MOJAVE. XVII. Jet Kinematics and Parent Population Properties of Relativistically Beamed Radio-loud Blazars

By M. Lister, D. Homan, T. Hovatta, K. Kellermann, S. Kiehlmann, Y. Kovalev, W. Max-Moerbeck, A. Pushkarev, A. Readhead, E. Ros and 1 more. Astrophysical Journal, 2019

146 citations recorded by the source corpus.

We present results from a parsec-scale jet kinematics study of 409 bright radio-loud active galactic nuclei (AGNs) based on 15 GHz Very Long Baseline Array (VLBA) data obtained between 1994 August 31 and 2016 December 26 as part of the 2 cm VLBA survey and Monitoring Of Jets in Active galactic nuclei with VLBA Experiments (MOJAVE) programs. We tracked 1744 individual bright features in 382 jets over at least 5 epochs. A majority (59%) of the best-sampled jet features showed evidence of accelerated motion at the >3σ level. Although most features within a jet typically have speeds within ∼40% of a characteristic median value, we identified 55 features in 42 jets that had unusually slow pattern speeds, nearly all of which lie within 4 pc (100 pc deprojected) of the core feature. Our results, combined with other speeds from the literature, indicate a strong correlation between apparent jet speed and synchrotron peak frequency, with the highest jet speeds being found only in low-peaked AGNs. Using Monte Carlo simulations, we find best-fit parent population parameters for a complete sample of 174 quasars above 1.5 Jy at 15 GHz. Acceptable fits are found with a jet population that has a simple unbeamed power-law luminosity function incorporating pure luminosity evolution and a power-law Lorentz factor distribution ranging from 1.25 to 50 with slope −1.4 ± 0.2. The parent jets of the brightest radio quasars have a space density of 261 ± 19 Gpc−3 and unbeamed 15 GHz luminosities above ∼1024.5 W Hz−1, consistent with FR II class radio galaxies.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c9a580d366ec600eba222c847bf00d536fe2165f

Citations in the corpus

• Open Questions in Cosmic-Ray Research at Ultrahigh Energies (2019, unknown): “Here, R = l · Ŵ , with l the comoving size of the source, and Ŵ the Lorentz factor of the motion, which is thought to be Ŵ ∼ 10 − 50 in AGN jets (e.g., Lister et al., 2019), and Ŵ ∼ 10 − 1, 000 in GRBs.”