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First galaxy SED: Contribution from pre-main-sequence stars

Published online by Cambridge University Press:  10 June 2020

Hiroto Mitani ,
Naoki Yoshida Open the ORCID record for Naoki Yoshida [Opens in a new window] ,
Kazuyuki Omukai  and
Takashi Hosokawa
Hiroto Mitani
Affiliation:
Department of Physics, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo113-0033, Japan email: mitani@utap.phys.s.u-tokyo.ac.jp
Naoki Yoshida
Affiliation:
Department of Physics, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo113-0033, Japan email: mitani@utap.phys.s.u-tokyo.ac.jp Kavli Institute for the Physics and Mathematics of the Universe (WPI), UT Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba277-8583, Japan
Kazuyuki Omukai
Affiliation:
Astronomical Institute, Tohoku University, Sendai980-8578, Japan
Takashi Hosokawa
Affiliation:
Department of Physics, Kyoto University, Kyoto606-8502, Japan
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Abstract

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We calculate the spectral energy distribution of the first galaxies which contain pre-main-sequence stars by using the stellar evolution code Modules for Experiments in Stellar Astrophysics, the spectra model BT-Settl, and the stellar population synthesis code PEGASE. We calculate the galaxy spectral energy distribution for Salpeter Initial Mass Function. We find that very young first galaxies are bright also in mid-infrared, and the contribution of pre-main-sequence stars can be significant over 0.1 Myr after a star-formation episode.

Keywords

galaxies: high-redshiftstars: pre–main-sequencestars: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S341: Challenges in Panchromatic Modelling with Next Generation Facilities , November 2019 , pp. 287 - 288
Copyright
© International Astronomical Union 2020

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