J/A+A/637/A58ivo://CDS.VizieR/J/A+A/637/A58doi:10.26093/cds/vizier.36370058CDSLiu A.Tozzi P.Ettori S.De Grandi S.Gastaldello F.Rosati P.,Norman C.2021-03-23T13:04:06Z2020-09-17T07:06:33ZCDS support team

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

cds-question@unistra.frgalaxy-clustersx-ray-sourcesredshiftedWe study the chemical evolution of galaxy clusters by measuring the iron mass in the ICM after dissecting the abundance profiles into different components. We used Chandra archival observations of 186 morphologically regular clusters in the redshift range of [0.04, 1.07]. For each cluster, we computed the azimuthally averaged iron abundance and gas density profiles. In particular, our aim is to identify a central peak in the iron distribution, which is associated with the central galaxy, and an approximately constant plateau reaching the largest observed radii, which is possibly associated with early enrichment that occurred before or shortly after achieving virialization within the cluster. We were able to firmly identify two components in the iron distribution in a significant fraction of the sample simply by relying on the fit of the iron abundance profile. From the abundance and ICM density profiles, we computed the iron mass included in the iron peak and iron plateau, and the gas mass-weighted iron abundance of the ICM out to an extraction radius of 0.4r_500_ and to r_500_ by extending the abundance profile as a constant. We find that the iron plateau shows no evolution with redshift. On the other hand, we find a marginal (<2{sigma} c.l.) decrease with redshift in the iron mass included in the iron peak rescaled by the gas mass. We measure that the fraction of iron peak mass is typically a few percent (~1%) of the total iron mass within r_500_. Therefore, since the total iron mass budget is dominated by the plateau, we find consistently that the global gas mass-weighted iron abundance does not evolve significantly across our sample. We were also able to reproduce past claims of evolution in the global iron abundance, which turn out to be due to the use of cluster samples with different selection methods combined with the use of emission-weighted, instead of gas mass-weighted, abundance values. Finally, while the intrinsic scatter in the iron plateau mass is consistent with zero, the iron peak mass exhibits a large scatter, in line with the fact that the peak is produced after the virialization of the halo and depends on the formation history of the hosting cool core and the strength of the associated feedback processes. We conclude that only a spatially resolved approach can resolve the issue of iron abundance evolution in the ICM, reconciling the contradictory results obtained in the last ten years. Evolutionary effects below z~1 are marginally measurable with present-day data, while at z>1 the constraints are severely limited by poor knowledge of the high-z cluster population. The path towards a full and comprehensive chemical history of the ICM requires the application of high angular resolution X-ray bolometers and a dramatic increase in the number of faint, extended X-ray sources.2020A&A...637A..58Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/637/A58CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toB/chandra : The Chandra Archive Log (CXC, 1999-)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/637/A58https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/637/A58http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/637/A58https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/637/A58https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/637/A58http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/637/A58GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/637/A58/tablea1 (Global properties we measured for the 186 clusters)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/637/A58/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/637/A58/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/637/A58/tablea1?GETtext/xml+votable180.050000true116.072837.88820.0055555555555555566/3 97 206-207 821 1603 2920 4206 4341 4394 4867 5099 5327 5438 5536 5701 5795 5881 5931 6019 6088 6337 6441 6536 6539 6873 7242 7513 7904 7928 8033 8220 8422 8648 8921 8963 8969 9052 9366 9466 9476 9498 9506 9764 9997 10312 10318 10544 10607 10664 11042 11063 11253 11591 11626 11807 11846 12253 12664 13384 15192 16229 16410 16492 16609 16702 16787 16953 16959 17124 17171 17237 17457 17499 17840 18016 18475 18534 18566 18584 18622 18746 18784 18800 18894 19009 19089 19097 19501 19848 20302 20507 20624 20874 21073 21211 21766 22771 23173 23324 23349 23451 24853 25302 25391 25451 26037 26135 26177 26189 26208 26302 26785 27075 27136 27428 27694 28220 28271 28430 28448 28622 31288 31398 31509 31537 32500 32503 32739 32960 33614 33628 34087 34174 34181 34443 34461 34954 35147 35271 35808 35950 36028 36082 36089 36242 36423 36846 37395 38822 38858 39043 39068 39079 40615 40777 41081 41326 43358 43706 43837 43939 44108 44502 44563 44802 45044 45421 45543 46005 46368 46424 46687 46763 46855 46889 46892 47043 47139 47573 48076 48174 48423 48688 49012https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/637/A58?format=asciiX-raydefaultJ/A+A/637/A58/tablea1Global properties we measured for the 186 clustersSimbadNameSimbad column added by the CDSmeta.idcharMgasGaz mass within r5001e+14solMassphys.massfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameNamemeta.id;meta.maincharRAJ2000Right ascension (J2000) of cluster emissiondegpos.eq.ra;meta.mainDEJ2000Declination (J2000) of cluster emissiondegpos.eq.dec;meta.mainzXX-ray redshift of the clustersrc.redshift;pos.heliocentricfloate_zXrms uncertainty on X-ray redshiftstat.errorfloatkTTemperature of the cluster measured within (0.1-0.4)_r500_keVphys.temperaturefloate_kTrms uncertainty on temperaturekeVstat.error;phys.energyfloatM500Mass within r5001e+14solMassphys.massfloate_M500rms uncertainty on mass within r5001e+14solMassstat.errorfloate_Mgasrms uncertainty on gaz mass within r5001e+14solMassstat.errorfloatZewEmission-weighted iron abundance within 0.4_r500_log(Sun)phys.abund.Fefloate_Zewrms uncertainty on emission-weighted iron abundance within 0.4_r500_log(Sun)stat.errorfloatZmw1Gas mass-weighted iron abundance within 0.4_r500_log(Sun)phys.abund.Fefloate_Zmw1rms uncertainty on gas mass-weighted iron abundance within 0.4_r500_log(Sun)stat.errorfloatZmw2Gas mass-weighted iron abundance within r500log(Sun)phys.abund.Fefloate_Zmw2rms uncertainty on gas mass-weighted iron abundance within r500log(Sun)stat.errorfloat