A Survey of Kiloparsec-Scale Radio Outflows in Radio-Quiet Active Galactic Nuclei

A. Pedlar; C. P. O'Dea; D. J. Axon; J. F. Gallimore; S. A. Baum

REVIEW

A Survey of Kiloparsec-Scale Radio Outflows in Radio-Quiet Active Galactic Nuclei

J. F. Gallimore, D. J. Axon, C. P. O'Dea, S. A. Baum, A. Pedlar

Astrophysics · Submitted 10 Apr 2006 · 21 references

Pith's verdict: A solid, useful survey whose headline 44% fraction is a real measurement, but the AGN-origin case rests partly on a by-eye classification and a partly circular radio-excess test.

T0 · AI review

How this review was made: An AI referee (deepseek-v4-flash) read the paper on August 28, 2026 and answered a fixed list of questions about it. T0 is the starting level every paper gets. The levels describe how deeply Pith has checked the paper, never the authors.

T0 AI review An AI read the paper and answered a fixed list of questions.
T1 Audit Automatic checks that the references and files the paper relies on exist and match.
T2 Compute The paper's code or calculations re-run with the same results.
T3 Formal statement The claims written out in a formal math language a computer can read.
T4 Proof Those claims proved, and the proof checked by computer.

How Pith checks papers →

· 4 major objections · 5 minor · Ask about this paper · The compiled record · Read the full review →

Challenge this review Comment (0) Read on arXiv ↗

Cite ▾

arXiv IDastro-ph/0604219 (version 1)

Pith IDVEVRPKYG, Pith's permanent record of this paper and its review

CitationA. Pedlar, C. P. O'Dea, D. J. Axon, J. F. Gallimore, S. A. Baum. "A Survey of Kiloparsec-Scale Radio Outflows in Radio-Quiet Active Galactic Nuclei." arXiv:astro-ph/0604219 (2006). https://pith.science/paper/VEVRPKYG

Cite this reviewBibTeX for Pith's review of this paper

Claim paper

Why Pith says this

Highlight any text to comment on it.

Editor's note

read the letter

The new number here is worth having: 44% (19/43) kiloparsec-scale radio structures in a complete, short-baseline VLA sample of Seyferts is the first unbiased estimate of this kind, and it genuinely updates the smaller targeted samples from Baum and Colbert. The survey design is sound: D-configuration at 5 GHz, careful point-source subtraction, KS tests for sample biases, and an honest set of caveats about projection and confusion. The L8.4 contrast between KSR and non-KSR Seyferts is the strongest piece of evidence for an AGN connection, and it is not itself built into the classification definition. The individual source notes are careful and the comparison with earlier surveys (Table 4) makes the resolution-dependence point clearly.

The soft spots are real but not fatal. The KSR/disk split in Section 3 is a visual match of radio contours to DSS images, with no blinded rating or inter-rater agreement, and the paper openly says ambiguous faint cases were put in the disk bin. Since that same split defines both the numerator of 44% and the grouping for every Table 5 test, a small number of mislabels could shift the detection fraction and weaken the statistical contrasts. Also, several KSRs (NGC 1241, 2992, 5506, 5929) are carried over from the literature rather than resolved here, so the survey is not the sole source of its own headline. The q test is partly circular: putting a source in the KSR bin because it has extra extended radio emission will naturally push its total radio flux up and lower q. The paper acknowledges some of this, but the abstract and Section 5 lean harder on the q result than the test can bear. The 'jet loses virtually all its power to the ISM' line is an order-of-magnitude ram-pressure estimate with several free parameters; the paper calls it that in the text, but the abstract says 'demonstrate,' which overshoots.

None of this sinks the core claim. The detection fraction is a direct measurement and a lower limit; even if a couple of classifications moved, the conclusion that KSRs are common in Seyferts would survive. The L8.4 result is independent of how q is defined. I'd want a referee to push for a blind reclassification or at least a quantitative criterion, and for the q test to be reframed as selection-related, but this is publishable work with a genuinely useful result. Send it to a serious referee, not the desk. I would cite it for the detection fraction and the D-configuration approach.

