Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/28882
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | ETTORI, STEFANO | en_US |
dc.contributor.author | Ghirardini, V. | en_US |
dc.contributor.author | Eckert, D. | en_US |
dc.contributor.author | Pointecouteau, E. | en_US |
dc.contributor.author | GASTALDELLO, FABIO | en_US |
dc.contributor.author | Sereno, Mauro | en_US |
dc.contributor.author | GASPARI, MASSIMO | en_US |
dc.contributor.author | GHIZZARDI, SIMONA | en_US |
dc.contributor.author | Roncarelli, M. | en_US |
dc.contributor.author | ROSSETTI, MARIACHIARA | en_US |
dc.date.accessioned | 2020-12-16T11:15:20Z | - |
dc.date.available | 2020-12-16T11:15:20Z | - |
dc.date.issued | 2019 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/28882 | - |
dc.description.abstract | Aims: We present the reconstruction of hydrostatic mass profiles in 13 X-ray luminous galaxy clusters that have been mapped in their X-ray and Sunyaev-Zeldovich (SZ) signals out to R<SUB>200</SUB> for the XMM-Newton Cluster Outskirts Project (X-COP). <BR /> Methods: Using profiles of the gas temperature, density, and pressure that have been spatially resolved out to median values of 0.9R<SUB>500</SUB>, 1.8R<SUB>500</SUB>, and 2.3R<SUB>500</SUB>, respectively, we are able to recover the hydrostatic gravitating mass profile with several methods and using different mass models. <BR /> Results: The hydrostatic masses are recovered with a relative (statistical) median error of 3% at R<SUB>500</SUB> and 6% at R<SUB>200</SUB>. By using several different methods to solve the equation of the hydrostatic equilibrium, we evaluate some of the systematic uncertainties to be of the order of 5% at both R<SUB>500</SUB> and R<SUB>200</SUB>. A Navarro-Frenk-White profile provides the best-fit in 9 cases out of 13; the remaining 4 cases do not show a statistically significant tension with it. The distribution of the mass concentration follows the correlations with the total mass predicted from numerical simulations with a scatter of 0.18 dex, with an intrinsic scatter on the hydrostatic masses of 0.15 dex. We compare them with the estimates of the total gravitational mass obtained through X-ray scaling relations applied to Y<SUB>X</SUB>, gas fraction, and Y<SUB>SZ</SUB>, and from weak lensing and galaxy dynamics techniques, and measure a substantial agreement with the results from scaling laws, from WL at both R<SUB>500</SUB> and R<SUB>200</SUB> (with differences below 15%), from cluster velocity dispersions. Instead, we find a significant tension with the caustic masses that tend to underestimate the hydrostatic masses by 40% at R<SUB>200</SUB>. We also compare these measurements with predictions from alternative models to the cold dark matter, like the emergent gravity and MOND scenarios, confirming that the latter underestimates hydrostatic masses by 40% at R<SUB>1000</SUB>, with a decreasing tension as the radius increases, and reaches ∼15% at R<SUB>200</SUB>, whereas the former reproduces M<SUB>500</SUB> within 10%, but overestimates M<SUB>200</SUB> by about 20%. <BR /> Conclusions: The unprecedented accuracy of these hydrostatic mass profiles out to R<SUB>200</SUB> allows us to assess the level of systematic errors in the hydrostatic mass reconstruction method, to evaluate the intrinsic scatter in the NFW c - M relation, and to robustly quantify differences among different mass models, different mass proxies, and different gravity scenarios. | en_US |
dc.language.iso | eng | en_US |
dc.title | Hydrostatic mass profiles in X-COP galaxy clusters | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/201833323 | en_US |
dc.identifier.isi | 000454875500013 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/abs/2019/01/aa33323-18/aa33323-18.html | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 621 | en_US |
dc.relation.firstpage | A39 | 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 | ASTRONOMY & ASTROPHYSICS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2019A&A...621A..39E | 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 | no | 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.fulltext | With Fulltext | - |
item.grantfulltext | open | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
item.cerifentitytype | Publications | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.orcid | 0000-0003-4117-8617 | - |
crisitem.author.orcid | 0000-0002-9112-0184 | - |
crisitem.author.orcid | 0000-0003-0302-0325 | - |
crisitem.author.orcid | 0000-0003-2754-9258 | - |
crisitem.author.orcid | 0000-0003-0879-7328 | - |
crisitem.author.orcid | 0000-0002-9775-732X | - |
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