Extreme photometric and polarimetric variability of blazar S4 0954+65 at its maximum optical and γ-ray brightness levels-Reference-Cited by-同舟云学术

Extreme photometric and polarimetric variability of blazar S4 0954+65 at its maximum optical and γ-ray brightness levels

Published:2023-10-09 Issue:3 Volume:526 Page:4502-4513
ISSN:0035-8711
Container-title:Monthly Notices of the Royal Astronomical Society
language:en
Short-container-title:

Author:

Raiteri C M¹^ORCID,Villata M¹^ORCID,Carnerero M I¹^ORCID,Savchenko S S²³⁴^ORCID,Kurtanidze S O⁵,Vlasyuk V V³,Marchini A⁶^ORCID,Matsumoto K⁷,Lorey C⁸,Joner M D⁹^ORCID,Gazeas K¹⁰^ORCID,Carosati D¹¹¹²,Mirzaqulov D O¹³^ORCID,Acosta Pulido J A¹⁴¹⁵,Agudo I¹⁶,Bachev R¹⁷,Benítez E¹⁸^ORCID,Borman G A¹⁹^ORCID,Calcidese P²⁰,Chen W P²¹,Damljanovic G²²^ORCID,Ehgamberdiev S A¹³²³^ORCID,Elsässer D⁸²⁴^ORCID,Feige M⁸,Frasca A²⁵^ORCID,Gaur H²⁶,Grishina T S²^ORCID,Gupta A C²⁶^ORCID,Hiriart D²⁷^ORCID,Holland M⁹,Horst B⁸,Ibryamov S²⁸,Ivanidze R Z⁵,Jensen J⁹,Jithesh V²⁹,Jovanovic M D²²^ORCID,Kiehlmann S³⁰³¹,Kimeridze G N⁵,Kishore S²⁶,Kopatskaya E N²^ORCID,Kurtanidze O M⁵³²,Larionova E G²^ORCID,Lin H C²¹,Mannheim K⁸³³,Marinelli C³⁴^ORCID,Moreira Reyes J³⁵,Morozova D A²^ORCID,Nikolashvili M G⁵,Reinhart D⁸³³,Romanov F D³⁶³⁷^ORCID,Semkov E¹⁷,Seufert J⁸,Shishkina E V²,Sigua L A⁵,Skalidis R³⁸,Spiridonova O I³,Stojanovic M²²^ORCID,Strigachev A¹⁷,Troitskaya Y V²^ORCID,Troitskiy I S²^ORCID,Tsai A²¹,Vasilyev A A²^ORCID,Vince O²²,Vrontaki K¹⁰,Wani K²⁶,Watts D⁹,Zhovtan A V¹⁹

Affiliation:

1. INAF, Osservatorio Astrofisico di Torino , via Osservatorio 20, I-10025 Pino Torinese , Italy

2. Saint Petersburg State University , 7/9 Universitetskaya nab., St. Petersburg 199034 , Russia

3. Special Astrophysical Observatory of Russian Academy of Sciences , Nyzhnij Arkhyz, Karachai-Circassia 369167 , Russia

4. Pulkovo Observatory , St. Petersburg 196140 , Russia

5. Abastumani Observatory , Mt. Kanobili, 0301 Abastumani , Georgia

6. Astronomical Observatory, University of Siena , I-53100 Siena , Italy

7. Astronomical Institute, Osaka Kyoiku University , Osaka 582-8582 , Japan

8. Hans-Haffner-Sternwarte (Hettstadt) , Naturwissenschaftliches Labor für Schüler, Friedrich-Koenig-Gymnasium, D-97082 Würzburg , Germany

9. Department of Physics and Astronomy , N283 ESC, Brigham Young University, Provo, UT 84602 , USA

10. Section of Astrophysics, Astronomy and Mechanics, Department of Physics, National and Kapodistrian University of Athens , GR-15784 Zografos, Athens , Greece

