Polarization and Spectral Energy Distribution in OJ 287 during the 2016/17 Outbursts

Valtonen, M. J.; Zoła, S.; Jermak, Helen; Ciprini, S.; Hudec, R.; Dey, Lankeswar; Gopakumar, A.; Reichart, Daniel L.; Caton, D. B.; Gazeas, K.; Matsumoto, Katsura; Ogłoza, W.; Dróżdż, M.; Aliçavuş, F.; Baransky, Alexander; Berdyugin, A.; Boumis, P.; Bufan, Y.; Dębski, B.; Er, H.; Erdem, A.; Godunova, V.; Haque, Shirin; Hoette, V.; Janík, Ján; Kidger, M.; Kundera, T.; Kurowski, Sebastian; Liakos, A.; Mohammed, I.; Nilsson, K.; Pajdosz, U.; Piirola, V.; Pursimo, T.; Rajkumar, Brandon; Simon, A.; Siwak, M.; Сонбас, Э.; Steele, I. A.; Vasylenko, V.; Żejmo, M.; Zieliński, Paweł

doi:10.3390/galaxies5040083

Cited by 21 publications

(17 citation statements)

References 20 publications

(20 reference statements)

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“…Most importantly, our model has accurately predicted the starting times of the widely observed 1995, 2005, 2007 and 2015 outbursts [8,[20][21][22] which places the model in much stronger ground than any of the alternative models. Let us note that the 1994 flare was also predicted successfully by Sillanpää et al [11], based on their constant period BBH model.…”

Section: Appendix Alternative Models For Oj 287mentioning

confidence: 78%

“…In contrast, the timescales associated with processes like jet turning are several months to years. • At the times of impact flares, the degree of polarization always goes down [20,21]. In the BBH model, this is due to an additional unpolarized component associated with the bremsstrahlung radiation at the time of outburst, which is in addition to the long-lived jet emission.…”

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confidence: 99%

“…• A natural (and a powerful) feature of the BBH impact model is its accurate predictive power. Indeed, the model accurately predicted the starting times for the widely observed 1995, 2005, 2007 and 2015 outbursts [8,[20][21][22]. It is rather difficult to make testable predictions using the alternative models for OJ 287 as they assume that the flares are strictly periodic which puts the prediction off by up to several years.…”

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confidence: 99%

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The Unique Blazar OJ 287 and Its Massive Binary Black Hole Central Engine

et al. 2019

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The bright blazar OJ 287 is the best-known candidate for hosting a nanohertz gravitational wave (GW) emitting supermassive binary black hole (SMBBH) in the present observable universe. The binary black hole (BBH) central engine model, proposed by Lehto and Valtonen in 1996, was influenced by the two distinct periodicities inferred from the optical light curve of OJ 287. The current improved model employs an accurate general relativistic description to track the trajectory of the secondary black hole (BH) which is crucial to predict the inherent impact flares of OJ 287. The successful observations of three predicted impact flares open up the possibility of using this BBH system to test general relativity in a hitherto unexplored strong field regime. Additionally, we briefly describe an on-going effort to interpret observations of OJ 287 in a Bayesian framework.

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Section: Appendix Alternative Models For Oj 287mentioning

confidence: 78%

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confidence: 99%

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confidence: 99%

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The Unique Blazar OJ 287 and Its Massive Binary Black Hole Central Engine

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“…Valtonen et al (2008aValtonen et al ( , 2010 explain the deviations of the outbursts from strict periodicity as arising from this gravitational wave driven in-spiraling of the binary black hole system present at the centre of OJ 287. According to the latest iteration of the model, the source is an inspiraling and precessing binary SMBH system with a current period of 12.055 years which decreases by 38 days/century and involves a minimum separation of 1.1 years between the twin outbursts associated with the disk impacts (Valtonen et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Characterizing Optical Variability of OJ 287 in 2016–2017

Gupta

Gaur

Wiita

et al. 2019

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We report on a recent multi-band optical photometric and polarimetric observational campaign of the blazar OJ 287 which was carried out during September 2016 -December 2017. We employed nine telescopes in Spain and the United States. We collected over 1800 photometric image frames in BVRI bands and over 100 polarimetric measurements over ∼175 nights. In 11 nights with many quasi-simultaneous multi-band (V, R, I) observations, we did not detect any genuine intraday variability in flux or color. On longer timescales, multiple flaring events were seen. Large changes in color with respect to time and in a color-magnitude diagram were seen, and while only a weak systematic variability trend was noticed in color with respect to time, the color-magnitude diagram shows a bluer-when-brighter trend. Large changes in the degree of polarization, and substantial swings in the polarization angle were detected. The fractional Stokes parameters of the polarization showed a systematic trend with time in the beginning of these observations, followed by chaotic changes and then an apparently systematic variation at the end. These polarization changes coincide with the detection and duration of the source at very high energies as seen by VERITAS. The spectral index shows a systematic variation with time and V-band magnitude. We briefly discuss possible physical mechanisms that could explain the observed flux, color, polarization, and spectral variability.

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“…Previously, the long-term (2005-2008) observing campaign data evidenced the possible existence of a ∼ 50-day quasi periodic primary ISCO [7]. The optical flux and polarization data of the following 2016-2017 observing season indicated a persisting activity with high levels of polarization degree indicating a synchrotron emission from the primary SMBH jet, explained as in-jet flares induced by accretion perturbations following the Nov. 2015 impact [15]. An intensive and continuous three-month observing campaign of OJ 287 was performed by the Kepler space telescope, with 1 minute sampling at >90% duty cycle and high S/N, during the K2 Campaign #5 (Apr.27-Jul.13 2015, [16,2] and Fig.…”

Section: Pos(ifs2017)041mentioning

confidence: 94%

Time-domain behavior of blazar OJ 287 and the binary supermassive black hole conjecture

Ciprini

Valtonen

Zoła³

et al. 2017

Proceedings of 7th International Fermi Symposium — PoS(IFS2017)

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The proper understanding of blazar variability at the various electromagnetic spectral bands is one goal of multifrequency astrophysics. In this frame a peculiar and controversial phenomenology is the periodicity, postulated for long-term radio or optical flux light curves of about a dozen of blazars. The well-known BL Lac object OJ 287 (PKS 0851+202, S3 0851+20, PG 0851+202, z = 0.306) is not only a high-variable, peculiar, extragalactic source with hints for approximatively cyclical optical outbursts, but it also represents a case of substantial intensive and extensive (longterm) multifrequency observations. This rich database allow us a deeper analysis based on a wide range of variability timescales with some recent results that are highlighted here.

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Polarization and Spectral Energy Distribution in OJ 287 during the 2016/17 Outbursts

Cited by 21 publications

References 20 publications

The Unique Blazar OJ 287 and Its Massive Binary Black Hole Central Engine

The Unique Blazar OJ 287 and Its Massive Binary Black Hole Central Engine

Characterizing Optical Variability of OJ 287 in 2016–2017

Time-domain behavior of blazar OJ 287 and the binary supermassive black hole conjecture

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