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tokens: dominates the fit below 1 keV, while the zeroth-order spectrum (MYTorusZ) dominates above 1 keV, with the scattered (MYTorusS) and line emission (MYTorusL) contributing at a significantly lower level. We present the soft (0.5–2 keV), hard (2–10 keV), and full (0.5–10 keV) X-ray fluxes of our quasars based on the MYTorus fits to our spectra in Table 4 . We also compute the intrinsic luminosities, which are corrected for absorption, scattering, and reflection, in Table 5 . Table 4 Observed X-Ray Fluxes Table 5 Absorption-corrected, Rest-frame X-Ray and Infrared Luminosities Note. a The 6 μ m luminosity was estimated by interpolating between the Wide-field Infrared Survey Explorer (WISE) photometric bands. 4. Discussion 4.1. The <inline-formula> <tex-math> </tex-math> <inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa88acieqn94.gif"></inline-graphic> </inline-formula> Relation Urrutia et al. ( 2012 ) used SED modeling to determine the bolometric luminosities of the quasars in our sample. When combined with broad line widths measured from our optical and near-infrared spectroscopy, their accretion rates are estimated and listed in Table 1 as . The X-ray photon index, Γ, has been shown to correlate with the BH accretion rate, , for high luminosity quasars ( e.g., Piconcelli et al. 2005 ; Shemmer et al. 2006 , 2008 ). In Figure 5 , we plot our derived Γ's versus , along with luminous unabsorbed quasars from Piconcelli et al. ( 2005 ), Shemmer et al. ( 2006 ), and Shemmer et al. ( 2008 ), as well as Compton-thick AGN from Brightman et al. ( 2016 ). The red quasars fall below the best-fit line from Shemmer et al. ( 2008 ), although they are largely consistent given the uncertainties on Γ. It is unclear if there is a systematic offset in the relation for red quasars given the small size of our sample. However, the trend of steepening photon index with increased accretion rate is apparent. Figure 5. X-ray photon index, Γ, vs. Eddington ratio, for luminous quasars. Gray filled squares are luminous unobscured quasars from Shemmer et al. ( 2006 , 2008 ). Open circles are Palomar-Green (PG) quasars with Γ from Piconcelli et al. ( 2005 ) and from Inoue et al. ( 2007 ). Gray filled triangles are local Compton-thick AGN from Brightman et al. ( 2016 ). Filled black circles are F2M quasars. The red line is the relation from Shemmer et al. ( 2008 ). The blue line is the Trakhtenbrot et al. ( 2017 ) relation based on their BCES (Y–X) and FITEXY linear regression analysis methods. Red quasars appear to have flatter Γ's relative to their optical/IR derived accretion rates, but obey the general trend of steeper Γ with increasing accretion rate. We note that a recent study by Trakhtenbrot et al. ( 2017 ), using a large set of low-redshift AGN with high-quality optical and X-ray data spanning 0.3–195 keV ( Swift /BAT AGN; Baumgartner et al. 2013 ), found weak to no correlation between the two quantities when Γ is computed over the full