Blazars are active galactic nuclei (AGN) with relativistic jets whose non-thermal radiation is extremely variable on various timescales1,2,3. This variability seems mostly random, although some quasi-periodic oscillations (QPOs), implying systematic processes, have been reported in blazars and other AGN. QPOs with timescales of days or hours are especially rare4 in AGN and their nature is highly debated, explained by emitting plasma moving helically inside the jet5, plasma instabilities6,7 or orbital motion in an accretion disc7,8. Here we report results of intense optical and γ-ray flux monitoring of BL Lacertae (BL Lac) during a dramatic outburst in 2020 (ref. 9). BL Lac, the prototype of a subclass of blazars10, is powered by a 1.7 × 108 MSun (ref. 11) black hole in an elliptical galaxy (distance = 313 megaparsecs (ref. 12)). Our observations show QPOs of optical flux and linear polarization, and γ-ray flux, with cycles as short as approximately 13 h during the highest state of the outburst. The QPO properties match the expectations of current-driven kink instabilities6 near a recollimation shock about 5 parsecs (pc) from the black hole in the wake of an apparent superluminal feature moving down the jet. Such a kink is apparent in a microwave Very Long Baseline Array (VLBA) image.
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The data taken and assembled by the WEBT collaboration are stored in the WEBT archive at the Osservatorio Astrofisico di Torino, INAF (https://www.oato.inaf.it/blazars/webt/). The published data are available on request to the WEBT President, Massimo Villata (email@example.com).
Raiteri, C. M. et al. Blazar spectral variability as explained by a twisted inhomogeneous jet. Nature 552, 374–377 (2017).
Wehrle, A. E. et al. Erratic flaring of BL Lac in 2012–2013: multiwavelength observations. Astrophys. J. 816, 53 (2016).
Larionov, V. M. et al. Multiwavelength behaviour of the blazar 3C 279: decade-long study from γ-ray to radio. Mon. Not. R. Astron. Soc. 492, 3829–3848 (2020).
Gupta, A. Multi-wavelength intra-day variability and quasi-periodic oscillation in blazars. Galaxies 6, 1 (2018).
Sarkar, A. et al. Multi-waveband quasi-periodic oscillations in the light curves of blazar CTA 102 during its 2016–2017 optical outburst. Astron. Astrophys. 642, 129–137 (2020).
Dong, L., Zhang, H. & Giannios, D. Kink instabilities in relativistic jets can drive quasi-periodic radiation signatures. Mon. Not. R. Astron. Soc. 494, 1817–1825 (2020).
Roy, A. et al. Transient quasi-periodic oscillations at γ-rays in the TeV blazar PKS 1510-089. Mon. Not. R. Astron. Soc. 510, 3641–3649 (2021).
Hong, S., Xiong, D. & Bai, J. Optical quasi-periodic oscillation of the BL Lacertae object S5 0716+714 during the faint state. Astron. J. 155, 31 (2018).
Grishina, T. S. & Larionov, V. M. The blazar BL Lac reaches historical maximum. The Astronomer’s Telegram, no. 13930 (2020).
Stickel, M. et al. The complete sample of 1 Jansky BL Lacertae objects. I - Summary properties. Astrophys. J. 374, 431–439 (1991).
Woo, J.-H. & Urry, C. M. Active galactic nucleus black hole masses and bolometric luminosities. Astrophys. J. 579, 530 (2002).
Bennett, C. L. et al. The 1% concordance Hubble constant. Astrophys. J. 794, 135 (2014).
Miller, J. S., French, H. B. & Hawley, S. A. The spectrum and magnitude of the galaxy associated with BL Lacertae. Astrophys. J. 219, L85–L87 (1978).
Remillard, R. A. & McClintock, J. E. X-ray properties of black-hole binaries. Annu. Rev. Astron. Astrophys. 44, 49–92 (2006).
Ashton, D. I. & Middleton, M. J. Searching for energy-resolved quasi-periodic oscillation in AGN. Mon. Not. R. Astron. Soc. 501, 5478–5499 (2021).
Abdollahi, S. et al. Fermi large area telescope fourth source catalog. Astrophys. J. Suppl. Ser. 247, 33 (2020).
Albert, J. et al. Discovery of very high energy γ-ray emission from the low-frequency-peaked BL Lacertae object BL Lacertae. Astrophys. J. 666, L17 (2007).
