研究者詳細 - 宮武　広直

論文 - 宮武　広直

分割表示 116 件中 41 - 60 件目／全件表示 >>

LoVoCCS. I. Survey Introduction, Data Processing Pipeline, and Early Science Results 査読有り国際共著

Fu, SM; Dell'Antonio, I; Chary, RR; Clowe, D; Cooper, MC; Donahue, M; Evrard, A; Lacy, M; Lauer, T; Liu, BY; McCleary, J; Meneghetti, M; Miyatake, H; Montes, M; Natarajan, P; Ntampaka, M; Pierpaoli, E; Postman, M; Sohn, J; Umetsu, K; Utsumi, Y; Wilson, G

ASTROPHYSICAL JOURNAL 933 巻 ( 1 ) 2022年7月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present the Local Volume Complete Cluster Survey (LoVoCCS; we pronounce it as "low-vox"or "law-vox,"with stress on the second syllable), an NSF's National Optical-Infrared Astronomy Research Laboratory survey program that uses the Dark Energy Camera to map the dark matter distribution and galaxy population in 107 nearby (0.03 < z < 0.12) X-ray luminous ([0.1-2.4 keV] L X500 > 1044 erg s-1) galaxy clusters that are not obscured by the Milky Way. The survey will reach Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) Year 1-2 depth (for galaxies r = 24.5, i = 24.0, signal-to-noise ratio (S/N) > 20; u = 24.7, g = 25.3, z = 23.8, S/N > 10) and conclude in 1/42023 (coincident with the beginning of LSST science operations), and will serve as a zeroth-year template for LSST transient studies. We process the data using the LSST Science Pipelines that include state-of-the-art algorithms and analyze the results using our own pipelines, and therefore the catalogs and analysis tools will be compatible with the LSST. We demonstrate the use and performance of our pipeline using three X-ray luminous and observation-time complete LoVoCCS clusters: A3911, A3921, and A85. A3911 and A3921 have not been well studied previously by weak lensing, and we obtain similar lensing analysis results for A85 to previous studies. (We mainly use A3911 to show our pipeline and give more examples in the Appendix.)

DOI： 10.3847/1538-4357/ac68e8

HSC Year 1 cosmology results with the minimal bias method: HSC x BOSS galaxy-galaxy weak lensing and BOSS galaxy clustering 査読有り国際共著

Sugiyama, S; Takada, M; Miyatake, H; Nishimichi, T; Shirasaki, M; Kobayashi, Y; Mandelbaum, R; More, S; Takahashi, R; Osato, K; Oguri, M; Coupon, J; Hikage, C; Hsieh, BC; Komiyama, Y; Leauthaud, A; Li, XC; Luo, WT; Lupton, RH; Murayama, H; Nishizawa, AJ; Park, Y; Price, PA; Simet, M; Speagle, JS; Strauss, MA; Tanaka, M

PHYSICAL REVIEW D 105 巻 ( 12 ) 2022年6月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Physical Review D

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 0.15<z<0.7. We use luminosity-limited samples as lens samples for Δς and as large-scale structure tracers for wp in three redshift bins, and use the HSC-Y1 galaxy catalog to define a secure sample of source galaxies at zph>0.75 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.

DOI： 10.1103/PhysRevD.105.123537

The eROSITA Final Equatorial-Depth Survey (eFEDS) X-ray observable-to-mass-and-redshift relations of galaxy clusters and groups with weak-lensing mass calibration from the Hyper Suprime-Cam Subaru Strategic Program survey 査読有り国際共著

Chiu, IN; Ghirardini, V; Liu, A; Grandis, S; Bulbul, E; Bahar, YE; Comparat, J; Bocquet, S; Clerc, N; Klein, M; Liu, T; Li, XC; Miyatake, H; Mohr, J; More, S; Oguri, M; Okabe, N; Pacaud, F; Ramos-Ceja, ME; Reiprich, TH; Schrabback, T; Umetsu, K

ASTRONOMY & ASTROPHYSICS 661 巻 2022年5月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astronomy and Astrophysics

We present the first weak-lensing mass calibration and X-ray scaling relations of galaxy clusters and groups selected in the eROSITA Final Equatorial Depth Survey (eFEDS) observed by Spectrum Roentgen Gamma/eROSITA over a contiguous footprint with an area of 140 deg2, using the three-year (S19A) weak-lensing data from the Hyper Suprime-Cam (HSC) Subaru Strategic Program survey. In this work, we study a sample of 434 optically confirmed galaxy clusters (and groups) at redshift 0.01 1.3 with a median of 0.35, of which 313 systems are uniformly covered by the HSC survey to enable the extraction of the weak-lensing shear observable. In a Bayesian population modeling, we perform a blind analysis for the weak-lensing mass calibration by simultaneously modeling the observed count rate η and the shear profile g+ of individual clusters through the count-rate-to-mass-and-redshift (η-M500-z) relation and the weak-lensing-mass-to-mass-and-redshift (MWL-M500-z) relation, respectively, while accounting for the bias in these observables using simulation-based calibrations. As a result, the count-rate-inferred and lensing-calibrated cluster mass is obtained from the joint modeling of the scaling relations, as the ensemble mass spanning a range of 1013h-1M M500 with a median of for the eFEDS sample. With the mass calibration, we further model the X-ray observable-to-mass-and-redshift relations, including the rest-frame soft-band and bolometric luminosity (LX and Lb), the emission-weighted temperature TX, the mass of intra-cluster medium Mg, and the mass proxy YX, which is the product of TX and Mg. Except for LX with a steeper dependence on the cluster mass at a statistically significant level, we find that the other X-ray scaling relations all show a mass trend that is statistically consistent with the self-similar prediction at a level of Meanwhile, all these scaling relations show no significant deviation from the self-similarity in their redshift scaling. Moreover, no significant redshift-dependent mass trend is present. This work demonstrates the synergy between the eROSITA and HSC surveys in preparation for the forthcoming first-year eROSITA cluster cosmology.

