Standard

Multiwavelength Variability of BL Lacertae Measured with High Time Resolution. / Weaver, Z. R.; Williamson, K. E.; Jorstad, S. G.; Marscher, A. P.; Larionov, V. M.; Raiteri, C. M.; Villata, M.; Acosta-Pulido, J. A.; Bachev, R.; Baida, G. V.; Balonek, T. J.; Benítez, E.; Borman, G. A.; Bozhilov, V.; Carnerero, M. I.; Carosati, D.; Chen, W. P.; Damljanovic, G.; Dhiman, V.; Dougherty, D. J.; Ehgamberdiev, S. A.; Grishina, T. S.; Gupta, A. C.; Hart, M.; Hiriart, D.; Hsiao, H. Y.; Ibryamov, S.; Joner, M.; Kimeridze, G. N.; Kopatskaya, E. N.; Kurtanidze, O. M.; Kurtanidze, S. O.; Larionova, E. G.; Matsumoto, K.; Matsumura, R.; Minev, M.; Mirzaqulov, D. O.; Morozova, D. A.; Nikiforova, A. A.; Nikolashvili, M. G.; Ovcharov, E.; Rizzi, N.; Sadun, A.; Savchenko, S. S.; Semkov, E.; Slater, J. J.; Smith, K. L.; Stojanovic, M.; Strigachev, A.; Troitskaya, Yu. V.; Troitsky, I. S.; Tsai, A. L.; Vince, O.; Valcheva, A.; Vasilyev, A. A.; Zaharieva, E.; Zhovtan, A. V.

в: The Astrophysical Journal, Том 900, № 2, 137, 10.09.2020, стр. 137.

Результаты исследований: Научные публикации в периодических изданиях › статья › Рецензирование

Harvard

Weaver, ZR, Williamson, KE, Jorstad, SG, Marscher, AP, Larionov, VM, Raiteri, CM, Villata, M, Acosta-Pulido, JA, Bachev, R, Baida, GV, Balonek, TJ, Benítez, E, Borman, GA, Bozhilov, V, Carnerero, MI, Carosati, D, Chen, WP, Damljanovic, G, Dhiman, V, Dougherty, DJ, Ehgamberdiev, SA, Grishina, TS, Gupta, AC, Hart, M, Hiriart, D, Hsiao, HY, Ibryamov, S, Joner, M, Kimeridze, GN, Kopatskaya, EN, Kurtanidze, OM, Kurtanidze, SO, Larionova, EG, Matsumoto, K, Matsumura, R, Minev, M, Mirzaqulov, DO, Morozova, DA, Nikiforova, AA, Nikolashvili, MG, Ovcharov, E, Rizzi, N, Sadun, A, Savchenko, SS, Semkov, E, Slater, JJ, Smith, KL, Stojanovic, M, Strigachev, A, Troitskaya, YV, Troitsky, IS, Tsai, AL, Vince, O, Valcheva, A, Vasilyev, AA, Zaharieva, E & Zhovtan, AV 2020, 'Multiwavelength Variability of BL Lacertae Measured with High Time Resolution', The Astrophysical Journal, Том. 900, № 2, 137, стр. 137. https://doi.org/10.3847/1538-4357/aba693

APA

Weaver, Z. R., Williamson, K. E., Jorstad, S. G., Marscher, A. P., Larionov, V. M., Raiteri, C. M., Villata, M., Acosta-Pulido, J. A., Bachev, R., Baida, G. V., Balonek, T. J., Benítez, E., Borman, G. A., Bozhilov, V., Carnerero, M. I., Carosati, D., Chen, W. P., Damljanovic, G., Dhiman, V., ... Zhovtan, A. V. (2020). Multiwavelength Variability of BL Lacertae Measured with High Time Resolution. The Astrophysical Journal, 900(2), 137. [137]. https://doi.org/10.3847/1538-4357/aba693

