New insights on the dissociative merging galaxy cluster Abell 2034

Autor(es)

Monteiro-Oliveira, R. ^{[1, 2]} ; Cypriano, E. S. ^[1] ; Vitorelli, A. Z. ^[1] ; Ribeiro, A. L. B. ^[3] ; Sodre, Jr., L. ^[1] ; Dupke, R. ^{[4, 5, 6, 7]} ; Mendes de Oliveira, C. ^[1]

Afiliação do(s) autor(es)

^[1] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Dept Astron, R Matao 1226, BR-05508090 Sao Paulo - Brazil

^[2] Univ Fed Rio Grande do Sul, Inst Fis, Dept Astron, Campus Vale, BR-91501970 Porto Alegre, RS - Brazil

^[3] Univ Estadual Santa Cruz, Lab Astrofis Teor & Observac, BR-45650000 Ilheus, BA - Brazil

^[4] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ - Brazil

^[5] Eureka Sci Inc, 2452 Delmer St, Suite 100, Oakland, CA 94602 - USA

^[6] Univ Alabama, Dept Phys & Astron, Box 870324, Tuscaloosa, AL 35487 - USA

^[7] Univ Michigan, Dept Astron, 311 West Hall, 1085 South Univ Ave, Ann Arbor, MI 48109 - USA

• Tipo de documento: Artigo Científico
• Fonte: Monthly Notices of the Royal Astronomical Society; v. 481, n. 1, p. 1097-1114, NOV 2018.
• Citações Web of Science: 1

Resumo

We present here new insights about the merging galaxy cluster Abell 2034 ((z) over bar = 0.114) based on a combined weak lensing and dynamical analysis. From our deep Subaru BR(C)z' images plus Gemini-GMOS/N low-resolution spectra accompanied by available redshift data, we have obtained the individual masses of the colliding subclusters as well as estimated a timeline of the process. The collision event happened 0.56(-0.22)(+0.15) Gyr ago between the subclusters A2034S (M-200(S) = 2.35(-0.99)(+0.84) x 10(14) M-circle dot) and A2034N (M-200(N) = 1.08(-0.71)(+0.51) x 10(14) M-circle dot) with the gas content of both subclusters displaced in relation to their galaxy and dark matter distributions, in a scenario similar to that found in the Bullet Cluster. Following our data and modelling the collision event is, most likely, taking place not so far from the plane of the sky, with an angle of 27 degrees +/- 14 degrees in relation to that. In spite of the intrinsic degeneracy inherent to the system (whether it has been observed incoming or outgoing), the comparison of our calculated time since the closest approximation with the estimated age of the observed X-ray shock front and the increment experienced by the velocity dispersion of the galaxy cluster members point towards an outgoing movement. Besides, we found a strong evidence for the presence of a third structure that we called A2034W. (AU)

• Processo FAPESP: 14/13723-3 - Aglomerados de galáxias como portais para o universo escuro
• Beneficiário: Eduardo Serra Cypriano
• Linha de fomento: 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
• Linha de fomento: Auxílio à Pesquisa - Programa Equipamentos Multiusuários
• Processo FAPESP: 12/00800-4 - O universo em 3-D: astrofísica com grandes levantamentos de galáxias
• Beneficiário: Laerte Sodré Junior
• Linha de fomento: Auxílio à Pesquisa - Temático