DOI： 10.1051/0004-6361/202141755

The eROSITA Final Equatorial-Depth Survey (eFEDS) A complete census of X-ray properties of Subaru Hyper Suprime-Cam weak lensing shear-selected clusters in the eFEDS footprint 査読有り国際共著

Ramos-Ceja, ME; Oguri, M; Miyazaki, S; Ghirardini, V; Chiu, I; Okabe, N; Liu, A; Schrabback, T; Akino, D; Bahar, YE; Bulbul, E; Clerc, N; Comparat, J; Grandis, S; Klein, M; Lin, YT; Merloni, A; Mitsuishi, I; Miyatake, H; More, S; Nandra, K; Nishizawa, AJ; Ota, N; Pacaud, F; Reiprich, TH; Sanders, JS

ASTRONOMY & ASTROPHYSICS 661 巻 2022年5月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astronomy and Astrophysics

Context. The eFEDS survey is a proof-of-concept mini-survey designed to demonstrate the survey science capabilities of SRG/eROSITA. It covers an area of 140 deg2 where ~540 galaxy clusters have been detected out to a redshift of 1.3. The eFEDS field is partly embedded in the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) S19A data release, which covers ~510 deg2, containing approximately 36 million galaxies. This galaxy catalogue has been used to construct a sample of ~180 shear-selected galaxy clusters. The common area to both surveys covers about 90 deg2, making it an ideal region to study galaxy clusters selected in different ways. Aims. The aim of this work is to investigate the effects of selection methods in the galaxy cluster detection by comparing the X-ray selected, eFEDS, and the shear-selected, HSC-SSP S19A, galaxy cluster samples. There are 25 shear-selected clusters in the eFEDS fooprint. Methods. The relation between X-ray bolometric luminosity and weak-lensing mass is investigated (Lbol - M relation), comparing this relation derived from a shear-selected cluster sample to the relation obtained from an X-ray selected sample. Moreover, the dynamical state of the shear-selected clusters is investigated and compared to the X-ray selected sample using X-ray morphological parameters and galaxy distribution. Results. The normalisation of the Lbol â ? ? M relation of the X-ray selected and shear-selected samples is consistent within 1Ï ? -. Moreover, the dynamical state and merger fraction of the shear-selected clusters is not different from the X-ray selected ones. Four shear-selected clusters are undetected in X-rays. A close inspection reveals that one is the result of projection effects, while the other three have an X-ray flux below the ultimate eROSITA detection limit. Finally, 43% of the shear-selected clusters lie in superclusters. Conclusions. Our results indicate that the scaling relation between X-ray bolometric luminosity and true cluster mass of the shear-selected cluster sample is consistent with the eFEDS sample. There is no significant population of X-ray underluminous clusters, indicating that X-ray selected cluster samples are complete and can be used as an accurate cosmological probe.

DOI： 10.1051/0004-6361/202142214

The eROSITA Final Equatorial-Depth Survey (eFEDS) Optical confirmation, redshifts, and properties of the cluster and group catalog 査読有り国際共著

Klein, M; Oguri, M; Mohr, JJ; Grandis, S; Ghirardini, V; Liu, T; Liu, A; Bulbul, E; Wolf, J; Comparat, J; Ramos-Ceja, ME; Buchner, J; Chiu, I; Clerc, N; Merloni, A; Miyatake, H; Miyazaki, S; Okabe, N; Ota, N; Pacaud, F; Salvato, M; Driver, SP

ASTRONOMY & ASTROPHYSICS 661 巻 2022年5月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astronomy and Astrophysics

Context. In 2019, the eROSITA telescope on board the Russian-German satellite Spectrum-Roentgen-Gamma (SRG) began to perform a deep all-sky X-ray survey with the aim of identifying ~100 000 clusters and groups over the course of four years. As part of its performance verification phase, a ~140 deg2 survey, called eROSITA Final Equatorial-Depth Survey (eFEDS), was performed. With a depth typical of the all-sky survey after four years, it allows tests of tools and methods as well as improved predictions for the all-sky survey. Aims. As part of this effort, a catalog of 542 X-ray selected galaxy group and cluster candidates was compiled. In this paper we present the optical follow-up, with the aim of providing redshifts and cluster confirmation for the full sample. Furthermore, we aim to provide additional information on the dynamical state, richness, and optical center of the clusters. Finally, we aim to evaluate the impact of optical cluster confirmation on the purity and completeness of the X-ray selected sample. Methods. We used optical imaging data from the Hyper Suprime-Cam Subaru Strategic Program and from the Legacy Survey to identify optical counterparts to the X-ray detected cluster candidates. We make use of the multi-component matched filter cluster confirmation tool (MCMF), as well as of the optical cluster finder CAMIRA to derive cluster redshifts and richnesses. MCMF provided the probabilities with which an optical structure would be a chance superposition with the X-ray candidate. These probabilities were used to identify the best optical counterpart as well as to confirm an X-ray candidate as a cluster. The impact of this confirmation process on catalog purity and completeness was estimated using optical to X-ray scaling relations as well as simulations. The resulting catalog was furthermore matched with public group and cluster catalogs. Optical estimators of the cluster dynamical state were constructed based on density maps of the red-sequence galaxies at the cluster redshift. Results. By providing redshift estimates for all 542 candidates, we construct an optically confirmed sample of 477 clusters and groups with a residual contamination of 6%. Of these, 470 (98.5%) are confirmed using MCMF, and 7 systems are added through cross-matching with spectroscopic group catalogs. Using observable-to-observable scaling and the applied confirmation threshold, we predict that 8 ± 2 real systems have been excluded with the MCMF cut required to build this low-contamination sample. This number agrees well with the 7 systems found through cross-matching that were not confirmed with MCMF. The predicted redshift and mass distribution of this catalog agree well with simulations. Thus, we expect that these 477 systems include >99% of all true clusters in the candidate list. Using an MCMF-independent method, we confirm that the catalog contamination of the confirmed subsample is 6 ± 3%. Application of the same method to the full candidate list yields 17 ± 3%, consistent with estimates coming from the fraction of confirmed systems of ~17% and with expectations from simulations of ~20%. We also present a sample of merging cluster candidates based on the derived estimators of the cluster dynamical state.

