VERY LARGE ARRAY IMAGES AT 8.4 GHz OF 40 FANAROFF-RILEY II 3CR RADIO SOURCES WITH 0.1 &lt;
                    <i>z</i>
                    &lt; 2.0

Fernini, Ilias

doi:10.1088/0067-0049/212/2/19

Cited by 14 publications

(11 citation statements)

References 67 publications

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“…Comparing this to the X-band image in the top-left-hand frame seems to indicate a jet entering the lobe on the eastern side that bends abruptly to the west at the working surface of the lobe against the ambient environment, before terminating at the hot spot. This morphology is very common in high-resolution images of FR II radio lobes (Kharb et al 2008;Fernini 2014). We note that this is a very high-resolution image with sparse u-v coverage.…”

Section: Radio Observationssupporting

confidence: 51%

“…To an excellent approximation, the vast majority of the emission from ν o =1.9 GHz to ν o =8.4 GHz is located in two unresolved blobs. The Gaussian fitting procedure indicates that there is not enough information to reliably decompose the lobes into diffuse steep-spectrum lobe plasma and finer-scale, flatter spectrum features (Liu et al 1992;Fernini 2007Fernini , 2014. Thus, we use simple homogeneous, uniform single-zone models of plasma in order to approximate the physics.…”

Section: Synchrotron Self-absorbed Homogeneous Plasmoidsmentioning

confidence: 99%

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The Energetics of Launching the Most Powerful Jets in Quasars: A Study of 3C 82

Punsly

Hill

Marziani

et al. 2020

ApJ

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3C 82 at a redshift of 2.87 is the most distant 3C (Third Cambridge Catalogue) quasar. Thus, it is a strong candidate to have the most-luminous radio lobes in the universe. 3C 82 belongs to the class of compact steepspectrum radio sources. We use single-dish and interferometric radio observations in order to model the plasma state of these powerful radio lobes. It is estimated that the long-term time-averaged jet power required to fill these lobes with leptonic plasma is » ´-Q 2.66 1.33 10 erg s 47 1 , among the largest time-averaged jet powers from a quasar. Positing protonic lobes is not tenable as they would require two orders of magnitude more mass transport to the lobes than was accreted to the central black hole during their formation. The first high signal-to-noise optical spectroscopic observation obtained of this object indicates that there is a powerful high-ionization broad-line wind with a kinetic power of ∼10 45 erg s −1 and a velocity of ∼0.01c. We also estimate from the broad lines in 2018 and the UV continuum in three epochs spread out over three decades that the accretion flow bolometric luminosity is L bol ≈3.2-5.8×10 46 erg s −1. The ratio of »  Q L 5.91 3.41 bol / is perhaps the largest of any known quasar. Extremely powerful jets tend to strongly suppress powerful winds of ionized baryonic matter. Consequently, 3C 82 provides a unique laboratory for studying the dynamical limits of the central engine of outflow initiation in quasars. Unified Astronomy Thesaurus concepts: Black hole physics (159); Radio jets (1347); Relativistic jets (1390); Radio loud quasars (1349)

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Section: Radio Observationssupporting

confidence: 51%

Section: Synchrotron Self-absorbed Homogeneous Plasmoidsmentioning

confidence: 99%

The Energetics of Launching the Most Powerful Jets in Quasars: A Study of 3C 82

Punsly

Hill

Marziani

et al. 2020

ApJ

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“…h : Bright core of almost compact appearance. a : 4C+49.22,extended emission plus very bright unresolved core with optical/X jet (Fernini 2014); flat spectrum and γ-ray detection (Cutini et al 2014). d : Core with faint extension to the West.…”

