tokens: Blandford 1990 ), and M 8 is the black hole mass in units of 10 8 M ⊙ . A was defined by Daly et al. ( 2018 ), A = α /( α + b ), a and b are the coefficients of the fundamental plane of black hole activity, where A = 0.43 (Merloni et al. 2003 ). L bol is the bolometric luminosity (Netzer 1990 ), L bol = 10 L BLR , and L Edd is the Eddington luminosity, L Edd = 1.3 × 10 38 ( M BH / M ⊙ ). The spin of the black hole can be estimated using the following formula (Daly 2019 ),where L j is the beam power, and g i = 0.1 and g bol = 1 are used (Daly 2019 ). The black hole spins obtained using this method can be compared with those obtained using other methods, such as the X-ray reflection method (Reynolds 2014 ). The spin values of GX 339-4 are 0.94 ± 0.02 (Miller et al. 2009 ) and (Garcĺa et al. 2009 ) using the X-ray reflection method, and the spin obtained using the method of Daly ( 2019 ) is 0.92 ± 0.06. The spin obtained using the method of Daly is consistent with those obtained with the X-ray reflection method. Because of the limitation of the observations, it is very difficult to directly measure the spin of large samples using the X-ray reflection method. Therefore, we use the method of Daly to measure the spin for our samples. The accretion disk magnetic field strength values of ∼10 4 G are also reported using other methods (Mikhailov et al. 2015 ). Thus, the accretion disk magnetic field strengths obtained here are similar to the values obtained using other methods. We use Equations ( 2 ) and ( 3 ) to estimate the magnetic field strength of the accretion disk and the spin of black hole, respectively. The values of the magnetic field strength and the spin of black hole are listed in columns (9) and (10) of Table 1 . 3.3. The Intrinsic <italic>γ</italic>-Ray Luminosity We estimate the intrinsic γ -ray luminosity using the formula (Nemmen et al. 2012 )where is the observational γ -ray luminosity. f b is the beaming factor, and f b is estimated as 1-cos(1/Γ), where Γ is the bulk Lorentz factor. The bulk Lorentz factor comes from Ghisellini et al. ( 2014 ). is the observed γ -ray luminosity from the catalog of LAT (Abdo et al. 2010 ; Ackermann et al. 2011 ). The values of and f b are listed in columns (7) and (11) of Table 1 , respectively. The values of the radiation jet power and the jet kinetic power come from Ghisellini et al. ( 2014 ). Ghisellini et al. ( 2014 ) used a simple one-zone leptonic model to get the radiation jet power and the jet kinetic power. They are listed in columns (12) and (13) of Table 1 , respectively. 4. Results and Discussions 4.1. The Distribution of Physical Parameters The density distributions of the spin of SMBHs and the magnetic field strength of the accretion disks are shown in Figure 1 . The average spins of SMBHs for FSRQs and BL Lacs are 〈 j FSRQs 〉 = 0.50 ± 0.23 and 〈 j BL Lacs 〉 = 0.44 ± 0.27, respectively. The average values of the magnetic field strength of the accretion disk for FSRQs and BL Lacs are and ,
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