On the intraday variability of O.j 287

Wingert, D. W.; McGimsey, B. Q.; Anderson, Eva; Mullikin, T. L.; Folsom, G. H.

doi:10.1086/111886

Cited by 5 publications

(2 citation statements)

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“…OJ 287 was observed more than 100 yr ago starting in 1894 (Visvanathan & Elliot 1973;Takalo 1994). The data used in the present paper are from the following literature (Kurochkin 1971a,b;Tsessevich 1972;Miller et al 1976;Pollock et al 1979;Smith et al 1982;Lloyd 1984;Sillanpää et al 1996a), the compiled data (Fan et al 1998b, Fan & Lin 2000 and our monitoring results (Qian & Tao 2003;Fan et al 2009a). The data are shown in Figure 1.…”

Section: Datamentioning

confidence: 93%

Long-term variation time scales in OJ 287

Fan¹,

Liu²,

Qian³

et al. 2010

Res. Astron. Astrophys.

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The light curve data from 1894 to 2008 are compiled for the BL Lacertae object OJ 287 from the available literature. Periodicity analysis methods (the Discrete Correlation Function-DCF, the Jurkevich method, the power spectral (Fourier) analysis, and the CLEANest method) are performed to search for possible periodicites in the light curve of OJ 287. Significance levels are given for the possible periods. The analysis results confirm the existence of the 12.2 ± 0.6 yr time scale and show a hint of a ∼53 yr time scale. The 12.2±0.6 yr period is used as the orbital period to investigate the supermassive binary black hole system parameters.

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Section: Datamentioning

confidence: 93%

Long-term variation time scales in OJ 287

Fan¹,

Liu²,

Qian³

et al. 2010

Res. Astron. Astrophys.

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“…It has been included in almost all optical and radio monitoring campaigns conducted on blazars (Takalo 1994). The historical light curves have been compiled by Craine & Warner (1973);Visvanathan & Elliot (1973);Miller et al (1976); Gadia & Roser (1982); Webb et al (1988); Sillanpää et al (1988); Kidger et al (1992); Takalo (1994). Takalo (1994) has collected all the available observations for this source published by the end of 1992, and found that the total range of variability observed for this object was 18.0 − 12.5 mag in the B band, more than 5 mag.…”

Section: Pks 0754+101mentioning

confidence: 99%

The intraday variability in the radio-selected and X-ray-selected BL Lacertae objects

Bai

Xie

et al. 1998

Astron. Astrophys. Suppl. Ser.

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Abstract. Seven BL Lac objects have been photometrically observed in an effort to study the difference of optical intraday variability between the radio-selected BL Lac objects (RBLs) and X-ray-selected BL Lac objects (XBLs). The objects we observed are selected arbitrarily. They are four RBLs, PKS 0735+178, PKS 0754+101, OJ 287 and BL Lac, and three XBLs, H 0323+022, H 0548−322 and H 2154−304. During the observation all of them exhibited microvariation, and H 0323+022 and H 0548−322 sometimes showed brightness oscillation. PKS 0735+178 and BL Lac were in their faint states and not very active. It seems that RBLs do not show microvariability more frequently than XBLs.

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OJ 287: The Rosetta stone of blazars

Takalo¹

1994

Vistas in Astronomy

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On the intraday variability of O.j 287

Cited by 5 publications

References 0 publications

Long-term variation time scales in OJ 287

Long-term variation time scales in OJ 287

The intraday variability in the radio-selected and X-ray-selected BL Lacertae objects

OJ 287: The Rosetta stone of blazars

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