Kinematics of the Active Radio Source at The Nucleus of NGC1275 (3C84)

Details Kinematics of the Active Radio Source at The Nucleus of NGC1275 (3C84) Kinematics of the Active Radio Source at The Nucleus of NGC1275 (3C84)

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21740807k&link_type=abstract

American Astronomical Society, AAS Meeting #217, #408.07; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

NGC1275 (3C84) was one of the earliest known radio galaxies and is also the site of moderately strong and variable gamma-ray emission. For the past 15 years we have used the VLBA at 2 cm wavelength to follow the internal motions in this AGN. Previously we used European and US antennas at 2.8 cm to extend our kinematic study as far back as the early 1970s. Combining these data sets shows a systematic motion of a southern feature receding from the core at 0.28 ± 0.04 mas/yr or v/c = 0.32 ± 0.05, while the more slowly moving northern feature is moving at 0.10 ± 0.02 mas/yr or v/c = 0.11±0.02. The calculated ejection time of the southern feature occurred in the mid 1950s close to the start of the large centimeter radio outburst first observed at the UMRAO. From the observed motions, we find an intrinsic velocity of 0.5c at an angle of 20 degrees to the line of sight. The corresponding Lorentz factor is only 1.2 with Doppler factors of 1.6 and 0.6 for the approaching and receding features respectfully. Thus Doppler boosting is small, and so the intrinsic luminosity is close to the observed value of 1026 W/Hz. It is not clear how the this mildly relativistic jet of this powerful radio and gamma-ray galaxy fits into the broader picture of ultrarelativistic jets feeding the powerful radio lobes, unless the radio observations refer to a relatively slowly moving outer jet surrounding a faster inner spine whose directed radio emission is beamed away from the observer.

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