The Global Jet Structure of the Archetypical Quasar 3C 273

Akiyama, Kazunori; Asada, Keiichi; Fish, Vincent L.; Nakamura, Masanori; Hada, Kazuhiro; Nagai, Hiroshi; Lonsdale, Colin J.

doi:10.3390/galaxies6010015

Cited by 29 publications

(24 citation statements)

References 21 publications

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“…Therefore the collimation of AGN jets from M BH = 10 8−9 M ⊙ might commonly break at distances around r SGI ∼ 3 × 10 5 R s . Note that the jet profile of 1H 0323+342 shown by red color in Figure 8 is also sufficiently overlapped with those of NGC 6251 (Tseng et al 2016;Nakamura et al 2018) and 3C 273 (Akiyama et al 2018).…”

Section: Jet Collimation Confinement Medium and Black Hole Massmentioning

confidence: 73%

“…Regarding the extended jet, there is a possible trend that the spectra on and right down the quasi-stationary feature S are slightly flatter than those in the upstream side of S. Although the uncertainties are still large, this might indicate reenergization of nonthermal electrons via shock in the feature S. Structural transition of jet profile has recently been discovered in some nearby radio galaxies (M87; Asada & Nakamura (2012), NGC 6251; Tseng et al (2016), 3C 273; Akiyama et al (2018), NGC 4261; Nakahara et al (2018)). This has triggered active discussion about the mechanisms of jet formation and collimation.…”

Section: Spectramentioning

confidence: 98%

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Collimation, Acceleration, and Recollimation Shock in the Jet of Gamma-Ray Emitting Radio-loud Narrow-line Seyfert 1 Galaxy 1H0323+342

Hada

Doi

Wajima

et al. 2018

ApJ

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We investigated the detailed radio structure of the jet of 1H 0323+342 using high-resolution multi-frequency Very Long Baseline Array observations. This source is known as the nearest γ-ray emitting radio-loud narrow line Seyfert 1 (NLS1) galaxy. We discovered that the morphology of the inner jet is well characterized by a parabolic shape, indicating the jet being continuously collimated near the jet base. On the other hand, we found that the jet expands more rapidly at larger scales, resulting in a conical-like shape. The location of the "collimation break" is coincident with a bright quasi-stationary feature at 7 mas from core (corresponding to a deprojected distance of the order of ∼100 pc), where the jet width locally contracts together with highly polarized signals, suggesting a recollimation shock. We found that the collimation region is coincident with the region where the jet speed gradually accelerates, suggesting the coexistence of the jet acceleration and collimation zone, ending up with the recollimation shock, which could be a potential site of high-energy γ-ray flares detected by the F ermi-LAT. Remarkably, these observational features of the 1H 0323+342 jet are overall very similar to those of the nearby radio galaxy M87 and HST-1 as well as some blazars, suggesting that a common jet formation mechanism might be at work. Based on the similarity of the jet profile between the two sources, we also briefly discuss the mass of the central black hole of 1H 0323+342, which is also still highly controversial on this source and NLS1s in general.

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Section: Jet Collimation Confinement Medium and Black Hole Massmentioning

confidence: 73%

Section: Spectramentioning

confidence: 98%

Collimation, Acceleration, and Recollimation Shock in the Jet of Gamma-Ray Emitting Radio-loud Narrow-line Seyfert 1 Galaxy 1H0323+342

Hada

Doi

Wajima

et al. 2018

ApJ

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“…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%

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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“…In particular, mm-VLBI studies (see Boccardi et al (2017) for a review) provide high resolution images of regions deep in the jet that are otherwise optically thick at longer centimeter wavelengths. Millimeter (mm)-wave VLBI images, therefore, give us a direct probe of the inner geometry and velocity structure of jets in different AGN classes: radio galaxies (Cygnus A - Boccardi et al (2016a,b); M 87 - Hada et al (2013), Kim et al (2018); NGC 4261 - Nakahara et al (2018); NGC 1052 - Baczko et al (2016Baczko et al ( , 2019; Nakahara et al (2020)), a narrowline Seyfert 1 (NLS1) galaxy, 1H 0323+342, Hada et al (2018), and few blazars (Mrk 501 - Giroletti et al (2004); 3C 273 Akiyama et al (2018); TXS 2013+370 -Traianou et al (2020). The picture is further complicated by synchrotron opacity effects (Blandford & Königl 1979) which can obscure the inner jet and shift the apparent location of the VLBI radio core at large distances from the black hole, ∼ 10 (4−6) Schwarzshild radii (R s ) (e.g.…”

Section: Introductionmentioning

confidence: 99%

The jet collimation profile at high resolution in BL Lacertae

Casadio,

MacDonald,

Boccardi

et al. 2021

Preprint

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Context. Controversial studies on the jet collimation profile of BL Lacertae (BL Lac), the eponymous blazar of BL Lac objects class, complicate the scenario in this already puzzling class of objects. Understanding the jet geometry, in connection with the jet kinematics and the physical conditions in the surrounding medium, is fundamental to better constrain the formation, acceleration and collimation mechanisms in extragalactic jets. Aims. With the aim of investigating the jet geometry in the innermost regions of the jet of BL Lac, and solving the controversy, we explore the radio jet in this source, using high resolution millimeter-wave Very Long Baseline Interferometric (VLBI) data. Methods. We collect 86 GHz GMVA and 43 GHz VLBA data to obtain stacked images that we use to infer the jet collimation profile by means of two comparable methods. We analyze the kinematics at 86 GHz, and we discuss it in the context of the jet expansion. Finally we consider a possible implication of the Bondi sphere in shaping the different expanding region observed along the jet. Results. The jet in BL Lac expands with an overall conical geometry. A higher expanding rate region is observed between ∼ 5 and 10 pc (de-projected) from the black hole. Such a region is associated with the decrease in brightness usually observed in highfrequency VLBI images of BL Lac. The jet retrieves the original jet expansion around 17 pc, where the presence of a recollimation shock is supported by both the jet profile and the 15 GHz kinematics (MOJAVE survey). The change in the jet expansion profile occurring at ∼ 5 pc could be associated with a change in the external pressure profile in correspondence of the Bondi radius (∼3.3×10 5 R S ).

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The Global Jet Structure of the Archetypical Quasar 3C 273

Cited by 29 publications

References 21 publications

Collimation, Acceleration, and Recollimation Shock in the Jet of Gamma-Ray Emitting Radio-loud Narrow-line Seyfert 1 Galaxy 1H0323+342

Collimation, Acceleration, and Recollimation Shock in the Jet of Gamma-Ray Emitting Radio-loud Narrow-line Seyfert 1 Galaxy 1H0323+342

Jet collimation in NGC 315 and other nearby AGN

The jet collimation profile at high resolution in BL Lacertae

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