11. EPT Observatories , Tijarafe, La Palma, E-38780, , Spain

12. INAF, TNG Fundación Galileo Galilei , La Palma, E-38712 , Spain

13. Ulugh Beg Astronomical Institute , Astronomy Street 33, Tashkent 100052 , Uzbekistan

14. Instituto de Astrofísica de Canarias (IAC) , E-38200 La Laguna, Tenerife , Spain

15. Departamento de Astrofísica, Universidad de La Laguna (ULL) , E-38206 La Laguna, Tenerife , Spain

16. Instituto de Astrofísica de Andalucía (CSIC) , Apartado 3004, E-18080 Granada , Spain

17. Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences , 72 Tsarigradsko shosse Blvd., 1784 Sofia , Bulgaria

18. Instituto de Astronomía, Universidad Nacional Autónoma de México , AP 70-264, CDMX 04510 , Mexico

19. Crimean Astrophysical Observatory RAS , P/O Nauchny 298409 , Russia

20. Osservatorio Astronomico della Regione Autonoma Valle d’Aosta , I-11020 Nus , Italy

21. Institute of Astronomy, National Central University , Taoyuan 32001 , Taiwan

22. Astronomical Observatory , Volgina 7, 11060 Belgrade , Serbia

23. National University of Uzbekistan , Tashkent 100174 , Uzbekistan

24. Technische Universität Dortmund , D-44221 Dortmund , Germany

25. INAF, Osservatorio Astrofisico di Catania , Via S. Sofia 78, I-95123 Catania , Italy

26. Aryabhatta Research Institute of Observational Sciences (ARIES) , Manora Peak, Nainital 263001 , India

27. Instituto de Astronomía, Universidad Nacional Autónoma de México , AP 106, Ensenada 22800, Baja California , Mexico

28. Department of Physics and Astronomy, Faculty of Natural Sciences, University of Shumen , 115, Universitetska Str., 9712 Shumen , Bulgaria

29. Department of Physics and Electronics, CHRIST (Deemed to be University) , Hosur Main Road, Bengaluru 560029 , India

30. Institute of Astrophysics, Foundation for Research and Technology - Hellas , Vasilika Vouton, GR-70013 Heraklion , Greece

31. Department of Physics, University of Crete , Voutes University Campus, GR-70013 Heraklion , Greece

32. Engelhardt Astronomical Observatory, Kazan Federal University , Tatarstan , Russia

33. Universität Würzburg , D-97074 Würzburg , Germany

34. Dip. di Scienze Fisiche, della Terra e dell’Ambiente, Università di Siena , via Roma 56, I-53100 Siena , Italy

35. Department of Physics, Astronomy and Geophysics, Connecticut College , New London, CT 06320 , USA

36. AAVSO observer , Russia

37. Remote observer of Burke-Gaffney Observatory , Canada

38. Owens Valley Radio Observatory, California Institute of Technology , MC 249-17, Pasadena, CA 91125 , USA

Abstract

ABSTRACT In 2022 the BL Lac object S4 0954+65 underwent a major variability phase, reaching its historical maximum brightness in the optical and γ-ray bands. We present optical photometric and polarimetric data acquired by the Whole Earth Blazar Telescope (WEBT) Collaboration from 2022 April 6 to July 6. Many episodes of unprecedented fast variability were detected, implying an upper limit to the size of the emitting region as low as $10^{-4}$ parsec. The WEBT data show rapid variability in both the degree and angle of polarization. We analyse different models to explain the polarization behaviour in the framework of a twisting jet model, which assumes that the long-term trend of the flux is produced by variations in the emitting region viewing angle. All the models can reproduce the average trend of the polarization degree, and can account for its general anticorrelation with the flux, but the dispersion of the data requires the presence of intrinsic mechanisms, such as turbulence, shocks, or magnetic reconnection. The WEBT optical data are compared to γ-ray data from the Fermi satellite. These are analysed with both fixed and adaptive binning procedures. We show that the strong correlation between optical and γ-ray data without measurable delay assumes different slopes in faint and high brightness states, and this is compatible with a scenario where in faint states we mainly see the imprint of the geometrical effects, while in bright states the synchrotron self-Compton process dominates.

Funder

NASA

Department of Science and Technology

Bulgarian National Science Fund

JSPS

European Research Council

Spanish Ministry of Science and Innovation

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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