Volume 442, Number 2, November I 2005
|Page(s)||479 - 493|
|Published online||07 October 2005|
Molecular gas in NUclei of GAlaxies (NUGA)
III. The warped LINER NGC 3718
Universität zu Köln, I.Physikalisches Institut, Zülpicher Str. 77, 50937 Köln, Germany e-mail: [krips;eckart]@ph1.uni-koeln.de
2 Institut de Radio-Astronomie Millimétrique (IRAM), 300 rue de la Piscine, 38406 St. Martin-d'Hères, France e-mail: email@example.com
3 ESO, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany; e-mail: firstname.lastname@example.org
4 Instituto de Astrofísica de Andalucía (CSIC), C/ Camino Bajo de Huétor 24, Apartado 3004, 18080 Granada, Spain e-mail: email@example.com
5 Observatoire de Paris, LERMA, 61 Av. de l'Observatoire, 75014 Paris, France; e-mail: firstname.lastname@example.org
6 Observatorio Astronómico Nacional (OAN)-Observatorio de Madrid, Alfonso XII 3, 28014 Madrid, Spain e-mail: email@example.com
7 Istituto di Radioastronomia/CNR, Sez. Firenze, Largo Enrico Fermi 5, 50125 Firenze, Italy e-mail: firstname.lastname@example.org
8 Jansky Fellow, National Radio Astronomy Observatory Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA; e-mail: email@example.com
9 Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, 85741 Garching, Germany; e-mail: firstname.lastname@example.org
10 Astronomisches Institut, Universität Basel, Venusstr. 7, 4102 Binningen, Switzerland; e-mail: email@example.com
11 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany; e-mail: firstname.lastname@example.org
12 Max Planck Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany e-mail: email@example.com
We present the first interferometric observations of CO(1–0) and CO(2–1) line emission from the warped LINER NGC 3718, obtained with the IRAM Plateau de Bure Interferometer (PdBI). This L1.9 galaxy has a prominent dust lane and on kiloparsec scales, a strongly warped atomic and molecular gas disk. The molecular gas is closely associated with the dust lane across the nucleus and its kinematic center is consistent with the millimeter continuum AGN. A comparison of our interferometric mosaic data, which fully cover the ~ warped disk, with a previously obtained IRAM 30 m single dish CO(1–0) map shows that the molecular gas distribution in the disk is heavily resolved by the PdBI map. On the nucleus the interferometric maps alone contain less than one half of the single dish line flux, and the overall mosaic accounts for about a tenth of the total molecular gas mass of ~ . After applying a short-spacing correction with the IRAM 30 m data to recover the missing extended flux, we find in total six main source components within the dust lane: one associated with the nucleus, four symmetrically positioned on either side at galactocentric distances of about 1.3 kpc and 4.0 kpc from the center, and a sixth on the western side at ~ with only a very weak eastern counterpart. In the framework of a kinematic model using tilted rings, we interpret the five symmetric source components as locations of strong orbital crowding. We further find indications that the warp appears not only on kpc scales, but continues down to ~ . Besides the sixth feature on the western side, the lower flux (a factor of ~2) of the eastern components compared to the western ones indicates an intrinsic large scale asymmetry in NGC 3718 that cannot be explained by the warp. Indications for a small scale asymmetry are also seen in the central 600 pc. These asymmetries might be evidence for a tidal interaction with a companion galaxy (large scales) and gas accretion onto the nucleus (small scales). Our study of NGC 3718 is part of the NUclei of GAlaxies (NUGA) project that aims at investigating the different processes of gas accretion onto Active Galactic Nuclei (AGN).
Key words: galaxies: individual: NGC 3718 / galaxies: active / Galaxy: kinematics and dynamics
© ESO, 2005
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