Referee report

Significance

If the central claims hold, the paper provides a valuable measurement: kiloparsec-scale radio outflows are common among radio-quiet Seyferts, with a detection fraction that is a firm lower limit because of projection and confusion effects. The survey fills a genuine gap by using short-baseline observations that recover low-surface-brightness emission missed by A-array surveys, and the sample-selection tests (KS tests on redshift and L12 distributions) are careful. The comparison with previous surveys (Table 4) nicely demonstrates the resolution bias. The paper also makes falsifiable predictions, e.g., strong spectral steepening in the frustated-jet model. However, the interpretation that KSRs are AGN-powered rests on statistical contrasts that are partly entangled with the KSR selection itself, and the classification of KSRs is subjective. The 'virtually all jet power lost' conclusion is an order-of-magnitude estimate depending on several assumed parameters. The paper is a useful contribution to the observational picture of Seyfert radio outflows, but its headline interpretive claims require more robustness testing.

Major objections (4)

[Section 3, Figures 1-3, Tables 2-3] The KSR classification is entirely qualitative: residual 5 GHz contours are overlaid on DSS images and judged by eye not to match 'the morphology of the disk or its associated star-forming regions.' No quantitative matching rule, blind rating, or inter-rater agreement is reported, and the paper concedes (Section 3) that 'several sources were difficult to distinguish owing to the faintness of the residual emission; we conservatively classified these ambiguous cases as disks.' This classification defines the 19/43 numerator and partitions every statistical test in Table 5, so a small number of reclassifications can change the headline detection fraction and potentially erase the q and L8.4 contrasts. Furthermore, four KSR entries (NGC 1241, NGC 2992, NGC 5506, NGC 5929) are not resolved by the present observations and are classified from literature data, so the detection fraction is not uniformly a product of this survey. I request that the authors provide a more quantitative classification criterion (e.g., residual surface brightness, angular offset from the optical disk, or a flux ratio), perform a sensitivity test in which ambiguous and literature-classified sources are reclassified as disks, and report the resulting ranges for the detection fraction and for the q and L8.4 statistics.
[Section 4.3, q test (Table 5, Figure 6)] The q test is partly circular. A source is classified as a KSR precisely because it contains extra kiloparsec-scale radio emission not matched to the disk; that same extra flux is included in the NVSS 1.4 GHz total flux used to compute q, thereby lowering q relative to the FIR-radio correlation. The statement in Section 5.1 that KSRs 'deviate from the radio–far infrared correlation' is therefore to some degree a selection effect rather than an independent physical diagnostic. The L8.4 comparison is much more convincing because it is based on A-array measurements of the compact nuclear source, which should resolve out the KSR. I recommend that the authors explicitly acknowledge this circularity and, if possible, recompute q after subtracting an estimate of the KSR contribution, or at least present the correlation in terms of a nuclear radio luminosity that is not part of the KSR flux.
[Table 5, Section 4.3] The paper performs nine statistical comparisons in Table 5 and highlights the two with P < 0.01 (q and L8.4). With nine tests, a Bonferroni-corrected significance threshold would be about 0.0056, and the reported P values are given only as '<0.01' and '0.9%', which are borderline. The authors should report exact P values and either apply a multiple-comparison correction or explicitly justify why the tests should be interpreted individually. The L10 result (P = 0.06) is not significant and should not be described as 'slightly greater' without noting this.
[Section 5.4, Eq. (1) and following derivation] The claim that 'the jet loses virtually all of its power to the ISM within the inner kiloparsec' rests on a chain of order-of-magnitude estimates: ram-pressure balance sets a lower limit on the jet density, the kinetic luminosity is then < 10^39 erg/s, and this is compared with an assumed pc-scale jet power of 10^42–10^43 erg/s. The conclusion is thus dependent on adopted values of rho_ISM, V_jet, r_j, tau_8, and on the assumption of a single outflow episode (n=1). While the authors describe this as a simple estimate, the conclusion appears in the abstract and conclusions as a firm result. I recommend softening the language to reflect the parametric dependence, and also noting that the buoyant velocity formula in Eq. (1) is garbled in the typeset text and should be corrected to a readable form.

