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Optical variability of the blazar 3C 371: From minute to year timescales. / Otero-Santos, J.; Raiteri, C. M.; Acosta-Pulido, J. A.; Carnerero, M. I.; Villata, M.; Savchenko, S. S.; Carosati, D.; Chen, W. P.; Kurtanidze, S. O.; Joner, M. D.; Semkov, E.; Pursimo, T.; Benítez, E.; Damljanovic, G.; Apolonio, G.; Borman, G. A.; Bozhilov, V.; Galindo-Guil, F. J.; Grishina, T. S.; Hagen-Thorn, V. A.; Hiriart, D.; Hsiao, H. Y.; Ibryamov, S.; Ivanidze, R. Z.; Kimeridze, G. N.; Kopatskaya, E. N.; Kurtanidze, O. M.; Larionov, V. M.; Larionova, E. G.; Larionova, L. V.; Minev, M.; Morozova, D. A.; Nikolashvili, M. G.; Ovcharov, E.; Sigua, L. A.; Stojanovic, M.; Troitskiy, I. S.; Troitskaya, Yu. V.; Tsai, A.; Valcheva, A.; Vasilyev, A. A.; Vince, O.; Zaharieva, E.; Zhovtan, A. V.

In: ASTRONOMY & ASTROPHYSICS, Vol. 686, A228, 14.06.2024.

Research output: Contribution to journalArticlepeer-review

Harvard

Otero-Santos, J, Raiteri, CM, Acosta-Pulido, JA, Carnerero, MI, Villata, M, Savchenko, SS, Carosati, D, Chen, WP, Kurtanidze, SO, Joner, MD, Semkov, E, Pursimo, T, Benítez, E, Damljanovic, G, Apolonio, G, Borman, GA, Bozhilov, V, Galindo-Guil, FJ, Grishina, TS, Hagen-Thorn, VA, Hiriart, D, Hsiao, HY, Ibryamov, S, Ivanidze, RZ, Kimeridze, GN, Kopatskaya, EN, Kurtanidze, OM, Larionov, VM, Larionova, EG, Larionova, LV, Minev, M, Morozova, DA, Nikolashvili, MG, Ovcharov, E, Sigua, LA, Stojanovic, M, Troitskiy, IS, Troitskaya, YV, Tsai, A, Valcheva, A, Vasilyev, AA, Vince, O, Zaharieva, E & Zhovtan, AV 2024, 'Optical variability of the blazar 3C 371: From minute to year timescales', ASTRONOMY & ASTROPHYSICS, vol. 686, A228. https://doi.org/10.1051/0004-6361/202449647

APA

Otero-Santos, J., Raiteri, C. M., Acosta-Pulido, J. A., Carnerero, M. I., Villata, M., Savchenko, S. S., Carosati, D., Chen, W. P., Kurtanidze, S. O., Joner, M. D., Semkov, E., Pursimo, T., Benítez, E., Damljanovic, G., Apolonio, G., Borman, G. A., Bozhilov, V., Galindo-Guil, F. J., Grishina, T. S., ... Zhovtan, A. V. (2024). Optical variability of the blazar 3C 371: From minute to year timescales. ASTRONOMY & ASTROPHYSICS, 686, [A228]. https://doi.org/10.1051/0004-6361/202449647

Vancouver

Otero-Santos J, Raiteri CM, Acosta-Pulido JA, Carnerero MI, Villata M, Savchenko SS et al. Optical variability of the blazar 3C 371: From minute to year timescales. ASTRONOMY & ASTROPHYSICS. 2024 Jun 14;686. A228. https://doi.org/10.1051/0004-6361/202449647

