The central black hole masses and Doppler factors of the $\gamma$-ray loud blazars

In this paper, The central black hole masses and the Doppler factors are derived for PKS 0528+134, PKS 0537-441, 3C279, PKS 1406-074, PKS 1622-297, Q1633+382, Mkn 501, and BL Lacertae. The masses obtained are in the range of (1 -7)$\times {10}^7{M}_{\odot }$ and compared with that obtained with the Klein-Nishina cross section considered (Dermer & Gehrels 1995). If we considered only the Thomson cross section, the masses are in the range of 2.6$\times {10}^6{M}_{\odot }$ - 2$\times 10^{11}M_{\odot}$. The masses obtained from our method are less sensitive to the flux than those obtained from Dermer & Gehrels (1995) method. The masses obtained from two flares (1991 and 1996 flares) of 3C279 are almost the same. For 3C279 and BL Lacertae, viewing angle, $\theta$, and Lorentz factor, $\mathrm{\Gamma }$, are estimated from the derived Doppler factor and the measured superluminal velocity. For 3C279, $\theta ={10}^{\circ }.9-{15}^{\circ }.6$, $\mathrm{\Gamma }$ = 2.4-14.4 for $\delta$ = 3.37; $\theta =8^{\circ }.45-9^{\circ }.7$, $\mathrm{\Gamma }$ = 2.95-11.20 for $\delta$ = 4.89; For BL Lacertae, $\theta ={25}^{\circ }-{29}^{\circ }.4$, $\mathrm{\Gamma }$ = 2.0-4.0.