DOI： 10.1051/0004-6361/202141123

Full-shape cosmology analysis of the SDSS-III BOSS galaxy power spectrum using an emulator-based halo model: A 5% determination of sigma(8) 査読有り

Kobayashi Yosuke, Nishimichi Takahiro, Takada Masahiro, Miyatake Hironao

PHYSICAL REVIEW D 105 巻 ( 8 ) 2022年4月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Physical Review D

We present the results obtained from the full-shape cosmology analysis of the redshift-space power spectra for four galaxy samples of the SDSS-III BOSS DR12 galaxy catalog over 0.2<z<0.75. For the theoretical template, we use an emulator that was built from an ensemble set of N-body simulations, which enables fast and accurate computation of the redshift-space power spectrum of "halos."Combining with the halo occupation distribution to model the galaxy-halo connection, we can compute the redshift-space power spectrum of BOSS-like galaxies in less than a CPU second, for an input model under flat ΛCDM cosmology. In our cosmology inference, we use the monopole, quadrupole, and hexadecapole moments of the redshift-space power spectrum and include seven nuisance parameters, with broad priors, to model uncertainties in the galaxy-halo connection for each galaxy sample, but do not use any information on the abundance of galaxies. We demonstrate a validation of our analysis pipeline using the mock catalogs of BOSS-like galaxies, generated using different recipes of the galaxy-halo connection and including the assembly bias effect. Assuming weak priors on cosmological parameters, except for the BBN prior on ωbh2 and the CMB prior on ns, we show that our model well reproduces the BOSS power spectra. Including the power-spectrum information up to kmax=0.25h Mpc-1, we find ωm=0.301-0.011+0.012, H0=68.2±1.4 km s-1 Mpc-1, and σ8=0.786-0.037+0.036 for the mode and 68% credible interval, after marginalization over galaxy-halo connection parameters. We find little improvement in the cosmological parameters beyond a maximum wavelength kmax≃0.2h Mpc-1 due to the shot noise domination and marginalization of the galaxy-halo connection parameters. Our results are consistent with the Planck CMB results within 1σ statistical uncertainties.

DOI： 10.1103/PhysRevD.105.083517

Cosmological constraints from cosmic shear two-point correlation functions with HSC survey first-year data (vol 72, psz138, 2020) 査読有り国際共著

Hamana, T; Shirasaki, M; Miyazaki, S; Hikage, C; Oguri, M; More, S; Armstrong, R; Leauthaud, A; Mandelbaum, R; Miyatake, H; Nishizawa, AJ; Simet, M; Takada, M; Aihara, H; Bosch, J; Komiyama, Y; Lupton, R; Murayama, H; Strauss, MA; Tanaka, M

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 74 巻 ( 2 ) 頁： 488 - 491 2022年4月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

In the original publication of "Cosmological constraints from cosmic shear two-point correlation functions with HSC survey first-year data"[PASJ, 72, 16 (2020); doi: 10.1093/pasj/psz138], we discovered a couple of bugs in the software used for numerical computations. Here we present revised results obtained from corrected computations.

DOI： 10.1093/pasj/psab117

Third data release of the Hyper Suprime-Cam Subaru Strategic Program 査読有り国際共著

Aihara, H; AlSayyad, Y; Ando, M; Armstrong, R; Bosch, J; Egami, E; Furusawa, H; Furusawa, J; Harasawa, S; Harikane, Y; Hsieh, BC; Ikeda, H; Ito, K; Iwata, I; Kodama, T; Koike, M; Kokubo, M; Komiyama, Y; Li, XC; Liang, YM; Lin, YT; Lupton, RH; Lust, NB; MacArthur, LA; Mawatari, K; Mineo, S; Miyatake, H; Miyazaki, S; More, S; Morishima, T; Murayama, H; Nakajima, K; Nakata, F; Nishizawa, AJ; Oguri, M; Okabe, N; Okura, Y; Ono, Y; Osato, K; Ouchi, M; Pan, YC; Malagón, AAP; Price, PA; Reed, SL; Rykoff, ES; Shibuya, T; Simunovic, M; Strauss, MA; Sugimori, K; Suto, Y; Suzuki, N; Takada, M; Takagi, Y; Takata, T; Takita, S; Tanaka, M; Tang, SL; Taranu, DS; Terai, T; Toba, Y; Turner, EL; Uchiyama, H; Vijarnwannaluk, B; Waters, CZ; Yamada, Y; Yamamoto, N; Yamashita, T

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 74 巻 ( 2 ) 頁： 247 - 272 2022年4月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

