| Texto completo | |
| Autor(es): |
Monteiro-Oliveira, R.
[1, 2, 3]
;
Morell, D. F.
[4]
;
Sampaio, V. M.
[5]
;
Ribeiro, A. L. B.
[1]
;
de Carvalho, R. R.
[5]
Número total de Autores: 5
|
| Afiliação do(s) autor(es): | [1] Univ Estadual Santa Cruz, Lab Astrofis Teor & Observac, BR-45650000 Ilheus, BA - Brazil
[2] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Dept Astron, R Matao 1226, BR-05508090 Sao Paulo - Brazil
[3] Acad Sinica, Inst Astron & Astrophys, 11F AS NTU Astron, Math Bldg 1, Sect 4, Roosevelt Rd, Taipei 10617 - Taiwan
[4] UNC, CCT Cordoba, CONICET, Inst Astron Teor & Expt, Laprida 854, X5000BGR, Cordoba - Argentina
[5] NAT Univ Cruzeiro do Sul, BR-01506000 Sao Paulo - Brazil
Número total de Afiliações: 5
|
| Tipo de documento: | Artigo Científico |
| Fonte: | Monthly Notices of the Royal Astronomical Society; v. 509, n. 3, p. 3470-3487, NOV 27 2021. |
| Citações Web of Science: | 0 |
| Resumo | |
We have investigated the structure of the Hercules supercluster (SCL160) based on data originally extracted from the Sloan Digital Sky Survey (SDSS-DR7). We have traced the mass distribution in the field through the numerical density, weighted by the r ` luminosity of the galaxies, and classified objects based on their spatial position and redshift. This has allowed us to address not only the kinematics of the supercluster as a whole, but also the internal kinematics of each cluster, which had not been explored further before. We have confirmed that the Hercules supercluster is composed of the galaxy clusters A2147, A2151, and A2152. A2151 consists of five subclusters, A2147 two, and A2152 at least two. They form the heart of the Hercules supercluster. We also have found two other gravitationally bound clusters, therefore increasing the known members of the supercluster. We have estimated a total mass of 2.1 +/- 0.2 x 10(15) M-circle dot for the Hercules supercluster. To determine the dynamical masses in this work, we have resorted to the M-200-sigma scaling relation and the caustic technique. Comparing both methods with simulated data of bimodal merging clusters, we found that the caustic, as well as the sigma-based masses, is biased through the merger age, showing a boost just after pericentric passage. This is not in line with the principle of the caustic method, which affirms it does not depend on the cluster dynamical state. (AU) | |
| Processo FAPESP: | 14/11156-4 - O que determina o crescimento da massa estelar de galáxias elípticas? Intrínseco ou ambiente: a saga contínua |
| Beneficiário: | Reinaldo Ramos de Carvalho |
| Modalidade de apoio: | Auxílio à Pesquisa - Temático |