Issue |
A&A
Volume 490, Number 2, November I 2008
|
|
---|---|---|
Page(s) | 589 - 600 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361:200810410 | |
Published online | 17 September 2008 |
VIMOS-VLT integral field kinematics of the giant low surface brightness galaxy ESO 323-G064*
1
Max-Plank-Institut für Extraterrestrische Physik, Giessenbachstrae, 85741 Garching bei München, Germany e-mail: lcoccato@mpe.mpg.de
2
Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA
3
Carnegie Institution of Washington, 5241 Broad Branch Road NW, Washington, DC 20015, USA
4
European Southern Observatory, Karl-Schwarzschild-Strae 2, 85748 Garching bei München, Germany
Received:
17
June
2008
Accepted:
12
September
2008
Aims. We have studied the bulge and the disk kinematics of the giant low surface brightness galaxy ESO 323-G064 in order to investigate its dynamical properties and the radial mass profile of the dark matter (DM) halo.
Methods. We observed the galaxy with integral field spectroscopy (VLT/VIMOS,
in IFU configuration), measured the positions of the ionized gas by
fitting Gaussian functions to the [O III]4959,5007 and Hβ emission lines,
and fit stellar templates to the galaxy spectra to determine velocity
and velocity dispersions. We modeled the stellar kinematics in the
bulge with spherical isotropic Jeans models and explored the
implications of self consistent and dark matter scenarios for NFW and
pseudo isothermal halos.
Results. In the bulge-dominated region, , the emission lines show
multi-peaked profiles. The disk dominated region of the galaxy,
, exhibits regular rotation, with a flat rotation curve
that reaches 248 ± 6 km s-1. From this we estimate the total
barionic mass to be Mbar ~ 1.9
1011
and the
total DM halo mass to be MDM ~ 4.8
1012
. The stellar
velocity and velocity dispersion have been measured only in the
innermost ≈ 5” of the bulge, and reveal a regular rotation
with an observed amplitude of 140 km s-1 and a central dispersion of
σ = 180 km s-1. Our simple Jeans modeling shows that dark matter is
needed in the central 5” to explain the kinematics of the bulge,
for which we estimate a mass of ≈(7 ± 3)
1010
. However, we are not able to disentangle different DM
scenarios.
The computed central mass density of the bulge of ESO
323-G064 resembles the central mass density of some high
surface brightness galaxies, rather than that of low surface brightness
galaxies.
Key words: galaxies: kinematics and dynamics / galaxies: spirals / galaxies: individual: ESO 323-G064
© ESO, 2008
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