS J2319+0038 and is more likely to be a non-cool-core cluster. The SZE centroid position is offset by more than 140 h−170 kpc from the peaks of galaxy distribution in HSC J0947−0119, suggesting a stronger influence of mergers in this cluster. We conclude that these distant clusters are at a very early stage of developing the cool cores typically found in clusters at lower redshifts.

DOI： 10.1093/pasj/psac110

A unified catalogue-level reanalysis of stage-III cosmic shear surveys Reviewed International coauthorship

Longley, EP; Chang, C; Walter, CW; Zuntz, J; Ishak, M; Mandelbaum, R; Miyatake, H; Nicola, A; Pedersen, EM; Pereira, MES; Prat, J; Sánchez, J; Secco, LF; Tröster, T; Troxel, M; Wright, AH

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 520 ( 4 ) page： 5016 - 5041 2023.2

Language：English Publishing type：Research paper (scientific journal) Publisher：Monthly Notices of the Royal Astronomical Society

Cosmological parameter constraints from recent galaxy imaging surveys are reaching percent-level accuracy on the effective amplitude of the lensing signal, S8. The upcoming Legacy Survey of Space and Time (LSST) of the Vera C. Rubin Observatory will produce subpercent level measurements of cosmological parameters, providing a milestone test of the CDM model. To supply guidance to the upcoming LSST analysis, it is important to understand thoroughly the results from different recent galaxy imaging surveys and assess their consistencies. In this work, we perform a unified catalogue-level reanalysis of three cosmic shear data sets: the first year data from the Dark Energy Survey (DES-Y1), the 1000 deg2 data set from the Kilo-Degree Survey (KiDS-1000), and the first year data from the Hyper Suprime-Cam Subaru Strategic Program (HSC-Y1). We utilize a pipeline developed and rigorously tested by the LSST Dark Energy Science Collaboration to perform the reanalysis and assess the robustness of the results to analysis choices. We find the S8 constraint to be robust to two different small-scale modelling approaches, and varying choices of cosmological priors. Our unified analysis allows the consistency of the surveys to be rigorously tested, and we find the three surveys to be statistically consistent. Due to the partially overlapping footprint, we model the cross-covariance between KiDS-1000 and HSC-Y1 approximately when combining all three data sets, resulting in a 1.6–1.9 per cent constraint on S8 given different assumptions on the cross-covariance.

DOI： 10.1093/mnras/stad246

Cluster cosmology with anisotropic boosts: validation of a novel forward modelling analysis and application on SDSS redMaPPer clusters Reviewed International coauthorship

Park, Y; Sunayama, T; Takada, M; Kobayashi, Y; Miyatake, H; More, S; Nishimichi, T; Sugiyama, S

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 518 ( 4 ) page： 5171 - 5189 2023.2

Language：English Publishing type：Research paper (scientific journal) Publisher：Monthly Notices of the Royal Astronomical Society

We present a novel analysis for cluster cosmology that fully forward models the abundances, weak lensing, and the clustering of galaxy clusters. Our analysis notably includes an empirical model for the anisotropic boosts impacting the lensing and clustering signals of optical clusters. These boosts arise from a preferential selection of clusters surrounded by anisotropic large-scale structure, a consequence of the limited discrimination between line-of-sight interlopers and true cluster members offered by photometric surveys. We validate our analysis via a blind cosmology challenge on mocks, and find that we can obtain tight and unbiased cosmological constraints without informative priors or external calibrations on any of our model parameters. We then apply our analysis on the SDSS redMaPPer clusters, and find results favoring low cm and high σ8, combining to yield the lensing strength constraint S8 = 0.715-0.021+0.024. We investigate potential drivers behind these results through a series of post-unblinding tests, noting that our results are consistent with existing cluster cosmology constraints but clearly inconsistent with other CMB/LSS based cosmology results. From these tests, we find hints that a suppression in the cluster lensing signal may be driving our results.