BEAM-ME program – Blazars Entering the Astrophysical Multi-Messenger Era http://www.bu.edu/blazars/BEAM-ME.html (2022).
Jorstad, S. G. et al. Polarimetric observations of 15 active galactic nuclei at high frequencies: jet kinematics from bimonthly monitoring with the Very Long Baseline Array. Astron. J. 130, 1418–1466 (2005).
Cohen, M. H. et al. Studies of the jet in BL Lacertae. I. Recollimation shock and moving emission features. Astrophys. J. 787, 151–160 (2014).
Jorstad, S. G. et al. Kinematics of parsec-scale jets of gamma-ray blazars at 43 GHz within the VLBA-BU-BLAZAR program. Astrophys. J. 846, 98–132 (2017).
Gómez, J. L. et al. Hydrodynamical models of superluminal sources. Astrophys. J. 482, L33 (1997).
Fuentes, A., Gómez, J. L., Martí, J. M. & Perucho, M. Total and linearly polarized synchrotron emission from overpressured magnetized relativistic jets. Astrophys. J. 860, 121 (2018).
Lister, M. L. et al. Monitoring of jets in active galactic nuclei with VLBA experiments. XVIII. Kinematics and inner jet evolution of bright radio-loud active galaxies. Astrophys. J. 923, 30 (2021).
O’Sullivan, S. P. & Gabuzda, D. C. Magnetic field strength and spectral distribution of six parsec-scale active galactic nuclei jets. Mon. Not. R. Astron. Soc. 400, 26–42 (2009).
Cohen, M. H. et al. Studies of the Jet in BL Lacertae. II. Superluminal Alfvén waves. Astrophys. J. 803, 3 (2015).
Schulz, M. & Mudelsee, M. REDFIT: estimating red-noise spectra directly from unevenly spaced paleoclimatic time series. Comput. Geosci. 28, 421–426 (2002).
Grossman, A., Kronland-Martinet & R. Morlet, J. in Wavelets: Time-Frequency Methods and Phase Space (eds Combes, J.-M., Grossman, A. & Tchamitchinan, P.) 2–20 (Springer, 1989).
Foster, G. Wavelets for period analysis of unevenly sampled time series. Astron. J. 112, 1709–1729 (1996).
Barniol, D. R., Tchekhovskoy, A. & Giannios, D. Simulations of AGN jets: magnetic kink instability versus conical shocks. Mon. Not. R. Astron. Soc. 469, 4957–4978 (2017).
Villata, M. et al. The WEBT BL Lacertae campaign 2000. Astron. Astrophys. 390, 407–421 (2002).
Raiteri, C. M. et al. WEBT multiwavelength monitoring and XMM-Newton observations of BL Lacertae in 2007–2008. Unveiling different emission components. Astron. Astrophys. 507, 769–779 (2009).
Weaver, Z. R. et al. Multiwavelength variability of BL Lacertae measured with high time resolution. Astrophys. J. 900, 137 (2020).
Fiorucci, M. & Tosti, G. VRI photometry of stars in the fields of 12 BL Lacertae objects. Astron. Astrophys. Suppl. Ser. 116, 403–407 (1996).
Schmidt, G. D., Elston, R. & Lupie, O. L. The Hubble Space Telescope northern-hemisphere grid of stellar polarimetric standards. Astron. J. 104, 1563–1567 (1992).
Nolan, P. L. et al. Fermi large area telescope second source catalog. Astrophys. J. Suppl. Ser. 199, 31 (2012).
Alexander, T. in Astronomical Time Series. Astrophysics and Space Science Library, Vol. 218 (eds Maoz, D. Sternberg, A. & Leibowitz, E. M.) 163–170 (Springer, 1997).
Alexander, T. Improved AGN light curve analysis with the z-transformed discrete correlation function. Preprint at https://arxiv.org/abs/1302.1508 (2013).
Emmanoulopoulos, D., McHardy, I. M. & Papadakis, I. E. Generating artificial light curves: revisited and updated. Mon. Not. R. Astron. Soc. 433, 907–927 (2013).
Done, C. et al. The X-ray variability of NGC 6814: power spectrum. Astrophys. J. 400, 138–152 (1992).
Uttley, P., McHardy, I. M. & Papadakis, I. E. Measuring broad-band power spectra of active galactic nuclei with RXTE. Mon. Not. R. Astron. Soc. 332, 231–250 (2005).
