Maqola

The dual nature of blazar fast variability: Space and ground observations of S5 0716+714

C. M. RaiteriINAF, Osservatorio Astrofisico di Torino, Via Osservatorio 20, I-10025 Pino Torinese, ItalyM. VillataINAF, Osservatorio Astrofisico di Torino, Via Osservatorio 20, I-10025 Pino Torinese, ItalyD. CarosatiEPT Observatories, Tijarafe, E-38780 La Palma, SpainE. BenítezInstituto de Astronomía, Universidad Nacional Autónoma de México, Cd. Universitaria, CDMX, MexicoS. O. KurtanidzeAbastumani Observatory, Mt. Kanobili, 0301 Abastumani, GeorgiaAlok C. GuptaAryabhatta Research Institute of Observational Sciences (ARIES), Manora Peak, Nainital-263 001, IndiaD. O. MirzaqulovUlugh Beg Astronomical Institute, Maidanak Observatory, Tashkent 100052, UzbekistanF. D’AmmandoINAF, Istituto di Radioastronomia, Via Gobetti 101, I-40129 Bologna, ItalyV. M. LarionovPulkovo Observatory, 196140 St. Petersburg, RussiaT. PursimoNordic Optical Telescope, Apartado 474, E-38700 Santa Cruz de La Palma, SpainJ. A. Acosta‐PulidoInstituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, SpainG. V. BaidaCrimean Astrophysical Observatory RAS, P/O Nauchny 298409, RussiaB. BalmaverdeINAF, Osservatorio Astrofisico di Torino, Via Osservatorio 20, I-10025 Pino Torinese, ItalyG. BonnoliUniversity of Siena, Department of Physical Sciences, Earth and Environment, Astronomical Observatory, Via Roma 56, I-53100 Siena, ItalyГ. А. БорманCrimean Astrophysical Observatory RAS, P/O Nauchny 298409, RussiaM. I. CarnereroINAF, Osservatorio Astrofisico di Torino, Via Osservatorio 20, I-10025 Pino Torinese, ItalyW-P ChenGraduate Institute of Astronomy, National Central University, 300 Jhongda Road, Zhongli, Taoyuan 32001, TaiwanVinit DhimanAryabhatta Research Institute of Observational Sciences (ARIES), Manora Peak, Nainital-263 001, IndiaA Di MaggioSh. A. EhgamberdievUlugh Beg Astronomical Institute, Maidanak Observatory, Tashkent 100052, UzbekistanD. HiriartInstituto de Astronomía, Universidad Nacional Autónoma de México, 22800 Ensenada, Baja California, MexicoG. N. KimeridzeAbastumani Observatory, Mt. Kanobili, 0301 Abastumani, GeorgiaO. M. KurtanidzeAbastumani Observatory, Mt. Kanobili, 0301 Abastumani, GeorgiaChien-Cheng LinGraduate Institute of Astronomy, National Central University, 300 Jhongda Road, Zhongli, Taoyuan 32001, TaiwanJ. LópezFacultad de Ciencias, Universidad Autónoma de Baja California, Campus El Sauzal, 22800 Ensenada, Baja California, MexicoAlessandro MarchiniUniversity of Siena, Department of Physical Sciences, Earth and Environment, Astronomical Observatory, Via Roma 56, I-53100 Siena, ItalyKatsura MatsumotoAstronomical Institute, Osaka Kyoiku University, Osaka 582-8582, JapanR. MújicaInstituto Nacional de Astrofísica, Óptica y Electrónica, Tonantzintla, 72840 Puebla, MexicoMasanori NakamuraDepartment of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo-ku, Sagamihara, Kanagawa 252-5258, JapanA. A. NikiforovaAstronomical Institute, St. Petersburg State University, 198504 St. Petersburg, RussiaM. G. NikolashviliAbastumani Observatory, Mt. Kanobili, 0301 Abastumani, GeorgiaD. N. OkhmatCrimean Astrophysical Observatory RAS, P/O Nauchny 298409, RussiaJorge Otero-SantosInstituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, SpainN. RizziT. SakamotoDepartment of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo-ku, Sagamihara, Kanagawa 252-5258, JapanE. SemkovInstitute of Astronomy and National Astronomical, Observatory, Bulgarian Academy of Sciences, BG-1784 Sofia, BulgariaL. A. SiguaAbastumani Observatory, Mt. Kanobili, 0301 Abastumani, GeorgiaLeonardo StiacciniUniversity of Siena, Department of Physical Sciences, Earth and Environment, Astronomical Observatory, Via Roma 56, I-53100 Siena, ItalyI. S. TroitskyAn-Li TsaiGraduate Institute of Astronomy, National Central University, 300 Jhongda Road, Zhongli, Taoyuan 32001, TaiwanA. A. VasilyevА. В. ЖовтанCrimean Astrophysical Observatory RAS, P/O Nauchny 298409, Russia

Monthly Notices of the Royal Astronomical Societyjournal2020en

ABI

Annotatsiya

ABSTRACT Blazar S5 0716+714 is well-known for its short-term variability, down to intraday time-scales. We here present the 2-min cadence optical light curve obtained by the TESS space telescope in 2019 December–2020 January and analyse the object fast variability with unprecedented sampling. Supporting observations by the Whole Earth Blazar Telescope Collaboration in B, V, R, and I bands allow us to investigate the spectral variability during the TESS pointing. The spectral analysis is further extended in frequency to the UV and X-ray bands with data from the Neil Gehrels Swift Observatory. We develop a new method to unveil the shortest optical variability time-scales. This is based on progressive de-trending of the TESS light curve by means of cubic spline interpolations through the binned fluxes, with decreasing time bins. The de-trended light curves are then analysed with classical tools for time-series analysis (periodogram, autocorrelation, and structure functions). The results show that below 3 d there are significant characteristic variability time-scales of about 1.7, 0.5, and 0.2 d. Variability on time-scales $\lesssim 0.2$ d is strongly chromatic and must be ascribed to intrinsic energetic processes involving emitting regions, likely jet substructures, with dimension less than about 10−3 pc. In contrast, flux changes on time-scales $\gtrsim 0.5$ d are quasi-achromatic and are probably due to Doppler factor changes of geometric origin.

Mavzular

Astrophysics and Cosmic Phenomena Radio Astronomy Observations and Technology Neutrino Physics Research

Identifikatorlar

DOI: 10.1093/mnras/staa3561

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