Volume 393, Number 2, October II 2002
|Page(s)||389 - 407|
|Section||Cosmology (including clusters of galaxies)|
|Published online||23 September 2002|
Instituto de Astrofísica de Andalucía (CSIC), Apartado 3004, 18080 Granada, Spain
2 Instituto de Matemáticas y Física Fundamental (CSIC), C) Serrano 113B, 28006 Madrid, Spain
3 Osservatorio Astronomico di Padova, Vicolo Osservatorio 5, 35122 Padova, Italy
4 Dipartimento di Astronomia, Università di Padova, Vicolo Osservatorio 2, 35122 Padova, Italy
Corresponding author: I. Márquez, firstname.lastname@example.org
Accepted: 25 June 2002
In this paper we study long slit spectra in the region of Hα emission line of a sample of 111 spiral galaxies with recognizable and well defined spiral morphology and with a well determined environmental status, ranging from isolation to non-disruptive interaction with satellites or companions. The form and properties of the rotation curves are considered as a function of the isolation degree, morphological type and luminosity. The line ratios are used to estimate the metallicity of all the detected HII regions, thus producing a composite metallicity profile for different types of spirals. We have found that isolated galaxies tend to be of later types and lower luminosity than the interacting galaxies. The outer parts of the rotation curves of isolated galaxies tend to be flatter than in interacting galaxies, but they show similar relations between global parameters. The scatter of the Tully-Fisher relation defined by isolated galaxies is significantly lower than that of interacting galaxies. The [NII]/Hα ratios, used as a metallicity indicator, show a clear trend between Z and morphological type, t, with earlier spirals showing higher ratios; this trend is tighter when instead of t the gradient of the inner rotation curve, G, is used; no trend is found with the change in interaction status. The Z-gradient of the disks depends on the type, being almost flat for early spirals, and increasing for later types. The [NII]/Hα ratios measured for disk HII regions of interacting galaxies are higher than for normal/isolated objects, even if all the galaxy families present similar distributions of Hα Equivalent Width.
Key words: galaxies: spiral / galaxies: kinematics and dynamics / galaxies: structure / galaxies: interactions
Tables 3 and 4 and Figs. 6, 7 and 21 are only available in electronic form at http://www.edpsciences.org. Table 5 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/393/389
© ESO, 2002
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