Strong lensing reveals jets in a sub-microJy radio-quiet quasar

Hartley, Philippa; Jackson, N.; Sluse, Dominique; Stacey, Hannah; Vives-Arias, H.

doi:10.1093/mnras/stz510

Cited by 44 publications

(49 citation statements)

References 118 publications

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“…The mm-continuum emission also shows a new feature labelled X near image B that is not present in the optical image. Component X also does not align with any of the radio components resolved in the e-MERLIN observations at 4.32 and 5.12 GHz of HS 0810+2554 (Hartley et al 2019).…”

Section: A Na Ly S I S O F T H E M M -C O N T I N U U M E M I S S I O N O F H S 0 8 1 0 +2 5 5mentioning

confidence: 76%

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Linking the small-scale relativistic winds and the large-scale molecular outflows in the z = 1.51 lensed quasar HS 0810+2554

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Davidson

Brusa³

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of the quadruply lensed z = 1.51 quasar HS 0810+2554 which provide useful insight on the kinematics and morphology of the CO molecular gas and the ∼ 2 mm-continuum emission in the quasar host galaxy. Lens modelling of the mm-continuum and the spectrally integrated CO(J = 3→2) images indicates that the source of the mm-continuum has an eccentricity of e ∼ 0.9 with a size of ∼1.6 kpc and the source of line emission has an eccentricity of e ∼ 0.7 with a size of ∼1 kpc. The spatially integrated emission of the CO(J = 2→1) and CO(J = 3→2) lines shows a triple peak structure with the outer peaks separated by Δv21 = 220 ± 19 km s−1 and Δv32 = 245 ± 28 km s−1, respectively, suggesting the presence of rotating molecular CO line emitting gas. Lensing inversion of the high spatial resolution images confirms the presence of rotation of the line emitting gas. Assuming a conversion factor of αCO = 0.8 M⊙ (K km s−1 pc2)−1 we find the molecular gas mass of HS 0810+2554 to be MMol = (5.2 ± 1.5)/μ32 × 1010 M⊙, where μ32 is the magnification of the CO(J = 3→2) emission. We report the possible detection, at the 3.0–4.7σ confidence level, of shifted CO(J = 3→2) emission lines of high-velocity clumps of CO emission with velocities up to 1702 km s−1. We find that the momentum boost of the large-scale molecular wind is below the value predicted for an energy-conserving outflow given the momentum flux observed in the small-scale ultrafast outflow.

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Section: A Na Ly S I S O F T H E M M -C O N T I N U U M E M I S S I O N O F H S 0 8 1 0 +2 5 5mentioning

confidence: 76%

“…More recently, Hartley et al (2019) using e-MERLIN and European VLBI Network observations have identified jet activity in HS 0810+2554. Specifically, their source reconstruction of the radio and HST data of HS 0810+2554 shows two jet components linearly aligned on opposing sides of the optical quasar core.…”

mentioning

confidence: 99%

Linking the small-scale relativistic winds and the large-scale molecular outflows in the z = 1.51 lensed quasar HS 0810+2554

Chartas

Davidson

Brusa³

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…It is possible that radio jets (typically associated with 'radio-loud' quasars) are being launched (e.g. Hartley et al 2019) but they are too small to be resolved in our radio images. Supporting this, earlier in the Symposium we were shown images of small jets in 'radio-silent' Seyfert galaxies (Lähteenmäki et al 2018), which are believed to be low-redshift analogues of quasars.…”

Section: What Accretion-related Mechanism Is Present?mentioning

confidence: 99%

Accretion and star formation in ‘radio-quiet’ quasars

et al. 2019

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Radio observations allow us to identify a wide range of active galactic nuclei (AGN), which play a significant role in the evolution of galaxies. Amongst AGN at low radio-luminosities is the ‘radio-quiet’ quasar (RQQ) population, but how they contribute to the total radio emission is under debate, with previous studies arguing that it is predominantly through star formation. In this talk, SVW summarised the results of recent papers on RQQs, including the use of far-infrared data to disentangle the radio emission from the AGN and that from star formation. This provides evidence that black-hole accretion, instead, dominates the radio emission in RQQs. In addition, we find that this accretion-related emission is correlated with the optical luminosity of the quasar, whilst a weaker luminosity-dependence is evident for the radio emission connected with star formation. What remains unclear is the process by which this accretion-related emission is produced. Understanding this for RQQs will then allow us to investigate how this type of AGN influences its surroundings. Such studies have important implications for modelling AGN feedback, and for determining the accretion and star-formation histories of the Universe.

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“…2). Indeed, the relatively few available studies of RQ AGN at high and low resolution (e.g., Kellermann et al 1989Kellermann et al , 1994; Barvainis et al 1996;Kukula et al 1998;Ulvestad et al 2005;Leipski et al 2006;Padovani et al 2011;Doi et al 2011;Zakamska et al 2016a,b;Hartley et al 2019) have generally led to mixed results. This is not surprising, as all RQ AGN are powered by a SMBH and emit X-rays (from a corona), most are in star-forming hosts, and many display outflows.…”

Section: Introductionmentioning

confidence: 99%

The origin of radio emission from radio-quiet active galactic nuclei

et al. 2019

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The central nuclei of galaxies, where super-massive black holes (SMBHs) are thought to reside, can experience phases of activity when they become Active Galactic Nuclei (AGN). An AGN can eject winds, jets, and produce radiation across the entire electromagnetic spectrum. The fraction of the bolometric emission in the radio spans a factor of ∼10 5 across the different AGN classes. The weakest radio sources, radio-quiet (RQ) AGN, are typically 1,000 times fainter than the radio-loud (RL) AGN, and represent the majority of the AGN population. In RL AGN, radio emission is essentially all produced by synchrotron emission from a relativistic jet. In contrast, in RQ AGN the absence of luminous jets allows us to probe radio emission from a wide range of possible mechanisms, from the host galaxy kpc scale down to the innermost region near the SMBHs: star formation, AGN driven wind, free-free emission from photo-ionized gas, low power jet, and the innermost accretion disc coronal activity. All these mechanisms can now be probed with unprecedented precision and spatial resolution, thanks to the current and forthcoming generation of highly sensitive radio arrays.

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Strong lensing reveals jets in a sub-microJy radio-quiet quasar

Cited by 44 publications

References 118 publications

Linking the small-scale relativistic winds and the large-scale molecular outflows in the z = 1.51 lensed quasar HS 0810+2554

Linking the small-scale relativistic winds and the large-scale molecular outflows in the z = 1.51 lensed quasar HS 0810+2554

Accretion and star formation in ‘radio-quiet’ quasars

The origin of radio emission from radio-quiet active galactic nuclei

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