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xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xmlns:xsi0="https://www.w3.org/2001/XMLSchema-instance" xmlns:xu="http://www.xmldb.org/xupdate"><oai:identifier>ivo://CDS.VizieR/J/ApJS/275/36</oai:identifier><oai:datestamp>2025-07-17T14:54:31Z</oai:datestamp><oai:setSpec>J.ApJS</oai:setSpec></oai:header><oai:metadata><eudc:resource xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xmlns:eudc="http://schema.eudat.eu/schema/kernel-1" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:oai="http://www.openarchives.org/OAI/2.0/" xmlns:dachs="urn:dachs" xsi:schemaLocation="http://schema.eudat.eu/schema/kernel-1           http://docs.g-vo.org/schemata/eudat-core.xsd"><eudc:community>IVOA</eudc:community><eudc:titles><eudc:title>ALMA Lensing Cluster Survey (ALCS) 1.2mm</eudc:title></eudc:titles><eudc:descriptions><eudc:description>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 133arcmin^2^ area, homogeneously observed at 1.2mm. 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 (N=141) with signal-to-noise ratio (S/N)&gt;~5.0 (a purity of &gt;0.99) or a secondary sample (N=39) with S/N=4.0-5.0 screened by priors. With the blind sample, we securely derive 1.2mm number counts down to ~7{mu}Jy, and find that the total integrated 1.2mm flux is 20.7_-6.5_^+8.5^Jy/deg^2^, 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 z=0.6-7.5 with the 1/Vmax 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 z&gt;4 is estimated to be 161_-21_^+25^% 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.</eudc:description></eudc:descriptions><eudc:keywords><eudc:keyword>galaxy-clusters</eudc:keyword><eudc:keyword>millimeter-astronomy</eudc:keyword><eudc:keyword>submillimeter-astronomy</eudc:keyword><eudc:keyword>surveys</eudc:keyword><eudc:keyword>redshifted</eudc:keyword><eudc:keyword>infrared-sources</eudc:keyword><eudc:keyword>interferometry</eudc:keyword><eudc:keyword>gravitational-lensing</eudc:keyword><eudc:keyword>astrophysical-processes</eudc:keyword><eudc:keyword>galactic-and-extragalactic-astronomy</eudc:keyword><eudc:keyword>cosmology</eudc:keyword><eudc:keyword>observational-astronomy</eudc:keyword></eudc:keywords><eudc:identifiers><eudc:identifier identifierType="URL">https://dc.g-vo.org/rr/q/lp/custom/CDS.VizieR/J/ApJS/275/36</eudc:identifier></eudc:identifiers><eudc:relatedIdentifiers><eudc:relatedIdentifier relatedIdentifierType="URL">https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/275/36</eudc:relatedIdentifier><eudc:relatedIdentifier relatedIdentifierType="bibcode">2024ApJS..275...36F</eudc:relatedIdentifier><eudc:relatedIdentifier relatedIdentifierType="URL">https://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJS/275/36</eudc:relatedIdentifier><eudc:description>Cone search capability for table J/ApJS/275/36/table1 (ALCS data properties for 33 lensing clusters)</eudc:description><eudc:description>Cone search capability for table J/ApJS/275/36/table12 (ALCS continuum source catalog)</eudc:description></eudc:relatedIdentifiers><eudc:creators><eudc:creator><eudc:creatorName>Fujimoto S.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Kohno K.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Ouchi M.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Oguri M.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Kokorev V.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Brammer G.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Sun F.,Gonzalez-Lopez J.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Bauer F.E.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Caminha G.B.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Hatsukade B.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Richard J.,Smail I.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Tsujita A.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Ueda Y.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Uematsu R.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Zitrin A.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Coe D.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Kneib J.-P.,Postman M.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Umetsu K.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>del P. 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