DOI： 10.1093/mnras/stac3410

The eROSITA Final Equatorial-Depth Survey (eFEDS) Reviewed International coauthorship

N. Ota, N. T. Nguyen-Dang, I. Mitsuishi, M. Oguri, M. Klein, N. Okabe, M. E. Ramos-Ceja, T. H. Reiprich, F. Pacaud, E. Bulbul, M. Brüggen, A. Liu, K. Migkas, I. Chiu, V. Ghirardini, S. Grandis, Y.-T. Lin, H. Miyatake, S. Miyazaki, J. S. Sanders

Astronomy & Astrophysics Vol. 669 page： A110 - A110 2023.1

Language：English Publishing type：Research paper (scientific journal) Publisher：EDP Sciences

Context. We present the results of a systematic X-ray analysis of optically rich galaxy clusters detected by the Subaru Hyper Suprime-Cam (HSC) survey in the eROSITA Final Equatorial-Depth Survey (eFEDS) field.

Aims. Through a joint analysis of the SRG (Spectrum Roentgen Gamma)/eROSITA and Subaru/HSC surveys, we aim to investigate the dynamical status of the optically selected clusters and to derive the cluster scaling relations.

Methods. The sample consists of 43 optically selected galaxy clusters with a richness >40 in the redshift range of 0.16–0.89. We systematically analyzed the X-ray images and emission spectra using the eROSITA data. We identified the brightest cluster galaxy (BCG) using the optical and far-infrared databases. We evaluated the cluster’s dynamical status by measuring three quantities: offset between the X-ray peak and BCG position, the gas concentration parameter, and the number of galaxy-density peaks. We investigated the luminosity–temperature and mass–luminosity relations based on eROSITA X-ray spectra and HSC weak-lensing data analyses.

Results. Based on these three measurements, we estimated the fraction of relaxed clusters to be 2(< 39)%, which is smaller than that of the X-ray-selected cluster samples. After correcting for a selection bias due to the richness cut, we obtained a shallow L−T slope of 2.1 ± 0.5, which is consistent with the predictions of the self-similar model and the baseline model incorporating a mass–concentration relation. The L−M slope of 1.5 ± 0.3 is in agreement with the above-cited theoretical models as well as the data on the shear-selected clusters in the eFEDs field.

Conclusions. Our analysis of high-richness optical clusters yields a small fraction of relaxed clusters and a shallow slope for the luminosity–temperature relation. This suggests that the average X-ray properties of the optical clusters are likely to be different from those observed in the X-ray samples. Thus, the joint eROSITA and HSC observations are a powerful tool in extending the analysis to a larger sample and understanding the selection effect with a view to establish cluster scaling relations.

DOI： 10.1051/0004-6361/202244260

Consistent lensing and clustering in a low-<i>S</i><sub>8</sub> Universe with BOSS, DES Year 3, HSC Year 1, and KiDS-1000 Reviewed International coauthorship

Amon, A; Robertson, NC; Miyatake, H; Heymans, C; White, M; DeRose, J; Yuan, S; Wechsler, RH; Varga, TN; Bocquet, S; Dvornik, A; More, S; Ross, AJ; Hoekstra, H; Alarcon, A; Asgari, M; Blazek, J; Campos, A; Chen, R; Choi, A; Crocce, M; Diehl, HT; Doux, C; Eckert, K; Elvin-Poole, J; Everett, S; Ferté, A; Gatti, M; Giannini, G; Gruen, D; Gruendl, RA; Hartley, WG; Herner, K; Hildebrandt, H; Huang, S; Huff, EM; Joachimi, B; Lee, S; MacCrann, N; Myles, J; Navarro-Alsina, A; Nishimichi, T; Prat, J; Secco, LF; Sevilla-Noarbe, ; Sheldon, E; Shin, T; Tröster, T; Troxel, MA; Tutusaus, ; Wright, AH; Yin, B; Aguena, M; Allam, S; Annis, J; Bacon, D; Bilicki, M; Brooks, D; Burke, DL; Rosell, AC; Carretero, J; Castander, FJ; Cawthon, R; Costanzi, M; da Costa, LN; Pereira, MES; de Jong, J; De Vicente, J; Desai, S; Dietrich, JP; Doel, P; Ferrero, ; Frieman, J; García-Bellido, J; Gerdes, DW; Gschwend, J; Gutierrez, G; Hinton, SR; Hollowood, DL; Honscheid, K; Huterer, D; Kannawadi, A; Kuehn, K; Kuropatkin, N; Lahav, O; Lima, M; Maia, MAG; Marshall, JL; Menanteau, F; Miquel, R; Mohr, JJ; Morgan, R; Muir, J; Paz-Chinchón, F; Pieres, A; Malagón, AAP; Porredon, A; Rodriguez-Monroy, M; Roodman, A; Sanchez, E; Serrano, S; Shan, H; Suchyta, E; Swanson, MEC; Tarle, G; Thomas, D; To, C; Zhang, Y

