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tokens: version of the full table is available. Table 3 The Spectral Parameters Associated with the H β Emission Line Note. Column information is as follows: Column [1]: 4FGL name; Column [2]: redshift; Column [3]: log-scale continuum luminosity at 5100 Å; Column [4]: FWHM of H β line, in km s −1 ; and Column [5]: log-scale H β line luminosity, in erg s −1 . (This table is available in its entirety in machine-readable form.) Only a portion of this table is shown here to demonstrate its form and content. A machine-readable version of the full table is available. Table 4 The Spectral Parameters Associated with the Mg ii Emission Line Note. Column information is as follows: Column [1]: 4FGL name; Column [2]: redshift; Column [3]: log-scale continuum luminosity at 3000 Å; Column [4]: FWHM of Mg ii line, in km s −1 ; and Column [5]: log-scale Mg ii line luminosity, in erg s −1 . (This table is available in its entirety in machine-readable form.) Only a portion of this table is shown here to demonstrate its form and content. A machine-readable version of the full table is available. Table 5 The Spectral Parameters Associated with the C iv Emission Line Note. Column information is as follows: Column [1]: 4FGL name; Column [2]: redshift; Column [3]: log-scale continuum luminosity at 1350 Å; Column [4]: FWHM of C iv line, in km s −1 ; and Column [5]: log-scale C iv line luminosity, in erg s −1 . (This table is available in its entirety in machine-readable form.) Only a portion of this table is shown here to demonstrate its form and content. A machine-readable version of the full table is available. 3.2. Absorption-line Spectrum The optical spectra of 346 γ -ray blazars show prominent absorption lines, e.g., the Ca HK doublet, primarily originating from the stellar population in the host galaxy. It has been shown in various works that the mass of the central black hole significantly correlates with the stellar velocity dispersion ( σ * , see Ferrarese Merritt 2000 ; Gültekin et al. 2009 ; Kormendy Ho 2013 ). Therefore, we have used the penalized PiXel Fitting tool ( pPXF ; Cappellari Emsellem 2004 ) to derive σ * for blazars present in the sample. This software works in pixel space and uses a maximum penalized likelihood approach to calculate the line-of-sight velocity distribution (LOSVD) from kinematic data (Merritt 1997 ). A large set of stellar population synthesis models (adopted from Vazdekis et al. 2010 ) with a spectral resolution of FWHM = 2.5 Å and the wavelength coverage of [3525, 7500] Å (Sánchez-Blázquez et al. 2006 ) was used in this work. The pPXF code first creates a template galaxy spectrum by convolving the stellar population models with the parameterized LOSVD. To mimic the nonthermal power-law contribution from the central nucleus, we further added a fourth-order Legendre polynomial to the model. The regions of bright emission lines were masked prior to the fitting. The model was then fitted on the rest-frame galaxy spectrum, and σ * and the