Vancouver

Weaver ZR, Williamson KE, Jorstad SG, Marscher AP, Larionov VM, Raiteri CM и пр. Multiwavelength Variability of BL Lacertae Measured with High Time Resolution. The Astrophysical Journal. 2020 Сент. 10;900(2):137. 137. https://doi.org/10.3847/1538-4357/aba693

Author

Weaver, Z. R. ; Williamson, K. E. ; Jorstad, S. G. ; Marscher, A. P. ; Larionov, V. M. ; Raiteri, C. M. ; Villata, M. ; Acosta-Pulido, J. A. ; Bachev, R. ; Baida, G. V. ; Balonek, T. J. ; Benítez, E. ; Borman, G. A. ; Bozhilov, V. ; Carnerero, M. I. ; Carosati, D. ; Chen, W. P. ; Damljanovic, G. ; Dhiman, V. ; Dougherty, D. J. ; Ehgamberdiev, S. A. ; Grishina, T. S. ; Gupta, A. C. ; Hart, M. ; Hiriart, D. ; Hsiao, H. Y. ; Ibryamov, S. ; Joner, M. ; Kimeridze, G. N. ; Kopatskaya, E. N. ; Kurtanidze, O. M. ; Kurtanidze, S. O. ; Larionova, E. G. ; Matsumoto, K. ; Matsumura, R. ; Minev, M. ; Mirzaqulov, D. O. ; Morozova, D. A. ; Nikiforova, A. A. ; Nikolashvili, M. G. ; Ovcharov, E. ; Rizzi, N. ; Sadun, A. ; Savchenko, S. S. ; Semkov, E. ; Slater, J. J. ; Smith, K. L. ; Stojanovic, M. ; Strigachev, A. ; Troitskaya, Yu. V. ; Troitsky, I. S. ; Tsai, A. L. ; Vince, O. ; Valcheva, A. ; Vasilyev, A. A. ; Zaharieva, E. ; Zhovtan, A. V. / Multiwavelength Variability of BL Lacertae Measured with High Time Resolution. в: The Astrophysical Journal. 2020 ; Том 900, № 2. стр. 137.