Minor objections (5)

[Title page / affiliations] The first affiliation contains a typo: 'Department of Physics & Astrronomy' should be 'Astronomy'.
[Section 1, paragraph 3] The phrase 'whether such kiloparsec-scale radio structures (KSRs) are truly are so common' contains a doubled verb and should be revised.
[Section 4.2, Figure 5] The caption for Figure 5 says 'resolved disk sources' but the comparison is between disk and KSR sources; please clarify whether the top panel includes all resolved disk sources and the bottom panel all resolved KSRs.
[Section 5.3, Eq. (1) and surrounding text] The buoyant-velocity formula (1) is rendered as an unreadable string of symbols; please provide a properly typeset equation and define all variables in the caption or text.
[Section 5.2, paragraph 2] The sentence beginning 'If instead the jet axis itself changes randomly...' is grammatically awkward; consider splitting it into two sentences for clarity.

How Pith checks papers → · Full audit of this paper →

The paper

The paper claims

Using short-baseline radio images that recover faint extended emission, this paper finds that 44% of radio-quiet Seyfert and LINER galaxies host kiloparsec-scale radio outflows, and it argues these outflows are AGN jets that dump nearly…

The reading

This paper reports a short-baseline radio survey of 43 Seyfert and LINER galaxies designed to detect structures larger than 1 kpc that earlier long-baseline surveys would have resolved out. It finds that 44% (19/43) of the sample show extended radio outflows that cannot be matched to disk or star-forming morphology, and argues this is a lower limit because of projection effects and confusion with faint disk emission. The paper aims to establish that these kiloparsec-scale outflows are powered by AGN jets rather than starburst winds: outflow hosts deviate from the far-infrared-radio correlation, tend toward radio excess, and host more luminous compact nuclear radio sources, even though their infrared colors, host morphologies, and nuclear gas properties are indistinguishable from other Seyferts. It further argues that the jets are 'frustrated,' decelerating from roughly $0.1c$ to tens of km s$^{-1}$, so that virtually all jet power is lost to the nuclear ISM within the inner kiloparsec. If correct, radio-quiet Seyfert nuclei are a substantial and long-lived source of mechanical feedback in their host galaxies.

What carries the argument

The central object is the kiloparsec-scale radio structure (KSR): radio continuum emission of at least 1 kpc total extent that cannot be matched to the optical galaxy disk or its star-forming regions, revealed here by subtracting unresolved nuclear point sources from ~15–20 arcsecond resolution 5 GHz images. The load-bearing statistical machinery is the far-infrared-radio correlation parameter $q$, defined as $q = \log([\mathrm{FIR}/3.75\times10^{12}\,\mathrm{Hz}]/S_{1.4\,\mathrm{GHz}})$, which cleanly separates KSR hosts from non-KSR Seyferts without requiring morphological judgment. The physical mechanism carrying the argument is the 'frustrated jet' model: a nuclear jet decelerates by ram pressure and entrainment in the nuclear ISM, so the large-scale lobes advance at buoyant speeds of tens of km s$^{-1}$ while the jet loses essentially all of its kinetic power in the inner kiloparsec.

Extended reading notes

Core claim

On the paper's own terms, the central discovery is that kiloparsec-scale radio structures (KSRs) are common in radio-quiet AGN: 44% (19/43) of a complete, distance-limited Seyfert and LINER sample show extended radio emission at least 1 kpc in total extent that does not match the morphology of the disk or its star-forming regions, and the true fraction is probably higher. The KSR Seyferts are statistically distinct from non-KSR Seyferts in their radio properties: they deviate from the far-infrared-radio correlation for star-forming galaxies, tending toward radio excess, and they have compact nuclear radio sources that are on average about an order of magnitude more luminous. The paper interprets this as evidence that the KSRs are fed by AGN-powered jets rather than starburst-driven superwinds, and it argues that these jets are strongly decelerated by interaction with the nuclear ISM. A simple ram-pressure argument gives kiloparsec-scale jet powers below $10^{39}$ erg s$^{-1}$, orders of magnitude weaker than the $10^{42}$–$10^{43}$ erg s$^{-1}$ powers inferred on 10–100 pc scales, so virtually all of the jet power must be dissipated into the ISM within the inner kiloparsec.