Section: Resultsmentioning

confidence: 99%

Radio loudness along the quasar main sequence

Ganci

Marziani

D’Onofrio

et al. 2019

A&A

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Context. When can an active galactic nucleus (AGN) be considered radio-loud? Following the established view of the AGNs inner workings, an AGN is radio-loud if associated with relativistic ejections emitting a radio synchrotron spectrum (i.e., it is a "jetted" AGN). In this paper we exploit the AGN main sequence that offers a powerful tool to contextualize radio properties. Aims. If large samples of optically-selected quasars are considered, AGNs are identified as radio-loud if their Kellermann's radio loudness ratio RK > 10. Our aims are to characterize the optical properties of different classes based on radioloudness within the main sequence and to test whether the condition RK > 10 is sufficient for the identification of RL AGNs, since the origin of relatively strong radio emission may not be necessarily due to relativistic ejection. Methods. A sample of 355 quasars was selected by cross-correlating the FIRST survey with the SDSS DR14 quasar catalog. We classified the optical spectra according to their spectral types along the main sequence of quasars. For each spectral type, we distinguished compact and extended morphology (providing a FIRST-based atlas of radio maps in the latter case), and three classes of radio-loudness: detected ( specific flux ratio in the g band and at 1.4GHz, R K <10), intermediate (10 ≤ R K < 70), and radio loud (R K ≥70).Results. The analysis revealed systematic differences between radio-detected (i.e., radio-quiet), radio-intermediate, and radio-loud in each spectral type along the main sequence. We show that spectral bins that contain the extreme Population A sources have radio power compatible with emission by mechanisms ultimately due to star formation processes. Radio-loud sources of Population B are characteristically jetted. Their broad Hβ profiles can be interpreted as due to a binary broad-line region. We suggest that RL Population B sources should be preferential targets for the search of black hole binaries, and present a sample of binary black hole AGN candidates. Conclusions. The validity of the Kellermann's criterion may be dependent on the source location along the quasar main sequence. The consideration of the MS trends allowed to distinguish between sources whose radio emission mechanisms is "jetted" from the ones where the mechanism is likely to be fundamentally different.

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“…3, we note that the location of the maximum absorption or optical depth does not always coincide with that of the peak radio continuum flux. This can be caused by the radio emission in the southern lobe resolving into structures at sub-kpc-scales, as indicated by the 5 GHz (Barthel et al 1988) and the 8.4 GHz (Fernini 2014) continuum maps of this source. However, it is interesting to note from this figure that the location of the maximum absorption shifts with velocity.…”

Section: Extent and Structure Of H I 21-cm Absorbing Gasmentioning

confidence: 94%

Mapping kiloparsec-scale structures in the extended H i disc of the galaxy UGC 000439 by H i 21-cm absorption

Dutta¹,

Gupta²,

Srianand³

et al. 2016

Mon. Not. R. Astron. Soc.

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We study the properties of H I gas in the outer regions (∼2r 25 ) of a spiral galaxy, UGC 00439 (z = 0.01769), using H I 21-cm absorption towards different components of an extended background radio source, J0041−0043 (z = 1.679). The radio source exhibits a compact core coincident with the optical quasar and two lobes separated by ∼7 kpc, all at an impact parameter ∼25 kpc. The H I 21-cm absorption detected towards the southern lobe is found to extend over ∼2 kpc 2 . The absorbing gas shows sub-kpc-scale structures with the line-of-sight velocities dominated by turbulent motions. Much larger optical depth variations over 4-7 kpc-scale are revealed by the non-detection of H I 21-cm absorption towards the radio core and the northern lobe, and the detection of Na I and Ca II absorption towards the quasar. This could reflect a patchy distribution of cold gas in the extended H I disc. We also detect H I 21-cm emission from UGC 00439 and two other galaxies within ∼150 kpc to it, that probably form an interacting group. However, no H I 21-cm emission from the absorbing gas is detected. Assuming a linear extent of ∼4 kpc, as required to cover both the core and the southern lobe, we constrain the spin temperature 300 K for the absorbing gas. The kinematics of the gas and the lack of signatures of any ongoing in situ star formation are consistent with the absorbing gas being at the kinematical minor axis and corotating with the galaxy. Deeper H I 21-cm observations would help to map in greater detail both the large-and small-scale structures in the H I gas associated with UGC 00439.

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VERY LARGE ARRAY IMAGES AT 8.4 GHz OF 40 FANAROFF-RILEY II 3CR RADIO SOURCES WITH 0.1 < z < 2.0

Cited by 14 publications

References 67 publications

The Energetics of Launching the Most Powerful Jets in Quasars: A Study of 3C 82

The Energetics of Launching the Most Powerful Jets in Quasars: A Study of 3C 82

Radio loudness along the quasar main sequence

Mapping kiloparsec-scale structures in the extended H i disc of the galaxy UGC 000439 by H i 21-cm absorption

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