Flaring radio lanterns along the ridge line: long-term oscillatory motion in the jet of S5 1803+784

Kun, Emma; Karouzos, Marios; Gabányi, K. É.; Britzen, S.; Kurtanidze, O. M.; Gergely, L.

doi:10.1093/mnras/sty981

Cited by 15 publications

(17 citation statements)

References 40 publications

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“…No definite periodicity was detected in our optical and 𝛾-ray light curves of S5 1803+784. In recent studies Kun et al (2018) a period of about 8 years for the precession of the relativistic jet has been claimed, based on the analysis of VLBI images. From the data that we collected, there is no clear optical or 𝛾-ray counterpart of this phenomenon.…”

Section: Discussionmentioning

confidence: 99%

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Multi-wavelength flare observations of the blazar S5 1803+784

Nesci,

Cutini,

Stanghellini

et al. 2021

Preprint

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The radio, optical, and 𝛾-ray light curves of the blazar S5 1803+784, from the beginning of the Fermi Large Area Telescope (LAT) mission in August 2008 until December 2018, are presented. The aim of this work is to look for correlations among different wavelengths useful for further theoretical studies. We analyzed all the data collected by Fermi LAT for this source, taking into account the presence of nearby sources, and we collected optical data from our own observations and public archive data to build the most complete optical and 𝛾-ray light curve possible. Several 𝛾-ray flares (F > 2.3 10 −7 ph(E > 0.1GeV) cm −2 s −1 ) with optical coverage were detected, all but one with corresponding optical enhancement; we also found two optical flares without a 𝛾-ray counterpart. We obtained two Swift Target of Opportunity observations during the strong flare of 2015. Radio observations performed with VLBA and EVN through our proposals in the years 2016-2020 were analyzed to search for morphological changes after the major flares. The optical/𝛾-ray flux ratio at the flare peak varied for each flare. Very minor optical V-I color changes were detected during the flares. The X-ray spectrum was well fitted by a power law with photon spectral index 𝛼=1.5, nearly independent of the flux level: no clear correlation with the optical or the 𝛾-ray emission was found. The 𝛾-ray spectral shape was well fitted by a power law with average photon index 𝛼= 2.2. These findings support an Inverse Compton origin for the high-energy emission of the source, nearly co-spatial with the optically emitting region. The radio maps showed two new components originating from the core and moving outwards, with ejection epochs compatible with the dates of the two largest 𝛾-ray flares.

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Section: Discussionmentioning

confidence: 99%

“…Roland et al 2008 and references therein). Evidence in support of a helical jet has been presented by Britzen et al (2010) and Kun et al (2018) from a long term monitoring at different frequencies.…”

Section: Data Reductionmentioning

confidence: 99%

Multi-wavelength flare observations of the blazar S5 1803+784

Nesci,

Cutini,

Stanghellini

et al. 2021

Preprint

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“…Modeling the observed high-resolution structure and kinematics of VLBI jets in quasars is usually applied to infer parameters of suspected SMBH binaries (e.g. Britzen et al 2001;Lobanov & Roland 2005;Britzen et al 2012;Valtonen & Wiik 2012;Caproni et al 2013;Kun et al 2014Kun et al , 2015Kun et al , 2018. In some of these cases, there is independent indication for the existence of the binary, e.g.…”

Section: Jet Modeling With Accurate Binary Parametersmentioning

confidence: 99%

A self-lensing supermassive binary black hole at radio frequencies: the story of Spikey continues

Kun

Frey

Gabányi

2020

Monthly Notices of the Royal Astronomical Society

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ABSTRACT The quasar J1918+4937 was recently suggested to harbour a milliparsec-separation binary supermassive black hole (SMBH), based upon modelling the narrow spike in its high-cadence Kepler optical light curve. Known binary SMBHs are extremely rare, and the tight constraints on the physical and geometric parameters of this object are unique. The high-resolution radio images of J1918+4937 obtained with very long baseline interferometry (VLBI) indicate a rich one-sided jet structure extending to 80 mas. Here we analyse simultaneously made sensitive 1.7- and 5-GHz archive VLBI images as well as snapshot 8.4/8.7-GHz VLBI images of J1918+4937, and show that the appearance of the wiggled jet is consistent with the binary scenario. We develop a jet structural model that handles eccentric orbits. By applying this model to the measured VLBI component positions, we constrain the inclination of the radio jet, as well as the spin angle of the jet emitter SMBH. We find the jet morphological model is consistent with the optical and radio data, and that the secondary SMBH is most likely the jetted one in the system. Furthermore, the decade-long 15-GHz radio flux density monitoring data available for J1918+4937 are compatible with a gradual overall decrease in the total flux density caused by a slow secular change of the jet inclination due to the spin–orbit precession. J1918+4937 could be an efficient high-energy neutrino source if the horizon of the secondary SMBH is rapidly rotating.

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“…The light variations may not be the only direct effect of the moving SMBHs. The effects of SMBBH system orbital motion should be also affecting the jet bending, which could be used to model the SMBBH system properties with jet observations (see, for example [41][42][43][44]) Unfortunately, quasi-periodicities in the jet emission can be induced by intrinsic oscillatory disk instabilities that can mimic periodical behavior.…”

Section: Supermassive Black Hole Binariesmentioning

confidence: 99%

On the Time Scales of Optical Variability of AGN and the Shape of Their Optical Emission Line Profiles

Bon

Marziani

Jovanović

et al. 2019

Atoms

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The mechanism of the optical variability of active galactic nuclei (AGN) is still very puzzling. It is now widely accepted that the optical variability of AGN is stochastic, producing red noise-like light curves. In case they were to be periodic or quasi-periodic, one should expect that the time scales of optical AGN variability should relate to orbiting time scales of regions inside the accretion disks with temperatures mainly emitting the light in this wavelength range. Knowing the reverberation scales and masses of AGN, expected orbiting time scales are in the order of decades. Unfortunately, most of monitored AGN light curves are not long enough to investigate such time scales of periodicity. Here we investigate the AGN optical variability time scales and their possible connections with the broad emission line shapes.

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Flaring radio lanterns along the ridge line: long-term oscillatory motion in the jet of S5 1803+784

Cited by 15 publications

References 40 publications

Multi-wavelength flare observations of the blazar S5 1803+784

Multi-wavelength flare observations of the blazar S5 1803+784

A self-lensing supermassive binary black hole at radio frequencies: the story of Spikey continues

On the Time Scales of Optical Variability of AGN and the Shape of Their Optical Emission Line Profiles

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