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Obscuring and Feeding Supermassive Black Holes with Evolving Nuclear Star Clusters

Published online by Cambridge University Press:  03 June 2010

M. Schartmann ,
A. Burkert ,
M. Krause ,
M. Camenzind ,
K. Meisenheimer  and
R. I. Davies
M. Schartmann
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, Germany Email: [email protected] Universitätssternwarte München, Scheinerstrasse 1, 81679 München, Germany
A. Burkert
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, Germany Email: [email protected] Universitätssternwarte München, Scheinerstrasse 1, 81679 München, Germany Max-Planck-Fellow
M. Krause
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, Germany Email: [email protected] Universitätssternwarte München, Scheinerstrasse 1, 81679 München, Germany
M. Camenzind
Affiliation:
ZAH – Landessternwarte Heidelberg, Königstuhl 12, 69117 Heidelberg, Germany
K. Meisenheimer
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
R. I. Davies
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, Germany Email: [email protected]
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Abstract

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Recently, high-resolution observations made with the help of the near-infrared adaptive optics integral field spectrograph SINFONI at the VLT proved the existence of massive and young nuclear star clusters in the centers of a sample of Seyfert galaxies. With the help of high-resolution hydrodynamical simulations with the pluto code, we follow the evolution of such clusters, especially focusing on mass and energy feedback from young stars. This leads to a filamentary inflow of gas on large scales (tens of parsecs), whereas a turbulent and very dense disk builds up on the parsec scale. Here we concentrate on the long-term evolution of the nuclear disk in NGC 1068 with the help of an effective viscous disk model, using the mass input from the large-scale simulations and accounting for star formation in the disk. This two-stage modeling enables us to connect the tens-of-parsecs scale region (observable with SINFONI) with the parsec-scale environment (MIDI observations). At the current age of the nuclear star cluster, our simulations predict disk sizes of the order 0.8 to 0.9 pc, gas masses of order 106M⊙, and mass transfer rates through the inner boundary of order 0.025 M⊙yr−1, in good agreement with values derived from observations.

Keywords

galaxies: Seyfertgalaxies: nucleigalaxies: ISMgalaxies: individual (NGC 1068)hydrodynamicsmethods: numericalISM: evolutionISM: kinematics and dynamicsblack hole physicsstars: mass loss
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S267: Co-Evolution of Central Black Holes and Galaxies , August 2009 , pp. 307 - 312
Copyright
Copyright © International Astronomical Union 2010

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