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Title: | Hydrostatic mass profiles in X-COP galaxy clusters | Authors: | ETTORI, STEFANO Ghirardini, V. Eckert, D. Pointecouteau, E. GASTALDELLO, FABIO Sereno, Mauro GASPARI, MASSIMO GHIZZARDI, SIMONA Roncarelli, M. ROSSETTI, MARIACHIARA |
Issue Date: | 2019 | Journal: | ASTRONOMY & ASTROPHYSICS | Number: | 621 | First Page: | A39 | 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. | URI: | http://hdl.handle.net/20.500.12386/28882 | URL: | https://www.aanda.org/articles/aa/abs/2019/01/aa33323-18/aa33323-18.html | ISSN: | 0004-6361 | DOI: | 10.1051/0004-6361/201833323 | Bibcode ADS: | 2019A&A...621A..39E | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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aa33323-18.pdf | Pdf editoriale | 1.05 MB | Adobe PDF | View/Open |
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