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tokens: high L 2–10 and powerful outflows. Assuming the material scattering X-rays has an outflowing component, we can also calculate its maximum kinetic energy power using the n e estimates of the warm scattering region. We assume the same velocities v ≈ 3000 km s −1 seen in Alexandroff et al. ( 2018 ) launched at scale height h = 10 pc: which makes up a small fraction of the bolometric output. Thus, the phase of gas responsible for producing the scattered X-rays is not an energetically important component of the quasar ouput. 4.4 Comparing with other observations While there are X-ray studies of highly obscured quasars, most have been limited to low-redshift samples. Another class of reddened quasars are the HotDOGs, which have properties similar to those of ERQs in terms of spectral energy distribution, luminosity, and redshift (Eisenhardt et al. 2012 ; Assef et al. 2015 ). Despite these similarities, there are some interesting differences stemming from somewhat different selection methods. One such difference is that HotDOGs are well below the Stern ( 2015 ) and Chen et al. ( 2017 ) relationships (Ricci et al. 2017 ; Vito et al. 2018 ), while also showing Compton-thick obscurations (Piconcelli et al. 2015 ), in contrast to ERQs explored in Goulding et al. ( 2018 ) and in this paper. We compare their L 6 μm – L 2–10 properties in Fig. 5 . A recent NuSTAR observation of a z = 2.298 HotDOG (W1835+4355) showed Compton-thick obscuration, N H ≈ 0.9 × 10 24 cm −2 , and absorption-corrected luminosity of L 2–10 = 1.6 × 10 45 erg s −1 (Zappacosta et al. 2018 ) similar to those of SDSSJ1652 presented here. Compared to other HotDOGs, this target also exhibited higher X-ray luminosity, nearly consistent with the Stern ( 2015 ) and Chen et al. ( 2017 ) relations, shown in Fig. 5 . In contrast to SDSSJ1652, their target was modelled with θ i = 70° and a larger model-dependent . This suggest remarkable similarities between ERQs and HotDOGs with the only differences in the obscuration properties: θ i and f sc . This indicates a variety in HotDOG properties with some that have overlapping L 6 μm – L 2–10 properties to ERQs. 5 CONCLUSION We report on deep ∼ 130-ks XMM–Newton and ∼ 218-ks NuSTAR observations of SDSSJ1652, an obscured, extremely red quasar at z = 2.94. We characterize the intrinsic X-ray properties and obscuration geometry using XMM–Newton , which is sensitive to the absorbing column, and NuSTAR , which probes the intrinsically unobscured X-rays. We determine the accretion luminosity and the obscuration properties of SDSSJ1652 to provide verification for severely photon-limited studies of the high-redshift, obscured quasar population. We extracted spectra from the XMM–Newton MOS and PN and the NuSTAR FPMA detectors. Unfortunately, we could only place a 3 σ upper limit for the NuSTAR FPMB. We fit 0.5–10 keV XMM–Newton and 6–79 keV NuSTAR spectra with a physically motivated MYTorus model that models the zeroth-order continuum reprocessing due to the