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

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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

[FIGURE] 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.

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© European Southern Observatory (ESO) 2000

Online publication: June 8, 2000