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

Autor(es):Mostrar menos -

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]

Afiliação do(s) autor(es)

^[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

• Tipo de documento: Artigo Científico
• Fonte: Monthly Notices of the Royal Astronomical Society; v. 498, n. 1, p. 835-849, OCT 2020.
• Citações Web of Science: 0

Resumo

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)

• Processo FAPESP: 18/02626-8 - Astrofísica de Raios-X: o histórico de enriquecimento químico de grupos e aglomerados de galáxias
• Beneficiário: Tatiana Ferraz Laganá
• Modalidade de apoio: Auxílio à Pesquisa - Regular
• Processo FAPESP: 09/54006-4 - Um cluster de computadores para o Departamento de Astronomia do IAG-USP e para o Núcleo de Astrofísica da UNICSUL
• Beneficiário: Elisabete Maria de Gouveia Dal Pino
• Modalidade de apoio: Auxílio à Pesquisa - Programa Equipamentos Multiusuários