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Issue A&A
Volume 464, Number 1, March II 2007
Page(s) 187 - 191
Section Extragalactic astronomy
DOI http://dx.doi.org/10.1051/0004-6361:20065832



A&A 464, 187-191 (2007)
DOI: 10.1051/0004-6361:20065832

Barred CO emission in HE 1029-1831

M. Krips1, 2, A. Eckart1, R. Neri3, T. Bertram1, C. Straubmeier1, S. Fischer1, J. G. Staguhn4, and S. N. Vogel5

1  I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany
2  Harvard-Smithsonian Center for Astrophysics, SMA project, 645 North A`ohoku Place, Hilo, HI 96720, USA
    e-mail: mkrips@cfa.harvard.edu
3  Institut de Radio Astronomie Millimetrique (IRAM), 300 rue de la Piscine, 38406 Saint Martin d'Hères, France
4  NASA/Goddard Space Flight Center, Code 665, Building 21, Greenbelt, MD 20771, USA
5  University of Maryland, College Park, MD 20742, USA

(Received 14 June 2006 / Accepted 29 November 2006)

Abstract
We present CO(1-0) and CO(2-1) line emission maps of the barred spiral active galaxy HE 1029-1831 (z=0.0403) obtained with the IRAM Plateau de Bure Interferometer (PdBI) and in part by the Berkeley-Illinois-Maryland Association (BIMA) observatory. The CO emission is well associated with the optical bar and extended along it. The FWHM of the CO emission is estimated to be ~($6\pm2$) kpc. The CO emission shows a strong velocity gradient along the minor axis of the bar ( ${\rm PA}=90^\circ$). The molecular gas mass is estimated to be ~ $1.2\times10^{10}\mathcal{M}_{\odot}$, which indicates a very gas rich host galaxy. Most of the molecular gas appears to be subthermally excited and cold but we also find weak evidence for a warmer and/or denser gas component at the southern part of the bar emission, about ~4 kpc from the galactic nucleus.


Key words: galaxies: active -- galaxies: kinematics and dynamics -- galaxies: individual: HE 1029-1831 -- radio lines: galaxies -- galaxies: Seyfert



© ESO 2007


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