2012/05/11 by Fan Xu-Liang, Xu-Liang Fan, Jin-Ming Bai +7 · 1 citation
Physics and Astronomy · #Amplitude #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Blazar #Dark Matter and Cosmic Phenomena #Fermi Gamma-ray Space Telescope #Galaxy #Gamma ray #Luminosity #Optics #Photon #Physics #Quasar #Radio Astronomy Observations and Technology #Spectral density #Spectral index #Spectral line #Statistics #Telescope #astro-ph.CO #astro-ph.HE
paper · pdf · doi:10.1088/1674-4527/12/11/003
published as 2012RAA....12.1475F · 10 pages, 10 figures, Accepted by RAA
arxiv created 2012/05/11 · openalex publication_date 2012/10/24 · arxiv updated 2014/09/03 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
We collect the second Large Area Telescope AGN catalog (2LAC) and Monitor of Jets in AGN with VLBA Equipment (MOJAVE) quasi-simultaneous data to investigate the radio-γ connection of blazars. The cross sample contains 166 sources. The statistical analysis based on this sample confirms positive correlations between these two bands, but the correlations become weaker as the γ-ray energy increases. The statistical results between various parameters show negative correlations of γ-ray photon spectral index with γ-ray loudness for both Flat Spectrum Radio Quasars (FSRQs) and BL Lacertae objects, positive correlations of γ-ray variability index with the γ-ray loudness for FSRQs, a negative correlation of the γ-ray variability index with the γ-ray photon spectral index for FSRQs, and negative correlations of γ-ray photon spectral index with γ-ray luminosity for FSRQs. These results suggest that the γ-ray variability may be due to changes inside the γ-ray emission region like the injected power, rather than changes in the photon density of the external radiation fields, and the variability amplitude tends to be larger as the γ-rays are closer to the high energy peak of the spectral energy distribution (SED). No correlation of variability index found for BL Lacertae objects implies that variability behavior may differ below and above the peak energy.