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Panchromatic Analysis for Nature of HIgh-z galaxies Tool (PANHIT)

Published online by Cambridge University Press:  10 June 2020

Ken Mawatari ,
Akio K. Inoue Open the ORCID record for Akio K. Inoue [Opens in a new window] ,
Satoshi Yamanaka ,
Takuya Hashimoto  and
Yoichi Tamura
Ken Mawatari
Affiliation:
Institute for Cosmic Ray Research, University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba277-8582, Japan email: [email protected] Department of Environmental Science and Technology, Fuculty of Design Technology, Osaka Sangyo University, 3-1-1, Nakagaito, Daito, Osaka, 574-8530, Japan
Akio K. Inoue
Affiliation:
Department of Environmental Science and Technology, Fuculty of Design Technology, Osaka Sangyo University, 3-1-1, Nakagaito, Daito, Osaka, 574-8530, Japan
Satoshi Yamanaka
Affiliation:
Department of Environmental Science and Technology, Fuculty of Design Technology, Osaka Sangyo University, 3-1-1, Nakagaito, Daito, Osaka, 574-8530, Japan
Takuya Hashimoto
Affiliation:
Department of Environmental Science and Technology, Fuculty of Design Technology, Osaka Sangyo University, 3-1-1, Nakagaito, Daito, Osaka, 574-8530, Japan National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo181-8588, Japan
Yoichi Tamura
Affiliation:
Division of Particle and Astrophysical Science, Graduate School of Science, Nagoya University, Nagoya464-8602, Japan
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Abstract

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We have developed a new SED fitting tool specialized for frontier redshift galaxies. It is a common case for high-z galaxies that the available data are restricted to rich optical to near-infrared photometry and few far-infrared (FIR) data deep enough to detect the faint object (e.g., HST/WFC3 + Spitzer/IRAC + ALMA). In such situation, one cannot perform a complicated modeling of dust emission in FIR regime. We then adopt simple treatment for the dust emission using empirical LIRG templates. Instead, we adopt a sophisticated and physically motivated modeling for stellar and nebular emission parts in rest-frame UV-to-optical regime. Our new code fits not only broad band photometry but also spectral emission line flux. There is an option to fit observed SED with two templates with different physical properties. Our new code, PANHIT, is now in public, and was already applied to some high-z frontier galaxies.

Keywords

methods: data analysisgalaxies: high-redshiftearly universe
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. 285 - 286
Copyright
© International Astronomical Union 2020

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