ner_tags: O O O O O O O B-Survey O O O B-Wavelength I-Wavelength O O O O O O O O O B-Software B-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O B-Wavelength O O O O O O O O B-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O B-Wavelength O O O B-Survey O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O B-Dataset O B-Citation I-Citation I-Citation I-Citation O O B-Survey O O O O O O O O O O O O O B-Dataset O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O B-Dataset O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O B-Survey O O O O O B-Formula I-Formula I-Formula O O O O O O O O O O O O O O O B-Wavelength I-Wavelength I-Wavelength O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O B-Survey I-Survey I-Survey O O B-Wavelength O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O B-Wavelength I-Wavelength O O O O O O B-Wavelength I-Wavelength O O O O O O B-Wavelength I-Wavelength O O O O O O O B-Wavelength O O O O O O O B-Survey O B-Instrument O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O B-Wavelength O O O O O O B-Instrument O O O O O O O O O O O B-Instrument O O O O O O O O O O O O O O B-Survey O O O O B-Wavelength O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O B-Wavelength O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O B-Wavelength O O O O O O O B-Survey O O O O O O O O O O O O O B-Survey O B-Instrument O
tokens: sources due to a bias from the FIRST sensitivity. The rest-frame g -band absolute magnitude was estimated by the SED template fitting Mizuki (Tanaka 2015 ; Tanaka et al. 2018 ). There may be two sequences of the g magnitude along the redshifts. The bright sequence with M g ≲ −21 does not strongly depend on the redshift. On the other hand, the number of sources belonging in the faint sequence seems to dramatically increase with increasing redshifts. The sources with faint absolute magnitudes are also faint in apparent magnitudes ( i > 24), and the optical SEDs of the HSC-SSP bands show that some sources on the faint sequence have a flat SED without distinct features. Thus, the redshifts of these sources are probably estimated incorrectly. In fact, the comparison of M g and redshifts with the COSMOS2015 catalog (Laigle et al. 2016 ) in UD-COSMOS shows the underestimated redshifts of the faint sequence sources, and the redshifts of COSMOS2015 indicate that most sources in the faint sequence should be at z L16 > 1.5. In this comparison, a source at z = 0.5 on the faint sequence was found to have redshift and M g consistent with the COSMOS2015 catalog. This source is really a local source with a faint optical luminosity. The faint sequence could be an apparent one due to both the effects of the underestimated redshifts and the Malmquist bias of the HSC-SSP sensitivity limits. Some sources at z ≲ 0.5 may be local galaxies with strong radio radiation from active star formation. Figure 13. Rest-frame 1.4 GHz radio luminosity (upper panel) and the absolute g -band magnitude at the rest frame (lower panel) as a function of photo- z . Only RG sources with reliable photometric redshifts, with z photo > 0, , and , are shown. The black circles and red circles denote the Wide and UD-COSMOS RGs, respectively. Radio loudness at the rest frame was estimated and is defined here as a ratio of the rest-frame 1.4 GHz flux to the rest-frame g -band flux. The wavelength of the rest-frame g -band flux is close to the rest-frame B -band, which is typically used for calculating the radio loudness. The rest-frame radio loudnesses of the SDSS- and HSC-level sources as a function of the apparent i -band magnitude are shown in Figure 14 . We found that RGs with high radio loudness () are found in the HSC-level subsample. Certainly, there are likely also low radio-loudness RGs in the HSC-level regime, but such sources are not included due to the sensitivity limit of the FIRST survey. Note that the radio loudness we use here is underestimated, because HSC band flux could be dominated by stellar light from host galaxies of RGs, and the rest-frame g -band flux is derived from the SED templates of galaxies. Figure 14. Radio loudness at the rest frame as a function of the apparent i -band magnitude. The RG sources with reliable photo- z in the Wide (black) and the UD-COSMOS (red) layers are shown. The blue dotted line is the border separating the SDSS-level and HSC-level samples