Volume 505, Number 2, October II 2009
|Page(s)||559 - 567|
|Published online||03 August 2009|
Is cold gas fuelling the radio galaxy NGC 315?*
Netherlands Foundation for Research in Astronomy, Postbus 2, 7990 AA, Dwingeloo, The Netherlands e-mail: email@example.com
2 Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, The Netherlands
3 Joint ALMA Office, Av El Golf 40, piso 18, Santiago 7550108, Chile
4 National Radio Astronomy Observatory, Socorro, NM 87801, USA
5 Osservatorio Astronomico di Torino, Strada Osservatorio 25, 10025 Pino Torinese, Italy
6 INAF, Istituto di Radioastronomia, Via Gobetti 101, 40129 Bologna, Italy
7 Dipartimento di Fisica dell'Università di Bologna, Via Irnerio 46, 40126 Bologna, Italy
8 Osservatorio Astronomico di Bologna, Via Ranzani, 1, 40127 Bologna, Italy
Accepted: 24 July 2009
We present WSRT, VLA and VLBI observations of the H i absorption in the radio galaxy NGC 315. The main result is that two H i absorbing systems are detected against the central region. In addition to the known highly redshifted, very narrow component, we detect relatively broad (FWZI ~ 150 km s-1) absorption. This broad component is redshifted by ~80 km s-1 compared to the systemic velocity, while the narrow absorption is redshifted ~490 km s-1. Both H i absorption components are spatially resolved at the pc-scale of the VLBI observations. The broad component shows strong gradients in density (or excitation) and velocity along the jet. We conclude that this gas is physically close to the AGN, although the nature of the gas resulting in the broad absorption is not completely clear. The possibility that it is entrained by the radio jet (and partly responsible of the deceleration of the jet) appears unlikely. Gas located in a thick circumnuclear toroidal structure, with orientation similar to the dusty, circumnuclear disk observed with HST, cannot be completely ruled out although it appears difficult to reconcile with the observed morphology and kinematics of the H i. A perhaps more likely scenario is that the gas producing the broad absorption could be (directly or indirectly) connected with the fueling of the AGN, i.e. gas that is falling into the nucleus. If this is the case, the accretion rate derived is similar (considering all uncertainties) to that found for other X-ray luminous elliptical galaxies, although lower than that derived from the radio core luminosity for NGC 315. The data also show that, in contrast to the broad component, the density distribution of the narrow component is featureless. Moreover, in the WSRT observations we do detect a small amount of H i in emission a few kpc SW of the AGN, coincident with faint optical absorption features and at velocities very similar to the narrow absorption. This suggests that the gas causing the narrow absorption is not close to the AGN and is more likely caused by clouds falling into NGC 315. The environment of NGC 315 turns out to be indeed quite gas rich since we detect five gas-rich companion galaxies in the immediate vicinity of NGC 315.
Key words: Galaxies: active / Galaxies: individual: NGC 315 / radio lines: Galaxies
© ESO, 2009
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