BibTeX

@article{0b5b430b635741f1a4922750f5108b3b,
title = "Multiwavelength Variability of BL Lacertae Measured with High Time Resolution",
abstract = "In an effort to locate the sites of emission at different frequencies and physical processes causing variability in blazar jets, we have obtained high time-resolution observations of BL Lacertae over a wide wavelength range: with the Transiting Exoplanet Survey Satellite (TESS) at 6000-10000 {\AA} with 2 minute cadence; with the Neil Gehrels Swift satellite at optical, UV, and X-ray bands; with the Nuclear Spectroscopic Telescope Array at hard X-ray bands; with the Fermi Large Area Telescope at γ-ray energies; and with the Whole Earth Blazar Telescope for measurement of the optical flux density and polarization. All light curves are correlated, with similar structure on timescales from hours to days. The shortest timescale of variability at optical frequencies observed with TESS is ∼0.5 hr. The most common timescale is 13 ± 1 hr, comparable with the minimum timescale of X-ray variability, 14.5 hr. The multiwavelength variability properties cannot be explained by a change solely in the Doppler factor of the emitting plasma. The polarization behavior implies that there are both ordered and turbulent components to the magnetic field in the jet. Correlation analysis indicates that the X-ray variations lag behind the γ-ray and optical light curves by up to ∼0.4 day. The timescales of variability, cross-frequency lags, and polarization properties can be explained by turbulent plasma that is energized by a shock in the jet and subsequently loses energy to synchrotron and inverse Compton radiation in a magnetic field of strength ∼3 G.",
keywords = "BL Lacertae objects, Active galaxies, 164, Eywords: galaxies: active, BL Lacertae objects: individual: BL Lacertae, 3C 454.3, WEBT CAMPAIGNS, LARGE-AREA TELESCOPE, LIGHT CURVES, OPTICAL VARIABILITY, GAMMA-RAY, ACTIVE GALACTIC NUCLEI, X-RAY, RADIO-SOURCES, MAGNETIC-FIELD",
author = "Weaver, {Z. R.} and Williamson, {K. E.} and Jorstad, {S. G.} and Marscher, {A. P.} and Larionov, {V. M.} and Raiteri, {C. M.} and M. Villata and Acosta-Pulido, {J. A.} and R. Bachev and Baida, {G. V.} and Balonek, {T. J.} and E. Ben{\'i}tez and Borman, {G. A.} and V. Bozhilov and Carnerero, {M. I.} and D. Carosati and Chen, {W. P.} and G. Damljanovic and V. Dhiman and Dougherty, {D. J.} and Ehgamberdiev, {S. A.} and Grishina, {T. S.} and Gupta, {A. C.} and M. Hart and D. Hiriart and Hsiao, {H. Y.} and S. Ibryamov and M. Joner and Kimeridze, {G. N.} and Kopatskaya, {E. N.} and Kurtanidze, {O. M.} and Kurtanidze, {S. O.} and Larionova, {E. G.} and K. Matsumoto and R. Matsumura and M. Minev and Mirzaqulov, {D. O.} and Morozova, {D. A.} and Nikiforova, {A. A.} and Nikolashvili, {M. G.} and E. Ovcharov and N. Rizzi and A. Sadun and Savchenko, {S. S.} and E. Semkov and Slater, {J. J.} and Smith, {K. L.} and M. Stojanovic and A. Strigachev and Troitskaya, {Yu. V.} and Troitsky, {I. S.} and Tsai, {A. L.} and O. Vince and A. Valcheva and Vasilyev, {A. A.} and E. Zaharieva and Zhovtan, {A. V.}",
year = "2020",
month = sep,
day = "10",
doi = "10.3847/1538-4357/aba693",
language = "English",
volume = "900",
pages = "137",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2",

}

RIS

TY - JOUR

T1 - Multiwavelength Variability of BL Lacertae Measured with High Time Resolution

AU - Weaver, Z. R.

AU - Williamson, K. E.

AU - Jorstad, S. G.

AU - Marscher, A. P.

AU - Larionov, V. M.

AU - Raiteri, C. M.

AU - Villata, M.

AU - Acosta-Pulido, J. A.

AU - Bachev, R.

AU - Baida, G. V.

AU - Balonek, T. J.

AU - Benítez, E.

AU - Borman, G. A.

AU - Bozhilov, V.

AU - Carnerero, M. I.

AU - Carosati, D.

AU - Chen, W. P.

AU - Damljanovic, G.

AU - Dhiman, V.

AU - Dougherty, D. J.

AU - Ehgamberdiev, S. A.

AU - Grishina, T. S.

AU - Gupta, A. C.

AU - Hart, M.

AU - Hiriart, D.

AU - Hsiao, H. Y.

AU - Ibryamov, S.

AU - Joner, M.

AU - Kimeridze, G. N.

AU - Kopatskaya, E. N.

AU - Kurtanidze, O. M.

AU - Kurtanidze, S. O.

AU - Larionova, E. G.

AU - Matsumoto, K.

AU - Matsumura, R.

AU - Minev, M.

AU - Mirzaqulov, D. O.

AU - Morozova, D. A.

AU - Nikiforova, A. A.

AU - Nikolashvili, M. G.

AU - Ovcharov, E.

AU - Rizzi, N.

AU - Sadun, A.

AU - Savchenko, S. S.

AU - Semkov, E.

AU - Slater, J. J.

AU - Smith, K. L.

AU - Stojanovic, M.

AU - Strigachev, A.

AU - Troitskaya, Yu. V.

AU - Troitsky, I. S.

AU - Tsai, A. L.

AU - Vince, O.

AU - Valcheva, A.