Chatterjee, R. et al. Correlated multi-wave band variability in the blazar 3C 279 from 1996 to 2007. Astrophys. J. 689, 79 (2008).
Shepherd, M. C. Difmap: an interactive program for synthesis imaging. ASP Conf. Ser. 125, 77–84 (1997).
Bach, U. et al. Structure and flux variability in the VLBI jet of BL Lacertae during the WEBT campaigns (1995–2004). Astron. Astrophys. 456, 105–115 (2006).
Scargle, J. D. Studies in astronomical time series analysis. IV. Modeling chaotic and random processes with linear filters. Astrophys. J. 359, 469–482 (1990).
Torrence, C. & Compo, G. P. A practical guide to wavelet analysis. Bull. Am. Meteorol. Soc. 79, 61–78 (1998).
An, T. et al. Periodic radio variabilities in NRAO 530: a jet–disc connection? Mon. Not. R. Astron. Soc. 434, 3487–3496 (2013).
O’Neill, S. et al. The unanticipated phenomenology of the blazar PKS 2131–021: a unique supermassive black hole binary candidate. Astrophys. J. Lett. 926, L35 (2022).
Mizuno, Y. et al. Three-dimensional relativistic magnetohydrodynamic simulations of current-driven instability. I. Instability of a static column. Astrophys. J. 700, 684 (2009).
Zhang, H. et al. Polarization signatures of kink instabilities in the blazar emission region from relativistic magnetohydrodynamic simulations. Astrophys. J. 835, 125 (2017).
Bodo, G., Tavecchio, F. & Sironi, L. Kink-driven magnetic reconnection in relativistic jets: consequences for X-ray polarimetry of BL Lacs. Mon. Not. R. Astron. Soc. 501, 2836–2847 (2021).
Acharya, S., Borse, N. S. & Vaidya, B. Numerical analysis of long-term variability of AGN jets through RMHD simulations. Mon. Not. R. Astron. Soc. 506, 1862–1878 (2021).
We dedicate this paper to Dr. Valeri M. Larionov, who was a prominent member of the WEBT collaboration. The research reported here is based on work supported in part by US National Science Foundation grants AST-2108622 and AST-2107806, and NASA Fermi GI grants 80NSSC20K1567, 80NSSC21K1917 and 80NSSC21K1951; by Shota Rustaveli National Science Foundation of Georgia under contract FR-19-6174; by the Bulgarian National Science Fund of the Ministry of Education and Science under grants DN 18-10/2017, DN 18-13/2017, KP-06-H28/3 (2018), KP-06-H38/4 (2019) and KP-06-KITAJ/2 (2020), and by National RI Roadmap Project D01-383/18.12.2020 of the Ministry of Education and Science of the Republic of Bulgaria; by JSPS KAKENHI grant #19K03930 of Japan; by the Ministry of Education, Science and Technological Development of the Republic of Serbia (contract 451-03-9/2021-14/200002) and observing grant support from the Institute of Astronomy and Rozhen NAO BAS through the bilateral joint research project ‘Gaia Celestial Reference Frame (CRF) and fast variable astronomical objects’; by the Agenzia Spaziale Italiana (ASI) through contracts I/037/08/0, I/058/10/0, 2014-025-R.0, 2014-025-R.1.2015 and 2018-24-HH.0 to the Italian Istituto Nazionale di Astrofisica (INAF). H.Z. is supported by the NASA Postdoctoral Program at Goddard Space Flight Center, administered by ORAU. M.V.P. is partially supported by the Russian Foundation for Basic Research grant 20-02-00490. G.B. acknowledges support from the State Agency for Research of the Spanish MCIU through the ‘Center of Excellence Severo Ochoa’ award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709) and from the Spanish ‘Ministerio de Ciencia e Innovacíon’ (MICINN) through grant PID2019-107847RB-C44. M.D.J. thanks the Brigham Young University Department of Physics and Astronomy for continued support of the extragalactic monitoring programme under way at the West Mountain Observatory. R.C. thanks ISRO for support under the AstroSat archival data utilization programme and BRNS for support through a project grant (sanction no. 57/14/10/2019-BRNS). The measurements at the Hans Haffner Observatory, Hettstadt, Germany, were supported by Baader Planetarium, Mammendorf, Germany. This study was based (in part) on observations conducted using the 1.8-m Perkins Telescope Observatory (PTO) in Arizona, USA, which is owned and operated by Boston University. These results made use of the Lowell Discovery Telescope (LDT) at Lowell Observatory. Lowell Observatory is a private, non-profit institution dedicated to astrophysical research and public appreciation of astronomy, and operates the LDT in partnership with Boston University, the University of Maryland and the University of Toledo. This paper is partly based on observations made with the IAC-80 operated on the island of Tenerife by the Instituto de Astrofisica de Canarias in the Spanish Observatorio del Teide and on observations made with the LCOGT telescopes, one of whose nodes is located at the Observatorios de Canarias del IAC on the island of Tenerife in the Observatorio del Teide. This paper is partly based on observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. The VLBA is an instrument of the NRAO, USA. The NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.
