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3D Studies of Galaxies in Compact Groups

Published online by Cambridge University Press:  09 February 2015

Claudia Mendes de Oliveira ,
Sergio Torres-Flores ,
Philippe Amram ,
Henri Plana  and
Benoit Epinat
Claudia Mendes de Oliveira
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosféricas da Universidade de São Paulo, Cidade Universitária, CEP:05508-900, São Paulo, SP, Brazil email: claudia.oliveira@iag.usp.br
Sergio Torres-Flores
Affiliation:
Departamento de Física, Universidad de La Serena, Av. Cisternas 1200 Norte, La Serena, Chile
Philippe Amram
Affiliation:
Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille), UMR 7326, 13388, Marseille, France
Henri Plana
Affiliation:
Laboratório de Astrofísica Teórica e Observacional, Universidade Estadual de Santa Cruz, Rodovia Ilhéus-Itabuna Km 16 45650-000 Ilhéus BA, Brazil
Benoit Epinat
Affiliation:
Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille), UMR 7326, 13388, Marseille, France
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Abstract

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Fabry-Perot data of compact group galaxies have been used to show that the Tully-Fisher relation in any photometric band, for galaxies with vmax > 100 km/s, is very similar to that for galaxies in other less dense environments. In the low-luminosity end, however, a few compact group galaxies fall above the relation apparently because they are too bright for their mass. Here we show that if the mass is properly computed from spectral energy distribution fitting or mass modelling, for the low-luminosity galaxies, their positions in the stellar-mass or baryonic Tully-Fisher relation are what is expected for a normal Tully-Fisher relation and the outlying positions observed in the B and K Tully-Fisher relation could be explained by brightening of the low-luminosity interacting galaxies due to strong star formation or AGN activity.

Keywords

galaxies: spiralelliptical and lenticular - galaxies: kinematics and dynamicsgalaxies: scaling relations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S309: Galaxies in 3D across the Universe , July 2014 , pp. 175 - 177
Copyright
Copyright © International Astronomical Union 2015 

References

Bell, E. F., McIntosh, D. H., Katz, N., & Weinberg, M. D. 2003 ApJS, 149, 289.CrossRefGoogle Scholar
Mendes de Oliveira, C., Amram, P., Plana, H., & Balkowski, C. 2003, AJ, 126, 2635.Google Scholar
McGaugh, S. 2012, AJ, 143, 40.CrossRefGoogle Scholar
Torres-Flores, S., Mendes de Oliveira, C., Amram, P., Plana, H., Epinat, B., Carignan, C., & Balkowski, C. 2010, A&A, 521A, 59.Google Scholar
Torres-Flores, S., Epinat, B., Amram, P., Plana, H., & Mendes de Oliveira, C. 2011, MNRAS, 416, 1936.CrossRefGoogle Scholar
Torres-Flores, S., Mendes de Oliveira, C., Plana, H., Amram, P., & Epinat, B. 2013, MNRAS, 432, 3085.Google Scholar