This paper presents the third data release of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP), a wide-field multi-band imaging survey with the Subaru 8.2 m telescope. HSC-SSP has three survey layers (Wide, Deep, and UltraDeep) with different area coverages and depths, designed to address a wide array of astrophysical questions. This third release from HSC-SSP includes data from 278 nights of observing time and covers about 670 deg2 in all five broad-band filters (grizy) at the full depth (∼26 mag at 5σ depending on filter) in the Wide layer. If we include partially observed areas, the release covers 1470 deg2. The Deep and UltraDeep layers have ∼ 80% of the originally planned integration times, and are considered done, as we have slightly changed the observing strategy in order to compensate for various time losses. There are a number of updates in the image processing pipeline. Of particular importance is the change in the sky subtraction algorithm; we subtract the sky on small scales before the detection and measurement stages, which has significantly reduced the number of false detections. Thanks to this and other updates, the overall quality of the processed data has improved since the previous release. However, there are limitations in the data (for example, the pipeline is not optimized for crowded fields), and we encourage the user to check the quality assurance plots as well as a list of known issues before exploiting the data.

DOI： 10.1093/pasj/psab122

The three-year shear catalog of the Subaru Hyper Suprime-Cam SSP Survey 査読有り国際共著

Li, XC; Miyatake, H; Luo, WT; More, S; Oguri, M; Hamana, T; Mandelbaum, R; Shirasaki, M; Takada, M; Armstrong, R; Kannawadi, A; Takita, S; Miyazaki, S; Nishizawa, AJ; Malagon, AAP; Strauss, MA; Tanaka, M; Yoshida, N

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 74 巻 ( 2 ) 頁： 421 - 459 2022年4月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

We present the galaxy shear catalog that will be used for the three-year cosmological weak gravitational lensing analyses using data from the Wide layer of the Hyper Suprime-Cam (HSC) Subaru Strategic Program (SSP) Survey. The galaxy shapes are measured from the i-band imaging data acquired from 2014 to 2019 and calibrated with image simulations that resemble the observing conditions of the survey based on training galaxy images from the Hubble Space Telescope in the COSMOS region. The catalog covers an area of 433.48 deg2 of the northern sky, split into six fields. The mean i-band seeing is 0″. 59. With conservative galaxy selection criteria (e.g., i-band magnitude brighter than 24.5), the observed raw galaxy number density is 22.9 arcmin-2, and the effective galaxy number density is 19.9 arcmin-2. The calibration removes the galaxy property-dependent shear estimation bias to the level |δm| < 9 × 10-3. The bias residual δm shows no dependence on redshift in the range 0 < z ≤ 3. We define the requirements for cosmological weak-lensing science for this shear catalog, and quantify potential systematics in the catalog using a series of internal null tests for systematics related to point-spread function modelling and shear estimation. A variety of the null tests are statistically consistent with zero or within requirements, but (i) there is evidence for PSF model shape residual correlations; and (ii) star-galaxy shape correlations reveal additive systematics. Both effects become significant on >1° scales and will require mitigation during the inference of cosmological parameters using cosmic shear measurements.

DOI： 10.1093/pasj/psac006

Joint Survey Processing. I. Compact Oddballs in the COSMOS Field-Low-luminosity Quasars at <i>z</i> > 6? 査読有り国際共著

Faisst, AL; Chary, RR; Fajardo-Acosta, S; Paladini, R; Rusholme, B; Stickley, N; Helou, G; Weaver, JR; Brammer, G; Koekemoer, AM; Miyatake, H

ASTROPHYSICAL JOURNAL 929 巻 ( 1 ) 2022年4月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

The faint-end slope of the quasar luminosity function at z ∼6 and its implication on the role of quasars in reionizing the intergalactic medium at early times has been an outstanding problem for some time. The identification of faint high-redshift quasars with luminosities of <1044.5 erg s-1 is challenging. They are rare (few per square degree), and the separation of these unresolved quasars from late-Type stars and compact star-forming galaxies is difficult from ground-based observations alone. In addition, source confusion becomes significant at >25 mag, with ∼1/430% of sources having their flux contaminated by foreground objects when the seeing resolution is ∼1/40″.7. We mitigate these issues by performing a pixel-level joint processing of ground and space-based data from Subaru/Hyper-SuprimeCam (HSC) and Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS). We create a deconfused catalog over the 1.64 deg2 of the COSMOS field, after accounting for spatial varying point-spread functions and astrometric differences between the two data sets. We identify twelve low-luminosity (M UV ∼-21 mag) z > 6 quasar candidates through (i) their red color measured between ACS/F814W and HSC/i band and (ii) their compactness in the space-based data. Nondetections of our candidates in Hubble DASH data argues against contamination from late-Type stars. Our constraints on the faint end of the quasar luminosity function at z ∼6.4 suggest a negligibly small contribution to reionization compared to the star-forming galaxy population. The confirmation of our candidates and the evolution of number density with redshift could provide better insights into how supermassive galaxies grew in the first billion years of cosmic time.

DOI： 10.3847/1538-4357/ac59b3

Lensing without borders - I. A blind comparison of the amplitude of galaxy-galaxy lensing between independent imaging surveys 査読有り国際共著

