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REVIEW 3 major objections 4 minor 1 cited by

VLASS-based survey of transition state galaxies and their relationship to compact peaked-spectrum radio sources

T0 review · 3 major / 4 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read These 24 recently brightened radio galaxies are not flaring blazars but newborn low-power AGN jets that will evolve into radio-quiet quasars and low-frequency peaked-spectrum sources.

desk verdict Valuable sample of 24 radio transients, but the 'young GPS' label rests on an untested 20-28 yr age assumption. read the letter →

arxiv 2412.07702 v1 pith:5SRLYKRF submitted 2024-12-10 astro-ph.GA astro-ph.HE

M. Kunert-Bajraszewska , A. Krauze , A.E. Kimball , L. Stawarz , P. Kharb , D. Stern , K. Mooley , K. Nyland
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D. Koziel-Wierzbowska
This is my paper · ORCID
classification astro-ph.GAastro-ph.HE
keywords radiotransientsgigahertz-peakedspectrumAGNjetsVLASSNVSSradio-quietquasarstidaldisruptioneventsaccretionratevariability
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

The paper reports 24 galaxies that were undetected or very faint in the 1990s NVSS and FIRST surveys but brightened dramatically by the time of the VLASS survey, 20 to 28 years later. It argues that these are not rare explosions or flaring blazars but low-power analogs of gigahertz-peaked spectrum sources: young AGN jets, radio-quiet in character, that have just switched on. Their convex spectra, parsec-scale sizes, and brightness temperatures place them at the low-luminosity end of the young-radio-source population. The paper's main interpretive claim is that after their radio activity stabilizes, such GHz-peaked transients will settle into radio-intermediate and radio-quiet quasars and low-frequency peaked-spectrum objects, with the most likely trigger being a rise in the black hole's accretion rate. A minority of the sample, including one source previously classified as a tidal disruption event, may instead be genuine TDEs.

What carries the argument

The central objects are 'transition state galaxies': galaxies caught between radio silence and steady AGN radio activity, identified through a flux jump of at least a factor of three between NVSS/FIRST and VLASS. The argument rides on two diagnostic diagrams: the radio power versus linear size ($P$-$D$) plane and the peak frequency versus linear size ($\nu_p$-$D$) plane, which together place a source in an age/power sequence relative to known GPS, CSS, low-luminosity compact, radio-intermediate/radio-quiet quasar, and Seyfert populations. Supporting machinery includes the curved synchrotron spectrum fit that yields the peak frequency $\nu_p$ and optically thick and thin spectral indices, plus VLBA-derived sizes and equipartition magnetic field estimates that tie the spectra to parsec-scale, self-absorbed emitting regions.

What would settle it

Re-image the 24 sources with VLBA at 8.7 GHz after a five-year baseline and measure component separations: the young-jet model predicts apparent expansions of roughly 0.1c to 8.9c, corresponding to milliarcsecond-scale motions at these distances, so an absence of any resolved motion or the discovery of pre-brightening parsec-scale structure in archival data would falsify the newborn-jet interpretation.

Watch

Extended reading notes

Core claim

The paper establishes a sample of 24 slow radio transients selected by comparing the NVSS 1.4 GHz catalog with the first epoch of VLASS at 3 GHz, then characterizes them with VLA, VLBA, GMRT, and LOFAR observations. The central discovery claim is that these objects occupy the low-power, small-size corner of the radio power versus linear size ($P$-$D$) diagram and the peak frequency versus linear size ($\nu_p$-$D$) diagram, exactly where the evolutionary tracks for young compact radio sources begin. They therefore represent the birth of low-power radio jets in galaxies whose stable descendants will look like radio-intermediate and radio-quiet quasars and low-frequency peaked-spectrum sources rather than powerful radio galaxies. The paper further concludes that the transient emission is most plausibly caused by changes in accretion rate that launch low-power ejecta, and it estimates that 8% to 17% of such radio-selected transient samples may be contaminated by tidal disruption events.

Load-bearing premise

The interpretation that these are newborn jets rests on assuming the entire parsec-scale radio structure appeared after the brightening within the 20 to 28 years between NVSS/FIRST and VLASS; if the radio structure existed before, the sources could be older variable AGNs and the evolutionary conclusion would not follow.

Editorial extensions

If this is right

  • The 24 transients will, if the interpretation holds, fade into ordinary radio-intermediate and radio-quiet quasars rather than growing into large FR I/FR II radio galaxies.
  • Low-frequency peaked-spectrum sources found by MHz-frequency surveys are the likely descendants of this population, so the two samples should share host-galaxy and spectral properties.
  • Changes in accretion rate, not high jet power, are sufficient to ignite low-power radio ejecta, implying many quiet galaxies can have short radio-active episodes without becoming radio-loud.
  • About 8% to 17% of radio-selected transient samples may be contaminated by tidal disruption events, so future transient surveys need multi-wavelength follow-up to separate the two populations.
  • The source 101841-13, an infrared-selected TDE candidate, is more naturally explained as a pre-existing Seyfert AGN whose accretion briefly increased, though a TDE contribution cannot be excluded.

