Coordinated observations of OJ 287 at radio and optical wavelengths

Kinman, T. D.; Wardle, J. F. C.; Conklin, E. K.; Andrew, B. H.; Harvey, G. A.; MacLeod, J. M.; Medd, W. J.

doi:10.1086/111549

Cited by 26 publications

(11 citation statements)

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“…Kinman et al (1974) reported that there are some indications of a radio flux increase after the optical and infrared outburst, O'Dell et al (1978) also reported that the 3 mm flux was related with that in the optical and infrared. But it is strange that no corresponding outburst was observed in radio band during OJ-94 project optical outburst.…”

Section: Variability Correlationmentioning

confidence: 97%

The infrared and optical variability of OJ 287

Jiang

Adam

Xie

et al. 1998

Astron. Astrophys. Suppl. Ser.

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Section: Variability Correlationmentioning

confidence: 97%

The infrared and optical variability of OJ 287

Jiang

Adam

Xie

et al. 1998

Astron. Astrophys. Suppl. Ser.

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“…Searching for reasons for this, Valtonen (2007) proposed a new orbit solution for the precessing binary black hole model. Besides the long‐term optical variability, OJ 287 has also exhibited some unruled fluctuations of brightness on time‐scales ranging from minutes (Carrasco, Dultzin‐Hacyan & Cruz‐Gonzalez 1985; Zhang et al 2007) to about a week (Kinman et al 1974). These variabilities cause confusion.…”

Section: Introductionmentioning

confidence: 99%

Long-term optical spectra variability of BL Lacertae object OJ 287

Zheng¹,

Zhang²,

Bi³

et al. 2008

Monthly Notices of the Royal Astronomical Society

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Based on the long‐term data in the literature, we present evidence for long‐term optical spectral index variability behaviour for BL Lacertae object OJ 287. First we find that the optical spectral index variability period of BL Lacertae object OJ 287 is in agreement with the optical flux variability period of about 11.96 yr. It is considered that different processes induce optical variability, and each process should have a definite signature in the spectral index, thus leading to the periodicity of the spectral index. We also find that the time lag between the optical spectral index and the optical flux density is half of the optical flux variability period. This result tends to support the argument that when the brightness of the long‐term variations increases, the optical spectra become bluer. These variations can be explained by energy loss of the electrons during the outburst. We show that the spectral index is different during the flares compared with outside the flares; between the first and second flare peaks of the superflares, the spectrum shapes are different. Disparate processes possibly induce the two peaks of OJ 287.

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“…Individual objects have been studied in many papers, e.g. 3C 120 (Usher 1972), BL Lac (Andrew et al 1974;Tornikoski et al 1994a), PKS 0420-01 (Dent et al 1979), 3C 446 (Bregman et al 1988), OJ 287 (Kikuchi et al 1973;Kinman et al 1974;Usher 1979;Valtaoja et al 1987) and AO 0235+164 (Balonek & Dent 1980;Roy et al 2000;Raiteri et al 2001).…”

Section: Introductionmentioning

confidence: 99%

Correlated radio and optical variations in a sample of AGN

Hanski

Takalo

Valtaoja

2002

A&A

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Abstract. Radio light curves of 20 sources from the Metsähovi monitoring program are compared with optical light curves collected from the literature. The Discrete Correlation Function analysis is applied to the data sets. A new qualitative method to study correlations is introduced, where the radio light curves are replaced by model light curves consisting of exponential outbursts. The optical flux level is compared to the phase and flux level of the model flares. Seven sources show clear correlations using the DCF analysis with six more showing a possible correlation between optical and radio events with time lags from zero to several hundred days. For twelve sources at least one simultaneous optical and radio event is seen. For eleven sources, when comparing optical flux levels with the phase of the model radio outbursts, the optical flux levels were high at the peak of the model radio outbursts. For sixteen sources, when comparing the optical flux level with the radio model flare flux level, the optical flux level was high when radio flux level was high, as well.

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Coordinated observations of OJ 287 at radio and optical wavelengths

Cited by 26 publications

References 0 publications

The infrared and optical variability of OJ 287

The infrared and optical variability of OJ 287

Long-term optical spectra variability of BL Lacertae object OJ 287

Correlated radio and optical variations in a sample of AGN

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