Load-bearing premise

The load-bearing premise is that looking at radio and optical images together correctly tells which extended radio emission is an outflow rather than ordinary star-forming disk emission; borderline faint cases were conservatively counted as disk emission, so if these judgments are systematically wrong the 44% detection rate and the comparisons between outflow and non-outflow galaxies would change.

Editorial extensions

If this is right

The reported 44% detection rate is explicitly a lower limit, so most or possibly all Seyfert galaxies may generate kiloparsec-scale radio outflows during an extended phase of their lifetime.
KSR hosts deviate from the far-infrared-radio correlation and host roughly ten times more luminous compact radio cores, so high-resolution nuclear radio luminosity can serve as a statistical marker of ongoing kiloparsec-scale AGN outflows even when star-forming disk emission dominates.
Seyfert 1 and Seyfert 2 galaxies show statistically indistinguishable KSR detection fractions and projected sizes, indicating that kiloparsec-scale outflows have effectively lost memory of the current AGN axis and are not simply foreshortened projections of a unified jet geometry.
The jet power on kiloparsec scales is orders of magnitude below the power on 10–100 pc scales, implying that Seyfert jets deposit roughly $10^{57}$ erg into the nuclear ISM over their lifetime, an energy comparable to that of a starburst-driven superwind.
The frustrated-jet model predicts strong spectral steepening across KSR lobes and extended soft X-ray emission at roughly 10% of the dissipated jet power, giving direct observational tests against the alternative 'roman candle' model of repeated short outbursts.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

If KSRs are nearly universal, then radio-quiet AGN feedback is not a rare or transient event; the inner kiloparsecs of Seyfert hosts should show widespread shock-heated gas, soft X-ray emission, and stirred atomic gas, with each outflow entraining on the order of 10% of the neutral ISM within the inner kiloparsec.
The random orientation of KSRs relative to both the galaxy minor axis and the small-scale jet axis suggests that measuring misalignment distributions in larger samples could statistically separate intrinsic black-hole spin-axis changes from ISM deflection, since only the latter should preferentially bend outflows toward the rotation axis in edge-on systems.
A natural extension is to use low-frequency radio surveys with high surface-brightness sensitivity to map spectral index gradients across KSRs: strong steepening toward the lobe edges would confirm frustration and old synchrotron ages, while flat or young spectra would favor reacceleration or recent re-energization.
The correlation between KSR presence and compact radio core luminosity implies that single-epoch, high-resolution radio snapshots of Seyfert cores could be used as a practical proxy for identifying galaxies with ongoing kiloparsec-scale outflows in future large-sample surveys.

Original abstract

Seyfert galaxies commonly host compact jets spanning 10-100 pc scales, but larger structures (KSRs) are resolved out in long baseline, aperture synthesis surveys. We report a new, short baseline Very Large Array (VLA) survey of a complete sample of Seyfert and LINER galaxies. Out of all of the surveyed radio-quiet sources, we find that 44% (19 / 43) show extended radio structures at least 1 kpc in total extent that do not match the morphology of the disk or its associated star-forming regions. The KSR Seyferts stand out by deviating significantly from the far-infrared - radio correlation for star-forming galaxies, and they are more likely to have a relatively luminous, compact radio source in the nucleus; these results argue that KSRs are powered by the AGN rather than starburst. KSRs probably originate from jet plasma that has been decelerated by interaction with the nuclear ISM. We demonstrate the jet loses virtually all of its power to the ISM within the inner kiloparsec to form the slow KSRs.

The compiled record

The paper's own sentences, arranged, kept beside the review and separate from it. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 5,105 input tokens.

What the abstract itself states, as probabilities: claims first 0.10 · states limitation 0.28 · human participants 0.02 · controlled comparison 0.50 · randomized assignment 0.01 · states quantitative result 0.99 · compares with prior results 0.83 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; show every role.

