Optical Variability and Periodicity Analysis for Blazars. I. Light Curves for Radio‐selected BL Lacertae Objects

Jiang, Fan; Lin, R. G.

doi:10.1086/308996

Cited by 85 publications

(82 citation statements)

References 100 publications

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“…We used the magnitudes of the field stars published in Villata et al (1998) to estimate the mean standard magnitude for PKS 0048−097 in each filter during our observations; resulting in 15.84 ± 0.05 mag in V, 15.44 ± 0.04 in R band the first night, and 15.89 ± 0.05 mag in V, 15.99 ± 0.05 in R band the second night. These magnitudes are in agreement with those presented by Fan & Lin (2000), who found V = 15.86 and R = 15.40. In the present work, this object showed small amplitude variability in the R band.…”

Section: Resultssupporting

confidence: 93%

“…Using the comparison stars and standard magnitudes published by Fiorucci et al (1998), the mean standard magnitudes for PKS 0754+100 are 16.72 ± 0.05 mag in V and 16.22 ± 0.05 mag in R bands. Compared with Fan & Lin (2000), who present mean values of V = 15.40 and R = 14.27, our observations clearly correspond to a minimum activity state.…”

Section: Resultssupporting

confidence: 50%

“…With the magnitudes given by Fiorucci & Tosti (1996) and González-Pérez et al (2001), we obtained mean standard estimates of 14.93±0.01 in V and 14.47±0.01 in R the first night, and 14.91 ± 0.01 in V, 14.44 ± 0.01 in R the second night. Fan & Lin (2000) propose a periodic light curve for PKS 0851+202, with a period of 12 years. Our results are in agreement with the magnitudes expected for this periodic variability and with the values observed by Bach et al (2007).…”

Section: Resultsmentioning

confidence: 99%

“…In standard magnitudes, taking mean values and using the magnitudes given by Fiorucci et al (1998), this detected variation resulted in a decrease in magnitude from 17.94 ± 0.04 mag in V and 17.10 ± 0.05 mag in R the first night to 17.23 ± 0.04 in V and 16.57 ± 0.04 in R the second night. According to the light curve given in Fan & Lin (2000), these values correspond to a minimum of activity.…”

Section: Pks 1510−089mentioning

confidence: 99%

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Optical flux behaviour of a sample ofFermiblazars

Marchesini

Andruchow

Cellone

et al. 2016

A&A

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Aims. We aim at investigating the time-behaviour of a sample of gamma-ray blazars. We present the results from a 13 monthlong optical photometry monitoring campaign of the blazars PKS 0048−097, PKS 0754+100, [HB89] 0827+243, PKS 0851+202, PKS 1253−055, PKS 1510−089, PKS 1749+096, PKS 2230+114 and PKS 2251+158. Methods. We analyse the variability of each object, focusing on different time-scales (long term, short term, and microvariability), in an attempt to achieve a statistical comparison of the results. Results. After applying a geometric model to explain the variability results, we found that it is possible that a slight change in the direction of the jet generates the variations detected in some objects during this campaign.

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Section: Resultssupporting

confidence: 93%

Section: Resultssupporting

confidence: 50%

Section: Resultsmentioning

confidence: 99%

Section: Pks 1510−089mentioning

confidence: 99%

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Optical flux behaviour of a sample ofFermiblazars

Marchesini

Andruchow

Cellone

et al. 2016

A&A

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“…Similar trend was found in V passband as shown in Figure 2 from which it is evident that the data sets for these events in both the bands are consistent with each other. The object reached the faintest level of 14.07 mag in R passband which is still ∼ 1 mag brighter than its historical maximum magnitude as reported by Fan & Lin (2000). While on the last day of our observation span i.e., on 22 November, source was found to be the brightest with a magnitude of 15.08, 14.15, 13.4, and 1.624 in B, V, R, and I passbands, respectively, indicating that the source might go into flaring state in near future.…”

Section: Flux and Colour Variability Resultsmentioning

confidence: 47%

Multiband optical variability studies of BL Lacertae

Agarwal¹,

Gupta²

2015

Monthly Notices of the Royal Astronomical Society

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We monitored BL Lacertae for 13 nights in optical B, V, R, and I bands during October and November 2014 including quasi-simultaneous observations in V and R bands using two optical telescopes in India. We have studied multi-band optical flux variations, colour variation and spectral changes in this blazar. Source was found to be active during the whole monitoring period and showed significant intraday variability on 3 nights in V and R filters while displayed hints of variability on 6 other dates in R passband and on 2 nights in V filter. From the colour-magnitude analysis of the source we found that the spectra of the target gets flatter as it becomes brighter on intra-night timescale. Using discrete correlation technique, we found that intraday light curves in both V and R filters are almost consistent and well correlated with each other. We also generated spectral energy distribution (SED) of the target using the B, V, R, and I data sets for all 13 nights which could help us investigate the physical process responsible for the observed variations in BL Lacertae objects. We also discuss possible physical causes of the observed spectral variability.

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The broad band spectral index of blazars in a low state

Zheng

Zhang

2007

Astrophys Space Sci

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Using the broad band spectral index of 164 blazars in a low state, we studied the possible correlation between different broad band spectral index (α r.ir We also studied the possible correlation between different broad band spectral index of high-frequency peaked Bl Lac object (HBL), low-frequency peaked BL Lac object (LBL) and flat spectral radio quasars (FSRQs), respectively. The strong anticorrelations were found between α r.o and α o.γ , between α r.o and α x.γ in a low state for our blazar sample. For LBL and FSRQs, the strong anti-correlations were found between α r.ir and α ir.x , between α r.o and α o.x , and between α r.o and α o.γ in a low state. Based on these results, we suggested that the seed photons of the γ -ray drive from both the jet and the external accretion disk or the broad-line region, and that the subclasses of blazars seem to the different emission mechanism.

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Optical Variability and Periodicity Analysis for Blazars. I. Light Curves for Radio‐selected BL Lacertae Objects

Cited by 85 publications

References 100 publications

Optical flux behaviour of a sample ofFermiblazars

Optical flux behaviour of a sample ofFermiblazars

Multiband optical variability studies of BL Lacertae

The broad band spectral index of blazars in a low state

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