Leauthaud, A; Amon, A; Singh, S; Gruen, D; Lange, JU; Huang, S; Robertson, NC; Varga, TN; Luo, Y; Heymans, C; Hildebrandt, H; Blake, C; Aguena, M; Allam, S; Andrade-Oliveira, F; Annis, J; Bertin, E; Bhargava, S; Blazek, J; Bridle, SL; Brooks, D; Burke, DL; Rosell, AC; Kind, MC; Carretero, J; Castander, FJ; Cawthon, R; Choi, A; Costanzi, M; da Costa, LN; Pereira, MES; Davis, C; De Vicente, J; DeRose, J; Diehl, HT; Dietrich, JP; Doel, P; Eckert, K; Everett, S; Evrard, AE; Ferrero, I; Flaugher, B; Fosalba, P; García-Bellido, J; Gatti, M; Gaztanaga, E; Gruendl, RA; Gschwend, J; Hartley, WG; Hollowood, DL; Honscheid, K; Jain, B; James, DJ; Jarvis, M; Joachimi, B; Kannawadi, A; Kim, AG; Krause, E; Kuehn, K; Kuijken, K; Kuropatkin, N; Lima, M; MacCrann, N; Maia, MAG; Makler, M; March, M; Marshall, JL; Melchior, P; Menanteau, F; Miquel, R; Miyatake, H; Mohr, JJ; Moraes, B; More, S; Surhud, M; Morgan, R; Myles, J; Ogando, RLC; Palmese, A; Paz-Chinchón, F; Malagón, AAP; Prat, J; Rau, MM; Rhodes, J; Rodriguez-Monroy, M; Roodman, A; Ross, AJ; Samuroff, S; Sánchez, C; Sanchez, E; Scarpine, V; Schlegel, DJ; Schubnell, M; Serrano, S; Sevilla-Noarbe, I; Sifón, C; Smith, M; Speagle, JS; Suchyta, E; Tarle, G; Thomas, D; Tinker, J; To, C; Troxel, MA; Van Waerbeke, L; Vielzeuf, P; Wright, AH

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 510 巻 ( 4 ) 頁： 6150 - 6189 2022年2月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society

Lensing without borders is a cross-survey collaboration created to assess the consistency of galaxy-galaxy lensing signals (Δς) across different data sets and to carry out end-to-end tests of systematic errors. We perform a blind comparison of the amplitude of Δς using lens samples from BOSS and six independent lensing surveys. We find good agreement between empirically estimated and reported systematic errors which agree to better than 2.3σ in four lens bins and three radial ranges. For lenses with zL > 0.43 and considering statistical errors, we detect a 3-4σ correlation between lensing amplitude and survey depth. This correlation could arise from the increasing impact at higher redshift of unrecognized galaxy blends on shear calibration and imperfections in photometric redshift calibration. At zL > 0.54, amplitudes may additionally correlate with foreground stellar density. The amplitude of these trends is within survey-defined systematic error budgets that are designed to include known shear and redshift calibration uncertainty. Using a fully empirical and conservative method, we do not find evidence for large unknown systematics. Systematic errors greater than 15 per cent (25 per cent) ruled out in three lens bins at 68 per cent (95 per cent) confidence at z < 0.54. Differences with respect to predictions based on clustering are observed to be at the 20-30 per cent level. Our results therefore suggest that lensing systematics alone are unlikely to fully explain the 'lensing is low' effect at z < 0.54. This analysis demonstrates the power of cross-survey comparisons and provides a promising path for identifying and reducing systematics in future lensing analyses.

DOI： 10.1093/mnras/stab3586

The Subaru HSC weak lensing mass-observable scaling relations of spectroscopic galaxy groups from the GAMA survey 査読有り国際共著

Rana, D; More, S; Miyatake, H; Nishimichi, T; Takada, M; Robotham, ASG; Hopkins, AM; Holwerda, BW

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 510 巻 ( 4 ) 頁： 5408 - 5425 2022年1月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society

We utilize the galaxy shape catalogue from the first-year data release of the Subaru Hyper Suprime-Cam (HSC) surv e y to study the dark matter content of galaxy groups in the Universe using weak lensing. We use galaxy groups from the Galaxy Mass and Assembly galaxy surv e y in approximately 100 sq. de grees of the sk y that o v erlap with the HSC surv e y as lenses. We restrict our analysis to the 1587 groups with at least five members. We divide these groups into six bins each of group luminosity and group member velocity dispersion and measure the lensing signal with a signal-to-noise ratio of 55 and 51 for these two different selections, respectively. We use a Bayesian halo model framework to infer the halo mass distribution of our groups binned in the two different observable properties and constrain the power-law scaling relation and the scatter between mean halo masses and the two-group observable properties. We obtain a 5 per cent constraint on the amplitude of the scaling relation between halo mass and group luminosity with (M) = (0.81 ±0.04) ×10 14 h −1 M ⊙for L grp = 10 11.5 h −2 L ⊙, and a power-law index of α= 1.01 ±0.07. We constrain the amplitude of the scaling relation between halo mass and velocity dispersion to be (M) = (0.93 ±0.05) ×10 14 h −1 M ⊙for σ= 500 km s −1 and a power-law index to be α= 1.52 ±0.10. Ho we ver, these scaling relations are sensitive to the exact cuts applied to the number of group members. Comparisons with similar scaling relations from the literature show that our results are consistent and have significantly reduced errors.

DOI： 10.1093/mnras/stac007

CLMM: a LSST-DESC cluster weak lensing mass modeling library for cosmology 査読有り国際共著

Aguena, M; Avestruz, C; Combet, C; Fu, S; Herbonnet, R; Malz, AI; Penna-Lima, M; Ricci, M; Vitenti, SDP; Baumont, L; Fan, H; Fong, M; Ho, M; Kirby, M; Payerne, C; Boutigny, D; Lee, B; Liu, B; McClintock, T; Miyatake, H; Sifón, C; von der Linden, A; Wu, H; Yoon, M

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 508 巻 ( 4 ) 頁： 6092 - 6110 2021年12月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society

We present the v1.0 release of CLMM, an open source python library for the estimation of the weak lensing masses of clusters of galaxies. CLMM is designed as a stand-alone toolkit of building blocks to enable end-to-end analysis pipeline validation for upcoming cluster cosmology analyses such as the ones that will be performed by the Vera C. Rubin Legacy Survey of Space and Time-Dark Energy Science Collaboration (LSST-DESC). Its purpose is to serve as a flexible, easy-to-install, and easy-to-use interface for both weak lensing simulators and observers and can be applied to real and mock data to study the systematics affecting weak lensing mass reconstruction. At the core of CLMM are routines to model the weak lensing shear signal given the underlying mass distribution of galaxy clusters and a set of data operations to prepare the corresponding data vectors. The theoretical predictions rely on existing software, used as backends in the code, that have been thoroughly tested and cross-checked. Combined theoretical predictions and data can be used to constrain the mass distribution of galaxy clusters as demonstrated in a suite of example Jupyter Notebooks shipped with the software and also available in the extensive online documentation.

