{"@context":{"@vocab":"https://cir.nii.ac.jp/schema/1.0/","rdfs":"http://www.w3.org/2000/01/rdf-schema#","dc":"http://purl.org/dc/elements/1.1/","dcterms":"http://purl.org/dc/terms/","foaf":"http://xmlns.com/foaf/0.1/","prism":"http://prismstandard.org/namespaces/basic/2.0/","cinii":"http://ci.nii.ac.jp/ns/1.0/","datacite":"https://schema.datacite.org/meta/kernel-4/","ndl":"http://ndl.go.jp/dcndl/terms/","jpcoar":"https://github.com/JPCOAR/schema/blob/master/2.0/"},"@id":"https://cir.nii.ac.jp/crid/1360568619413727872.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.3847/1538-4357/ab6596"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4357/ab6596/pdf"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4357/ab6596"}},{"identifier":{"@type":"DOI","@value":"10.48550/arxiv.1912.10954"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"Balmer Break Galaxy Candidates at z ∼ 6: A Potential View on the Star Formation Activity at z ≳ 14"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title>\n               <jats:p>We search for galaxies with a strong Balmer break (Balmer break galaxies; BBGs) at <jats:italic>z</jats:italic> ∼ 6 over a 0.41 deg<jats:sup>2</jats:sup> effective area in the COSMOS field. Based on rich imaging data, including data obtained with the Atacama Large Millimeter/submillimeter Array (ALMA), three candidates are identified by their extremely red <jats:italic>K</jats:italic>–[3.6] colors, as well as by nondetection in the X-ray, optical, far-infrared, and radio bands. The nondetection in the deep ALMA observations suggests that they are not dusty galaxies but BBGs at <jats:italic>z</jats:italic> ∼ 6, although contamination from active galactic nuclei at <jats:italic>z</jats:italic> ∼ 0 cannot be completely ruled out for the moment. Our spectral energy distribution analyses reveal that the BBG candidates at <jats:italic>z</jats:italic> ∼ 6 have stellar masses of ≈5 × 10<jats:sup>10</jats:sup>\n                  <jats:italic>M</jats:italic>\n                  <jats:sub>⊙</jats:sub> dominated by old stellar populations with ages of ≳ 700 Myr. Assuming that all three candidates are real BBGs at <jats:italic>z</jats:italic> ∼ 6, we estimate the stellar mass density to be <jats:inline-formula>\n                     <jats:tex-math>\n\n</jats:tex-math>\n                     <jats:inline-graphic xmlns:xlink=\"http://www.w3.org/1999/xlink\" xlink:href=\"apjab6596ieqn1.gif\" xlink:type=\"simple\"/>\n                  </jats:inline-formula> Mpc<jats:sup>−3</jats:sup>. This is consistent with an extrapolation from the lower-redshift measurements. The onset of star formation in the three BBG candidates is expected to be several hundred million yr before the observed epoch of <jats:italic>z</jats:italic> ∼ 6. We estimate the star formation rate density (SFRD) contributed by progenitors of the BBGs to be 2.4–12 × 10<jats:sup>−5</jats:sup>\n                  <jats:italic>M</jats:italic>\n                  <jats:sub>⊙</jats:sub> yr<jats:sup>−1</jats:sup> Mpc<jats:sup>−3</jats:sup> at <jats:italic>z</jats:italic> > 14 (99.7% confidence range). Our result suggests a smooth evolution of the SFRD beyond <jats:italic>z</jats:italic> = 8.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1420564276170112384","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"00838287"},{"@type":"NRID","@value":"1000000838287"},{"@type":"NRID","@value":"9000403296305"},{"@type":"NRID","@value":"9000409846938"},{"@type":"RESEARCHMAP","@value":"https://researchmap.jp/kenmawatari"}],"foaf:name":[{"@value":"Ken Mawatari"}]},{"@id":"https://cir.nii.ac.jp/crid/1380568619413727622","@type":"Researcher","foaf:name":[{"@value":"Akio K. Inoue"}]},{"@id":"https://cir.nii.ac.jp/crid/1380568619413727877","@type":"Researcher","foaf:name":[{"@value":"Takuya Hashimoto"}]},{"@id":"https://cir.nii.ac.jp/crid/1380568619413727892","@type":"Researcher","foaf:name":[{"@value":"John Silverman"}]},{"@id":"https://cir.nii.ac.jp/crid/1420564276187481728","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"60535334"},{"@type":"NRID","@value":"1000060535334"},{"@type":"NRID","@value":"9000409849382"},{"@type":"NRID","@value":"9000024559831"},{"@type":"NRID","@value":"9000411963364"},{"@type":"NRID","@value":"9000368412020"},{"@type":"RESEARCHMAP","@value":"https://researchmap.jp/mkajisawa"}],"foaf:name":[{"@value":"Masaru Kajisawa"}]},{"@id":"https://cir.nii.ac.jp/crid/1380568619413727627","@type":"Researcher","foaf:name":[{"@value":"Satoshi Yamanaka"}]},{"@id":"https://cir.nii.ac.jp/crid/1380568619413727886","@type":"Researcher","foaf:name":[{"@value":"Toru Yamada"}]},{"@id":"https://cir.nii.ac.jp/crid/1380568619413727878","@type":"Researcher","foaf:name":[{"@value":"Iary Davidzon"}]},{"@id":"https://cir.nii.ac.jp/crid/1380568619413727496","@type":"Researcher","foaf:name":[{"@value":"Peter Capak"}]},{"@id":"https://cir.nii.ac.jp/crid/1380568619413728003","@type":"Researcher","foaf:name":[{"@value":"Lihwai Lin"}]},{"@id":"https://cir.nii.ac.jp/crid/1380568619413727497","@type":"Researcher","foaf:name":[{"@value":"Bau-Ching Hsieh"}]},{"@id":"https://cir.nii.ac.jp/crid/1380568619413727749","@type":"Researcher","foaf:name":[{"@value":"Yoshiaki Taniguchi"}]},{"@id":"https://cir.nii.ac.jp/crid/1380568619413727872","@type":"Researcher","foaf:name":[{"@value":"Masayuki 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