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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

Kinematics of galaxies in compact groups Studying the B-band Tully-Fischer relation

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Author(s):
Torres-Flores, S. [1, 2, 3] ; Mendes de Oliveira, C. [1] ; Amram, P. [2, 3] ; Plana, H. [4, 2, 3] ; Epinat, B. [5, 6] ; Carignan, C. [7, 8, 9] ; Balkowski, C. [10, 11]
Total Authors: 7
Affiliation:
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[1] Univ Sao Paulo, Dept Astron, Inst Astron Geofis & Ciencias Atmosfer, BR-05508090 Sao Paulo - Brazil
[2] CNRS, F-13388 Marseille 13 - France
[3] Univ Aix Marseille 1, Lab Astrophys Marseille, OAMP, F-13388 Marseille 13 - France
[4] Univ Estadual Santa Cruz, Lab Astrofis Teor & Observac, Ilheus - Brazil
[5] CNRS, F-31400 Toulouse - France
[6] Univ Toulouse, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse - France
[7] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7 - Canada
[8] Univ Montreal, LAE, Observ Mt Megant, Montreal, PQ H3C 3J7 - Canada
[9] Univ Ouagadougou UFR SEA, Observ Astrophys, Ouagadougou 03 - Burkina Faso
[10] Univ Paris, Observ Paris, GEPI, Meudon - France
[11] CNRS, Meudon - France
Total Affiliations: 11
Document type: Journal article
Source: Astronomy & Astrophysics; v. 521, OCT 2010.
Web of Science Citations: 9
Abstract

We obtained new Fabry-Perot data cubes and derived velocity fields, monochromatic, and velocity dispersion maps for 28 galaxies in the Hickson compact groups 37, 40, 47, 49, 54, 56, 68, 79, and 93. We also derived rotation curves for 9 of the studied galaxies, 6 of which are strongly asymmetric. Combining these new data with previously published 2D kinematic maps of compact group galaxies, we investigated the differences between the kinematic and morphological position angles for a sample of 46 galaxies. We find that one third of the unbarred compact group galaxies have position angle misalignments between the stellar and gaseous components. This and the asymmetric rotation curves are clear signatures of kinematic perturbations, probably because of interactions among compact group galaxies. A comparison between the B-band Tully-Fisher relation for compact group galaxies and for the GHASP field-galaxy sample shows that, despite the high fraction of compact group galaxies with asymmetric rotation curves, these lay on the TF relation defined by galaxies in less dense environments, although with more scatter. This agrees with previous results, but now confirmed for a larger sample of 41 galaxies. We confirm the tendency for compact group galaxies at the low-mass end of the Tully-Fisher relation (HCG 49b, 89d, 96c, 96d, and 100c) to have either a magnitude that is too bright for its mass (suggesting brightening by star formation) and/or a low maximum rotational velocity for its luminosity (suggesting tidal stripping). These galaxies are outside the Tully Fisher relation at the 1 sigma level, even when the minimum acceptable values of inclinations are used to compute their maximum velocities. Including such galaxies with nu < 100 km s(-1) in the determination of the zero point and slope of the compact group B-band Tully-Fisher relation would strongly change the fit, making it different from the relation for field galaxies, which has to be kept in mind when studying scaling relations of interacting galaxies, especially at high redshifts. (AU)

FAPESP's process: 07/07973-3 - The internal kinematics of galaxies in Hickson compact groups
Grantee:Sergio Patricio Torres Flores
Support type: Scholarships in Brazil - Doctorate (Direct)
FAPESP's process: 06/56213-9 - New physics from space: formation and evolution of structures in the universe
Grantee:Claudia Lucia Mendes de Oliveira
Support type: Research Projects - Thematic Grants