A multiband study and exploration of the radio wave - $γ$-ray connection in 3C 84

Paraschos, Georgios Filippos; Mpisketzis, V.; Kim, J. -Y.; Witzel, G.; Krichbaum, T. P.; Zensus, J. A.; Gurwell, M. A.; Lähteenmäki, A.; Tornikoski, M.; Kiehlmann, S.; Readhead, A. C. S.

doi:10.48550/arxiv.2210.09795

Cited by 1 publication

(3 citation statements)

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“…This range is also in agreement with another core shift estimate presented in [6,34]. The interested reader is referred to [18] for a more in-depth presentation of the analysis.…”

Section: Pos(evn2022)019supporting

confidence: 88%

“…Using the DCF approach (see Fig. 3), we find that the 𝛾-rays may either precede the 230 GHz flux by 𝜏 𝛾−230 GHz = 1.56 ± 0.27 years or trail the 230 GHz flux by 𝜏 230 GHz−𝛾 = 1.43 ± 0.30 years Since we find positive and negative time lags between the radio emission and the 𝛾-rays (see [18] for a detailed presentation and discussion of the results), this might indicate multiple locations of emission of the 𝛾-rays, both upstream and downstream of the radio emission, depending on individual flares. At 345 GHz we see a similar effect.…”

Section: Location Of 𝛾-Ray Emissionmentioning

confidence: 71%

“…fitting function (see also [14,23,31,32]). A detailed discussion about both methods is presented in [18].…”

Section: Light Curve Cross-correlation Analysis 31 Core Shiftmentioning

confidence: 99%

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An extensive analysis of the sub-parsec region of 3C 84

Paraschos¹,

Krichbaum²,

Oh³

et al. 2023

Proceedings of 15th European VLBI Network Mini-Symposium and Users' Meeting — PoS(EVN2022)

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The study of jet launching in AGN is an important research method to better understand supermassive black holes (SMBHs) and their immediate surroundings. The main theoretical jet launching scenarios invoke either magnetic field lines anchored to the black holes's (BH) accretion disc [1] or a magnetic field, which is directly connected to its rotating ergosphere [2]. The nearby and bright radio galaxy 3C 84 (NGC 1275) is a very suitable target for testing different jet launching mechanisms, as well as for the study of the innermost, sub-parsec scale AGN structure and the jet origin. Very long baseline interferometry (VLBI) -specifically at millimetre wavelengths -offers an unparalleled view into the physical processes in action, in the close vicinity of SMBHs. Utilising such mm-VLBI observations of 3C 84, we study the jet kinematics of the VLBI core region of 3C 84 by employing all available, high sensitivity 3 mm-VLBI data sets of this source. As part of this analysis we associate the component ejection events with the variability light-curves at different radio frequencies and in the 𝛾-rays. Furthermore, by cross-correlating these light-curves, we determine their time-lags and draw conclusions regarding the location of the high energy emission close to the jet base.

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“…This range is also in agreement with another core shift estimate presented in [6,34]. The interested reader is referred to [18] for a more in-depth presentation of the analysis.…”

Section: Pos(evn2022)019supporting

confidence: 88%

Section: Location Of 𝛾-Ray Emissionmentioning

confidence: 71%