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Intermediate mass black hole feedback in dwarf galaxy simulations with a resolved ISM and accurate nuclear stellar dynamics

Published online by Cambridge University Press:  28 October 2024

Christian Partmann Open the ORCID record for Christian Partmann [Opens in a new window] ,
Thorsten Naab ,
Natalia Lahén ,
Eugene Churazov ,
Jessica M. Hislop ,
Antti Rantala ,
Peter H. Johansson Open the ORCID record for Peter H. Johansson [Opens in a new window]  and
Michaela Hirschmann
Christian Partmann*
Affiliation:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, D-85748 Garching b. München, Germany
Thorsten Naab
Affiliation:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, D-85748 Garching b. München, Germany
Natalia Lahén
Affiliation:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, D-85748 Garching b. München, Germany
Eugene Churazov
Affiliation:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, D-85748 Garching b. München, Germany
Jessica M. Hislop
Affiliation:
Department of Physics, University of Helsinki, Gustaf Hällströmin katu 2a, FI-00014 Helsinki, Finland
Antti Rantala
Affiliation:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, D-85748 Garching b. München, Germany
Peter H. Johansson
Affiliation:
Department of Physics, University of Helsinki, Gustaf Hällströmin katu 2a, FI-00014 Helsinki, Finland
Michaela Hirschmann
Affiliation:
Institute for Physics, Laboratory for galaxy evolution, Ecole Polytechnique Federale de Lausanne, Observatoire de Sauverny, Chemin Pegasi 51, 1290 Versoix, Switzerland
*
email: [email protected]
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Abstract

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Recent observations have established that dwarf galaxies can host black holes of intermediate mass (IMBH, 100Mȯ < MIMBH ≲ 105 Mȯ). With modern numerical models, we can test the growth of IMBHs as well as their evolutionary impact on the host galaxy. Our novel subsolar-mass (0.8 solar mass) resolution simulations of dwarf galaxies (M* = 2 × 107 Mȯ) have a resolved three-phase interstellar medium and account for non-equilibrium heating, cooling, and chemistry processes. The stellar initial mass function is fully sampled between 0.08–150 Mȯ while massive stars can form HII regions and explode as resolved supernovae. The stellar dynamics around the IMBH is integrated accurately with a regularization scheme. We present a viscous accretion disk model for the IMBH with momentum, energy, and mass conserving wind feedback. We demonstrate how the IMBH can grow from accretion of the cold and warm gas phase and how the presence of the IMBH and its feedback impacts the gas phase structure.

Keywords

intermediate mass black holesdwarf galaxy evolutionactive galactic nuclei
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 19 , Symposium S378: Black Hole Winds at All Scales , December 2023 , pp. 68 - 71
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Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution and reproduction, provided the original article is properly cited.
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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