{"created":"2021-03-01T06:36:28.294202+00:00","id":28388,"links":{},"metadata":{"_buckets":{"deposit":"9f517610-cdfe-4fb9-97b7-92e90c3cbcb4"},"_deposit":{"id":"28388","owners":[],"pid":{"revision_id":0,"type":"depid","value":"28388"},"status":"published"},"_oai":{"id":"oai:nagoya.repo.nii.ac.jp:00028388","sets":["2026:2027:2028"]},"author_link":["92822","92823","92824","92825","92826","92827","92828","92829","92830","92831","92832","92833","92834","92835","92836","92837","92838","92839","92840","92841","92842","92843","92844","92845","92846","92847","92848","92849","92850","92851","92852","92853","92854","92855","92856","92857","92858","92859","92860","92861","92862","92863","92864","92865","92866","92867","92868","92869","92870","92871","92872","92873","92874","92875","92876","92877","92878","92879","92880","92881"],"item_10_biblio_info_6":{"attribute_name":"書誌情報","attribute_value_mlt":[{"bibliographicIssueDates":{"bibliographicIssueDate":"2019-04","bibliographicIssueDateType":"Issued"},"bibliographicIssueNumber":"1","bibliographicPageStart":"63","bibliographicVolumeNumber":"875","bibliographic_titles":[{"bibliographic_title":"The Astrophysical Journal","bibliographic_titleLang":"en"}]}]},"item_10_description_4":{"attribute_name":"抄録","attribute_value_mlt":[{"subitem_description":"We present weak-lensing measurements using the first-year data from the Hyper Suprime-Cam Strategic Survey Program on the Subaru telescope for eight galaxy clusters selected through their thermal Sunyaev–Zel'dovich (SZ) signal measured at 148 GHz with the Atacama Cosmology Telescope Polarimeter experiment. The overlap between the two surveys in this work is 33.8 square degrees, before masking bright stars. The signal-to-noise ratio of individual cluster lensing measurements ranges from 2.2 to 8.7, with a total of 11.1 for the stacked cluster weak-lensing signal. We fit for an average weak-lensing mass distribution using three different profiles, a Navarro–Frenk–White profile, a dark-matter-only emulated profile, and a full cosmological hydrodynamic emulated profile. We interpret the differences among the masses inferred by these models as a systematic error of 10%, which is currently smaller than the statistical error. We obtain the ratio of the SZ-estimated mass to the lensing-estimated mass (the so-called hydrostatic mass bias 1−b) of ${0.74}_{-0.12}^{+0.13}$, which is comparable to previous SZ-selected clusters from the Atacama Cosmology Telescope and from the Planck Satellite. We conclude with a discussion of the implications for cosmological parameters inferred from cluster abundances compared to cosmic microwave background primary anisotropy measurements.","subitem_description_language":"en","subitem_description_type":"Abstract"}]},"item_10_publisher_32":{"attribute_name":"出版者","attribute_value_mlt":[{"subitem_publisher":"IOP publishing","subitem_publisher_language":"en"}]},"item_10_relation_11":{"attribute_name":"DOI","attribute_value_mlt":[{"subitem_relation_type":"isVersionOf","subitem_relation_type_id":{"subitem_relation_type_id_text":"https://doi.org/10.3847/1538-4357/ab0af0","subitem_relation_type_select":"DOI"}}]},"item_10_rights_12":{"attribute_name":"権利","attribute_value_mlt":[{"subitem_rights":"© 2019. 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