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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/8207
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dc.contributor.authorDiwan, Rishank-
dc.contributor.authorPrince, Raj-
dc.contributor.authorAgarwal, Aditi-
dc.contributor.authorBose, Debanjan-
dc.contributor.authorMajumdar, Pratik-
dc.contributor.author¨Ozd ¨onmez, Aykut-
dc.contributor.authorChandra, Sunil-
dc.contributor.authorKhatoon, Rukaiya-
dc.contributor.authorEge, Erg ¨un-
dc.date.accessioned2024-01-30T06:00:22Z-
dc.date.available2024-01-30T06:00:22Z-
dc.date.issued2023-07-14-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society,2023,Vol.524, p4333en_US
dc.identifier.issn0035-8711 (print)-
dc.identifier.issn1365-2966 (online)-
dc.identifier.urihttp://hdl.handle.net/2289/8207-
dc.descriptionOpen Accessen_US
dc.description.abstractWe report on a multiwavelength study of the high-synchrotron-peaked BL Lac 1ES 1218 + 304 using near simultaneous dataobtained during the period from 2018 January 1 to 2021 May 31 (MJD 58119–59365) from various instruments, including Fermi–LAT , Swift–XRT , AstroSat , and optical data from Swift-UVOT and the TUBITAK observatory in Turkey. The source was reported to be flaring in the TeV γ-ray band during 2019, but no significant variation was observed with Fermi–LAT . A sub-hour variability is seen in the SXT light curve, suggesting a compact emission region for the v ariability. Ho we ver, hour-scale v ariability is observed in the γ-ray light curve. A ‘softer-when-brighter’ trend is observed in the γ-ray, and an opposite trend is seen in the X-ray, suggesting that the two emissions are produced through two different processes, as expected from a high-frequency- peaked BL Lac source. We have chosen the two epochs in 2019 January to study and compare their physical parameters. A joint fit of SXT and LAXPC provides a constraint on the synchrotron peak, estimated to be ∼1.6 keV. A clear shift in the synchrotronpeak is observed from ∼1 keV to abo v e 10 keV, revealing its extreme nature or behaviour like an extreme blazar-type source.The optical observation provides a colour-index variation as ‘blue-when-brighter’. The broad-band spectral energy distribution is fitted with a single-zone synchrotron-self Compton model, and their parameters are discussed in the context of a TeV blazar and the possible mechanism behind the broad-band emissionen_US
dc.language.isoenen_US
dc.publisherRoyal Astronomical Societyen_US
dc.relation.urihttps://ui.adsabs.harvard.edu/abs/2023MNRAS.524.4333D/abstracten_US
dc.relation.urihttps://arxiv.org/abs/2301.00991en_US
dc.relation.urihttps://doi.org/10.1093/mnras/stad2088en_US
dc.rights2023, The Author(s)en_US
dc.subjectGalaxiesen_US
dc.subjectacti ve –galaxies:en_US
dc.subjectJets –gamma-raysen_US
dc.subjectGalaxies –radiation mechanismsen_US
dc.subjectNon-thermal –BL Lacertae objectsen_US
dc.subjectIndividualen_US
dc.subject1ES 1218 + 304en_US
dc.titleMultiwavelength study of TeV blazar 1ES 1218 + 304 using gamma-ray,X-ray and optical obser v ationsen_US
dc.typeArticleen_US
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