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Galaxy evolution and radiative properties in the early universe: Multi-wavelength analysis in cosmological simulations

Published online by Cambridge University Press:  04 June 2020

Shohei Arata Open the ORCID record for Shohei Arata [Opens in a new window] ,
Hidenobu Yajima ,
Kentaro Nagamine Open the ORCID record for Kentaro Nagamine [Opens in a new window] ,
Yuexing Li  and
Sadegh Khochfar
Shohei Arata
Affiliation:
Theoretical Astrophysics, Department of Earth and Space Science, Graduate School of Science, Osaka University, Toyonaka, Osaka560-0043, Japan email: arata@astro-osaka.jp
Hidenobu Yajima
Affiliation:
Center of Computational Sciences University of Tsukuba, Ibaraki305-8577, Japan
Kentaro Nagamine
Affiliation:
Theoretical Astrophysics, Department of Earth and Space Science, Graduate School of Science, Osaka University, Toyonaka, Osaka560-0043, Japan email: arata@astro-osaka.jp Department of Physics & Astronomy, University of Nevada, Las Vegas, 4505 S. Maryland Pkwy, Las Vegas, NV89154-4002, USA Kavli IPMU (WPI), The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba, 277-8583, Japan
Yuexing Li
Affiliation:
Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA16802, USA Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA16802, USA
Sadegh Khochfar
Affiliation:
SUPA, Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, EH9 3HJ, UK
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Abstract

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Recent observations have successfully detected UV or infrared flux from galaxies at the epoch of reionization. However, the origin of their radiative properties has not been fully understood yet. Combining cosmological hydrodynamic simulations and radiative transfer calculations, we present theoretical predictions of multi-wavelength radiative properties of the first galaxies at z = 6–15. We find that most of the gas and dust are ejected from star-forming regions due to supernova (SN) feedback, which allows UV photons to escape. We show that the peak of SED rapidly shifts between UV and infrared wavelengths on a timescale of 100 Myr due to intermittent star formation and feedback. When dusty gas covers the star-forming regions, the galaxies become bright in the observed-frame sub-millimeter wavelengths. In addition, we find that the escape fraction of ionizing photons also changes between 1–40% at z > 10. The mass fraction of H ii region changes with star formation history, resulting in fluctuations of metal lines and Lyman-α line luminosities. In the starbursting phase of galaxies with a halo mass ∼1011Mȯ (1012Mȯ), the simulated galaxy has L[OIII] ∼ 1042 (1043) erg s−1, which is consistent with the observed star-forming galaxies at z > 7. Our simulations suggest that deep [Cii] observation with ALMA can trace the distribution of neutral gas extending over ∼20 physical kpc. We also find that the luminosity ratio L[OIII]/L[CII] decreases with bolometric luminosity due to metal enrichment. Our simulations show that the combination of multi-wavelength observations by ALMA and JWST will be able to reveal the multi-phase ISM structure and the transition from starbursting to outflowing phases of high-z galaxies.

Keywords

hydrodynamicsradiative transfergalaxies: evolutiongalaxies: high-redshift
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S352: Uncovering Early Galaxy Evolution in the ALMA and JWST Era , June 2019 , pp. 55 - 59
Copyright
© International Astronomical Union 2020

References

Arata, S., Yajima, H., Nagamine, K., et al. 2019, MNRAS, 488, 262910.1093/mnras/stz1887CrossRefGoogle Scholar
Bouwens, R. J., Illingworth, G. D., Oesch, P. A., et al. 2015, ApJ, 803, 3410.1088/0004-637X/803/1/34CrossRefGoogle Scholar
Carniani, S., Maiolino, R., Pallottini, A., et al. 2017, A&A, 605, A42Google Scholar
Fujimoto, S., Ouchi, M., Ferrara, A., et al. 2019, arXiv e-prints, arXiv:1902.06760Google Scholar
Hashimoto, T., Laporte, N., Mawatari, K., et al. 2018, Nature, 557, 392CrossRefGoogle Scholar
Hashimoto, T., Inoue, A., Mawatari, K., et al. 2019, PASJ, 71, 7110.1093/pasj/psz049CrossRefGoogle Scholar
Inoue, A. K., Tamura, Y., Matsuo, H., et al. 2016, Science, 352, 155910.1126/science.aaf0714CrossRefGoogle Scholar
Johnson, J. L., Dalla Vecchia, C., & Khochfar, S. 2013, MNRAS, 428, 185710.1093/mnras/sts011CrossRefGoogle Scholar
Laporte, N., Ellis, R. S., Boone, F., et al. 2017, ApJ, 837, L2110.3847/2041-8213/aa62aaCrossRefGoogle Scholar
Li, Y., Hopkins, P. F., Hernquist, L., et al. 2008, ApJ, 678, 41CrossRefGoogle Scholar
Ma, X., Hayward, C. C., Casey, C. M., et al. 2019, MNRAS, 487, 184410.1093/mnras/stz1324CrossRefGoogle Scholar
Knudsen, K. K., Watson, D., Frayer, D., et al. 2017, MNRAS, 466, 138CrossRefGoogle Scholar
Marrone, D. P., Spilker, J. S., Hayward, C. C., et al. 2018, Nature, 553, 51CrossRefGoogle Scholar
Riechers, D. A., Bradford, C. M., Clements, D. L., et al. 2013, Nature, 496, 32910.1038/nature12050CrossRefGoogle Scholar
Schaye, J., Dalla Vecchia, C., Booth, C. M., et al. 2010, MNRAS, 402, 153610.1111/j.1365-2966.2009.16029.xCrossRefGoogle Scholar
Tamura, Y., Mawatari, K., Hashimoto, T., et al. 2019, ApJ, 874, 27CrossRefGoogle Scholar
Watson, D., Christensen, L., Knudsen, K. K., et al. 2015, Nature, 519, 32710.1038/nature14164CrossRefGoogle Scholar
Yajima, H., Li, Y., Zhu, Q., & Abel, T., 2012, MNRAS, 424, 88410.1111/j.1365-2966.2012.21228.xCrossRefGoogle Scholar
Yajima, H., Nagamine, K., Zhu, Q., et al. 2017, ApJ, 846, 3010.3847/1538-4357/aa82b5CrossRefGoogle Scholar