Multi-Component Models For Disc Galaxies |
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| Authors: | E Pignatelli |
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| Institution: | (1) Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, I 35122 Padova, Italy |
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| Abstract: | We present an application of a new set of detailed, self-consistent, dynamical models for disc galaxies. We start from the
hypothesis that each galaxy can be decomposed into a bulge, following the r
1/4law, and a disc with an exponential projected density profile; and that the isodensity surfaces of each component can be represented
by similar concentric spheroids. After taking into account both the asymmetric drift effects and the integration along the
line of sight, we produce the rotational velocity and velocity-dispersion profile, andthe approximate shape of the line-of-sight velocity distributions for the stars as parameterized by the h
3 and h
4 coefficients of theGauss–Hermite expansion of the line profile. Photometric and kinematical data have been taken from the
literature for the test case of the S0 galaxy NGC 5866, for which detailed stellar kinematical data are available at different
positions across the galaxy. Apart from the innermost, dust-obscured regions of the galaxy, where observational effects are
likely to be dominant, the model successfully reproduces the whole set of dynamical data available as well as giving a good
fit to the photometry. The galaxy is shown to have an isotropic velocity-dispersion tensor, thus hinting at a dissipational
formation process.
This revised version was published online in July 2006 with corrections to the Cover Date. |
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