tokens: the best-fit model yielding erg s −1 . Figure 1. Top: deconvolved spectrum (crosses) and best-fit model (solid line) observed with XMM-Newton. PN, MOS1, and MOS2 cameras are plotted in black, red, and blue, respectively. Bottom: residuals are shown. The spectrum is rebinned for visual clarity. Table 1 CQ 4479 X-Ray Fitting Parameters Note. X-ray spectrum fit parameter results from an absorbed power-law fit corrected for galactic absorption. When both parameters are left free, or one of each parameter is fixed using previous fit results, we consistently find an upper limit solution to characteristic of an unobscured quasar. 2.3. Far-ultraviolet to Far-infrared Photometry Far-ultraviolet (FUV) to far-infrared (FIR) observations are obtained from the Stripe 82X catalog (Ananna et al. 2017 ). The target has FUV and NUV coverage from GALEX (Martin et al. 2005 ), and optical coverage from the coadded SDSS catalogs (Jiang et al. 2014 ; Fliri Trujillo 2015 ). In the infrared, Stripe 82X was observed with the Spitzer Space Telescope at 3.6 and 4.5 μ m (Papovich et al. 2016 ; Timlin et al. 2016 ) as well as the WISE 3.4, 4.6, 12, and 22 μ m bands (Wright et al. 2010 ). Herschel/SPIRE observations using 250, 350, and 500 μ m bands are also available for the Stripe82X field from the Herschel Stripe82 Survey (HerS; Viero et al. 2014 ). For more information on the Stripe 82X catalog and its counterpart identification protocol, please see LaMassa et al. ( 2016 ) and Ananna et al. ( 2017 ). 2.4. SOFIA HAWC+ Observations Due to the large gap in spectral coverage from 22 to 250 μ m, crucial for measuring the dust-obscured star formation rate (SFR) and the AGN contribution to the mid-IR, new observations using SOFIA/HAWC+ (Dowell et al. 2013 ; Smith et al. 2014 ) were taken using band C at 89 μ m (PI: A. Kirkpatrick, PID: 07-0096). CQ 4479 was observed for ∼7223 s on 2019 September 7 during SOFIA Cycle 7 using the HAWC+ total intensity OTFMAP mode with a Lissajous pattern in nominal water vapor conditions. At this redshift, each 155 pixel subtends a linear width of 8.4 kpc. The total field of view of HAWC+ in this setup is 42 by 27, with an FWHM of 78. Following data acquisition, the observations were reduced using the HAWCDPR PIPELINE (Harper et al. 2018 ). Flux calibration was performed using an average reference calibration factor across the detector. Source extraction was performed using the CRUSH V. 2.50-2 detect routine (Kovács 2006 , 2008 ) in the faint object mode, yielding a flux measurement of 75.42 ± 14.2 mJy in a 78 FWHM beam (SNR = 5.31). The SOFIA HAWC+ band C image is shown in Figure 2 . Figure 2. Left: SOFIA HAWC+ Band C observation of CQ 4479 centered at the target coordinates of R.A. J2000 of 1 h 40 m 4071 and Decl. J2000 of 0°17′ 5817. For reference, the SOFIA HAWC+ Band C (89 μ m) PSF FWHM is the circle in the lower left (78). At z = 0.405, the spatial scale is 5.413 kpc/′′ (Wright 2006 ). Each pixel is 155, subtending a linear width of 8.4
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