The blazar S4 0133+47 in a flaring state with R~16.1 magnitude
ATel #15626; V. V. Vlasyuk, O. I. Spiridonova, A. S. Moskvitin, O. A. Maslennikova (Special Astrophysical Observatory of the Rus. Ac. Sci.)
on 24 Sep 2022; 14:02 UT
Credential Certification: Alexander Moskvitin (mosk@sao.ru)
Subjects: Optical, Blazar
The blazar S4 0133+47 is observing by SAO RAS team on a regular basis in search of possible correlation between its optical and radio activity events using by 1-meter Zeiss reflector, equipped with CCD photometer. Since January 2021 we have started more intense optical observations with two SAO RAS telescopes: the 1-meter reflector and the 0.5-meter RC500 reflector, manufactured by Russian company ASTROSIB. We have observed object with RC500 telescope in R passband few times every week within its visibility period. The observations with Zeiss-1000 were less extensive and realized according to telescope's time schedule.
Our data, taken with both telescopes in last July-August showed that it's brightness had been varied about R~17.4 magnitude till July 23th. Within 5-day interval between July 23th and July 29th the blazar became brighter up to R~16.9 mag. New period of a quasistability was longed about 1 month --- our data from 0.5-m telescope (Sep 10th) still gave its R-magnitude as 16.9+/-0.1. Our next observations, provided by 1-m reflector on September 17th, demonstrated new increase of S4 0133+47 brightness --- at 0.5 magnitudes again. At least, the current maximum of the blazar brightness was reached at R=16.07+/-0.02 magnitude at epoch MJD=59842.0 (September 19/20 night). Our last data from the both telescopes, taken over the last night - September 23/24 --- gave current magnitude as R=16.15+/-0.02 magnitudes. It indicates on possible new growth of blazar brightness, as was noted in 2013 at ATel#4779.
All photometrical data were calibrated by us using by stars from standard field 3C66A (Gonzales-Perez et al., AJ, 122, 2001). The absolute accuracy of our estimates is about 0.02 magnitudes.
More accurate reduction is necessary. We strongly encourage further multi-wavelength observations.
