D. C. Mei | Searcharxiv

arXiv2002

The Supermassive Black Hole in the Gamma-ray Loud Blazar PKS 1510-089

We present the optical light curve for the gamma-ray blazar PKS 1510-089 with a significant variability of 2.0 mag within about 41 minutes in the R band which is the most violently rapid variability detected in our optical monitoring campaign operating since 1982. In the framework of the relativistic beaming model, the central supermassive black hole mass of PKS 1510-089 is of $(1.16-1.98)\times10^8M_\odot$. This is larger than some previous estimates for the central mass in blazars that have been based on models for nonthermal emission, but is consistent with the estimated result of the $M_\bullet-σ_\star$ correlation. Some other physical parameters, including the emission region size, Doppler factor $δ$, the efficiency $η$ for conversion of accreted matter into energy and luminosity are calculated. The value of $η$ = 62.2 strongly implies that the relativistic beaming is responsible for the rapid variability of the gamma-ray loud blazar PKS 1510-089.

astro-ph↗

arXiv2002

Radio Luminosities and Classificatory Criteria of BL Lacertae Objects

Using the sample of radio selected BL Lacertae objects (RBLs) and X-ray selected BL Lacertae objects (XBLs) presented by Sambruna et al. (1996), we calculated the luminosities of radio, optical and X-ray of each source and made the statistical analysis among the luminosities at different wave-bands, broad-band spectral indices from radio to X-ray ($α_{\rm rx}$) and peak frequencies ($ν_p$). Our results are as follows: (i) there is a positive correlation between radio luminosity $L_{\rm r}$ and $α_{\rm rx}$ and a negative correlation between $L_{\rm r}$ and $ν_p$. High-energy peak BL Lacs (HBLs) and low-energy peak BL Lacs (LBLs) can be distinguished very well, the dividing lines are probably those of $\log {L_{\rm r}}=43.25$ (erg/sec) and $α_{\rm rx}>$(or $\leq $)0.75 for $L_{\rm r}$ - $α_{\rm rx}$ plot and those of $\log {L_{\rm r}}\leq 43.25$ (erg/sec) and $\log {ν_p}>14.7$ for the $L_{\rm r}$ - $ν_p$ plot; (ii) there is a weak positive correlation between optical luminosity $L_o$ and $α_{\rm rx}$ and a negatively weak correlation between $L_{\rm o}$ and $ν_p$; (iii) there is no correlation between X-ray luminosity $L_X$ and $α_{\rm rx}$ or between $L_X$ and $ν_p$. From our analysis, we find that synchrotron radiation is the main X-ray radiation mechanism for HBLs while inverse Compton scattering for LBLs.

astro-ph↗