Optical intra-day variability in 3C 66A: a decade of observations

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dc.contributor.author Kaur, Navpreet
dc.contributor.author Sameer
dc.contributor.author Kiran, S. Baliyan
dc.contributor.author Ganesh, Shashikiran
dc.date.accessioned 2017-06-05T12:29:44Z
dc.date.available 2017-06-05T12:29:44Z
dc.date.issued 2017-05
dc.identifier.citation Kaur, Navpreet; Sameer; Baliyan, Kiran S.; and Ganesh, S., “Optical intra-day variability in 3C 66A: a decade of observations”, Monthly Notices of the Royal Astronomical Society, DOI: 10.1093/mnras/stx965, vol. 469, no. 2, pp. 2305-2312, May 2017. en_US
dc.identifier.issn 1365-2966
dc.identifier.issn 0035-8711
dc.identifier.uri https://repository.iitgn.ac.in/handle/123456789/2963
dc.identifier.uri http://dx.doi.org/10.1093/mnras/stx965
dc.description.abstract We present results based on the observations of the blazar 3C 66A from 2005 November 06 to 2016 February 14 in the BVR and I broad-bands using the 1.2-m telescope of the Mt Abu InfraRed Observatory (MIRO). The source was observed on 160 nights; on 89 of these nights, it was monitored for more than 1 h to check for the presence of any intra-day variability (IDV). The blazar 3C 66A exhibited significant variations in the optical flux on short- and long-term time-scales. However, unlike the highly variable S5 0716+71, it showed an IDV duty cycle of about 8 per cent only. Our statistical studies suggest IDV time-scales ranging from ∼37 min to about 3.12 h and, in one case, the possibility of quasi-periodic variations with a characteristic time-scale of ∼1.4 h. The IDV amplitudes in the R band were found to vary from 0.03 mag to as much as 0.6 mag, with a larger amplitude of variation when the source was relatively fainter. The typical rate of the flux variation was estimated to be ∼0.07 mag h−1 in both the rising and the falling phases. However, rates of brightness variation as high as 1.38 mag h−1 were also detected. The shortest time-scale of the variation (i.e. 37 min) sets an upper limit of 6.92 × 1014 cm on the size of the emission region and about 3.7 × 108 M⊙ as an estimate of the mass of the black hole, assuming that the origin of the rapid optical variability is in close vicinity to the central supermassive black hole. The long-term study suggests a mild bluer-when-brighter behaviour, typical for BL Lacertae objects. en_US
dc.description.statementofresponsibility by Navpreet Kaur, Sameer, Kiran S. Baliyan and S. Ganesh
dc.format.extent Vol. 469, no. 2, pp. 2305-2312
dc.language.iso en_US en_US
dc.publisher Oxford University Press Journals en_US
dc.subject methods: observational en_US
dc.subject Techniques: photometric en_US
dc.subject Galaxies: active en_US
dc.subject BL Lacertae objects: general en_US
dc.subject BL Lacertae objects: individual: 3C66A en_US
dc.subject Quasars: supermassive black hole en_US
dc.title Optical intra-day variability in 3C 66A: a decade of observations en_US
dc.type Article en_US
dc.relation.journal Monthly Notices of the Royal Astronomical Society

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