A Wide and Deep Exploration of Radio Galaxies with Subaru HSC (WERGS). II. 
Physical Properties Derived from the SED Fitting with Optical, Infrared, and 
Radio Data

Toba, Yoshiki; Yamashita, Takuji; Nagao, Tohru; Wang, Wei-Hao; Ueda, Yoshihiro; Ichikawa, Kohei; Kawaguchi, Toshihiro; Akiyama, Masayuki; Hsieh, Bau-Ching; Kajisawa, Masaru; Lee, Chien-Hsiu; Matsuoka, Yoshiki; Noboriguchi, Akatoki; Onoue, Masafusa; Schramm, Malte; Tanaka, Masayuki; Komiyama, Yutaka

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Journal Article

A Wide and Deep Exploration of Radio Galaxies with Subaru HSC (WERGS). II. Physical Properties Derived from the SED Fitting with Optical, Infrared, and Radio Data

MPS-Authors

Toba, Yoshiki
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Yamashita, Takuji
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Nagao, Tohru
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Wang, Wei-Hao
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Ueda, Yoshihiro
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Ichikawa, Kohei
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Kawaguchi, Toshihiro
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Akiyama, Masayuki
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Hsieh, Bau-Ching
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Kajisawa, Masaru
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Lee, Chien-Hsiu
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Matsuoka, Yoshiki
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Noboriguchi, Akatoki
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Onoue, Masafusa
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Schramm, Malte
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Tanaka, Masayuki
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Komiyama, Yutaka
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

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https://ui.adsabs.harvard.edu/abs/2019ApJS..243...15T
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Citation

Toba, Y., Yamashita, T., Nagao, T., Wang, W.-H., Ueda, Y., Ichikawa, K., et al. (2019). A Wide and Deep Exploration of Radio Galaxies with Subaru HSC (WERGS). II. Physical Properties Derived from the SED Fitting with Optical, Infrared, and Radio Data. The Astrophysical Journal Supplement Series, 243.

Cite as: https://hdl.handle.net/21.11116/0000-0005-CF9C-3

Abstract

We present physical properties of radio galaxies (RGs) with f _{1.4 GHz} > 1 mJy discovered by Subaru Hyper Suprime-Cam (HSC) and Very Large Array Faint Images of the Radio Sky at Twenty-Centimeters (FIRST) survey. For 1056 FIRST RGs at 0 < z ≤ 1.7 with HSC counterparts in about 100 deg², we compiled multi-wavelength data of optical, near-infrared (IR), mid-IR, far-IR, and radio (150 MHz). We derived their color excess (E(B − V)_*), stellar mass, star formation rate (SFR), IR luminosity, the ratio of IR and radio luminosity (q _IR), and radio spectral index (α _radio) that are derived from the spectral energy distribution (SED) fitting with CIGALE. We also estimated Eddington ratio based on stellar mass and integration of the best-fit SEDs of active galactic nucleus (AGN) component. We found that E(B − V)_*, SFR, and IR luminosity clearly depend on redshift while stellar mass, q _IR, and α _radio do not significantly depend on redshift. Since optically faint (i _AB ≥ 21.3) RGs that are newly discovered by our RG survey tend to be high redshift, they tend to not only have a large dust extinction and low stellar mass but also have high SFR and AGN luminosity, high IR luminosity, and high Eddington ratio compared with optically bright ones. The physical properties of a fraction of RGs in our sample seem to differ from a classical view of RGs with massive stellar mass, low SFR, and low Eddington ratio, demonstrating that our RG survey with HSC and FIRST provides us curious RGs among entire RG population.