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Vol. 518 ( 1 ) page： 477 - 503 2023.1

Language：English Publishing type：Research paper (scientific journal) Publisher：Monthly Notices of the Royal Astronomical Society

We evaluate the consistency between lensing and clustering based on measurements from Baryon Oscillation Spectroscopic Survey combined with galaxy-galaxy lensing from Dark Energy Survey (DES) Year 3, Hyper Suprime-Cam Subaru Strategic Program (HSC) Year 1, and Kilo-Degree Survey (KiDS)-1000. We find good agreement between these lensing data sets. We model the observations using the Dark Emulator and fit the data at two fixed cosmologies: Planck (S8 = 0.83), and a Lensing cosmology (S8 = 0.76). For a joint analysis limited to large scales, we find that both cosmologies provide an acceptable fit to the data. Full utilization of the higher signal-to-noise small-scale measurements is hindered by uncertainty in the impact of baryon feedback and assembly bias, which we account for with a reasoned theoretical error budget. We incorporate a systematic inconsistency parameter for each redshift bin, A, that decouples the lensing and clustering. With a wide range of scales, we find different results for the consistency between the two cosmologies. Limiting the analysis to the bins for which the impact of the lens sample selection is expected to be minimal, for the Lensing cosmology, the measurements are consistent with A = 1; A = 0.91 ± 0.04 (A = 0.97 ± 0.06) using DES+KiDS (HSC). For the Planck case, we find a discrepancy: A = 0.79 ± 0.03 (A = 0.84 ± 0.05) using DES+KiDS (HSC). We demonstrate that a kinematic Sunyaev-Zeldovich-based estimate for baryonic effects alleviates some of the discrepancy in the Planck cosmology. This analysis demonstrates the statistical power of small-scale measurements; however, caution is still warranted given modelling uncertainties and foreground sample selection effects.

DOI： 10.1093/mnras/stac2938

Cosmological inference from an emulator based halo model. I. Validation tests with HSC and SDSS mock catalogs Reviewed International coauthorship

Hironao Miyatake, Yosuke Kobayashi, Masahiro Takada, Takahiro Nishimichi, Masato Shirasaki, Sunao Sugiyama, Ryuichi Takahashi, Ken Osato, Surhud More, Youngsoo Park

Physical Review D Vol. 106 ( 8 ) 2022.10

A pair of early- and late-forming galaxy cluster samples: A novel way of studying halo assembly bias assisted by a constrained simulation Reviewed International coauthorship

Lin, YT; Miyatake, H; Guo, H; Chiang, YK; Chen, KF; Lan, TW; Chang, YY

ASTRONOMY & ASTROPHYSICS Vol. 666 2022.10

Language：English Publishing type：Research paper (scientific journal) Publisher：Astronomy and Astrophysics

