| Texto completo | |
| Autor(es): |
Torres-Flores, S.
[1]
;
Scarano, Jr., S.
[2, 3, 4]
;
Mendes de Oliveira, C.
[4]
;
de Mello, D. F.
[5]
;
Amram, P.
[6]
;
Plana, H.
[7]
Número total de Autores: 6
|
| Afiliação do(s) autor(es): | [1] Univ La Serena, Dept Fis, La Serena - Chile
[2] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508900 Sao Paulo - Brazil
[3] Univ Fed Sergipe, Dept Fis CCET, BR-49100000 Sao Cristovao, SE - Brazil
[4] Southern Astrophys Res Telescope SOAR, La Serena - Chile
[5] Catholic Univ Amer, Washington, DC 20064 - USA
[6] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, F-13388 Marseille - France
[7] Univ Estadual Santa Cruz, Lab Astrofis Teor & Observac, Ilheus - Brazil
Número total de Afiliações: 7
|
| Tipo de documento: | Artigo Científico |
| Fonte: | Monthly Notices of the Royal Astronomical Society; v. 438, n. 2, p. 1894-1908, FEB 2014. |
| Citações Web of Science: | 13 |
| Resumo | |
We present new Gemini/GMOS spectroscopic and archival imaging data of the interacting galaxy NGC 92, which is part of a compact group and displays an extended tidal tail. We have studied the physical properties of 20 star-forming complexes in this system. We found that the star-forming regions located in the tidal tail of NGC 92 have ages younger than similar to 8 Myr, which suggests that these objects were formed in situ. The spectroscopic data reveal that these regions have slightly sub-solar metallicities, suggesting that they were formed from pre-enriched material. Using the oxygen abundances derived for each system, we found that the extended tidal tail of NGC 92 has a flat metallicity distribution. Although this scenario is consistent with N-body simulations of interacting systems, where there is gas mixing triggered by the interaction, archival H alpha Fabry-Perot data cubes of NGC 92 have not shown a velocity gradient along the tail of this galaxy, which under certain assumptions could be interpreted as a lack of gas flow in the tail. Our results suggest that a fraction of the enriched gas that was originally located in the centre of the galaxy was expelled into the tidal tail when the interacting process that formed the tail happened. However, we cannot exclude the scenario in which the star formation in the tail has increased its original oxygen abundance. (AU) | |
| Processo FAPESP: | 09/05181-8 - Determinação da Orientação Espacial de Galáxias Utilizando Braços Espirais e Campos de Velocidade |
| Beneficiário: | Sergio Scarano Junior |
| Modalidade de apoio: | Bolsas no Brasil - Pós-Doutorado |