RadioAstron reveals a spine-sheath jet structure in 3C 273

Bruni, G.; Gómez, J. L.; Vega-García, L.; Lobanov, A. P.; Fuentes, Antonio; Savolainen, Tuomas; Kovalev, Y. Y.; Perucho, M.; Martí, J.; Anderson, J. M.; Edwards, P. G.; Gurvits, L. I.; Lisakov, M. M.; Pushkarev, A. B.; Sokolovsky, K. V.; Zensus, J. A.

doi:10.1051/0004-6361/202039423

Cited by 16 publications

(15 citation statements)

References 62 publications

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“…In Figure 5, we show lower-frequency images of 3C 273 observed with the HSA and VLBA, which were all averaged over the top-set reconstructions similar to the GMVA images in Figure 3. The overall jet morphology is consistent with previous ground-based (MOJAVE: Lister et al 2018; VLBA-BU-Blazar 39 : Jorstad et al 2017) and space-based VLBI observations (Radio Astron: Bruni et al 2017Bruni et al , 2021. Regardless of the observing frequency, the 3C 273 jet extends in the southwest direction with multiple bright knots whose relative locations are consistent between different frequencies.…”

Section: Hsa and Vlba Imagessupporting

confidence: 86%

“…In this paper, we study the quasar 3C 273 (1226+023), well known as one of the brightest extragalactic objects and the closest quasars (Schmidt 1963) with prominent jets (Davis et al 1985;Conway et al 1993;Bahcall et al 1995;Jester et al 2005;Perley & Meisenheimer 2017). The 3C 273 jets have been observed many times since their discovery because the elongated jet is a unique target for resolving down to the central (sub)parsec scale with VLBI observations (Krichbaum et al 1990;Lobanov & Zensus 2001;Savolainen et al 2006;Kovalev et al 2016;Bruni et al 2017Bruni et al , 2021Jorstad et al 2017;Lister et al 2019Lister et al , 2021. Furthermore, recent infrared interferometric observations with the GRAVITY instrument on the Very Large Telescope Interferometer (Gravity Collaboration et al 2017) precisely estimated the BH mass and viewing angle for 3C 273 as M BH = (2.6 ± 1.1) × 10 8 M e and θ = 12°± 2° (Gravity Collaboration et al 2018).…”

Section: Introductionmentioning

confidence: 99%

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Collimation of the Relativistic Jet in the Quasar 3C 273

Okino

Akiyama

Asada

et al. 2022

ApJ

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The collimation of relativistic jets launched from the vicinity of supermassive black holes (SMBHs) at the centers of active galactic nuclei (AGNs) is one of the key questions to understand the nature of AGN jets. However, little is known about the detailed jet structure for AGN like quasars since very high angular resolutions are required to resolve these objects. We present very long baseline interferometry (VLBI) observations of the archetypical quasar 3C 273 at 86 GHz, performed with the Global Millimeter VLBI Array, for the first time including the Atacama Large Millimeter/submillimeter Array. Our observations achieve a high angular resolution down to ∼60 μas, resolving the innermost part of the jet ever on scales of ∼105 Schwarzschild radii. Our observations, including close-in-time High Sensitivity Array observations of 3C 273 at 15, 22, and 43 GHz, suggest that the inner jet collimates parabolically, while the outer jet expands conically, similar to jets from other nearby low-luminosity AGNs. We discovered the jet collimation break around 107 Schwarzschild radii, providing the first compelling evidence for structural transition in a quasar jet. The location of the collimation break for 3C 273 is farther downstream from the sphere of gravitational influence (SGI) from the central SMBH. With the results for other AGN jets, our results show that the end of the collimation zone in AGN jets is governed not only by the SGI of the SMBH but also by the more diverse properties of the central nuclei.

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Section: Hsa and Vlba Imagessupporting

confidence: 86%

Section: Introductionmentioning

confidence: 99%

Collimation of the Relativistic Jet in the Quasar 3C 273

Okino

Akiyama

Asada

et al. 2022

ApJ

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“…Such a structure would consist of two flows: a faster, lower-density component streaming along the central axis (spine), and a slower, denser component along the edges of the jet. As the Doppler beaming would be stronger for the faster flow if viewed at a narrow angle, the spine would be expected to dominate the overall jet emission, while the sheath would be more intense at wider viewing angles (e.g., RGs; Bruni et al 2021). Evidence for a spine-sheath structure in several blazar jets comes from linear polarization of VLBI images (e.g., Pushkarev et al 2005;Asada et al 2010;Gabuzda et al 2014;Mertens et al 2016), especially when including the space-based RadioAstron antenna in the array (Bruni et al 2021).…”

