Issue |
A&A
Volume 443, Number 1, November III 2005
|
|
---|---|---|
Page(s) | 133 - 141 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361:20053587 | |
Published online | 21 October 2005 |
The contribution of rotational velocity to the FP of elliptical galaxies
1
Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, 40127 Bologna, Italy e-mail: andrea.riciputi@bo.astro.it
2
INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
3
Department of Astronomy & Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON, M5S 3H8, Canada
Received:
7
June
2005
Accepted:
28
July
2005
The contribution of ordered rotation to the observed tilt
and thickness of the Fundamental Plane of elliptical galaxies is
studied by means of oblate, two-integrals cuspy galaxy models with
adjustable flattening, variable amount of ordered rotational
support, and possible presence of a dark matter halo and of a
central super-massive black hole. We find that, when restricting
the measure of the velocity dispersion to the central galactic
regions, rotation has a negligible effect, and so cannot be
responsible of the observed tilt. However, streaming velocity
effect can be significant when observing small and rotationally
supported galaxies through large (relative) aperture (as for
example in Fundamental Plane studies at high redshift), and can
lead to unrealistically low mass-to-light ratios. The effect of a
central supermassive black hole on the kinematical fields, and the
models position in the -ellipticity plane are also
discussed.
Key words: galaxies: elliptical and lenticular, cD / galaxies: fundamental parameters / galaxies: photometry / galaxies: kinematics and dynamics
© ESO, 2005
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