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tokens: There are no noteworthy objects adjacent to IMS J2204+0112, and we found no spectral features with respect to the velocity as one can expect from its redshift. 3 3 At z = 5.926, the prominent [C ii ] 158 μ m line is located at the band gap between bands 6 and 7. In the defined spectral windows, there could be a highly excited CO( J = 21–20) line and several H 2 O lines, but they are expected to be weak and/or rare at z ∼ 6 (Narayanan et al. 2008 ; Bañados et al. 2015 ). Using the IMFIT task of the CASA package, we fitted the source on each continuum map with a simple 2D Gaussian model, resulting in the integrated flux densities at 250 and 343.5 GHz being f 250 GHz = 1.474 ± 0.023 and mJy, respectively. Note that the peak flux densities are 1.289 ± 0.020 and 2.966 ± 0.027 mJy beam −1 , respectively. These flux densities are higher than the value expected from the relation between and of other high-redshift quasars (Equation (2) in Venemans et al. 2016 ; see details in Section 4.1 ) by a factor of six, although there has been a recent suggestion that there is no correlation between and (Venemans et al. 2018 ). Assuming that the FIR flux is dominated by the host galaxy, no features in the residual maps after the point source model subtraction (right panels of Figure 1 ) is consistent with its host galaxy being as compact as (or about 4 kpc in physical scale at z ∼ 6), like those of other high-redshift quasars (Wang et al. 2013 ; Willott et al. 2015 , 2017 ; Venemans et al. 2016 , 2017a ; Mazzucchelli et al. 2017 ; Decarli et al. 2018 ). The central positions of the ALMA detection are offset by only about 02 from the z -band position (see crosses in Figure 1 ). These small offsets between the optical and submillimeter detections are in agreement with the previously reported uncertainties of ALMA astrometry (Capak et al. 2015 ; Willott et al. 2015 ; Pentericci et al. 2016 ), disfavoring the possibility that the submillimeter flux comes from a neighboring or foreground galaxy. Figure 2 shows the spectral energy distribution (SED) of IMS J2204+0112 in the observed frame. The black filled circles represent the flux densities of IMS J2204+0112 from Kim et al. ( 2015b , 2018 ) and the values derived from the archival data (see Section 2.2 ), while the red filled circles are from our ALMA observation. Also plotted are the composite quasar spectrum (gray line; Selsing et al. 2016 ), the intrinsic SED of a type 1 quasar (green line; Lyu Rieke 2017 ), and the empirical SED of ULIRGs hosting AGN at z ∼ 2 (purple line; AGN4 of Kirkpatrick et al. 2015 ). The ULIRG AGN template is consistent with the submillimeter data, which suggests that the host of IMS J2204+0112 is ULIRG-like, similar to the hosts of other high-redshift quasars (Wang et al. 2013 ; Willott et al. 2013 , 2015 , 2017 ; Venemans et al. 2016 ; Decarli et al. 2018 ; Izumi et al. 2018 ). Note that the templates were redshifted to the observed frame using z = 5.926 (Kim et al. 2018 ), including