Author

Otero-Santos, J. ; Raiteri, C. M. ; Acosta-Pulido, J. A. ; Carnerero, M. I. ; Villata, M. ; Savchenko, S. S. ; Carosati, D. ; Chen, W. P. ; Kurtanidze, S. O. ; Joner, M. D. ; Semkov, E. ; Pursimo, T. ; Benítez, E. ; Damljanovic, G. ; Apolonio, G. ; Borman, G. A. ; Bozhilov, V. ; Galindo-Guil, F. J. ; Grishina, T. S. ; Hagen-Thorn, V. A. ; Hiriart, D. ; Hsiao, H. Y. ; Ibryamov, S. ; Ivanidze, R. Z. ; Kimeridze, G. N. ; Kopatskaya, E. N. ; Kurtanidze, O. M. ; Larionov, V. M. ; Larionova, E. G. ; Larionova, L. V. ; Minev, M. ; Morozova, D. A. ; Nikolashvili, M. G. ; Ovcharov, E. ; Sigua, L. A. ; Stojanovic, M. ; Troitskiy, I. S. ; Troitskaya, Yu. V. ; Tsai, A. ; Valcheva, A. ; Vasilyev, A. A. ; Vince, O. ; Zaharieva, E. ; Zhovtan, A. V. / Optical variability of the blazar 3C 371: From minute to year timescales. In: ASTRONOMY & ASTROPHYSICS. 2024 ; Vol. 686.

BibTeX

@article{709f14b4754e408397ba896f54fe0ce3,
title = "Optical variability of the blazar 3C 371: From minute to year timescales",
abstract = "The BL Lac object 3C 371 was observed by the Transiting Exoplanet Survey Satellite (TESS) for approximately a year, between July 2019 and July 2020, with an unmatched two-minute imaging cadence. In parallel, the Whole Earth Blazar Telescope (WEBT) Collaboration organized an extensive observing campaign, providing three years of continuous optical monitoring between 2018 and 2020. These datasets allow for a thorough investigation of the variability of the source. The goal of this study is to evaluate the optical variability of 3C 371. Taking advantage of the remarkable cadence of TESS data, we aim to characterize the intra-day variability (IDV) displayed by the source and identify its shortest variability timescale. With this estimate, constraints on the size of the emitting region and black hole mass can be calculated. Moreover, WEBT data are used to investigate long-term variability (LTV), including in terms of the spectral behavior of the source and the polarization variability. Based on the derived characteristics, we aim to extract information on the origin of the variability on different timescales. We evaluated the variability of 3C 371 by applying the variability amplitude tool, which quantifies variability of the emission. Moreover, we employed common tools, such as ANOVA (ANalysis Of VAariance) tests, wavelet and power spectral density (PSD) analyses to characterize the shortest variability timescales present in the emission and the underlying noise affecting the data. We evaluated the short- and long-term color behavior to understand to understand its spectral behavior. The polarized emission was analyzed, studying its variability and possible rotation patterns of the electric vector position angle (EVPA). Flux distributions of the IDV and LTV were also studied with the aim being to link the flux variations to turbulent and/or accretion-disk-related processes. Our ANOVA and wavelet analyses reveal several entangled variability timescales. We observe a clear increase in the variability amplitude with increasing width of the time intervals evaluated. We are also able to resolve significant variations on timescales of as little as sim 0.5 hours. The PSD analysis reveals a red-noise spectrum with a break at IDV timescales. The spectral analysis shows a mild bluer-when-brighter (BWB) trend on long timescales. On short timescales, mixed BWB, achromatic and redder-when-brighter (RWB) signatures can be observed. The polarized emission shows an interesting slow EVPA rotation during the flaring period where a simple stochastic model can be excluded as the origin with a 3sigma significance . The flux distributions show a preference for a Gaussian model for the IDV, and suggest it may be linked to turbulent processes, while the LTV is better represented by a log-normal distribution and may have a disk-related.",
author = "J. Otero-Santos and Raiteri, {C. M.} and Acosta-Pulido, {J. A.} and Carnerero, {M. I.} and M. Villata and Savchenko, {S. S.} and D. Carosati and Chen, {W. P.} and Kurtanidze, {S. O.} and Joner, {M. D.} and E. Semkov and T. Pursimo and E. Ben{\'i}tez and G. Damljanovic and G. Apolonio and Borman, {G. A.} and V. Bozhilov and Galindo-Guil, {F. J.} and Grishina, {T. S.} and Hagen-Thorn, {V. A.} and D. Hiriart and Hsiao, {H. Y.} and S. Ibryamov and Ivanidze, {R. Z.} and Kimeridze, {G. N.} and Kopatskaya, {E. N.} and Kurtanidze, {O. M.} and Larionov, {V. M.} and Larionova, {E. G.} and Larionova, {L. V.} and M. Minev and Morozova, {D. A.} and Nikolashvili, {M. G.} and E. Ovcharov and Sigua, {L. A.} and M. Stojanovic and Troitskiy, {I. S.} and Troitskaya, {Yu. V.} and A. Tsai and A. Valcheva and Vasilyev, {A. A.} and O. Vince and E. Zaharieva and Zhovtan, {A. V.}",
year = "2024",
month = jun,
day = "14",
doi = "10.1051/0004-6361/202449647",
language = "English",
volume = "686",
journal = "ASTRONOMY & ASTROPHYSICS",
issn = "0004-6361",
publisher = "EDP Sciences",

