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<ri:Resource created="2022-11-16T10:18:18Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>Sparsity &amp; gas mass fraction of galaxy clusters</title><shortName>J/ApJ/911/82</shortName><identifier>ivo://CDS.VizieR/J/ApJ/911/82</identifier><altIdentifier>doi:10.26093/cds/vizier.19110082</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Corasaniti P.-S.</name></creator><creator><name>Sereno M.</name></creator><creator><name>Ettori S.</name></creator><date role="Updated">2022-12-16T22:27:03Z</date><date role="Created">2022-11-16T10:18:18Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>galaxy-clusters</subject><subject>surveys</subject><subject>redshifted</subject><subject>visible-astronomy</subject><subject>x-ray-sources</subject><description>In recent years, the availability of large, complete cluster samples has enabled numerous cosmological parameter inference analyses using cluster number counts. These have provided constraints on the cosmic matter density {Omega}_m_ and the amplitude of matter density fluctuations {sigma}_8_ alternative to that obtained from other standard probes. However, systematics uncertainties, such as the mass calibration bias and selection effects, may still significantly affect these data analyses. Hence, it is timely to explore other proxies of galaxy cluster cosmology that can provide cosmological constraints complementary to those obtained from cluster number counts. Here we use measurements of the cluster sparsity from weak-lensing mass estimates of the LC^2^-single and HSC-XXL cluster catalogs to infer constraints on a flat {Lambda}CDM model. The cluster sparsity has the advantage of being insensitive to selection and mass calibration bias. On the other hand, it primarily constrains a degenerate combination of {Omega}_m_ and {sigma}_8_ (along approximately constant curves of S_8_={sigma}_8_({Omega}_m_/0.3)^0.5^ and, to a lesser extent, the reduced Hubble parameter h. Hence, in order to break the internal parameter degeneracies, we perform a combined likelihood analysis of the cluster sparsity estimates with cluster gas mass fraction measurements and BAO data. We find marginal constraints that are competitive with those from other standard cosmic probes: {Omega}_m_=0.316+/-0.013, {sigma}_8_=0.757+/-0.067 (corresponding to S_8_=0.776+/-0.064), and h=0.696+/-0.017 at 1{sigma}. Moreover, assuming a conservative Gaussian prior on the mass bias of gas mass fraction data, we find a lower limit on the gas depletion factor Y_b,500c_&gt;~0.89.</description><source format="bibcode">2021ApJ...911...82C</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/911/82</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/B/xmm">B/xmm : XMM-Newton Obs. 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First results (Bohringer+, 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/465/4914">J/MNRAS/465/4914 : R-band light curves of HE 0435-1223 (Bonvin+, 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/601/A145">J/A+A/601/A145 : Catalogue of cluster members (Foex+, 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/617/A64">J/A+A/617/A64 : 3D density &amp; temp. profiles of clusters (Bartalucci+, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/878/55">J/ApJ/878/55 : SPT-SZ clusters with optical &amp; X-ray data (Bocquet+, 2019)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/633/A69">J/A+A/633/A69 : KiDS-VIKING-450 cosmic shear (Hildebrandt+, 2020)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/890/148">J/ApJ/890/148 : Concentration-mass relation for XXL clusters (Umetsu+, 2020)</relatedResource><relatedResource>http://github.com/pierste75/Halo_Sparsity : 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