Volume 415, Number 2, February IV 2004
|Page(s)||451 - 469|
|Published online||11 February 2004|
The isolated interacting galaxy pair NGC 5426/27 (Arp 271)*
Instituto de Astronomí a, Universidad Nacional Autónoma de México (UNAM), Apdo. Postal 70-264, 04510, México, D.F., México
2 Laboratoire d'Astrophysique de Marseille, 2 place Le Verrier, Marseille Cedex 4, France
3 Department of Physical Sciences, Division of Astronomy, University of Oulu, 90570 Oulu, Finland
4 Observatoire de Grenoble, BP 53X, 38041 Grenoble Cedex 9, France
Corresponding author: I. Fuentes-Carrera, email@example.com
Accepted: 30 September 2003
We present Hα observations of the isolated interacting galaxy pair NGC 5426/27 using the scanning Fabry-Perot interferometer PUMA. The velocity field, various kinematical parameters and rotation curve for each galaxy were derived. The FWHM map and the residual velocities map were also computed to study the role of non-circular motions of the gas. Most of these motions can be associated with the presence of spiral arms and structure such as central bars. We found a small bar-like structure in NGC 5426, a distorted velocity field for NGC 5427 and a bridge-like feature between both galaxies which seems to be associated with NGC 5426. Using the observed rotation curves, a range of possible masses was computed for each galaxy. These were compared with the orbital mass of the pair derived from the relative motion of the participants. The rotation curve of each galaxy was also used to fit different mass distribution models considering the most common theoretical dark halo models. An analysis of the interaction process is presented and a possible 3D scenario for this encounter is also suggested.
Key words: galaxies: interactions / galaxies: kinematics and dynamics / galaxies: spiral / galaxies: individual: NGC 5426 / galaxies: individual: NGC 5427
© ESO, 2004
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