}

RIS

TY - JOUR

T1 - Optical variability of the blazar 3C 371: From minute to year timescales

AU - Otero-Santos, J.

AU - Raiteri, C. M.

AU - Acosta-Pulido, J. A.

AU - Carnerero, M. I.

AU - Villata, M.

AU - Savchenko, S. S.

AU - Carosati, D.

AU - Chen, W. P.

AU - Kurtanidze, S. O.

AU - Joner, M. D.

AU - Semkov, E.

AU - Pursimo, T.

AU - Benítez, E.

AU - Damljanovic, G.

AU - Apolonio, G.

AU - Borman, G. A.

AU - Bozhilov, V.

AU - Galindo-Guil, F. J.

AU - Grishina, T. S.

AU - Hagen-Thorn, V. A.

AU - Hiriart, D.

AU - Hsiao, H. Y.

AU - Ibryamov, S.

AU - Ivanidze, R. Z.

AU - Kimeridze, G. N.

AU - Kopatskaya, E. N.

AU - Kurtanidze, O. M.

AU - Larionov, V. M.

AU - Larionova, E. G.

AU - Larionova, L. V.

AU - Minev, M.

AU - Morozova, D. A.

AU - Nikolashvili, M. G.

AU - Ovcharov, E.

AU - Sigua, L. A.

AU - Stojanovic, M.

AU - Troitskiy, I. S.

AU - Troitskaya, Yu. V.

AU - Tsai, A.

AU - Valcheva, A.

AU - Vasilyev, A. A.

AU - Vince, O.

AU - Zaharieva, E.

AU - Zhovtan, A. V.

