The Two-sided Jet Structures of NGC 1052 at Scales from 300 to 4 × 10<sup>7</sup> Schwarzschild Radii

Nakahara, Satomi; Doi, Akira; Murata, Yasuhiro; Nakamura, Masanori; Hada, Kazuhiro; Asada, Keiichi; Sawada-Satoh, Satoko; Kameno, Seiji

doi:10.3847/1538-3881/ab465b

Cited by 31 publications

(50 citation statements)

References 38 publications

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“…In the case of NGC 1052, one of the two LERG placed on the HERG region, high resolution VLBI observations with the GMVA (Baczko et al 2016) do not clearly resolve the jet base, thus it is plausible that this jet was initially narrow and has experienced a fast expansion at larger distances. Moreover, Nakahara et al (2020) did not confirm a parabolic expansion for this source, suggesting instead a transition from cylindrical to conical shape at a distance of ∼10 4 R S . 3C 84, the other LERG in the HERG region, shows evidence for a more complex profile as well.…”

Section: Mass-scaled Expansion Profilesmentioning

confidence: 65%

“…The transition distance expressed in projected milliarcseconds is reported in Col. 12. We note that some sources in the MOJAVE subsample (e.g., 3C 84, NGC 1052, NGC 6251) have also been studied by other authors (e.g., Tseng et al 2016;Giovannini et al 2018;Nakahara et al 2020) but we refer to the MOJAVE results for uniformity. The dedicated studies are discussed in the text.…”

Section: The Parabolic Jet In Different Sourcesmentioning

confidence: 97%

“…Several observational studies have been performed with the aim of determining the extension of the acceleration and collimation region, thus providing constraints for theoretical models. Such studies were mostly focused on the analysis of low-luminosity radio galaxies, such as NGC 6251 (Tseng et al 2016), 3C 84 (Giovannini et al 2018), 3C 270 (Nakahara et al 2018), 3C 264 (Boccardi et al 2019), NGC 1052 (Nakahara et al 2020) and M 87 (Asada & Nakamura 2012;Mertens et al 2016;Hada et al 2016;Kim et al 2018;Nokhrina et al 2019), but some constraints for high-luminosity radio galaxies, like Cygnus A (Boccardi et al 2016a,b;Nakahara et al 2019), and blazars (Giroletti et al 2008;Akiyama et al 2018;Hada et al 2018;Algaba et al 2019;Traianou et al 2020) were also provided. Moreover, part of the MOJAVE sample was investigated by Pushkarev et al (2017), Kovalev et al (2020).…”

Section: Introductionmentioning

confidence: 99%

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Jet collimation in NGC 315 and other nearby AGN

Boccardi

Perucho

Casadio

et al. 2021

A&A

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Aims. The collimation of relativistic jets in galaxies is a poorly understood process. Detailed radio studies of the jet collimation region have been performed so far in a few individual objects, providing important constraints for jet formation models. However, the extent of the collimation zone as well as the nature of the external medium possibly confining the jet are still debated. Methods. In this article, we present a multifrequency and multiscale analysis of the radio galaxy NGC 315, including the use of mm-VLBI data up to 86 GHz, aimed at revealing the evolution of the jet collimation profile. We then consider results from the literature to compare the jet expansion profile in a sample of 27 low-redshift sources, mainly comprising radio galaxies and BL Lacs, which were classified based on the accretion properties as low-excitation (LEG) and high-excitation (HEG) galaxies. Results. We propose that the jet collimation in NGC 315 is completed on sub-parsec scales. A transition from a parabolic to conical jet shape is detected at zt = 0.58 ± 0.28 parsecs or ∼5 × 103 Schwarzschild radii (RS) from the central engine, a distance which is much smaller than the Bondi radius, rB ∼ 92 pc, estimated based on X-ray data. The jet in this and in a few other LEG in our sample may be initially confined by a thick disk extending out to ∼103 − 104RS. A comparison between the mass-scaled jet expansion profiles of all sources indicates that jets in HEG are surrounded by thicker disk-launched sheaths and collimate on larger scales with respect to jets in LEG. These results suggest that disk winds play an important role in the jet collimation mechanism, particularly in high-luminosity sources. The impact of winds on the origin of the FRI and FRII dichotomy in radio galaxies is also discussed.