The authors declare no competing interests.
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Extended data figures and tables
a, R-band flux density light curve (n = 16,497). The solid magenta curve during the outburst plots a spline approximation of the long-term trend. b, Degree of polarization versus time (n = 1,285). c, Position angle of polarization versus time (n = 1,285). The red and blue dotted lines mark directions along and transverse to the jet axis, respectively. d, γ-Ray light curve (n = 1,398). The grey area denotes the 1σ uncertainty in the time of ejection of superluminal knot K (dotted grey line). Different symbols and colours indicate observations conducted by different telescopes, designations of which are given in Extended Data Table 1. The error bars are 1σ uncertainties (in plot a, they are smaller than the symbols).
a, z-Transformed discrete correlation function correlations between the γ-ray and R-band light curves for the entire dataset (black), between the γ-ray flux and R-band flux density residuals (blue) and between the theoretical γ-ray and R-band light curves (red) during the highest outburst state shown in Fig. 2. b, z-Transformed discrete correlation function correlations between the R-band flux density and degree of polarization for similar periods as in plot a. The dotted red horizontal lines correspond to 3σ probability of chance occurrence.
The global intensity peak is 3.148 Jy beam−1 and contour levels start at 0.4% of the peak, then increase by factors of √2. Images are convolved with a circular beam of radius 0.1 mas (bottom-left circle). The coloured circles represent the FWHM areas of Gaussian components used to model the intensity distribution at each epoch, with colours matching those in Fig. 3b.
a, For optical flux densities. b, For γ-ray fluxes. c, For degree of polarization. The black curves show the corrected periodograms; the blue lines represent the theoretical red-noise spectra; the red lines mark the 99% (solid) and 95% (dashed) significance levels. The periods corresponding to the most significant peaks, touching or exceeding the 99% levels, are indicated.
For the R-band light curve (a), the γ-ray light curve (b) and the fractional polarization curve (c). Black contours in a and b indicate periods significant at the 99% level; grey contours in c indicate periods significant at the 92% level. Dashed white curves represent a cone of influence (COI), in which the information outside is affected by edge artefacts; numbers near contours indicate some periods for clarity.
For the R-band light curve (a), the γ-ray light curve (b) and the fractional polarization curve (c). Dashed black curves indicate periods significant at the 99% level; numbers near contours indicate some periods for clarity.
a, Oscillations in optical R-band flux density during the outburst over the time interval 13 August 2020 to 18 September 2020 (n = 8,106), with the long-term trend subtracted. For comparison, the red curve represents a sinusoidal function with a period of 0.55 days and an amplitude of 20 mJy. b, Average profile of the optical flux density pulse (solid red curve). different colours indicate different pulses (2, 5, 7, 8, 9 and 12, as numbered in Fig. 1b). c, Average profile (solid black curve) of fractional polarization pulses (colour symbols), each normalized by its maximum, and normalized average profile of R-band flux density pulse (solid red curve). In all plots, error bars represent 1σ uncertainties.
a, Triangle plot of posterior distributions of model parameters, sampled from 64 walkers with 60,000 iterations through MCMC; dashed lines in the histogram represent 16%, 50% and 84% quantiles, respectively (from left to right), for each parameter (see Methods). b–e, Distributions of residuals between the data and the model presented in Fig. 2 for R-band flux density (b), degree (c) and position angle (d) of polarization, and γ-ray flux (e).
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Jorstad, S.G., Marscher, A.P., Raiteri, C.M. et al. Rapid quasi-periodic oscillations in the relativistic jet of BL Lacertae. Nature 609, 265–268 (2022). https://doi.org/10.1038/s41586-022-05038-9