A two-sided but significantly beamed jet in the supercritical accretion quasar IRAS F11119+3257

Yang, Jun; Paragi, Zsolt; An, Tao; Baan, Willem A.; Mohan, Prashanth; Liu, Xiang

doi:10.1093/mnras/staa836

Cited by 13 publications

(8 citation statements)

References 66 publications

(70 reference statements)

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“…The sub-relativistic speed of the background jet flow is suggestive of outflows driven from the inner region, powered by the accretion disc winds (e.g., Yang et al 2021). This is especially the case for highly luminous AGN where the bolometric luminosity can be super-Eddington, indicative of a high accretion rate and hence a prominent accretion disc (e.g., Yang et al 2020Yang et al , 2021. The specific scenarios are elaborated below.…”

Section: Discussionmentioning

confidence: 99%

The obstructed jet in Mrk 231

Wang,

An,

Jaiswal

et al. 2021

Preprint

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Mrk 231 is the closest radio-quiet quasar known and one of the most luminous infrared galaxies in the local Universe. It is characterised by the co-existence of a radio jet and powerful multi-phase multi-scale outflows, making it an ideal laboratory to study active galactic nucleus (AGN) feedback. We analyse the multi-epoch very long baseline interferometry data of Mrk 231 and estimate the jet head advance speed to be 0.013 𝑐, suggesting a sub-relativistic jet flow. The jet position angle changes from −113 • in the inner parsec to −172 • at a projected distance of 25 parsec. The jet structure change might result from either a jet bending following the rotation of the circum-nuclear disc or the projection of a helical jet on the plane of the sky. In the large opening angle (∼ 60 • ) cone, the curved jet interacts with the interstellar medium and creates wide-aperture-angle shocks which subsequently dissipate a large portion of the jet power through radiation and contribute to powering the large-scale outflows. The low power and bent structure of the Mrk 231 jet, as well as extensive radiation dissipation, are consistent with the obstruction of the short-length jet by the host galaxy's environment.

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Section: Discussionmentioning

confidence: 99%

The obstructed jet in Mrk 231

Wang,

An,

Jaiswal

et al. 2021

Preprint

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“…Moreover, the Gaia astrometry of compact AGNs generally has no significant systematic errors of >10 mas with respect to the radio cores of VLBI catalogues (e.g. Petrov et al 2019;Yang et al 2020a;Titov et al 2022).…”

Section: Location Of the Accreting Imbhmentioning

confidence: 99%

Is there a sub-parsec-scale jet base in the nearby dwarf galaxy NGC 4395?

Yang,

Wrobel

et al. 2022

Preprint

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NGC 4395 is a dwarf galaxy at a distance of about 4.3 Mpc (scale: ∼0.021 pc mas −1 ). It hosts an intermediate-mass black hole (IMBH) with a mass between ∼10 4 and ∼10 5 solar masses. The early radio observations of NGC 4395 with the very long baseline interferometry (VLBI) network, High Sensitivity Array (HSA), at 1.4 GHz in 2005 showed that its nucleus has a sub-mJy outflow-like feature (E) extending over 15 mas. To probe the possibility of the feature E as a continuous jet with a base physically coupled with the accretion disc, we performed deep VLBI observations with the European VLBI Network (EVN) at 5 GHz, and analysed the archival data obtained with the HSA at 1.4 GHz in 2008, NSF's Karl G. Jansky Very Large Array (VLA) at 12-18 GHz and the Atacama Large Millimetre/submillimetre Array (ALMA) at 237 GHz. The feature E displays more diffuse structure in the HSA image of 2008 and has no compact substructure detected in the EVN image. Together with the optically thin steep spectrum and the extremely large angular offset (about 220 mas) from the accurate optical Gaia position, we explain the feature E as nuclear shocks likely formed by the IMBH's episodic ejection or wide-angle outflow. The VLA and ALMA observations find a sub-mJy pc-scale diffuse feature, possibly tracing a thermal free-free emission region near the IMBH. There is no detection of a jet base at the IMBH position in the VLBI maps. The non-detections give an extremely low luminosity of ≤ 4.7 × 10 33 erg s −1 at 5 GHz and indicate no evidence of a disc-jet coupling on sub-pc scales.

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“…Although a few near/super Eddington objects have demonstrated jet activity [42-44, 46-49, 51, 53, 54], in most of these systems, such as super-Eddington active galactic nuclei (AGNs) [13] and ultraluminous X-ray sources [45], it remains doubtful whether there is jet emission. Recent observations [13,[55][56][57][58] suggest that the radio emission in near/super-Eddington AGNs comes from the nuclear region, with possible contributions from hot corona, accretion disk winds, fossil radio jet, or a combination of all above [13,55,[58][59][60][61][62]. In particular, unambiguous detection of both powerful radio jets and radio-emitting winds was reported only in the Galactic microquasar SS 433 [63][64][65], while accretion disk wind is believed to be ubiquitous in the near/super-Eddington accretion mode.…”

Section: Extremely High and Super-eddington Accretionmentioning

confidence: 99%

The Unified Models for Black Hole Accretions

Yang¹

2022

Astronomy and Planetary Science - From Cryovolcanism to Black Holes and Galactic Evolution

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Decades of observations and theoretical studies present intriguing results about black hole accretions: supermassive black holes (SMBHs), located in the centers of galaxies, are accreting similar to Galactic stellar-mass black hole systems (GBHs). This is the unified model of black hole accretion, which indicates active galactic nuclei (AGNs, the accreting SMBHs) are only the scaled-up version of galactic X-ray binaries (XRBs, the accreting GBHs). The analogy between AGNs and XRBs ensures us to determine AGN evolutions on cosmological timescales by simply studying the quick-playing Galactic systems, which is much easy in observation and modeling. X-ray emission is produced by the inner region of the accretion disk and corona, which is close to the black holes and provides the diagnostics of accretion strength. Meanwhile, radio emission is an indicator of the ejection process, which is another fundamental part of accreting black holes. Furthermore, accreting flows are also regulated by black hole masses and accretion rates/Eddington ratios. Therefore, the unified model of black hole accretion is the correlation between accretion and ejection process and black hole masses. In this chapter, we will review models concerning the unified model of black hole accretions and present recent updates in this area.

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A two-sided but significantly beamed jet in the supercritical accretion quasar IRAS F11119+3257

Cited by 13 publications

References 66 publications

The obstructed jet in Mrk 231

The obstructed jet in Mrk 231

Is there a sub-parsec-scale jet base in the nearby dwarf galaxy NGC 4395?

The Unified Models for Black Hole Accretions

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