DOI： 10.1093/mnras/stab2764

Cosmology with the <i>Roman Space Telescope</i>: synergies with the Rubin Observatory Legacy Survey of Space and Time 査読有り国際共著

Eifler, T; Simet, M; Krause, E; Hirata, C; Huang, HJ; Fang, X; Miranda, V; Mandelbaum, R; Doux, C; Heinrich, C; Huff, E; Miyatake, H; Hemmati, S; Xu, JC; Rogozenski, P; Capak, P; Choi, A; Doré, O; Jain, B; Jarvis, M; Kruk, J; MacCrann, N; Masters, D; Rozo, E; Spergel, DN; Troxel, M; von der Linden, A; Wang, Y; Weinberg, DH; Wenzl, L; Wu, HY

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 507 巻 ( 1 ) 頁： 1514 - 1527 2021年10月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society

We explore synergies between the Nancy Grace Roman Space Telescope and the Vera Rubin Observatory's Legacy Survey of Space and Time (LSST). Specifically, we consider scenarios where the currently envisioned survey strategy for the Roman Space Telescope's High Latitude Survey (HLS reference), i.e. 2000 deg2 in four narrow photometric bands is altered in favour of a strategy of rapid coverage of the LSST area (to full LSST depth) in one band. We find that in only five months, a survey in the W-band can cover the full LSST survey area providing high-resolution imaging for >95 per cent of the LSST Year 10 gold galaxy sample. We explore a second, more ambitious scenario where the Roman Space Telescope spends 1.5 yr covering the LSST area. For this second scenario, we quantify the constraining power on dark energy equation-of-state parameters from a joint weak lensing and galaxy clustering analysis. Our survey simulations are based on the Roman Space Telescope exposure-time calculator and redshift distributions from the CANDELS catalogue. Our statistical uncertainties account for higher order correlations of the density field, and we include a wide range of systematic effects, such as uncertainties in shape and redshift measurements, and modelling uncertainties of astrophysical systematics, such as galaxy bias, intrinsic galaxy alignment, and baryonic physics. We find a significant increase in constraining power for the joint LSST + HLS wide survey compared to LSST Y10 (FoMHLSwide = 2.4 FoMLSST) and compared to LSST + HLS (FoMHLSwide = 5.5 FoMHLSref).

DOI： 10.1093/mnras/stab533

Cosmology with the <i>Roman Space Telescope</i> - multiprobe strategies 査読有り国際共著

Eifler, T; Miyatake, H; Krause, E; Heinrich, C; Miranda, V; Hirata, C; Xu, JC; Hemmati, S; Simet, M; Capak, P; Choi, A; Doré, O; Doux, C; Fang, X; Hounsell, R; Huff, E; Huang, HJ; Jarvis, M; Kruk, J; Masters, D; Rozo, E; Scolnic, D; Spergel, DN; Troxel, M; von der Linden, A; Wang, Y; Weinberg, DH; Wenzl, L; Wu, HY

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 507 巻 ( 2 ) 頁： 1746 - 1761 2021年10月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society

We simulate the scientific performance of the Nancy Grace Roman Space Telescope High Latitude Survey (HLS) on dark energy and modified gravity. The 1.6-yr HLS Reference survey is currently envisioned to image 2000 deg2 in multiple bands to a depth of ∼26.5 in Y, J, H and to cover the same area with slit-less spectroscopy beyond z = 3. The combination of deep, multiband photometry and deep spectroscopy will allow scientists to measure the growth and geometry of the Universe through a variety of cosmological probes (e.g. weak lensing, galaxy clusters, galaxy clustering, BAO, Type Ia supernova) and, equally, it will allow an exquisite control of observational and astrophysical systematic effects. In this paper, we explore multiprobe strategies that can be implemented, given the telescope's instrument capabilities. We model cosmological probes individually and jointly and account for correlated systematics and statistical uncertainties due to the higher order moments of the density field. We explore different levels of observational systematics for the HLS survey (photo-z and shear calibration) and ultimately run a joint likelihood analysis in N-dim parameter space. We find that the HLS reference survey alone can achieve a standard dark energy FoM of >300 when including all probes. This assumes no information from external data sets, we assume a flat universe however, and includes realistic assumptions for systematics. Our study of the HLS reference survey should be seen as part of a future community-driven effort to simulate and optimize the science return of the Roman Space Telescope.

