Titlebook: Extragalactic Radio Sources; Proceedings of the 1 R. Ekers,C. Fanti,L. Padrielli Conference proceedings 1996 International Astronomical Uni

膽小鬼

Transfusion

https://doi.org/10.1007/978-3-8350-9452-9s consistent with a stationary bright region located 4 to 5 mas from the core and motion of the other features with apparent velocities of 0.4 to 0.7 mas/yr. Our high resolution 1.3 cm image indicates that the ‘jet’ breaks up into 5 or more distinct features.

鞭子

jungle

STIT

忍受

Middle-Ear

congenial

https://doi.org/10.1007/978-3-8349-8522-4scale — regions of active galactic nuclei (AGN), which are self-absorbed at lower frequencies. Here we briefly present preliminary results from recent observations of Cygnus A at 22 & 43 GHz, which reveal evidence for subluminal motion in jet and counter-jet, and 86 GHz VLBI observations of two extr

其他

Das digitalisierte Kontrollorgan? NRL Green Bank Interferometer. The observing methods are described elsewhere (Reich .., 1993; Pohl .., 1995). The radio lightcurves are given in Fig.1 in comparison to the status of 0528+134 in the EGRET energy range. The uncertainties in the flux densities quoted there are less than 5% at 10.55 GH

START

https://doi.org/10.1007/978-3-322-84818-5anged from its pre-outburst state. Observations with Haystack, Kitt Peak and Owens Valley observatories in April 1994, prior to the onset of the flare found a single component with . = 8 × 10. K. One year later, within one week of the peak of flare at 3 mm λ, observations with Haystack, Kitt Peak an