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<ri:Resource created="2014-11-25T12:31:00Z" 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>Relaxation parameter of 2092 rich galaxy clusters</title><shortName>J/MNRAS/436/275</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/436/275</identifier><altIdentifier>doi:10.26093/cds/vizier.74360275</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Wen Z.L.</name></creator><creator><name>Han J.L.</name></creator><date role="Updated">2024-08-07T20:11:59Z</date><date role="Created">2014-11-25T12:31:00Z</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>galaxy-classification-systems</subject><description>Dynamical state of galaxy clusters is closely related to their observational properties in X-ray, optical and radio wavelengths. We develop a method to diagnose the substructure and dynamical state of galaxy clusters by using photometric data of Sloan Digital Sky Survey (SDSS). To trace mass distribution, the brightness distribution of member galaxies is smoothed by using a Gaussian kernel with a weight of their optical luminosities. After deriving the asymmetry, the ridge flatness and the normalized deviation of the smoothed optical map, we define a relaxation parameter, {Gamma}, to quantify dynamical state of clusters. This method is applied to a test sample of 98 clusters of 0.05&lt;z&lt;~0.42 collected from literature with known dynamical states and can recognize dynamical state for relaxed ({Gamma}&gt;=0) and unrelaxed ({Gamma}&lt;0) clusters with a success rate of 94 percent. We then calculate relaxation parameters of 2092 rich clusters previously identified from the SDSS, of which 28 percent clusters are dynamically relaxed with {Gamma}&gt;=0. We find that the dominance and absolute magnitude of the brightest cluster galaxies closely correlate with dynamical states of clusters. The emission power of radio haloes is quantitatively related to cluster dynamical state, beside the known dependence on the X-ray luminosity.</description><source format="bibcode">2013MNRAS.436..275W</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/436/275</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/J/ApJS/183/197">J/ApJS/183/197 : Galaxy clusters identified from the SDSS-DR6 (Wen+, 2009)</relatedResource><relatedResource>http://www.sdss3.org/dr8 : SDSS DR8 Home 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Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>WHL</name><description>Cluster name (JHHMMSS.s+DDMMSS)</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="16*">char</dataType></column><column><name>RAJ2000</name><description>BCG right ascension (J2000) (1)</description><unit>deg</unit><ucd>pos.eq.ra;meta.main</ucd></column><column><name>DEJ2000</name><description>BCG declination (J2000) (1)</description><unit>deg</unit><ucd>pos.eq.dec;meta.main</ucd></column><column><name>z</name><description>[0.05/0.42] photometric or spectroscopic redshift</description><ucd>src.redshift</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>f_z</name><description>[0/1] 0 for photometric, 1 for spectroscopic redshift</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>rmag</name><description>[13/20] BCG r magnitude (1)</description><unit>mag</unit><ucd>phot.mag;em.opt.R</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>R200</name><description>[1.2/2.3] Radius r_200_ of cluster</description><unit>Mpc</unit><ucd>phys.size.radius</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>N200</name><description>[30/178] Number of member galaxies within R200</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Gamma</name><description>Relaxation parameter {Gamma} (2)</description><ucd>stat.fit.param</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_Gamma</name><description>rms uncertainty on Gamma</description><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Sloan</name><description>Display the SDSS data for this cluster</description><ucd>meta.ref.url</ucd><dataType xsi:type="vs:VOTableType" arraysize="*">char</dataType></column></table></schema></tableset></ri:Resource>