DOI： 10.1093/mnras/stab1762

The Stellar Mass in and around Isolated Central Galaxies: Connections to the Total Mass Distribution through Galaxy-Galaxy Lensing in the Hyper Suprime-Cam Survey 査読有り国際共著

Wang, WT; Li, XC; Shi, JJ; Han, JX; Yasuda, N; Jing, YP; More, S; Takada, M; Miyatake, H; Nishizawa, AJ

ASTROPHYSICAL JOURNAL 919 巻 ( 1 ) 2021年9月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

Using photometrically selected galaxies from the Hyper Suprime-Cam (HSC) survey, we measure the stellar-mass density profiles for satellite galaxies around isolated central galaxies (ICGs) from SDSS/DR7 at z ~ 0.1. By stacking HSC images, we also measure the projected stellar-mass density profiles for ICGs and their stellar halos. The total mass distributions are further measured from HSC weak-lensing signals. ICGs dominate within ~0.15 times the halo virial radius (0.15 R200). The stellar mass versus total mass fractions drop with the increase in projected distance up to ~0.15 R200, beyond which they are less than 1% while staying almost constant. The integrated stellar mass in satellites is proportional to the virial mass of the host halo, M200, for ICGs more massive than 1010.5Me, i.e., M*,sat ?M200, whereas the relation between the stellar mass of ICGs + stellar halos and M200 is close to M ,ICG+diffuse µ M200 1 2*. Below 1010.5Me, the change in M200 is much slower with the decrease in M*,ICG+diffuse. At fixed stellar mass, red ICGs are hosted by more massive dark matter halos and have more satellites. At M200 ~ 1012.7Me, both M*,sat and the fraction of stellar mass in satellites versus total stellar mass, fsat, tend to be marginally higher around blue ICGs. fsat increases with the increase in both M*,ICG+diffuse and M200, and scales more linearly with M200. We provide best-fitting relations to M200 versus M*,ICG+diffuse, M*,sat or M*,ICG+diffuse +M*,sat, and to fsat versus M200 or M*,ICG+diffuse, for red and blue ICGs separately.

DOI： 10.3847/1538-4357/ac0e38

Hundreds of weak lensing shear-selected clusters from the Hyper Suprime-Cam Subaru Strategic Program S19A data 査読有り国際共著

Oguri, M; Miyazaki, S; Li, XC; Luo, WT; Mitsuishi, I; Miyatake, H; More, S; Nishizawa, AJ; Okabe, N; Ota, N; Plazas Malagón, AA; Utsumi, Y

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 73 巻 ( 4 ) 頁： 817 - 829 2021年8月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

We use the Hyper Suprime-Cam Subaru Strategic Program S19A shape catalog to construct weak lensing shear-selected cluster samples. From aperture mass maps covering ∼510 deg2 created using a truncated Gaussian filter, we construct a catalog of 187 shear-selected clusters that correspond to mass map peaks with signal-to-noise ratio larger than 4.7. Most of the shear-selected clusters have counterparts in optically selected clusters, from which we estimate the purity of the catalog to be higher than 95%. The sample can be expanded to 418 shear-selected clusters with the same signal-to-noise ratio cut by optimizing the shape of the filter function and by combining weak lensing mass maps created with several different background galaxy selections. We argue that dilution and obscuration effects of cluster member galaxies can be mitigated by using background source galaxy samples and adopting a filter function with its inner boundary larger than about 2'. The large samples of shear-selected clusters that are selected without relying on any baryonic tracer are useful for detailed studies of cluster astrophysics and cosmology.

DOI： 10.1093/pasj/psab047

The Atacama Cosmology Telescope: A Catalog of >4000 Sunyaev-Zel'dovich Galaxy Clusters 査読有り国際共著

Hilton, M; Sifón, C; Naess, S; Madhavacheril, M; Oguri, M; Rozo, E; Rykoff, E; Abbott, TMC; Adhikari, S; Aguena, M; Aiola, S; Allam, S; Amodeo, S; Amon, A; Annis, J; Ansarinejad, B; Aros-Bunster, C; Austermann, JE; Avila, S; Bacon, D; Battaglia, N; Beall, JA; Becker, DT; Bernstein, GM; Bertin, E; Bhandarkar, T; Bhargava, S; Bond, JR; Brooks, D; Burke, DL; Calabrese, E; Kind, MC; Carretero, J; Choi, SK; Choi, A; Conselice, C; da Costa, LN; Costanzi, M; Crichton, D; Crowley, KT; Dünner, R; Denison, EV; Devlin, MJ; Dicker, SR; Diehl, HT; Dietrich, JP; Doel, P; Duff, SM; Duivenvoorden, AJ; Dunkley, J; Everett, S; Ferraro, S; Ferrero, I; Ferté, A; Flaugher, B; Frieman, J; Gallardo, PA; García-Bellido, J; Gaztanaga, E; Gerdes, DW; Giles, P; Golec, JE; Gralla, MB; Grandis, S; Gruen, D; Gruendl, RA; Gschwend, J; Gutierrez, G; Han, D; Hartley, WG; Hasselfield, M; Hill, JC; Hilton, GC; Hincks, AD; Hinton, SR; Ho, SPP; Honscheid, K; Hoyle, B; Hubmayr, J; Huffenberger, KM; Hughes, JP; Jaelani, AT; Jain, B; James, DJ; Jeltema, T; Kent, S; Knowles, K; Koopman, BJ; Kuehn, K; Lahav, O; Lima, M; Lin, YT; Lokken, M; Loubser, SI; MacCrann, N; Maia, MAG; Marriage, TA; Martin, J; McMahon, J; Melchior, P; Menanteau, F; Miquel, R; Miyatake, H; Moodley, K; Morgan, R; Mroczkowski, T; Nati, F; Newburgh, LB; Niemack, MD; Nishizawa, AJ; Ogando, RLC; Orlowski-Scherer, J; Page, LA; Palmese, A; Partridge, B; Paz-Chinchón, F; Phakathi, P; Plazas, AA; Robertson, NC; Romer, AK; Rosell, AC; Salatino, M; Sanchez, E; Schaan, E; Schillaci, A; Sehgal, N; Serrano, S; Shin, T; Simon, SM; Smith, M; Soares-Santos, M; Spergel, DN; Staggs, ST; Storer, ER; Suchyta, E; Swanson, MEC; Tarle, G; Thomas, D; To, C; Trac, H; Ullom, JN; Vale, LR; Van Lanen, J; Vavagiakis, EM; De Vicente, J; Wilkinson, RD; Wollack, EJ; Xu, Z; Zhang, Y