The halo assembly bias, a phenomenon referring to dependencies of the large-scale bias of a dark matter halo other than its mass, is a fundamental property of the standard cosmological model. First discovered in 2005 from the Millennium Run simulation, it has been proven very diffcult to be detected observationally, with only a few convincing claims of detection so far. The main obstacle lies in finding an accurate proxy of the halo formation time. In this study, by utilizing a constrained simulation that can faithfully reproduce the observed structures larger than 2 Mpc in the local universe, for a sample of 634 massive clusters at z ≤ 0.12, we found their counterpart halos in the simulation and used the mass growth history of the matched halos to estimate the formation time of the observed clusters. This allowed us to construct a pair of early- and late-forming clusters, with a similar mass as measured via weak gravitational lensing, and large-scale biases differing at the ≈3σ level, suggestive of the signature of assembly bias, which is further corroborated by the properties of cluster galaxies, including the brightest cluster galaxy and the spatial distribution and number of member galaxies. Our study paves a way to further detect assembly bias based on cluster samples constructed purely on observed quantities.

DOI： 10.1051/0004-6361/202244404

Towards 1% accurate galaxy cluster masses: including baryons in weak-lensing mass inference Reviewed International coauthorship

Cromer, D; Battaglia, N; Miyatake, H; Simet, M

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS Vol. 2022 ( 10 ) 2022.10

Language：English Publishing type：Research paper (scientific journal) Publisher：Journal of Cosmology and Astroparticle Physics

Galaxy clusters are a promising probe of late-time structure growth, but constraints on cosmology from cluster abundances are currently limited by systematics in their inferred masses. One unmitigated systematic effect in weak-lensing mass inference is ignoring the presence of baryons and treating the entire cluster as a dark matter halo. In this work we present a new flexible model for cluster densities that captures both the baryonic and dark matter profiles, a new general technique for calculating the lensing signal of an arbitrary density profile, and a methodology for stacking those lensing signal to appropriately model stacked weak-lensing measurements of galaxy cluster catalogues. We test this model on 1400 simulated clusters. Similarly to previous studies, we find that a dark matter-only model overestimates the average mass by 7.5%, but including our baryonic term reduces that to 0.7%. Since two more variables are marginalized over when we include our baryonic term the posteriors on the cluster mass calibration are larger than the dark matter-only model. Additionally, to mitigate the computational complexity of our model, we construct an emulator (surrogate model) which accurately interpolates our model for parameter inference, while being much faster to use than the raw model. We also provide an open-source software framework for our model and emulator, called maszcal, which will serve as a platform for continued efforts to improve these mass-calibration techniques. In this work, we detail our model, the construction of the emulator, and the tests which we used to validate that our model does mitigate bias. Lastly, we describe tests of the emulator's accuracy.

DOI： 10.1088/1475-7516/2022/10/034

The halo model with beyond-linear halo bias: unbiasing cosmological constraints from galaxy-galaxy lensing and clustering Reviewed International coauthorship

Constance Mahony, Andrej Dvornik, Alexander Mead, Catherine Heymans, Marika Asgari, Hendrik Hildebrandt, Hironao Miyatake, Takahiro Nishimichi, Robert Reischke

Monthly Notices of the Royal Astronomical Society Vol. 515 ( 2 ) page： 2612 - 2623 2022.8

Language：English Publishing type：Research paper (scientific journal)

We determine the error introduced in a joint halo model analysis of galaxy-galaxy lensing and galaxy clustering observables when adopting the standard approximation of linear halo bias. Considering the Kilo-Degree Survey, we forecast that ignoring the non-linear halo bias would result in up to 5σ offsets in the recovered cosmological parameters describing structure growth, S8, and the matter density parameter, m. We include the scales 10-1.3< rp/h-1Mpc< 10 in the data vector, and the direction of these offsets are shown to depend on the freedom afforded to the halo model through other nuisance parameters. We conclude that a beyond-linear halo bias correction must therefore be included in future cosmological halo model analyses of large-scale structure observables on non-linear scales.

DOI： 10.1093/mnras/stac1858

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