Mon. Not. R. Astron. Soc., 362, 127-166 (2005/September-1)
GHASP: an Hα kinematic survey of spiral and irregular galaxies - IV. 44 new velocity fields. Extension, shape and asymmetry of Hα rotation curves.
GARRIDO O., MARCELIN M., AMRAM P., BALKOWSKI C., GACH J.L. and BOULESTEIX J.
Abstract (from CDS):
We present Fabry-Perot observations obtained in the frame of the GHASP survey (Gassendi HAlpha survey of SPirals). We have derived the Hα map, the velocity field and the rotation curve for a new set of 44 galaxies. The data presented in this paper are combined with the data published in the three previous papers providing a total number of 85 of the 96 galaxies observed up to now. This sample of kinematical data has been divided into two groups: isolated (ISO) and softly interacting (SOFT) galaxies. In this paper, the extension of the Hα discs, the shape of the rotation curves, the kinematical asymmetry and the Tully-Fisher relation have been investigated for both ISO and SOFT galaxies. The Hα extension is roughly proportional to R25for ISO as well as for SOFT galaxies. The smallest extensions of the ionized disc are found for ISO galaxies. The inner slope of the rotation curves is found to be correlated with the central concentration of light more clearly than with the type or the kinematical asymmetry, for ISO as well as for SOFT galaxies. The outer slope of the rotation curves increases with the type and with the kinematical asymmetry for ISO galaxies but shows no special trend for SOFT galaxies. No decreasing rotation curve is found for SOFT galaxies. The asymmetry of the rotation curves is correlated with the morphological type, the luminosity, the (B-V) colour and the maximal rotational velocity of galaxies. Our results show that the brightest, the most massive and the reddest galaxies, which are fast rotators, are the least asymmetric, meaning that they are the most efficient with which to average the mass distribution on the whole disc. Asymmetry in the rotation curves seems to be linked with local star formation, betraying disturbances of the gravitational potential. The Tully-Fisher relation has a smaller slope for ISO than for SOFT galaxies.
catalogues - galaxies: dwarf - galaxies: interactions - galaxies: irregular - galaxies: kinematics and dynamics - galaxies: spiral
In Table 3 : For UGC 1886 : coordinates are 02 26 00.5 +39 28 14.4 instead of 02 26 00.5 +06 00 08.2, For UGC 3384 : coordinates are 06 01 37.35 +73 07 00.0 instead of 05 59 47.7 +62 09 29
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