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES 253 巻 ( 1 ) 2021年3月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal, Supplement Series

We present a catalog of 4195 optically confirmed Sunyaev–Zel’dovich (SZ) selected galaxy clusters detected with signal-to-noise ratio >4 in 13,211 deg2 of sky surveyed by the Atacama Cosmology Telescope (ACT). Cluster candidates were selected by applying a multifrequency matched filter to 98 and 150 GHz maps constructed from ACT observations obtained from 2008 to 2018 and confirmed using deep, wide-area optical surveys. The clusters span the redshift range 0.04 < z < 1.91 (median z = 0.52). The catalog contains 222 z > 1 clusters, and a total of 868 systems are new discoveries. Assuming an SZ signal versus mass-scaling relation calibrated from X-ray observations, the sample has a 90% completeness mass limit of M500c > 3.8 × 1014 Me, evaluated at z = 0.5, for clusters detected at signal-to-noise ratio >5 in maps filtered at an angular scale of 2 4. The survey has a large overlap with deep optical weak-lensing surveys that are being used to calibrate the SZ signal mass-scaling relation, such as the Dark Energy Survey (4566 deg2), the Hyper Suprime-Cam Subaru Strategic Program (469 deg2), and the Kilo Degree Survey (825 deg2). We highlight some noteworthy objects in the sample, including potentially projected systems, clusters with strong lensing features, clusters with active central galaxies or star formation, and systems of multiple clusters that may be physically associated. The cluster catalog will be a useful resource for future cosmological analyses and studying the evolution of the intracluster medium and galaxies in massive clusters over the past 10 Gyr.

DOI： 10.3847/1538-4365/abd023

A comparative study of satellite galaxies in Milky Way-like galaxies from HSC, DECaLS, and SDSS 査読有り国際共著

Wang, WT; Takada, M; Li, XC; Carlsten, SG; Lan, TW; Shi, JJ; Miyatake, H; More, S; Beaton, RL; Lupton, R; Lin, YT; Qiu, T; Luo, WT

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 500 巻 ( 3 ) 頁： 3776 - 3801 2021年1月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society

We conduct a comprehensive and statistical study of the luminosity functions (LFs) for satellite galaxies, by counting photometric galaxies from HSC, DECaLS, and SDSS around isolated central galaxies (ICGs) and paired galaxies from the SDSS/DR7 spectroscopic sample. Results of different surveys show very good agreement. The satellite LFs can be measured down to MV ∼ -10, and for central primary galaxies as small as 8.5 < log10M /M⊙ < 9.2 and 9.2 < log10M /M⊙ < 9.9, which implies there are on average 3-8 satellites with MV < -10 around LMC-mass ICGs. The bright end cutoff of satellite LFs and the satellite abundance are both sensitive to the magnitude gap between the primary and its companions, indicating galaxy systems with larger magnitude gaps are on average hosted by less massive dark matter haloes. By selecting primaries with stellar mass similar to our Milky Way (MW), we discovered that (i) the averaged satellite LFs of ICGs with different magnitude gaps to their companions and of galaxy pairs with different colour or colour combinations all show steeper slopes than the MWsatellite LF; (ii) there are on average more satellites with -15 < MV < -10 than those in our MW; (iii) there are on average 1.5 to 2.5 satellites with MV < -16 around ICGs, consistent with our MW; (iv) even after accounting for the large scatter predicted by numerical simulations, the MW satellite LF is uncommon at MV > -12. Hence, the MWand its satellite system are statistically atypical of our sample of MW-mass systems. In consequence, our MW is not a good representative of other MW-mass galaxies. Strong cosmological implications based on only MW satellites await additional discoveries of fainter satellites in extra-galactic systems. Interestingly, the MW satellite LF is typical among other MW-mass systems within 40 Mpc in the local Universe, perhaps implying the Local Volume is an underdense region.

DOI： 10.1093/mnras/staa3495

FPFS Shear Estimator: Systematic Tests on the Hyper Suprime-Cam Survey First-year Data 査読有り

Li, XC; Oguri, M; Katayama, N; Luo, WT; Wang, WT; Han, JX; Miyatake, H; Nakamura, K; More, S

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES 251 巻 ( 2 ) 2020年12月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal, Supplement Series

We apply the Fourier Power Function Shapelets (FPFS) shear estimator to the first-year data of the Hyper Suprime-Cam survey to construct a shape catalog. The FPFS shear estimator has been demonstrated to have a multiplicative bias less than 1% in the absence of blending, regardless of complexities of galaxy shapes, smears of point spread functions (PSFs), and contamination from noise. The blending bias is calibrated with realistic image simulations, which include the impact of neighboring objects, using the COSMOS Hubble Space Telescope images. Here we carefully test the influence of PSF model residual on the FPFS shear estimation and the uncertainties in the shear calibration. Internal null tests are conducted to characterize potential systematics in the FPFS shape catalog, and the results are compared with those measured using a catalog where the shapes were estimated using the re-Gaussianization algorithms. Furthermore, we compare various weak-lensing measurements between the FPFS shape catalog and the re-Gaussianization shape catalog and conclude that the weak-lensing measurements between these two shape catalogs are consistent with each other within the statistical uncertainty.

DOI： 10.3847/1538-4365/abbad1

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