Bibcode
Takalo, L. O.; Sillanpaeae, A.; Pursimo, T.; Lehto, H. J.; Nilsson, K.; Teerikorpi, P.; Heinaemaeki, P.; Lainela, M.; Kidger, M. R.; de Diego, J. A.; Gonzalez-Perez, J. N.; Rodríguez-Espinosa, J. M.; Mahoney, T.; Boltwood, P.; Dultzin-Hacyan, D.; Benitez, E.; Turner, G. W.; Robertson, J. W.; Honeycut, R. K.; Efimov, Yu. S.; Shakhovskoy, N.; Charles, P. A.; Schramm, K. J.; Borgeest, U.; Linde, J. V.; Weneit, W.; Kuehl, D.; Schramm, T.; Sadun, A.; Grashuis, R.; Heidt, J.; Wagner, S.; Bock, H.; Kuemmel, M.; Pfeiffer, M.; Heines, A.; Fiorucci, M.; Tosti, G.; Ghisellini, G.; Raiteri, C. M.; Villata, M.; de Francesco, G.; Bosio, S.; Latini, G.; Poyner, G.; Aller, M. F.; Aller, H. D.; Hughes, P.; Valtaoja, E.; Teraesranta, H.; Tornikoski, M.
Bibliographical reference
Astronomy and Astrophysics Supplement, v.120, p.313-321
Advertised on:
12
1996
Citations
43
Refereed citations
35
Description
We present results from a two year intensive monitoring of BL Lac object
3C 66A (PKS 0219+428). This object was observed in outburst during these
two years. It reached the brightest ever observed magnitude on V=13.59
(1.2.1995) and on K=10.59 (15.2.1994). The optical and infrared light
curves are characterised by randomly distributed fast flares, lasting a
few days and well defined outbursts lasting a week or two. On top of
these flares we can occasionally see small amplitude microvariability.
No clear correlation can be found between the spectral behaviour and the
occurrence of these flares. In the radio bands 3C 66A was quite faint
and very stable compared to the optical variations. The light curves
will be presented with preliminary analysis and discussions on the
possible causes for the observed variations.