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The Impact of Nuclear Star Formation on Gas Inflow to AGN

Published online by Cambridge University Press:  03 June 2010

R. I. Davies ,
E. Hicks ,
M. Schartmann ,
R. Genzel ,
L. J. Tacconi ,
H. Engel ,
A. Burkert ,
M. Krause ,
A. Sternberg  and
F. Mueller Sánchez
...Show all authors
R. I. Davies
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Garching, Germany Email: davies@mpe.mpg.de
E. Hicks
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Garching, Germany Email: davies@mpe.mpg.de
M. Schartmann
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Garching, Germany Email: davies@mpe.mpg.de Universitäts-Sternwarte München, Germany
R. Genzel
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Garching, Germany Email: davies@mpe.mpg.de
L. J. Tacconi
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Garching, Germany Email: davies@mpe.mpg.de
H. Engel
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Garching, Germany Email: davies@mpe.mpg.de
A. Burkert
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Garching, Germany Email: davies@mpe.mpg.de Universitäts-Sternwarte München, Germany
M. Krause
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Garching, Germany Email: davies@mpe.mpg.de Universitäts-Sternwarte München, Germany
A. Sternberg
Affiliation:
School of Physics and Astronomy, Tel Aviv University, Tel Aviv, Israel
F. Mueller Sánchez
Affiliation:
Instituto de Astrofisica de Canarias, La Laguna, Tenerife, Spain
W. Maciejewski
Affiliation:
Astrophysics Research Institute, Liverpool John Moores University, UK
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Abstract

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Our adaptive optics observations of nearby AGN at spatial resolutions as small as 0.″085 show strong evidence for recent, but no longer active, nuclear star formation. We begin by describing observations that highlight two contrasting methods by which gas can flow into the central tens of parsecs. Gas accumulation in this region will inevitably lead to a starburst, and we discuss the evidence for such events. We then turn to the impact of stellar evolution on the further inflow of gas by combining a phenomenological approach with analytical modelling and hydrodynamic simulations. These complementary perspectives paint a picture in which all the processes are ultimately regulated by the mass accretion rate into the central hundred parsecs, and the ensuing starburst that occurs there. The resulting supernovae delay accretion by generating a starburst wind, which leaves behind a clumpy interstellar medium. This provides an ideal environment for slower stellar outflows to accrete inwards and form a dense turbulent disk on scales of a few parsecs. Such a scenario may resolve the discrepancy between the larger scale structure seen with adaptive optics and the small-scale structure seen with VLTI.

Keywords

galaxies: activegalaxies: kinematics and dynamicsgalaxies: nucleigalaxies: Seyfertgalaxies: starburstinfrared: galaxies
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. 283 - 289
Copyright
Copyright © International Astronomical Union 2010

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