{"@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/1360588381069159296.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.3847/1538-4365/ad5ae2"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4365/ad5ae2"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4365/ad5ae2/pdf"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title>\n               <jats:p>We present a statistical study of 180 dust continuum sources identified in 33 massive cluster fields by the Atacama Large Millimeter/submillimeter Array Lensing Cluster Survey (ALCS) over a total of 133 arcmin<jats:sup>2</jats:sup> area, homogeneously observed at 1.2 mm. ALCS enables us to detect extremely faint millimeter sources by lensing magnification, including near-infrared (NIR) dark objects showing no counterparts in existing Hubble Space Telescope and Spitzer images. The dust continuum sources belong to a blind sample (<jats:italic>N</jats:italic> = 141) with signal-to-noise ratio (S/N) ≳ 5.0 (a purity of >0.99) or a secondary sample (<jats:italic>N</jats:italic> = 39) with S/N = 4.0–5.0 screened by priors. With the blind sample, we securely derive 1.2 mm number counts down to ∼7 <jats:italic>μ</jats:italic>Jy, and find that the total integrated 1.2 mm flux is <jats:inline-formula>\n                     <jats:tex-math>\n\n</jats:tex-math>\n                     <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\">\n                        <mml:msubsup>\n                           <mml:mrow>\n                              <mml:mn>20.7</mml:mn>\n                           </mml:mrow>\n                           <mml:mrow>\n                              <mml:mo>−</mml:mo>\n                              <mml:mn>6.5</mml:mn>\n                           </mml:mrow>\n                           <mml:mrow>\n                              <mml:mo>+</mml:mo>\n                              <mml:mn>8.5</mml:mn>\n                           </mml:mrow>\n                        </mml:msubsup>\n                     </mml:math>\n                  </jats:inline-formula> Jy deg<jats:sup>−2</jats:sup>, resolving ≃80% of the cosmic infrared background light. The resolved fraction varies by a factor of 0.6–1.1 due to the completeness correction depending on the spatial size of the millimeter emission. We also derive infrared (IR) luminosity functions (LFs) at <jats:italic>z</jats:italic> = 0.6–7.5 with the <jats:inline-formula>\n                     <jats:tex-math>\n\n</jats:tex-math>\n                     <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\">\n                        <mml:mn>1</mml:mn>\n                        <mml:mrow>\n                           <mml:mo stretchy=\"true\">/</mml:mo>\n                        </mml:mrow>\n                        <mml:msub>\n                           <mml:mrow>\n                              <mml:mi>V</mml:mi>\n                           </mml:mrow>\n                           <mml:mrow>\n                              <mml:mi>max</mml:mi>\n                           </mml:mrow>\n                        </mml:msub>\n                     </mml:math>\n                  </jats:inline-formula> method, finding the redshift evolution of IR LFs characterized by positive luminosity and negative density evolution. The total (= UV + IR) cosmic star formation rate density (SFRD) at <jats:italic>z</jats:italic> > 4 is estimated to be <jats:inline-formula>\n                     <jats:tex-math>\n\n</jats:tex-math>\n                     <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\">\n                        <mml:msubsup>\n                           <mml:mrow>\n                              <mml:mn>161</mml:mn>\n                           </mml:mrow>\n                           <mml:mrow>\n                              <mml:mo>−</mml:mo>\n                              <mml:mn>21</mml:mn>\n                           </mml:mrow>\n                           <mml:mrow>\n                              <mml:mo>+</mml:mo>\n                              <mml:mn>25</mml:mn>\n                           </mml:mrow>\n                        </mml:msubsup>\n                     </mml:math>\n                  </jats:inline-formula>% of the Madau and Dickinson measurements mostly based on rest-frame UV surveys. Although our general understanding of the cosmic SFRD is unlikely to change beyond a factor of 2, these results add to the weight of evidence for an additional (≈60%) SFRD component contributed by the faint millimeter population, including NIR-dark objects.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380588381069159297","@type":"Researcher","foaf:name":[{"@value":"Seiji Fujimoto"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159311","@type":"Researcher","foaf:name":[{"@value":"Kotaro Kohno"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159329","@type":"Researcher","foaf:name":[{"@value":"Masami Ouchi"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159460","@type":"Researcher","foaf:name":[{"@value":"Masamune Oguri"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159428","@type":"Researcher","foaf:name":[{"@value":"Vasily Kokorev"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159184","@type":"Researcher","foaf:name":[{"@value":"Gabriel Brammer"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159729","@type":"Researcher","foaf:name":[{"@value":"Fengwu Sun"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159448","@type":"Researcher","foaf:name":[{"@value":"Jorge