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Issue A&A
Volume 468, Number 3, June IV 2007
Extended baselines for the IRAM Plateau de Bure interferometer: First results
Page(s) L71 - L75
DOI http://dx.doi.org/10.1051/0004-6361:20077599



A&A 468, L71-L75 (2007)
DOI: 10.1051/0004-6361:20077599

Letter

Fueling the central engine of radio galaxies

I. The molecular/dusty disk of 4C 31.04
S. García-Burillo1, F. Combes2, R. Neri3, A. Fuente1, A. Usero1, 4, S. Leon5, and J. Lim6

1  Observatorio Astronómico Nacional, Alfonso XII, 3, 28014 Madrid, Spain
    e-mail: s.gburillo@oan.es, a.fuente@oan.es
2  Observatoire de Paris, LERMA, 61 Av. de l'Observatoire, 75014 Paris, France
    e-mail: francoise.combes@obspm.fr
3  Institut de Radioastronomie Millimétrique, 300 rue de la Piscine, 38406 St. Martin d'Hères, France
    e-mail: neri@iram.fr
4  Centre for Astrophysics Research, University of Hertfordshire, College Lane, AL10 9AB, UK
    e-mail: a.usero@herts.ac.uk
5  Instituto de Astrofísica de Andalucía, C Bajo de Huétor, 50, 18008 Granada, Spain
    e-mail: stephane@iaa.es
6  Inst. of Astron. and Astrophysics, Academia Sinica, PO Box 23-141, Taipei 106, Taiwan
    e-mail: jlim@asiaa.sinica.edu.tw

(Received 3 April 2007 / Accepted 25 April 2007)

Abstract
We report the detection of a massive ( $M_{\rm gas}>5\times10^{9}~M_{\odot}$) molecular/dusty disk of 1.4 kpc-size fueling the central engine of the compact symmetric object (CSO) 4C 31.04, based on high-resolution (0.5$\arcsec$-1.2$\arcsec$) observations done with the IRAM Plateau de Bure interferometer (PdBI). These observations allow us for the first time to detect and map the continuum emission from dust at 218 GHz in the disk of a CSO. The case for a massive disk is confirmed by detection of strong HCO+(1-0) line emission and absorption. The molecular gas mass of 4C 31.04 is in the range $0.5\times10^{10}{-}5\times10^{10}~M_{\odot}$. While the distribution and kinematics of the gas roughly correspond to those of a rotating disk, we find evidence of distortions and non-circular motions that suggest the disk is not in a dynamically relaxed state. We discuss the implications of these results for the understanding of the evolution of radio galaxies.


Key words: galaxies: individual: 4C 31.04 -- galaxies: ISM -- galaxies: kinematics and dynamics -- galaxies: active -- galaxies: nuclei



© ESO 2007

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