Seyfert galaxies commonly host compact jets spanning 10-100 pc scales, but larger structures (KSRs) are resolved out in long baseline, aperture synthesis surveys. We report a new, short baseline Very Large Array (VLA) survey of a complete sample of Seyfert and LINER galaxies. Out of all of the surveyed radio-quiet sources, we find that 44% (19 / 43) show extended radio structures at least 1 kpc in total extent that do not match the morphology of the disk or its associated star-forming regions. The KSR Seyferts stand out by deviating significantly from the far-infrared - radio correlation for star-forming galaxies, and they are more likely to have a relatively luminous, compact radio source in the nucleus; these results argue that KSRs are powered by the AGN rather than starburst. KSRs probably originate from jet plasma that has been decelerated by interaction with the nuclear ISM. We demonstrate the jet loses virtually all of its power to the ISM within the inner kiloparsec to form the slow KSRs.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	Seyfert galaxies commonly host compact jets spanning 10-100 pc scales, but larger structures (KSRs) are resolved out in long baseline, aperture synthesis surveys.	background 0.83	0.08	0.03	asserted 1.00
s1	We report a new, short baseline Very Large Array (VLA) survey of a complete sample of Seyfert and LINER galaxies.	contribution 0.87	0.96	0.03	asserted 0.97
s2	Out of all of the surveyed radio-quiet sources, we find that 44% (19 / 43) show extended radio structures at least 1 kpc in total extent that do not match the morphology of the disk or its associated star-forming regions.	result 1.00	0.97	0.37	asserted 1.00
s3	The KSR Seyferts stand out by deviating significantly from the far-infrared - radio correlation for star-forming galaxies, and they are more likely to have a relatively luminous, compact radio source in the nucleus; these results argue that KSRs are powered by the AGN rather than starburst.	interpretation 0.76	0.88	0.57	asserted 0.91
s4	KSRs probably originate from jet plasma that has been decelerated by interaction with the nuclear ISM.	interpretation 1.00	0.36	0.29	hedged possibility 1.00
s5	We demonstrate the jet loses virtually all of its power to the ISM within the inner kiloparsec to form the slow KSRs.	interpretation 0.74	0.85	0.33	asserted 1.00

What kind of paper the classifier reports this is: empirical study 0.96 · evidence from observation or experiment 1.00.

What was examined, and what was not

sources read

arXiv listing abstract v1

not examined

full text
figures and tables
references and citing sentences
relations to other papers

levels run

P abstract

not run

S sections
T body sentences
C citations
R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

Figures

**Figure 1.** Seyfert galaxies classified as point sour

**Figure 2.** Seyfert galaxies classified as galaxy dis

**Figure 3.** Seyfert galaxies classified as candidate

**Figure 4.** A detailed view of the Seyfert galaxy NGC

**Figure 5.** Distribution of <Tb>, the average 5 GHz brightness temperature of disk emission in resolved disk sources (top panel) and outflow emission in resolved KSR sources. Since the surface brightness of radio emission from disks compares to the surface brightness of KSRs, KSRs may have been missed in disk sources owing to confusion

**Figure 6.** A comparison of the distribution of q (far-infrared / radio continuum ratio) for non-KSR Seyferts (top panel) and KSR Seyferts (bottom panel). The narrow range of q characteristic of normal spiral galaxies is indicated in both panels by the horizontal double arrows

**Figure 7.** A comparison of the distribution of the luminosity of the nuclear radio source (8.4 GHz luminosity in W Hz−1 ) for non-KSR Seyferts (top panel) and KSR Seyferts (bottom panel). Leftward pointing arrows mark bins containing upper limits

**Figure 8.** Histogram of the position angle differenc

**Figure 9.** Histogram of the position angle differenc

Figures reproduced from arXiv:astro-ph/0604219 by the authors.

