Astron. Astrophys. 358, 451-461 (2000)

6. Flux density variations of the VLBI-components

The flux densities of the compact components as functions of time are shown in Fig. 16, which indicates

Fig. 16. Relative flux density variations during cycle C3. Filled circles and left y-axis correspond to total flux densities after subtraction of the long-term trend; open symbols and right y-axis correspond to VLBA and VLBI data: open circles - core, squares - component B. 8 GHz component B is shifted up for convenience.

that at 8 GHz the main maximum in the total flux density curve coincides with the maximum in the core flux and peak 2 with the maximum in the flux of component B. Unfortunately, both peaks 1 and 2 at 37 GHz are located within gaps in the VLBA observations at 43 GHz, so we can only follow a slow decline of the core flux density and a possible secondary maximum of the flux density of component B between 1996.9 and 1997.58.

© European Southern Observatory (ESO) 2000

Online publication: June 8, 2000
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