AU - Vasilyev, A. A.

AU - Zaharieva, E.

AU - Zhovtan, A. V.

PY - 2020/9/10

Y1 - 2020/9/10

N2 - In an effort to locate the sites of emission at different frequencies and physical processes causing variability in blazar jets, we have obtained high time-resolution observations of BL Lacertae over a wide wavelength range: with the Transiting Exoplanet Survey Satellite (TESS) at 6000-10000 Å with 2 minute cadence; with the Neil Gehrels Swift satellite at optical, UV, and X-ray bands; with the Nuclear Spectroscopic Telescope Array at hard X-ray bands; with the Fermi Large Area Telescope at γ-ray energies; and with the Whole Earth Blazar Telescope for measurement of the optical flux density and polarization. All light curves are correlated, with similar structure on timescales from hours to days. The shortest timescale of variability at optical frequencies observed with TESS is ∼0.5 hr. The most common timescale is 13 ± 1 hr, comparable with the minimum timescale of X-ray variability, 14.5 hr. The multiwavelength variability properties cannot be explained by a change solely in the Doppler factor of the emitting plasma. The polarization behavior implies that there are both ordered and turbulent components to the magnetic field in the jet. Correlation analysis indicates that the X-ray variations lag behind the γ-ray and optical light curves by up to ∼0.4 day. The timescales of variability, cross-frequency lags, and polarization properties can be explained by turbulent plasma that is energized by a shock in the jet and subsequently loses energy to synchrotron and inverse Compton radiation in a magnetic field of strength ∼3 G.

AB - In an effort to locate the sites of emission at different frequencies and physical processes causing variability in blazar jets, we have obtained high time-resolution observations of BL Lacertae over a wide wavelength range: with the Transiting Exoplanet Survey Satellite (TESS) at 6000-10000 Å with 2 minute cadence; with the Neil Gehrels Swift satellite at optical, UV, and X-ray bands; with the Nuclear Spectroscopic Telescope Array at hard X-ray bands; with the Fermi Large Area Telescope at γ-ray energies; and with the Whole Earth Blazar Telescope for measurement of the optical flux density and polarization. All light curves are correlated, with similar structure on timescales from hours to days. The shortest timescale of variability at optical frequencies observed with TESS is ∼0.5 hr. The most common timescale is 13 ± 1 hr, comparable with the minimum timescale of X-ray variability, 14.5 hr. The multiwavelength variability properties cannot be explained by a change solely in the Doppler factor of the emitting plasma. The polarization behavior implies that there are both ordered and turbulent components to the magnetic field in the jet. Correlation analysis indicates that the X-ray variations lag behind the γ-ray and optical light curves by up to ∼0.4 day. The timescales of variability, cross-frequency lags, and polarization properties can be explained by turbulent plasma that is energized by a shock in the jet and subsequently loses energy to synchrotron and inverse Compton radiation in a magnetic field of strength ∼3 G.

KW - BL Lacertae objects

KW - Active galaxies

KW - 164

KW - Eywords: galaxies: active

KW - BL Lacertae objects: individual: BL Lacertae

KW - 3C 454.3

KW - WEBT CAMPAIGNS

KW - LARGE-AREA TELESCOPE

KW - LIGHT CURVES

KW - OPTICAL VARIABILITY

KW - GAMMA-RAY

KW - ACTIVE GALACTIC NUCLEI

KW - X-RAY

KW - RADIO-SOURCES

KW - MAGNETIC-FIELD

UR - http://www.scopus.com/inward/record.url?scp=85091014449&partnerID=8YFLogxK

UR - https://www.mendeley.com/catalogue/db1bc8f8-9ea7-3cf9-9163-58762d30a2b9/

U2 - 10.3847/1538-4357/aba693

DO - 10.3847/1538-4357/aba693

M3 - Article

VL - 900

SP - 137

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 137

ER -

ID: 71063298