References

Works cited (21)

[1]

Neff & de Bruyn 1983

View on Pith 1983
[2]

Ulvestad et al. 1999

View on Pith 1999
[3]

Wilson & Ulvestad 1983

View on Pith 1983
[5]

Colbert et al. 1996a

View on Pith
[8]

Morganti et al. 1999

View on Pith 1999
[9]

Duric & Seaquist 1988

View on Pith 1988
[10]

Wehrle & Morris 1988

View on Pith 1988
[11]

Wrobel & Heeschen 1988

View on Pith 1988
[14]

Schmitt & Kinney 2000

View on Pith 2000
[15]

Hummel & Saikia 1991

View on Pith 1991
[16]

Wehrle & Morris 1987

View on Pith 1987
[17]

Wilson & Ulvestad 1982a

View on Pith
[18]

Wrobel 2000 Notes – S5 refers to the flux density of the extranuclear, KSR emission at 5 GHz. “Lobes” morphology refers to radio structure disconnected from the nucleus; “Tongue” refers to a smooth, broad extension of radio emission from the nucleus; and “Linear” refers to jet- like structures. Additional details are given in Section 3.1. p. 51 Table 4 KS...

View on Pith 2000
[19]

Wilson & Ulvestad 1987

View on Pith 1987
[20]

Gallimore et al. 1996c

View on Pith
[21]

Carral, Turner, & Ho 1990

View on Pith 1990
[22]

Anderson, Ulvestad, & Ho 2004

View on Pith 2004
[23]

Ulvestad & Wilson 1984b

View on Pith
[24]

Middelberg et al. 2004

View on Pith 2004
[25]

Ulvestad & Wilson 1989

View on Pith 1989
[27]

Su et al. 1996 Notes. − MERLIN / VLA refers to observations arcsecond and sub-arcsecond resolution observations with either MERLIN or the VLA, or aper ture synthesis measurements with comparable angular resolution (i.e., ~ 0.1 ″ – 1.0 ″ ). VLBI refers to mas-scale angular p. 53 resolution. In the MERLIN / VLA column, “U” means t he nuclear source is unres...

View on Pith 1996

Forward citations

Cited by 4 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

H 0557$-$385: A Candidate Missing Link Between Radio-Quiet Seyferts and Young Radio Galaxies
astro-ph.GA 2026-11 accept novelty 6.0 of 10

The Seyfert 1 galaxy H 0557-385 has a radio spectrum requiring a two-component model with a compact self-absorbed core and extended lobe, yielding a source size of ~15 pc, age <1800 yr, and jet power ~5e41-5e44 erg/s,...
Non-thermal emission in jets and winds: Expected emission and spectral index distributions
astro-ph.HE 2026-07 conditional novelty 6.0 of 10

Self-consistent CRE evolution in RMHD simulations produces distinct spectral-index gradients that distinguish compact AGN jets from winds even when morphology is ambiguous.
Evidence for the Sombrero Galaxy as an Accelerator of the Highest-Energy Cosmic Rays
astro-ph.HE 2024-12 conditional novelty 6.0 of 10

A maximum-likelihood search of Pierre Auger data finds a 3.3 sigma (global) association between a cosmic-ray multiplet and the Sombrero Galaxy, supporting AGN jet and lobe acceleration of UHECRs.
Supermassive black holes and their surroundings: MeV signatures
astro-ph.HE 2025-07 unverdicted novelty 2.0 of 10

A review of open questions in supermassive black hole physics that argues the MeV gamma-ray band is the critical missing observational window.

How later papers used it

58 later papers cite it

Evidence: substantial. 52 of the citing papers share no author with it, and 7 of those carry a confident label from Pith's citation classifier.

Pith read 13 of the 101 citing sentences, choosing only those whose citation markers point at this paper alone, and wrote the paraphrases from them. The summary, the counts, the evidence level, the links and the quotes come from code; the summary counts the papers listed below. A later paper is listed under a label when Pith's citation classifier gives one of its sentences that label at probability 0.8 or more (0.95 for support), Pith's reading finds that the citing paper itself did it, and a second check confirms the paraphrase against the sentence. This section lists uses only. It does not list criticism or disagreement, so their absence here says nothing about how the paper has been received. Papers that share an author with this one are listed apart, under "By the same authors". A quote is the citing authors' own sentence, shown when their paper's licence is CC BY, CC BY-SA or CC0. JSON

1 paper by the same authors is listed below: 1 used its data or values and 1 cited it as support. It appears under more than one label.

