Optical monitoring of BL Lac object S5 0716+714 and FSRQ 3C 273 from 2000 to 2014

Yuan, Yu-Hai; Fan, J. H.; Tao, Jun; Qian, Bochen; Costantin, D.; Xiao, H. B.; Pei, Z. Y.; Lin, Chao

doi:10.1051/0004-6361/201630338

Cited by 23 publications

(27 citation statements)

References 78 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Several authors have reported a similar behaviour to what we have noticed. Agarwal et al (2016) and Yuan et al (2017) notice a very mild trend of larger A var when the source was brighter. Montagni et al (2006) estimated rates of magnitude variation for 102 nights during 1996-2003 for S5 0716+71 and found faster (∼ 0.08/h) rates when source was brighter (R < 13.4), though the dependence was weak, compared to average rate of change (∼ 0.027mag/h) irrespective of the state of the source brightness.…”

Section: Variability Amplitude (Avar) and The Brightness State Of Sourcementioning

confidence: 96%

“…Agarwal et al (2016), during their 130 day study, found a change of about 0.3 mag in spectral color with no significant dependence on the time or brightness phase. Yuan et al (2017) reported a complex pattern for spectral index with time without any specific trend during the period 2000-2014. The color variations are caused by differential cooling of energetic electrons behind the shock front.…”

Section: Spectral Behavior Of S5 0716+71mentioning

confidence: 98%

See 1 more Smart Citation

Optical Variability in IBL S5 0716+714 during the 2013–2015 Outbursts

Kaur

Baliyan

Chandra

et al. 2018

View full text Add to dashboard Cite

With an aim to explore optical variability at diverse timescales in BL Lac source S5 0716+714, it was observed for 46 nights during 2013 January 14 to 2015 June 01 when it underwent two major outbursts. The observations were made using the 1.2-m Mount Abu InfraRed Observatory telescope mounted with a CCD camera. On 29 nights, the source was monitored for more than two hours, resulting in 6256 data points in R-band, to check for the intra-night variability. Observations in B, V and I bands with 159, 214, and 177 data points, respectively, along with daily averaged R-band data are used to address inter-night and long-term variability and the color behavior of S5 0716+71. The study suggests that the source shows significant intra-night variability with a duty cycle of more than 31% and night-to-night variations. The average brightness magnitudes in B, V, R & I bands were found to be 14.42(0.02), 14.02(0.01), 13.22(0.01) & 13.02(0.03), respectively, while S5 0716+714 was historically brightest with R = 11.68 mag on 2015 January 18, indicating that source was in relatively high state during this period. A mild bluer when brighter behavior, typical of BL Lacs, supports the shock-in-jet model. We notice larger amplitudes of variation when the source was relatively brighter. Based on the shortest time scale of variability and causality argument, upper bound on the size of the emission region is estimated to be 9.32 × 10 14 cm and the mass of the black hole to be 5.6 × 10 8 M .

show abstract

Section: Variability Amplitude (Avar) and The Brightness State Of Sourcementioning

confidence: 96%

Section: Spectral Behavior Of S5 0716+71mentioning

confidence: 98%

Optical Variability in IBL S5 0716+714 during the 2013–2015 Outbursts

Kaur

Baliyan

Chandra

et al. 2018

View full text Add to dashboard Cite

show abstract

“…The described change in δ would be reflected on the long-term light curve of the object, which would have prominent peaks. There are no such peaks on the observed light curve (e.g., Raiteri et al 2003;Dai et al 2013Dai et al , 2015Liao et al 2014;Yuan et al 2017;Xiong et al 2020). This could be explained by the fact that other peaks on the light curve are formed by physical processes, but then there is no enough evidence that variability caused by geometrical effects is not superimposed on changes in brightness that are the result of physical processes.…”

Section: Discussionmentioning

confidence: 99%

A geometrical interpretation for the properties of multiband optical variability of the blazar S5 0716+714

Butuzova

2020

Preprint

View full text Add to dashboard Cite

We present the results of multiband observations of the blazar S5 0716+714 intra-night variability performed during 23 nights in the period from 04.2014 through 04.2015. The bluer-when-brighter trend is detected in both intra-and inter-night data. We assume that the jet component crossing the region where the medium becomes transparent to the optical radiation forms almost all optical emission of S5 0716+714. Deviations of some parts of the component from the general trajectory of the component can cause the Doppler factor of these parts to increase. Various maximum Doppler factors achieved by these parts of the component and different volumes occupied by them with the concave synchrotron self-absorption spectrum result in both the observed various color index behavior in variability and explain the absence of dependence of the bluer-when-brighter behavior on the object magnitude. We estimated spectral maximum frequencies from intra-and inter-night data. Both the agreement of the obtained values of ν m ≈ (1.0 − 2.5) • 10 14 GHz and the fact that ν m is less than the frequencies of optical observations confirm our assumption about the nature of the blazar S5 0716+714 region radiating in the optical range.

show abstract

“…Periodic light curve candidates also include a blazar OJ 287, with 11.5-year period, as the most famous SMBBH candidate [4,5], the quasar PG 1302-102 (6 year period, [29]), the blazar PG 1553+113 (2 year period, [40]), a 13-and 21-year periodicity found in 3C 273 [12,13].…”

Section: Supermassive Black Hole Binariesmentioning

confidence: 99%

“…Unfortunately, most AGN monitoring campaign time intervals are not sufficiently long for detecting periodicity in optical domain of spectra, since expected orbiting time scales in AGN ADs that would affect the optical part of the spectrum are of the order of years and decades. Luckily, significant periodicities are detected in several AGN which are extensively monitored for sufficiently long time, such as OJ287 [4,5], NGC 4151 [6][7][8], NGC 5548 [9,10], Ark 120 [11], 3c273 [12,13].…”

Section: Introductionmentioning

confidence: 99%

On the Time Scales of Optical Variability of AGN and the Shape of Their Optical Emission Line Profiles

Bon

Marziani

Jovanović

et al. 2019

Atoms

View full text Add to dashboard Cite

The mechanism of the optical variability of active galactic nuclei (AGN) is still very puzzling. It is now widely accepted that the optical variability of AGN is stochastic, producing red noise-like light curves. In case they were to be periodic or quasi-periodic, one should expect that the time scales of optical AGN variability should relate to orbiting time scales of regions inside the accretion disks with temperatures mainly emitting the light in this wavelength range. Knowing the reverberation scales and masses of AGN, expected orbiting time scales are in the order of decades. Unfortunately, most of monitored AGN light curves are not long enough to investigate such time scales of periodicity. Here we investigate the AGN optical variability time scales and their possible connections with the broad emission line shapes.

show abstract

Optical monitoring of BL Lac object S5 0716+714 and FSRQ 3C 273 from 2000 to 2014

Cited by 23 publications

References 78 publications

Optical Variability in IBL S5 0716+714 during the 2013–2015 Outbursts

Optical Variability in IBL S5 0716+714 during the 2013–2015 Outbursts

A geometrical interpretation for the properties of multiband optical variability of the blazar S5 0716+714

On the Time Scales of Optical Variability of AGN and the Shape of Their Optical Emission Line Profiles

Contact Info

Product

Resources

About