mentioning

confidence: 99%

“…(Giovannini et al 2018), 1055+018(Attridge et al 1999;MacDonald et al 2017), 1226+023 (MacDonald et al 2017Bruni et al 2021), 1510-089 (MacDonald et al 2015, 1652 +398(Giroletti et al 2004;Pushkarev et al 2005), 0836+710, 1253-055, and 2230+114 (MacDonald et al 2017). Neither 1652+398 nor 0316+413 have enough reliable superluminal knots for us to determine their jet structure (see Section 5.5 to obtain estimates of their physical parameters).…”

mentioning

confidence: 99%

Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program

Weaver

Jorstad

Marscher

et al. 2022

ApJS

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We analyze the parsec-scale jet kinematics from 2007 June to 2018 December of a sample of γ-ray bright blazars monitored roughly monthly with the Very Long Baseline Array (VLBA) at 43 GHz under the VLBA-BU-BLAZAR program. We implement a novel piecewise linear fitting method to derive the kinematics of 521 distinct emission knots from a total of 3705 total intensity images in 22 quasars, 13 BL Lacertae objects, and 3 radio galaxies. Apparent speeds of these components range from 0.01c to 78c, and 18.6% of knots (other than the “core”) are quasi-stationary. One-fifth of moving knots exhibit nonballistic motion, with acceleration along the jet within 5 pc of the core (projected) and deceleration farther out. These accelerations occur mainly at locations coincident with quasi-stationary features. We calculate the physical parameters of 273 knots with statistically significant motion, including their Doppler factors, Lorentz factors, and viewing angles. We determine the typical values of these parameters for each jet and the average for each subclass of active galactic nuclei. We investigate the variability of the position angle of each jet over the 10 yr of monitoring. The fluctuations in position of the quasi-stationary components in radio galaxies tend to be parallel to the jet, while no directional preference is seen in the components of quasars and BL Lacertae objects. We find a connection between γ-ray states of blazars and their parsec-scale jet properties, with blazars with brighter 43 GHz cores typically reaching higher γ-ray maxima during flares.

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“…In the case of the Barbell GRG, we observe that the jet on the western side develops a kink-like feature and undergoes recollimation before connecting to the WL. The helical patterns in jets have been observed in a few sources (Pasetto et al 2021;Bruni et al 2021;Worrall et al 2007;Lobanov & Zensus 2001) in a different range of spatial scales.…”

Section: Jet and The Kinkmentioning

confidence: 99%

Barbell-shaped giant radio galaxy with ∼100 kpc kink in the jet

Dabhade

Shimwell

Saikia

et al. 2022

A&A

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We present for the first time a study of peculiar giant radio galaxy (GRG) J223301+131502 using deep multi-frequency radio observations from GMRT (323, 612, and 1300 MHz) and LOFAR (144 MHz) along with optical spectroscopic observations with the WHT 4.2m optical telescope. Our observations have firmly established its redshift of 0.09956 and unveiled its exceptional jet structure extending more than ∼ 200 kpc leading to a peculiar kink structure of ∼ 100 kpc. We measure the overall size of this GRG to be ∼ 1.83 Mpc; it exhibits lobes without any prominent hotspots and closely resembles a barbell. Our deep low-frequency radio maps clearly reveal the steep-spectrum diffuse emission from the lobes of the GRG. The magnetic field strength of ∼ 5 µG and spectral ages between about 110 to 200 mega years for the radio lobes were estimated using radio data from LOFAR 144 MHz observations and GMRT 323 and 612 MHz observations. We discuss the possible causes leading to the formation of the observed kink feature for the GRG, which include precession of the jet axis, development of instabilities and magnetic reconnection. Despite its enormous size, the Barbell GRG is found to be residing in a low-mass (M200 ∼ 10 14 M ) galaxy cluster. This GRG with two-sided large-scale jets with a kink and diffuse outer lobes residing in a cluster environment, provides an opportunity to explore the structure and growth of GRGs in different environments.

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RadioAstron reveals a spine-sheath jet structure in 3C 273

Cited by 16 publications

References 62 publications

Collimation of the Relativistic Jet in the Quasar 3C 273

Collimation of the Relativistic Jet in the Quasar 3C 273

Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program

Barbell-shaped giant radio galaxy with ∼100 kpc kink in the jet

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