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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

The dynamical state of Abell 2399: a bullet-like cluster

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Lourenco, Ana C. C. [1, 2] ; Lopes, P. A. A. [1] ; Lagana, T. F. [3] ; Nascimento, R. S. [4] ; Machado, R. E. G. [5] ; Moura, M. T. [5] ; Jaffe, Y. L. [2] ; Ribeiro, A. L. [6] ; Vulcani, B. [7] ; Moretti, A. [7] ; Riguccini, L. A. [1]
Total Authors: 11
[1] Univ Fed Rio de Janeiro, Observ Valongo, Ladeira Pedro Antonio 43, BR-20080090 Rio De Janeiro, RJ - Brazil
[2] Univ Valparaiso, Inst Fis & Astron, Avda Gran Bretana 1111, Valparaiso - Chile
[3] Univ Cidade Sao Paulo, Univ Cruzeiro Sul, Nucleo Astrofis, Galvao Bueno 868, BR-01506000 Sao Paulo, SP - Brazil
[4] Lab Nacl Astrofis MCTI, BR-37504364 Itajuba, MG - Brazil
[5] Univ Tecnol Fed Parana, Dept Acad Fis, Sete Setembro 3165, BR-80230901 Curitiba, Parana - Brazil
[6] Univ Estadual Santa Cruz, Lab Astrofis Teor & Observac, BR-45650000 Ilheus, BA - Brazil
[7] Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua - Italy
Total Affiliations: 7
Document type: Journal article
Source: Monthly Notices of the Royal Astronomical Society; v. 498, n. 1, p. 835-849, OCT 2020.
Web of Science Citations: 0

While there are many ways to identify substructures in galaxy clusters using different wavelengths, each technique has its own caveat. In this paper, we conduct a detailed substructure search and dynamical state characterization of Abell 2399, a galaxy cluster in the local Universe (z similar to 0.0579), by performing a multiwavelength analysis and testing the results through hydrodynamical simulations. In particular, we apply a Gaussian mixture model to the spectroscopic data from SDSS, WINGS, and OmegaWINGS Surveys to identify substructures. We further use public XMM-Newton data to investigate the intracluster medium (ICM) thermal properties, creating temperature, metallicity, entropy, and pressure maps. Finally, we run hydrodynamical simulations to constrain the merger stage of this system. The ICM is very asymmetrical and has regions of temperature and pressure enhancement that evidence a recent merging process. The optical substructure analysis retrieves the two main X-ray concentrations. The temperature, entropy, and pressure are smaller in the secondary clump than in the main clump. On the other hand, its metallicity is considerably higher. This result can be explained by the scenario found by the hydrodynamical simulations where the secondary clump passed very near to the centre of the main cluster possibly causing the galaxies of that region to release more metals through the increase of ram-pressure stripping. (AU)

FAPESP's process: 18/02626-8 - X-ray astronomy: the history of chemical enrichment of groups and clusters of galaxies
Grantee:Tatiana Ferraz Laganá
Support type: Regular Research Grants
FAPESP's process: 09/54006-4 - A computer cluster for the Astronomy Department of the University of São Paulo Institute of Astronomy, Geophysics and Atmospheric Sciences and for the Cruzeiro do Sul University Astrophysics Center
Grantee:Elisabete Maria de Gouveia Dal Pino
Support type: Multi-user Equipment Program