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A&A 407, 485-502 (2003)
DOI: 10.1051/0004-6361:20030866
Molecular Gas in NUclei of GAlaxies (NUGA)
I. The counter-rotating LINER NGC 4826
S. García-Burillo1, F. Combes2, L. K. Hunt3, F. Boone4, A. J. Baker5, L. J. Tacconi5, A. Eckart6, R. Neri7, S. Leon8, E. Schinnerer9 and P. Englmaier101 Observatorio Astronómico Nacional (OAN)-Observatorio de Madrid, Alfonso XII, 3, 28014 Madrid, Spain
e-mail: burillo@oan.es
2 Observatoire de Paris, LERMA, 61 Av. de l'Observatoire, 75014 Paris, France
e-mail: francoise.combes@obspm.fr
3 Istituto di Radioastronomia/CNR, Sez. Firenze, Largo Enrico Fermi, 5, 50125 Firenze, Italy
e-mail: hunt@arcetri.astro.it
4 Astronomisches Institut der Ruhr-Universität Bochum, Universitätstrasse 150, 44780, Germany
e-mail: fboone@astro.ruhr-uni-bochum.de
5 Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, 85741 Garching, Germany
e-mail: ajb@mpe.mpg.de, linda@mpe.mpg.de
6 Universität zu Köln, I. Physikalisches Institut, Zülpicherstrasse 77, 50937 Köln, Germany
e-mail: eckart@ph1.uni-koeln.de
7 Institut de Radio-Astronomie Millimétrique (IRAM), 300 Rue de la Piscine, 38406 St. Mt. D'Hères, France
e-mail: neri@iram.fr
8 Instituto de Astrofísica de Andalucía (CSIC), C/ Bajo de Huétor, 24, Apartado 3004, 18080 Granada, Spain
e-mail: stephane@iaa.es
9 National Radio Astronomy Observatory, PO Box 0, Socorro, NM87801, USA
e-mail: eschinne@nrao.edu
10 Astronomisches Institut, Universität Basel, Venusstrasse 7, 4102 Binningen, Siwtzerland
e-mail: ppe@astro.unibas.ch
(Received 10 February 2003 / Accepted 3 June 2003 )
Abstract
We present new high-resolution observations of the nucleus of the counter-rotating
LINER NGC 4826, made in the
J=1-0 and
J=2-1 lines of
12CO with the IRAM Plateau de
Bure mm-interferometer(PdBI).The CO maps, which achieve 0.8
(16 pc) resolution in the 2-1
line, fully resolve an inner molecular gas disk which is truncated at an outer radius of 700 pc.
The total molecular gas mass (
) is distributed in a lopsided nuclear
disk of 40 pc radius, containing 15% of the total gas mass, and two one-arm spirals, which
develop at different radii in the disk. The distribution and kinematics of molecular gas in the
inner 1 kpc of NGC 4826 show the prevalence of different types of
m=1 perturbations in the
gas. Although dominated by rotation, the gas kinematics are perturbed by streaming motions related
to the
m=1 instabilities. The non-circular motions associated with the inner
m=1
perturbations (lopsided instability and inner one-arm spiral) agree qualitatively with the pattern
expected for a trailing wave developed outside corotation ("fast" wave). In contrast, the streaming
motions in the outer
m=1 spiral are better explained by a "slow" wave. A paradoxical
consequence is that the inner
m=1 perturbations would not favour AGN feeding. An independent
confirmation that the AGN is not being generously fueled at present is found in the low values of
the gravitational torques exerted by the stellar potential for
R<530 pc. The distribution of star
formation in the disk of NGC 4826 is also strongly asymmetrical. The observed asymmetries,
revealed by HST images of the inner disk, follow the scales of the various
m=1 perturbations
identified in the molecular gas disk. Massive star formation is still vigorous, fed by the
significant molecular gas reservoir at
R<700 pc. There is supporting evidence for a recent large mass inflow episode in NGC 4826. The
onset of
m=1 instabilities of the type observed in NGC 4826 may be a consequence of secular
evolution of disks with high gas mass contents.
Key words: galaxies: individual: NGC 4826 -- galaxies: ISM -- galaxies: kinematics and dynamics -- galaxies: nuclei -- radio lines: galaxies
Offprint request: S. García-Burillo, burillo@oan.es
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