Multiband optical flux density and polarization microvariability study of optically bright blazars

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dc.authoridTroitskaya, Yuliya/0000-0002-9907-9876
dc.authoridItoh, Ryosuke/0000-0002-1183-8955
dc.authoridTroitskiy, Ivan/0000-0002-4218-0148
dc.authoridPasierb, Magdalena/0000-0003-0674-429X
dc.authoridKawabata, Miho/0000-0002-4540-4928
dc.authoridLarionova, Elena/0000-0002-2471-6500
dc.authoridLarionov, Valeri/0000-0002-4640-4356
dc.contributor.authorPasierb, Magdalena
dc.contributor.authorGoyal, Arti
dc.contributor.authorOstrowski, Michal
dc.contributor.authorStawarz, Lukasz
dc.contributor.authorWiita, Paul J.
dc.contributor.authorGopal-Krishna
dc.contributor.authorLarionov, Valeri M.
dc.date.accessioned2025-01-27T20:11:51Z
dc.date.available2025-01-27T20:11:51Z
dc.date.issued2020
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractWe present the results of flux density, spectral index, and polarization intra-night monitoring studies of a sample of eight optically bright blazars, carried out by employing several small to moderate aperture (0.4 to 1.5 m diameter) telescopes fitted with CCDs and polarimeters located in Europe, India, and Japan. The duty cycle of flux variability for the targets is found to be similar to 45 per cent, similar to that reported in earlier studies. The computed two-point spectral indices are found to be between 0.65 to 1.87 for our sample, comprised of low- and intermediate-frequency peaked blazars, with one exception: they are also found to be statistically variable for about half the instances where 'confirmed' variability is detected in flux density. In the analysis of the spectral evolution of the targets on hourly time-scale, a counterclockwise loop (soft-lagging) is noted in the flux-spectral index plane on two occasions, and in one case a clear spectral flattening with the decreasing flux is observed. In our data set, we also observe a variety of flux-polarization degree variability patterns, including instances with a relatively straightforward anticorrelation, correlation, or counterclockwise looping. These changes are typically reflected in the flux-polarization angle plane: the anticorrelation between the flux and polarization degree is accompanied by an anticorrelation between the polarization angle and flux, while the counterclockwise flux-PD looping behaviour is accompanied by a clockwise looping in the flux-polarization angle representation. We discuss our findings in the framework of the internal shock scenario for blazar sources.
dc.description.sponsorshipPolish National Science Centre (NCN) [2018/29/B/ST9/02298]; NCN [2018/29/B/ST9/01793, 2016/22/E/ST9/00061]; Indian National Science Academy; Russian Science Foundation [17-12-01029]; Russian Science Foundation [17-12-01029] Funding Source: Russian Science Foundation
dc.description.sponsorshipWe thank the referee for providing constructive comments on the manuscript. We thank the staff of ARIES and Kanata for carrying out some of the observations presented in this study. AG acknowledges support from the Polish National Science Centre (NCN) through the grant 2018/29/B/ST9/02298. LS acknowledges the support of NCN via 2016/22/E/ST9/00061. SZ's work is supported by NCN via 2018/29/B/ST9/01793. GK would like to thank Indian National Science Academy for a Senior Scientist fellowship.The St. Petersburg University team acknowledges support from Russian Science Foundation grant 17-12-01029.
dc.identifier.doi10.1093/mnras/stz3533
dc.identifier.endpage1317
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.issue1
dc.identifier.scopus2-s2.0-85092676108
dc.identifier.scopusqualityQ1
dc.identifier.startpage1295
dc.identifier.urihttps://doi.org/10.1093/mnras/stz3533
dc.identifier.urihttps://hdl.handle.net/20.500.12428/20754
dc.identifier.volume492
dc.identifier.wosWOS:000512329900099
dc.identifier.wosqualityQ1
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherOxford Univ Press
dc.relation.ispartofMonthly Notices of The Royal Astronomical Society
dc.relation.publicationcategoryinfo:eu-repo/semantics/openAccess
dc.rightsinfo:eu-repo/semantics/openAccess
dc.snmzKA_WoS_20250125
dc.subjectpolarization
dc.subjectradiation mechanisms: non-thermal
dc.subjectgalaxies: active
dc.subjectgalaxies: individual: 0109+224, 3C 66A, S5 0716+714, OJ 287, 3C 279, PG 1553+113, CTA102, and 3C 454.3
dc.subjectgalaxies: jets
dc.titleMultiband optical flux density and polarization microvariability study of optically bright blazars
dc.typeArticle

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