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The formation of Supersonically Induced Gas Objects (SIGOs) with H2 cooling

Published online by Cambridge University Press:  20 January 2023

Yurina Nakazato Open the ORCID record for Yurina Nakazato [Opens in a new window] ,
Gen Chiaki ,
Naoki Yoshida ,
Smadar Naoz ,
William Lake  and
Chiou Yeou
Yurina Nakazato
Affiliation:
Department of Physics, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan, email: yurina.nakazato@phys.s.u-tokyo.ac.jp
Gen Chiaki
Affiliation:
Astronomical Institute, Tohoku University, 6-3, Aramaki, Aoba-ku, Sendai, Miyagi 980-8578, Japan
Naoki Yoshida
Affiliation:
Kavli Institute for the Physics and Mathematics of the Universe (WPI), UT Institute for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan Research Center for the Early Universe, School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan
Smadar Naoz
Affiliation:
Department of Physics and Astronomy, UCLA, Los Angeles, CA 90095 Mani L. Bhaumik Institute for Theoretical Physics, Department of Physics and Astronomy, UCLA, Los Angeles, CA 90095, USA
William Lake
Affiliation:
Department of Physics and Astronomy, UCLA, Los Angeles, CA 90095 Mani L. Bhaumik Institute for Theoretical Physics, Department of Physics and Astronomy, UCLA, Los Angeles, CA 90095, USA
Chiou Yeou
Affiliation:
Department of Physics and Astronomy, UCLA, Los Angeles, CA 90095 Mani L. Bhaumik Institute for Theoretical Physics, Department of Physics and Astronomy, UCLA, Los Angeles, CA 90095, USA
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Abstract

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During the recombination of the universe, supersonic relative motion between baryons and dark matter (DM) generally existed. In the presence of such streaming motions, gas clumps can collapse outside of virial radii of their closest dark matter halos. Such baryon dominant objects are thought to be self-gravitating and are called supersonically induced gas objects; SIGOs. We perform three-dimensional hydrodynamical simulations by including H2 chemical reactions and stream velocity and follow SIGO’s formation from z = 200 to z = 25. SIGOs can be formed under the influence of stream velocity, and cooling is effective in contracting gas clouds. We follow its further evolution with higher resolution. We find that there are SIGOs which become Jeans unstable outside of the virial radius of the closest DM halos. Those SIGOs are gravitationally unstable and trigger star formation.

Keywords

cosmology: theorymethods: numericalgalaxies: high-redshiftstars: Population III
Type
Contributed 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. 45 - 50
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 (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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