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(Referência obtida automaticamente do Web of Science, por meio da informação sobre o financiamento pela FAPESP e o número do processo correspondente, incluída na publicação pelos autores.)

The H alpha kinematics of interacting galaxies in 12 compact groups

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Autor(es):
Torres-Flores, S. [1] ; Amram, P. [2] ; Mendes de Oliveira, C. [3] ; Plana, H. [4] ; Balkowski, C. [5, 6] ; Marcelin, M. [2] ; Olave-Rojas, D. [1]
Número total de Autores: 7
Afiliação do(s) autor(es):
[1] Univ La Serena, Dept Fis, La Serena - Chile
[2] Aix Marseille Univ, Lab Astrophys Marseille, CNRS, F-13388 Marseille - France
[3] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Dept Astron, BR-05508900 Sao Paulo - Brazil
[4] Univ Estadual Santa Cruz, Lab Astrofis Teor & Observac, BR-45650000 Ilheus, BA - Brazil
[5] Paris Univ Denis Diderot, Observ Paris, GEPI, F-92195 Meudon - France
[6] CNRS, F-92195 Meudon - France
Número total de Afiliações: 6
Tipo de documento: Artigo Científico
Fonte: Monthly Notices of the Royal Astronomical Society; v. 442, n. 3, p. 2188-2201, AUG 11 2014.
Citações Web of Science: 9
Resumo

We present new Fabry-Perot observations for a sample of 42 galaxies located in 12 compact groups of galaxies: HCG 1, HCG 14, HCG 25, HCG 44, HCG 53, HCG 57, HCG 61, HCG 69, HCG 93, VV 304, LGG 455 and Arp 314. From the 42 observed galaxies, a total of 26 objects are spiral galaxies, which range from Sa to Im morphological types. The remaining 16 objects are E, S0 and S0a galaxies. Using these observations, we have derived velocity maps, monochromatic and velocity dispersion maps for 24 galaxies, where 18 are spiral, three are S0a, two are S0 and one is an Im galaxy. From the 24 velocity fields obtained, we could derive rotation curves for 15 galaxies; only two of them exhibit rotation curves without any clear signature of interactions. Based on kinematic information, we have evaluated the evolutionary stage of the different groups of the current sample. We identify groups that range from having no H alpha emission to displaying an extremely complex kinematics, where their members display strongly perturbed velocity fields and rotation curves. In the case of galaxies with no H alpha emission, we suggest that past galaxy interactions removed their gaseous components, thereby quenching their star formation. However, we cannot discard that the lack of H alpha emission is linked with the detection limit for some of our observations. (AU)

Processo FAPESP: 06/56213-9 - Nova física no espaço: formação e evolução de estruturas no universo
Beneficiário:Claudia Lucia Mendes de Oliveira
Linha de fomento: Auxílio à Pesquisa - Temático