Evidence of Jet–Clump Interaction: A Flip of the Radio Jet Head of 3C 84

Kino, Motoki; Wajima, Kiyoaki; Kawakatu, Nozomu; Nagai, Hiroshi; Orienti, M.; Giovannini, G.; Hada, Kazuhiro; Niinuma, Kotaro; Giroletti, M.

doi:10.3847/1538-4357/aad6e3

Cited by 28 publications

(33 citation statements)

References 71 publications

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“…The complex pc-scale radio structure of 3C 84 has been investigated by many authors using VLBI observations at different observing frequencies (e.g., [4][5][6][7][8][9]). The radio structure of 3C 84 does not resemble the typical core-jet sources mapped with VLBI observations (e.g., [10]).…”

Section: Vlbi Observations Of 3c 84mentioning

confidence: 99%

“…Several authors (e.g., [4]) have mentioned that the well-known radio structure of 3C 84 contains substructure. This substructure is usually not modeled.…”

Section: Re-analysis Of Vlba Datamentioning

confidence: 99%

“…We compare the light-curve evolution of 3C 84 at low energies in the radio regime with high energy GeV data provided by the Fermi Gamma-ray Space Telescope (Fermi-LAT). To generate the GeV light curves we analyzed Pass 8 photon data 3 using version v11r5p3 of the Fermi ScienceTools 4 , including all photon data within 15 • around the position of 3C84. We fit 3C84 with a log-parabola of the form…”

Section: Fermi-lat Data Analysismentioning

confidence: 99%

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3C 84: Observational Evidence for Precession and a Possible Relation to TeV Emission

et al. 2019

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3C 84 (NGC 1275, Perseus A) is a bright radio source at the center of an ongoing merger, where HST observations show two colliding spiral galaxies. 3C 84 holds promise to improve our understanding about how of the activity of active galactic nuclei, the formation of supermassive binary black holes, feedback processes, and galaxy collisions are interrelated. 3C,84 is one of only six radio galaxies, which reveal TeV emission. The origin of this TeV emission is still a matter of debate. Our present study is based on high resolution radio interferometric observations (15 GHz) of the pc-scale jet in this complex radio galaxy. We have re-modeled and re-analyzed 42 VLBA observations of 3C 84, performed between 1999.99 and 2017.65. In order to enable a proper alignment of the VLBA observations, we developed a method of a “differential” alignment whereby we select one reference point and minimize the deviations from this reference point in the remaining epochs. As a result, we find strong indication for a precession of the 3C 84 jet—not only for its central regions, but also for the outer lobe at 10 mas distance. These findings are further supported by our kinematic precession modeling of the radio flux-density monitoring data provided by the University of Michigan Radio Observatory and the Owens Valley Radio Observatory, which yields a precession time scale of about 40 yr. This time scale is further supported by literature maps obtained about 40 yr ago (1973 and 1974.1) which reveal a similar central radio structure. We suggest that the TeV flare detected by MAGIC may correlate with the precession of 3C 84, as we disentangle a projected reversal point of the precessing motion that correlates with the flaring time. This may physically be explained by a precessing jet sweeping over a new region of so far undisturbed X-ray gas which would then lead to shock-produced TeV-emission. In addition, we perform a correlation analysis between the radio data and GeV data obtained by the Fermi Gamma-ray Space Telescope and find that the γ -ray data are lagging the radio data by 300–400 days. A possible explanation could be that the radio and the GeV data stem from different emission regions. We discuss our findings and propose that the detected jet precession can also account for the observed cavities in the X-ray emission on kpc-scales.

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Section: Vlbi Observations Of 3c 84mentioning

confidence: 99%

“…Several authors (e.g., [4]) have mentioned that the well-known radio structure of 3C 84 contains substructure. This substructure is usually not modeled.…”

Section: Re-analysis Of Vlba Datamentioning

confidence: 99%

Section: Fermi-lat Data Analysismentioning

confidence: 99%

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3C 84: Observational Evidence for Precession and a Possible Relation to TeV Emission

et al. 2019

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“…In this context, some clues to the pc-scale circumnuclear environments have been found by monitoring the long-term trajectory of C3: the head of the restarted jet. While C3 was traveling straight towards the south after its ejection [103], during mid 2015, C3 showed a sudden change of direction, moving towards the east by 0.4 mas (0.14 pc in linear scale) [102] (Figure 4 right), together with enhanced radio emission in both total [102,104] and polarized fluxes [105]. This peculiar behavior is hard to be explained by the intrinsic motion of the jet, whereas it would be naturally explained if C3 is interacting with an inhomogeneous dense clumpy medium [106].…”

Section: C 84mentioning

confidence: 99%

Relativistic Jets from AGN Viewed at Highest Angular Resolution

Hada

2019

Galaxies

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Accreting supermassive black holes in active galactic nuclei (AGN) produce powerful relativistic jets that shine from radio to GeV/TeV γ-rays. Over the past decade, AGN jets have extensively been studied in various energy bands and our knowledge about the broadband emission and rapid flares are now significantly updated. Meanwhile, the progress of magnetohydrodynamic simulations with a rotating black hole have greatly improved our theoretical understanding of powerful jet production. Nevertheless, it is still challenging to observationally resolve such flaring sites or jet formation regions since the relevant spatial scales are tiny. Observations with very long baseline interferometry (VLBI) are currently the only way to directly access such compact scales. Here we overview some recent progress of VLBI studies of AGN jets. As represented by the successful black hole shadow imaging with the Event Horizon Telescope, the recent rapid expansion of VLBI capability is remarkable. The last decade has also seen a variety of advances thanks to the advent of RadioAstron, GMVA, new VLBI facilities in East Asia as well as to the continued upgrade of VLBA. These instruments have resolved the innermost regions of relativistic jets for a number of objects covering a variety of jetted AGN classes (radio galaxies, blazars, and narrow-line Seyfert 1 galaxies), and the accumulated results start to establish some concrete (and likely universal) picture on the collimation, acceleration, recollimation shocks, magnetic field topology, and the connection to high-energy flares in the innermost part of AGN jets.

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“…This opens a new opportunity for detailed high-resolution monitoring studies of AGN jets along with other existing VLBI facilities such as the VLBA. An increasing number of sources including nearby radio galaxies, γray blazars, and high redshift quasars are intensively monitored with KaVA [9,10,11,12,13,14]. However, KaVA is just the first step towards the larger East Asian collaboration including China and other nearby countries.…”

Section: Introductionmentioning

confidence: 99%