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An idealized setup for cosmological evolution of baryonic gas in isolated halos

Published online by Cambridge University Press:  20 January 2023

S. Dattathri Open the ORCID record for S. Dattathri [Opens in a new window]  and
P. Sharma
S. Dattathri
Affiliation:
Department of Physics, Indian Institute of Science, Bangalore-560012, India Department of Astronomy, University of Michigan, 1085 S. University Avenue, Ann Arbor, MI, 48109, USA
P. Sharma
Affiliation:
Department of Physics, Indian Institute of Science, Bangalore-560012, India
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Abstract

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We use hydrodynamical simulations to study the evolution of baryonic gas in a cosmologically evolving dark matter halo. We model both the inner and outer regions of the halo using a density profile that transitions from an inner NFW profile to a flat profile far from the halo. Metallicity-dependent radiative cooling and AGN jet feedback are implemented, which lead to heating and cooling cycles in the core. We analyze the evolution of gas and the central supermassive black hole (SMBH) across cosmological time. We find that the properties of the gas and the SMBH are correlated across halo masses and feedback efficiencies.

Keywords

Galaxyactive-Galaxiesintergalactic medium-Galaxieshalos
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S362: The Predictive Power of Computational Astrophysics as a Discovery Tool , June 2020 , pp. 51 - 53
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

References

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Prasad, D., Sharma, P., & Babul, A., 2015, ApJ, 811, 108 CrossRefGoogle Scholar
Choudhury, P. P., Kauffmann, G., & Sharma, P., 2019, MNRAS, 485, 3430 Google Scholar