Abstract
Abstract Blazars show extreme observational properties that are due to the beaming effect with the jet being close to the line of sight. It was found that the observed luminosity is anticorrelated with the synchrotron peak frequency but the debeamed luminosity and the frequency is positively correlated. In this work, we revisit this correlation for a large sample of 255 blazars from the fourth Fermi catalog with available Doppler factors. Our analysis comes to the following conclusions. (1) The observed radio, X-ray, γ-ray, and synchrotron peak luminosity are all anticorrelated with the peak frequency, but the debeamed luminosity is positively correlated with the debeamed peak frequency. The anticorrelation is due to a selection effect or a beaming effect. (2) The Compton dominance parameter is correlated with both the bolometric luminosity and Doppler factor, implying that the more highly Compton-dominated sources are more luminous. (3) The bolometric luminosity can be represented by the γ-ray luminosity for Fermi blazars.
Highlights
Active galactic nuclei (AGNs) are very interesting, their specially observational properties have attracted many astronomers
There are two subclasses for blazars: flat spectrum radio quasars(FSRQs) and BL Lacertae objects (BLs), the latter can be classified further as radio selected BL Lacertae objects (RBLs) and X-ray selected BL Lacertae objects-XBLs from surveys, or high-peaked BL Lacertae objects (HBLs) and low-peaked BL Lacertae objects (LBLs) from spectral energy distribution-SED
We will compile a sample with available radio Doppler factors and the γ-ray detections, and discuss the dependence of the γ-ray luminosity on the Doppler factors
Summary
Active galactic nuclei (AGNs) are very interesting, their specially observational properties have attracted many astronomers. As proposed by Dermer (1995), the dependence of the γ-ray flux on the Doppler factor can be used to investigate the γ-ray emission mechanism, different emission mechanism has different dependence of the flux density (Sγ) on the γ-ray Doppler factor (δγ ), namely Sγ ∝ δ3+α for a synchrotron self-Compton (SSC) model, and Sγ ∝ δ4+2α for an external Compton (EC) model. These indexes (3+α and 4+2α) are true for transient emission features, whereas in a steady jet, the indexes are smaller by one, namely, 2+α and 3+2α.
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