PY - 2024/6/14

Y1 - 2024/6/14

N2 - The BL Lac object 3C 371 was observed by the Transiting Exoplanet Survey Satellite (TESS) for approximately a year, between July 2019 and July 2020, with an unmatched two-minute imaging cadence. In parallel, the Whole Earth Blazar Telescope (WEBT) Collaboration organized an extensive observing campaign, providing three years of continuous optical monitoring between 2018 and 2020. These datasets allow for a thorough investigation of the variability of the source. The goal of this study is to evaluate the optical variability of 3C 371. Taking advantage of the remarkable cadence of TESS data, we aim to characterize the intra-day variability (IDV) displayed by the source and identify its shortest variability timescale. With this estimate, constraints on the size of the emitting region and black hole mass can be calculated. Moreover, WEBT data are used to investigate long-term variability (LTV), including in terms of the spectral behavior of the source and the polarization variability. Based on the derived characteristics, we aim to extract information on the origin of the variability on different timescales. We evaluated the variability of 3C 371 by applying the variability amplitude tool, which quantifies variability of the emission. Moreover, we employed common tools, such as ANOVA (ANalysis Of VAariance) tests, wavelet and power spectral density (PSD) analyses to characterize the shortest variability timescales present in the emission and the underlying noise affecting the data. We evaluated the short- and long-term color behavior to understand to understand its spectral behavior. The polarized emission was analyzed, studying its variability and possible rotation patterns of the electric vector position angle (EVPA). Flux distributions of the IDV and LTV were also studied with the aim being to link the flux variations to turbulent and/or accretion-disk-related processes. Our ANOVA and wavelet analyses reveal several entangled variability timescales. We observe a clear increase in the variability amplitude with increasing width of the time intervals evaluated. We are also able to resolve significant variations on timescales of as little as sim 0.5 hours. The PSD analysis reveals a red-noise spectrum with a break at IDV timescales. The spectral analysis shows a mild bluer-when-brighter (BWB) trend on long timescales. On short timescales, mixed BWB, achromatic and redder-when-brighter (RWB) signatures can be observed. The polarized emission shows an interesting slow EVPA rotation during the flaring period where a simple stochastic model can be excluded as the origin with a 3sigma significance . The flux distributions show a preference for a Gaussian model for the IDV, and suggest it may be linked to turbulent processes, while the LTV is better represented by a log-normal distribution and may have a disk-related.

AB - The BL Lac object 3C 371 was observed by the Transiting Exoplanet Survey Satellite (TESS) for approximately a year, between July 2019 and July 2020, with an unmatched two-minute imaging cadence. In parallel, the Whole Earth Blazar Telescope (WEBT) Collaboration organized an extensive observing campaign, providing three years of continuous optical monitoring between 2018 and 2020. These datasets allow for a thorough investigation of the variability of the source. The goal of this study is to evaluate the optical variability of 3C 371. Taking advantage of the remarkable cadence of TESS data, we aim to characterize the intra-day variability (IDV) displayed by the source and identify its shortest variability timescale. With this estimate, constraints on the size of the emitting region and black hole mass can be calculated. Moreover, WEBT data are used to investigate long-term variability (LTV), including in terms of the spectral behavior of the source and the polarization variability. Based on the derived characteristics, we aim to extract information on the origin of the variability on different timescales. We evaluated the variability of 3C 371 by applying the variability amplitude tool, which quantifies variability of the emission. Moreover, we employed common tools, such as ANOVA (ANalysis Of VAariance) tests, wavelet and power spectral density (PSD) analyses to characterize the shortest variability timescales present in the emission and the underlying noise affecting the data. We evaluated the short- and long-term color behavior to understand to understand its spectral behavior. The polarized emission was analyzed, studying its variability and possible rotation patterns of the electric vector position angle (EVPA). Flux distributions of the IDV and LTV were also studied with the aim being to link the flux variations to turbulent and/or accretion-disk-related processes. Our ANOVA and wavelet analyses reveal several entangled variability timescales. We observe a clear increase in the variability amplitude with increasing width of the time intervals evaluated. We are also able to resolve significant variations on timescales of as little as sim 0.5 hours. The PSD analysis reveals a red-noise spectrum with a break at IDV timescales. The spectral analysis shows a mild bluer-when-brighter (BWB) trend on long timescales. On short timescales, mixed BWB, achromatic and redder-when-brighter (RWB) signatures can be observed. The polarized emission shows an interesting slow EVPA rotation during the flaring period where a simple stochastic model can be excluded as the origin with a 3sigma significance . The flux distributions show a preference for a Gaussian model for the IDV, and suggest it may be linked to turbulent processes, while the LTV is better represented by a log-normal distribution and may have a disk-related.

UR - https://www.mendeley.com/catalogue/cf2ec96f-a31c-39ca-bad5-fca520cbe829/

U2 - 10.1051/0004-6361/202449647

DO - 10.1051/0004-6361/202449647

M3 - Article

VL - 686

JO - ASTRONOMY & ASTROPHYSICS

JF - ASTRONOMY & ASTROPHYSICS

SN - 0004-6361

M1 - A228

ER -

ID: 120896316