Uses its data or values 1 of 3 papers with this label · 1 by the same authors

By the same authors

Selected sources whose total lobe to lobe extents derived from this paper exceeded 20 arcseconds.

A Radio Polarimetric Study to Disentangle AGN Activity and Star-Formation in Seyfert Galaxies (2020) (same authors) · 0.99 · paraphrased: the licence does not allow quoting

Cites it as support 1 of 5 papers with this label · 1 by the same authors

By the same authors

Cited the observed misalignment between the KSRs and their host galaxy minor axes from this paper as favoring an AGN-jet-driven scenario.

A Radio Polarimetric Study to Disentangle AGN Activity and Star-Formation in Seyfert Galaxies (2020) (same authors) · 0.98 · paraphrased: the licence does not allow quoting

How the literature uses it

7 arXiv papers cite this in 8 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 5 sentences without a confident label

Compares with it 1 paper

They have a size of about 10 kpc above and below the GC, which is similar to kpc scale radio lobes observed in Seyfert galaxies [ref] .

Supermassive black holes and their surroundings: MeV signatures · SgrA* and Bubbles · 0.90

Cites it as support 1 paper

RQ LINERs and Seyferts exhibit sub-relativistic and not collimated jets (e.g., [ref] ).

The nature of compact radio sources: the case of FR0 radio galaxies · Low-luminosity CRSs: the FR0s · 0.97

Cites it as background 1 paper

Radio outflows of extents ranging from tens to hundreds of parsecs on one end, and ten to twenty kiloparsecs (kpc) on the other, have been detected in Seyfert and LINER galaxies [ref] .

Parsec-scale Nuclear Radio Structures in Seyfert Galaxies · Introduction · 0.96

Discussion

Disagree with the review, or know something it missed? Leave a comment, highlight any passage above to comment on it, or challenge this review formally.

[1] [1]

Neff & de Bruyn 1983

View on Pith 1983

[2] [2]

Ulvestad et al. 1999

View on Pith 1999

[3] [3]

Wilson & Ulvestad 1983

View on Pith 1983

[4] [5]

Colbert et al. 1996a

View on Pith

[5] [8]

Morganti et al. 1999

View on Pith 1999

[6] [9]

Duric & Seaquist 1988

View on Pith 1988

[7] [10]

Wehrle & Morris 1988

View on Pith 1988

[8] [11]

Wrobel & Heeschen 1988

View on Pith 1988

[9] [14]

Schmitt & Kinney 2000

View on Pith 2000

[10] [15]

Hummel & Saikia 1991

View on Pith 1991

[11] [16]

Wehrle & Morris 1987

View on Pith 1987

[12] [17]

Wilson & Ulvestad 1982a

View on Pith

[13] [18]

Wrobel 2000 Notes – S5 refers to the flux density of the extranuclear, KSR emission at 5 GHz. “Lobes” morphology refers to radio structure disconnected from the nucleus; “Tongue” refers to a smooth, broad extension of radio emission from the nucleus; and “Linear” refers to jet- like structures. Additional details are given in Section 3.1. p. 51 Table 4 KS...

View on Pith 2000

[14] [19]

Wilson & Ulvestad 1987

View on Pith 1987

[15] [20]

Gallimore et al. 1996c

View on Pith

[16] [21]

Carral, Turner, & Ho 1990

View on Pith 1990

[17] [22]

Anderson, Ulvestad, & Ho 2004

View on Pith 2004

[18] [23]

Ulvestad & Wilson 1984b

View on Pith

[19] [24]

Middelberg et al. 2004

View on Pith 2004

[20] [25]

Ulvestad & Wilson 1989

View on Pith 1989

[21] [27]

Su et al. 1996 Notes. − MERLIN / VLA refers to observations arcsecond and sub-arcsecond resolution observations with either MERLIN or the VLA, or aper ture synthesis measurements with comparable angular resolution (i.e., ~ 0.1 ″ – 1.0 ″ ). VLBI refers to mas-scale angular p. 53 resolution. In the MERLIN / VLA column, “U” means t he nuclear source is unres...

View on Pith 1996