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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/A+A/710/A202</oai:identifier><oai:datestamp>2026-06-18T00:10:11Z</oai:datestamp><oai:setSpec>J.A_A</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>CAMIRA clusters in the eFEDS field</eudc:title></eudc:titles><eudc:descriptions><eudc:description>This is the second paper in a series exploring the X-ray properties of galaxy clusters optically selected by the Subaru Hyper Suprime-Cam (HSC) survey, using data from the SRG/eROSITA Final Equatorial-Depth Survey (eFEDS). We aim to investigate scaling relations between observable cluster properties and mass, and to study the radial X-ray profiles of a large sample of optically selected clusters. We analyze a sample of 997 CAMIRA clusters with richness N&gt;15 and redshifts of 0.1&lt;z&lt;1.3. Using bolometric luminosities derived from count rates and a weak-lensing mass calibration, we study the L-M and N-M scaling relations through stacking analysis, while accounting for selection effects and redshift evolution. We also compare clusters with and without X-ray counterparts in the eFEDS catalog in terms of their scaling relations and surface brightness profiles. The best-fit L-M slope (1.56^+0.14^_-0.12_) is slightly steeper than the self-similar prediction, yet remains consistent with our previous findings. The N-M slope (0.766^+0.070^_-0.060_) broadly agrees with theoretical expectations and other optical samples. The data do not require any additional redshift evolution beyond the standard self-similar scaling, although current constraints on evolution remain weak. X-ray detected clusters exhibit a marginally steeper L-M slope, higher central surface brightness, and more centrally concentrated X-ray profiles than undetected systems. Our results highlight systematic differences in the X-ray properties between optically and X-ray selected cluster samples. This study extends scaling relation analyses into lower mass and luminosity regimes, demonstrating the value of combining deep X-ray and optical surveys like eROSITA and Subaru HSC.</eudc:description></eudc:descriptions><eudc:keywords><eudc:keyword>galaxy-clusters</eudc:keyword><eudc:keyword>x-ray-sources</eudc:keyword><eudc:keyword>galaxy-classification-systems</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/A+A/710/A202</eudc:identifier></eudc:identifiers><eudc:relatedIdentifiers><eudc:relatedIdentifier relatedIdentifierType="URL">https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/710/A202</eudc:relatedIdentifier><eudc:relatedIdentifier relatedIdentifierType="bibcode">2026A&amp;A...710A.202N</eudc:relatedIdentifier><eudc:relatedIdentifier relatedIdentifierType="URL">https://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/710/A202</eudc:relatedIdentifier><eudc:description>Cone search capability for table J/A+A/710/A202/table1 (CAMIRA clusters in the eFEDS field)</eudc:description></eudc:relatedIdentifiers><eudc:creators><eudc:creator><eudc:creatorName>Nguyen-Dang N.T.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Ota N.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Okabe N.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Oguri M.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Mitsuishi I.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Reiprich T.H.,Pacaud F.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Bulbul E.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Sanders J.S.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Brueggen M.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Liu A.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Tsujita Y.,Chiu I.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Ghirardini V.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Grandis S.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Klein M.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Migkas K.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Miyatake H.,Miyazaki S.</eudc:creatorName></eudc:creator><eudc:creator><eudc:creatorName>Ramos-Ceja M.E.</eudc:creatorName></eudc:creator></eudc:creators><eudc:publishers><eudc:publisher>CDS</eudc:publisher></eudc:publishers><eudc:instruments/><eudc:publicationYear>2026</eudc:publicationYear><eudc:rightsList><eudc:rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</eudc:rights></eudc:rightsList><eudc:fundingReferences/><eudc:contacts><eudc:contact>CDS support team &lt;cds-question@unistra.fr&gt;</eudc:contact></eudc:contacts><eudc:resourceTypes><eudc:resourceType>Dataset</eudc:resourceType><eudc:resourceType>AstroObjects</eudc:resourceType></eudc:resourceTypes><eudc:disciplines><eudc:discipline>astronomy</eudc:discipline></eudc:disciplines></eudc:resource></oai:metadata></oai:record></oai:GetRecord></oai:OAI-PMH>