OJ 287 is one of the best studied blazars (e.g. Takalo 1994). After
constructing its historical light curve
Sillanpää
et al. (1988) found a periodicity in the strong optical outbursts of
the object (with years) and predicted that the
next large flare should occur in 1994. This prediction was based on a
binary black hole model for OJ 287 (see also Lehto & Valtonen 1996).
Verification of this prediction is one of the goals of the
international OJ-94 project,
during which the object has been intensively monitored at all
available wavelengths since fall 1993 (Kidger et al. 1998).
In November 1994 the brightness increase in the
IR-optical and UV regions was observed, confirming the
prediction (Sillanpää et al. 1996a). This is the first case when
a predicted photometric behaviour of extragalactic object has
been confirmed. Another large and expected flare was observed
during December 1995 (Sillanpää et al. 1996b).
By current understanding of the blazar emission the most of it at lower frequencies (in radio bands perhaps all) is due to synchrotron radiation coming from the jet (e.g. Urry & Padovani 1996). The synchrotron nature of the emission is supported by the observed power-law type spectra and the strong and variable polarization (e.g. Efimov & Shakhovskoy 1996).
This paper is devoted to the analysis of the OJ 287 colour behaviour in IR-optical-UV region before and during the outburst.
Copyright The European Southern Observatory (ESO)