González-López"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159706","@type":"Researcher","foaf:name":[{"@value":"Dan Coe"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159303","@type":"Researcher","foaf:name":[{"@value":"Jean-Paul Kneib"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159700","@type":"Researcher","foaf:name":[{"@value":"Marc Postman"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159553","@type":"Researcher","foaf:name":[{"@value":"Adi Zitrin"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159186","@type":"Researcher","foaf:name":[{"@value":"Keiichi Umetsu"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159471","@type":"Researcher","foaf:name":[{"@value":"Claudia del P. Lagos"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159315","@type":"Researcher","foaf:name":[{"@value":"Gergö Popping"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159296","@type":"Researcher","foaf:name":[{"@value":"Yiping Ao"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159309","@type":"Researcher","foaf:name":[{"@value":"Larry Bradley"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159569","@type":"Researcher","foaf:name":[{"@value":"Karina Caputi"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159695","@type":"Researcher","foaf:name":[{"@value":"Miroslava Dessauges-Zavadsky"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159433","@type":"Researcher","foaf:name":[{"@value":"Eiichi Egami"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159205","@type":"Researcher","foaf:name":[{"@value":"Daniel Espada"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159450","@type":"Researcher","foaf:name":[{"@value":"R. J. Ivison"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159044","@type":"Researcher","foaf:name":[{"@value":"Mathilde Jauzac"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159453","@type":"Researcher","foaf:name":[{"@value":"Kirsten K. Knudsen"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159461","@type":"Researcher","foaf:name":[{"@value":"Anton M. Koekemoer"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159193","@type":"Researcher","foaf:name":[{"@value":"Guillaume Mahler"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159300","@type":"Researcher","foaf:name":[{"@value":"Georgios E. Magdis"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159716","@type":"Researcher","foaf:name":[{"@value":"Franz E. Bauer"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159564","@type":"Researcher","foaf:name":[{"@value":"Gabriel B. Caminha"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159046","@type":"Researcher","foaf:name":[{"@value":"Bunyo Hatsukade"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159319","@type":"Researcher","foaf:name":[{"@value":"A. M. Muñoz Arancibia"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159313","@type":"Researcher","foaf:name":[{"@value":"Johan Richard"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159316","@type":"Researcher","foaf:name":[{"@value":"Timothy Rawle"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159204","@type":"Researcher","foaf:name":[{"@value":"Ian Smail"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159732","@type":"Researcher","foaf:name":[{"@value":"Kazuhiro Shimasaku"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159565","@type":"Researcher","foaf:name":[{"@value":"Akiyoshi Tsujita"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159192","@type":"Researcher","foaf:name":[{"@value":"Sune 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Uematsu"}]},{"@id":"https://cir.nii.ac.jp/crid/1420001326212169728","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"60783678"},{"@type":"NRID","@value":"1000060783678"},{"@type":"NRID","@value":"9000107396561"},{"@type":"NRID","@value":"9000403296322"},{"@type":"NRID","@value":"9000409846940"},{"@type":"NRID","@value":"9000319057224"},{"@type":"RESEARCHMAP","@value":"https://researchmap.jp/hideki_umehata"}],"foaf:name":[{"@value":"Hideki Umehata"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159171","@type":"Researcher","foaf:name":[{"@value":"Francesco Valentino"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159060","@type":"Researcher","foaf:name":[{"@value":"Tao Wang"}]},{"@id":"https://cir.nii.ac.jp/crid/1380588381069159447","@type":"Researcher","foaf:name":[{"@value":"Wei-Hao Wang"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"00670049"},{"@type":"EISSN","@value":"15384365"}],"prism:publicationName":[{"@value":"The 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of cosmic web filaments and galaxies in the early universe"}]},{"@id":"https://cir.nii.ac.jp/crid/1040018506566623616","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"24KJ0562"},{"@type":"JGN","@value":"JP24KJ0562"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-24KJ0562/"}],"notation":[{"@language":"ja","@value":"ALMA×JWST×重力レンズで探るダストに隠された銀河進化過程の解明"},{"@language":"en","@value":"Resolving dust-obscured galaxy evolution with ALMA, JWST, and gravitational lensing"}]},{"@id":"https://cir.nii.ac.jp/crid/1040295027725050752","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"22KK0231"},{"@type":"JGN","@value":"JP22KK0231"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-22KK0231/"}],"notation":[{"@language":"ja","@value":"初期宇宙における宇宙網と銀河の共進化の研究"},{"@language":"en","@value":"Co-evolution of cosmic web filaments and galaxies in the early 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