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Section: Mass-scaled Expansion Profilesmentioning

confidence: 65%

Section: The Parabolic Jet In Different Sourcesmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

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Jet collimation in NGC 315 and other nearby AGN

Boccardi

Perucho

Casadio

et al. 2021

A&A

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“…Radio jets are seen in other low-luminosity AGNs, e.g. NGC 1052 (Baczko et al 2016(Baczko et al , 2019Nakahara et al 2020). However there are significant differences between both the jet properties and the host galaxy properties between NGC 4151 and these other AGNs.…”

Section: Ngc 4151 and Jets In Other Low-luminosity Agnsmentioning

confidence: 99%

The curious activity in the nucleus of NGC 4151: jet interaction causing variability?

Williams

Baldi

McHardy

et al. 2020

Monthly Notices of the Royal Astronomical Society

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A key characteristic of many active galactic nuclei (AGNs) is their variability, but its origin is poorly understood, especially in the radio domain. Williams et al. (2017) reported a ∼50 per cent increase in peak flux density of the AGN in the Seyfert galaxy NGC 4151 at 1.5 GHz with the e-MERLIN array. We present new high-resolution e-MERLIN observations at 5 GHz and compare these to archival MERLIN observations to investigate the reported variability. Our new observations allow us to probe the nuclear region at a factor three times higher resolution than the previous e-MERLIN study. We separate the core component, C4, into three separate components: C4W, C4E, and X. The AGN is thought to reside in component C4W, but this component has remained constant between epochs within uncertainties. However, we find that the Eastern-most component, C4E, has increased in peak flux density from 19.35 ± 1.10 to 37.09 ± 1.86 mJy beam−1, representing an 8.2σ increase on the MERLIN observations. We attribute this peak flux density increase to continue interaction between the jet and the emission line region (ELR), observed for the first time in a low-luminosity AGNs such as NGC 4151. We identify discrete resolved components at 5 GHz along the jet axis, which we interpret as areas of jet–ELR interaction.

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“…This includes sources such as NGC 4261 [109,110], NGC 6251 [111], NGC 1052 [112][113][114], Cygnus A [115][116][117], Centaurus A [118][119][120], 3C 111 [121,122], 3C 120 [122][123][124], 3C 264 [125], and PKS 1514+00 [122]. Remarkably, all of these jets show parabolic (or possibly cylindrical for NGC 1052 [114]) shapes at pc-subpc scales, indicating that the collimation zone is well resolved in these radio galaxies. Moreover, 6 out of these jets (NGC 4261, NGC 6251, NGC 1052, 3C 111, 3C 120, and PKS 1514+00) show parabolic (cylindrical) to conical transitions near the sphere of gravitational influence of SMBH, akin to M87, implying a common jet collimation mechanism being at work in these sources.…”

Section: Other Radio Galaxiesmentioning

confidence: 99%

Relativistic Jets from AGN Viewed at Highest Angular Resolution

Hada

2019

Galaxies

Self Cite

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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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The Two-sided Jet Structures of NGC 1052 at Scales from 300 to 4 × 10⁷ Schwarzschild Radii

Cited by 31 publications

References 38 publications

Jet collimation in NGC 315 and other nearby AGN

Jet collimation in NGC 315 and other nearby AGN

The curious activity in the nucleus of NGC 4151: jet interaction causing variability?

Relativistic Jets from AGN Viewed at Highest Angular Resolution

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The Two-sided Jet Structures of NGC 1052 at Scales from 300 to 4 × 107 Schwarzschild Radii

Cited by 31 publications

References 38 publications

Jet collimation in NGC 315 and other nearby AGN

Jet collimation in NGC 315 and other nearby AGN

The curious activity in the nucleus of NGC 4151: jet interaction causing variability?

Relativistic Jets from AGN Viewed at Highest Angular Resolution

Contact Info

Product

Resources

About

The Two-sided Jet Structures of NGC 1052 at Scales from 300 to 4 × 10⁷ Schwarzschild Radii