J/A+A/527/A134ivo://CDS.VizieR/J/A+A/527/A134doi:10.26093/cds/vizier.35270134CDSMatsushita K.2020-09-03T08:27:26Z2011-09-03T14:52:06ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgalaxy-clustersx-ray-sourcesmetallicityThe abundances of Fe in the intracluster medium of nearby (z<0.08) clusters were measured up to 0.3~0.5r_180_. We analyzed 28 clusters of galaxies observed with XMM-Newton. We derived Fe abundances from the flux ratios of Fe lines to the continuum within an energy range of 3.5-6keV to minimize and evaluate systematic uncertainties.2011A&A...527A.134Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/527/A134CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toB/xmm : XMM-Newton Observation Log (XMM-Newton Science Operation Center, 2009)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/527/A134https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/527/A134http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/527/A134https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/527/A134https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/527/A134http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/527/A134GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/527/A134/clusters (Clusters studied (from table 1 of paper))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/527/A134/clusters?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/527/A134/clusters?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/527/A134/clusters?GETtext/xml+votable180.050000true28.2136.1461110.0055555555555555566/1701 2388 2432 8220 8264 8268 8271 9468 10312 10379 12121 16543 17237 20021 22577 24943 27767 28249 33235 38853 40777 40809 41423 43627 43837-43838 43849 45984https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/527/A134?format=asciiX-raydefaultJ/A+A/527/A134/clustersClusters studied (from table 1 of paper)SimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintClusterCluster namemeta.id;meta.maincharprimaryONameOther name of clustermeta.idcharzRedshiftsrc.redshiftfloat<kT>Adopted average temperature of ICM used to calculate the virial radius r_180_keVphys.temperaturefloatNHGalactic value of the hydrogen column density (Dickey & Lockman, 1990ARA&A..28..215D)1e+20cm**-2phys.columnDensity;pos.galacticfloatTypeType of cluster: cD or non-cD (G1)src.classchar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/A+A/527/A134/table1Cluster samples in the XMM-Newton archival datarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintClusterCluster namemeta.id;meta.maincharObsIDXMM Obs IDmeta.id;obsExpPNExposure time of PN camera (2)kstime.duration;obs.exposurefloatExpMOS1Exposure time of MOS1 camera (2)kstime.duration;obs.exposurefloatExpMOS2Exposure time of MOS2 camera (2)kstime.duration;obs.exposurefloatJ/A+A/527/A134/table2Results of spectral fitting of annular spectrarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintClusterCluster namemeta.id;meta.maincharrlLower value of radius interval, in units of r180phys.size.radius;arith.ratiofloatruUpper value of radius interval, in units of r180phys.size.radius;arith.ratiofloatkTBest-fit ICM temperature derived from the 1T model fitskeVphys.temperaturefloate_kT1{sigma} statistical error on kTkeVphys.temperaturefloatFeABest-fit Fe abundance using the ICM temperature derived from the 1T model fits (from F_FeHeK_/F_3.5-6_)log(Sun)phys.abund.Fe;meta.modelledfloate_FeA1{sigma} statistical error on FeA (1)log(Sun)stat.errorfloatDFeADifference in the derived FeA abundances using the best-fit multi-T model and the 1T modellog(Sun)stat.param;meta.modelledfloatFeB? Best-fit Fe abundance using the ICM temperature derived from the 1T model fits (for F_FeHK_/F_3.5-6_)log(Sun)phys.abund.Fe;meta.modelledfloatnullablee_FeB? 1{sigma} statistical error on FeB (1)log(Sun)stat.errorfloatnullableDFeB? Difference in the derived FeB abundances using the best-fit multi-T model and the 1T modellog(Sun)stat.param;meta.modelledfloatnullable