Abstract
ABSTRACT The jet in active galactic nuclei (AGN) is a key ingredient in understanding the co-evolution of galaxies and their central supermassive black holes (SMBHs). Unfortunately, the mechanism of jet launching and collimation is still elusive. The observational evidence of decreasing radio loudness with increasing Eddington ratio implies that the jet should be coupled with the accretion process. To further explore the relationship between the jet and accretion, it is necessary to extend our knowledge of the jet to an extreme end of the Eddington ratio distribution of AGN. Using Very Long Baseline Array (VLBA), we report the detection of the parsec-scale radio structure in Mrk 335, a radio-quiet narrow-line Seyfert 1 galaxy with an Eddington ratio close to/above unity. The VLBA image at 1.5 GHz reveals an elongated structure extending ∼20 pc in north–south direction with a peak flux density of 1.98 ± 0.05 mJy beam−1 and radio brightness temperatures as high as 6 × 107 K. This feature provides a strong evidence of a parsec-scale (bipolar) jet launched from a highly accreting SMBH. We discuss the result by comparing Mrk 335 with other highly accreting systems, e.g. Galactic black holes and tidal disruption events, and recall the discovery of collimated corona in the vicinity of SMBH in Mrk 335 by previous X-ray observations, whose relation to the parsec-scale radio jet should be explored by future simultaneous X-ray spectroscopy and high resolution radio observations.
Highlights
The collimated outflowing plasma, termed as ‘jet’, launched from active galactic nuclei (AGN) is suggested to be one of the important forms of AGN feedback that regulates the coevolution of supermassive black hole (SMBH) and their host galaxy (Fabian 2012; Kormendy & Ho 2013)
The observational evidence of a strong anticorrelation between the radio loudness parameter R1 and the bolometric luminosity expressed in Eddington units, i.e. Eddington ratios λEdd, implies coupling of the jet and accretion process (Ho 2002, 2008; Greene, Ho & Ulvestad 2006; Sikora, Stawarz & Lasota 2007; Yang et al 2020); the launch of jet may be dependent on the Eddington ratio and underlying physics such as the mass accretion rate, the state of accretion disc, and the growth of SMBH
The naturally weighted images of Mrk 335 observed by the VLA Aarray configurature at 1.4 and 8.4 GHz, and by the Very Long Baseline Array (VLBA) at 1.5 GHz are shown in Figs 1(a), (b), and (c), respectively
Summary
The collimated outflowing plasma, termed as ‘jet’, launched from active galactic nuclei (AGN) is suggested to be one of the important forms of AGN feedback that regulates the coevolution of supermassive black hole (SMBH) and their host galaxy (Fabian 2012; Kormendy & Ho 2013). 2002), indicating that not all of the AGN launch jets This raises the questions of why we only observe jets in a small fraction of AGN and how the jets are formed. The observational evidence of a strong anticorrelation between the radio loudness parameter R1 and the bolometric luminosity expressed in Eddington units, i.e. Eddington ratios λEdd, implies coupling of the jet and accretion process (Ho 2002, 2008; Greene, Ho & Ulvestad 2006; Sikora, Stawarz & Lasota 2007; Yang et al 2020); the launch of jet may be dependent on the Eddington ratio and underlying physics such as the mass accretion rate, the state of accretion disc, and the growth of SMBH. With milli-arcsecond (mas) resolution radio images achieved by very long baseline interferometry (VLBI), it was found that some of the radio-quiet AGN reveal compact parsec-scale
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
