Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/26836
Campo DC | Valore | Lingua |
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dc.contributor.author | Andrade-Santos, Felipe | en_US |
dc.contributor.author | Jones, Christine | en_US |
dc.contributor.author | Forman, William R. | en_US |
dc.contributor.author | LOVISARI, LORENZO | en_US |
dc.contributor.author | Vikhlinin, Alexey | en_US |
dc.contributor.author | van Weeren, Reinout J. | en_US |
dc.contributor.author | Murray, Stephen S. | en_US |
dc.contributor.author | Arnaud, Monique | en_US |
dc.contributor.author | Pratt, Gabriel W. | en_US |
dc.contributor.author | Démoclès, Jessica | en_US |
dc.contributor.author | Kraft, Ralph | en_US |
dc.contributor.author | Mazzotta, Pasquale | en_US |
dc.contributor.author | Böhringer, Hans | en_US |
dc.contributor.author | Chon, Gayoung | en_US |
dc.contributor.author | Giacintucci, Simona | en_US |
dc.contributor.author | Clarke, Tracy E. | en_US |
dc.contributor.author | BORGANI, STEFANO | en_US |
dc.contributor.author | David, Larry | en_US |
dc.contributor.author | Douspis, Marian | en_US |
dc.contributor.author | Pointecouteau, Etienne | en_US |
dc.contributor.author | Dahle, Håkon | en_US |
dc.contributor.author | Brown, Shea | en_US |
dc.contributor.author | Aghanim, Nabila | en_US |
dc.contributor.author | RASIA, ELENA | en_US |
dc.date.accessioned | 2020-08-26T11:14:12Z | - |
dc.date.available | 2020-08-26T11:14:12Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/26836 | - |
dc.description.abstract | We derive and compare the fractions of cool-core clusters in the Planck Early Sunyaev-Zel’dovich sample of 164 clusters with z≤slant 0.35 and in a flux-limited X-ray sample of 100 clusters with z≤slant 0.30, using Chandra observations. We use four metrics to identify cool-core clusters: (1) the concentration parameter, which is the ratio of the integrated emissivity profile within 0.15 r <SUB>500</SUB> to that within r <SUB>500</SUB>; (2) the ratio of the integrated emissivity profile within 40 kpc to that within 400 kpc; (3) the cuspiness of the gas density profile, which is the negative of the logarithmic derivative of the gas density with respect to the radius, measured at 0.04 r <SUB>500</SUB>; and (4) the central gas density, measured at 0.01 r <SUB>500</SUB>. We find that the sample of X-ray-selected clusters, as characterized by each of these metrics, contains a significantly larger fraction of cool-core clusters compared to the sample of SZ-selected clusters (44% ± 7% versus 28% ± 4% using the concentration parameter in the 0.15-1.0 r <SUB>500</SUB> range, 61% ± 8% versus 36% ± 5% using the concentration parameter in the 40-400 kpc range, 64% ± 8% versus 38% ± 5% using the cuspiness, and 53% ± 7% versus 39 ± 5% using the central gas density). Qualitatively, cool-core clusters are more X-ray luminous at fixed mass. Hence, our X-ray, flux-limited sample, compared to the approximately mass-limited SZ sample, is overrepresented with cool-core clusters. We describe a simple quantitative model that uses the excess luminosity of cool-core clusters compared to non-cool-core clusters at fixed mass to successfully predict the observed fraction of cool-core clusters in X-ray-selected samples. | en_US |
dc.language.iso | eng | en_US |
dc.title | The Fraction of Cool-core Clusters in X-Ray versus SZ Samples Using Chandra Observations | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/aa7461 | en_US |
dc.identifier.scopus | 2-s2.0-85021742251 | en_US |
dc.identifier.isi | 000404847500012 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/aa7461 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 843 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 76 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2017ApJ...843...76A | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_9 Clusters of galaxies and large scale structures | en_US |
dc.description.apc | sì | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.orcid | 0000-0001-6151-6439 | - |
crisitem.author.orcid | 0000-0003-4175-002X | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
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