Reading between the lines

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

  • Inference: if these are newborn jets, multi-epoch VLBA should resolve the parsec-scale structures expanding over a few years; the predicted apparent speeds of 0.1c to 8.9c are testable within a decade.
  • Inference: the model predicts that each source's spectral peak should drift to lower frequencies as the source grows, so systematic monitoring of $\nu_p$ over years would confirm the young-jet reading independently of the diagrams.
  • Inference: applying the same NVSS-to-VLASS selection to deeper or higher-cadence surveys should find many more transitional objects and measure their number density as a function of radio power, which would test whether the radio-quiet AGN path is the dominant outcome.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 4 minor

Summary. The paper presents 24 radio transients selected by comparing NVSS (1.4 GHz, 1993–1996) with VLASS (3 GHz, 2017–2019), requiring a large flux increase and positional coincidence with a nearby r<20 mag galaxy nucleus. The authors report multi-frequency VLA, VLBA, GMRT, and LOFAR observations, plus optical spectroscopy for redshifts and one detailed case study. They find that most sources have convex spectra, parsec-scale sizes of 0.9–20.5 pc, brightness temperatures of 10^6–10^9 K, and jet-like or compact morphologies, and they classify the sample as low-power GPS-like AGNs. Using the power–size and peak-frequency–size diagrams, they argue that these objects are at the beginning of an evolutionary path toward radio-intermediate/radio-quiet quasars and low-frequency peaked-spectrum sources. They identify accretion-rate changes as the most likely origin of the transients, while considering TDE contamination for a few sources.

Significance. If the central interpretation holds, this is a valuable sample linking slow radio transients to low-power GPS-like AGNs and changing-state accretion phenomena. The paper's strengths are the multi-frequency, multi-resolution dataset, the systematic spectral modeling, the comparison with independent external samples in the P–D and nu_p–D planes, and the candid discussion of alternative explanations, including TDE contamination. The individual source characterizations, especially the VLBA morphologies and the optical analysis of 101841–13, are useful in their own right. However, the evolutionary conclusion rests on an age assumption that is not independently tested, and one of the paper's statements about selection biases is internally inconsistent. The data support the classification of most sources as compact, low-power AGN-like radio emitters, but the specific evolutionary trajectory is a hypothesis that needs to be clearly labelled as such.

major comments (3)
  1. [Section 4.2, Table 5] The central youth interpretation is load-bearing for the evolutionary claims in Sections 4.4 and 4.5, and it rests on the assumption stated in Section 4.2 that the entire VLBA structures formed within the 20–28 years between NVSS/FIRST and VLASS. The resulting expansion velocities in Table 5 range up to 8.94c for 110239–06, which is a strong warning that the adopted time window is not the true formation time for at least some structures, or that beaming is important. If the parsec-scale emission pre-existed the brightening, the measured sizes are not dynamical ages, the P–D and nu_p–D placements do not by themselves prove an early evolutionary stage, and the 'newborn jet' interpretation would not follow. The paper itself calls these estimates 'only a very rough estimate of the lower limit,' but the abstract and conclusions present the youth scenario more firmly. I request that the authors either obtain or cite proper-motion or two-epoch VLBA constraints for at least a subset of sources, or explicitly re-frame the youth interpretation as one of several alternatives and soften the evolutionary claims accordingly.
  2. [Section 4, second paragraph] The statement that 'the selection criteria used in this study do not bias toward limiting the source power' is contradicted by the r<20 mag host-galaxy selection criterion described in Section 2. That criterion restricts the sample to relatively nearby galaxies (the paper itself notes z<0.3), which for a fixed 3 GHz flux limit of 8 mJy imposes an upper limit on the radio luminosity of selected sources. The absence of transients above 10^25 W Hz^-1 is therefore at least partly a selection effect, not an unambiguously real physical limit. The authors should quantify the luminosity selection function or remove the claim that the luminosity distribution reflects a real physical limit, since the subsequent comparison to higher-power GPS/CSS samples is affected.
  3. [Section 4.5, Figure 9] The conclusion that the low-power transients may be progenitors of low-frequency peaked-spectrum objects relies in part on the placement of the Callingham et al. (2017) sample in the nu_p–D diagram using equipartition angular sizes estimated from assumed median redshift and flux densities, rather than from direct size measurements. These estimated sizes have a large model dependence, and the resulting positions are therefore not directly comparable to the measured VLBA sizes of the present sample. Please either present the estimated sizes with their systematic uncertainties and show how the conclusion changes under different assumptions, or explicitly mark these points as model-dependent and reduce the weight given to them in the evolutionary scenario.
minor comments (4)
  1. [Section 4.1] In the paragraph discussing spectral shapes, the source '180940−24' should be '180940+24' to match Table 1 and the rest of the text.
  2. [Section 2] The phrase 'implied spectral index α > 2 between 1.4 GHz and 3 GHz' compares flux densities at two different epochs (NVSS 1993–1996 and VLASS 2017–2019), so it is not a simultaneous spectral index. This should be worded as a variability-based selection condition, not a spectral slope, to avoid confusion with the measured SEDs in Section 4.1.
  3. [Table 2 and Figure 10] For the four sources with fixed parameters or no fitted peak (180940+24, 203909−30, 070837+32, 105035−07), the figure should make clear which plotted curves are constrained and which are not; currently the reader must check the table notes to infer this.
  4. [Section 4.5 and Figure 9] Please state explicitly whether the plotted 'intrinsic turnover frequency' is the rest-frame peak frequency, and describe the k-correction applied to the measured peak frequencies in Table 2.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: the 'young GPS / evolutionary path' interpretation is an assumption-caveated inference built on new VLBA/VLA/GMRT data and external comparison samples, not a reduction of the conclusion to its inputs.

full rationale

The derivation chain is not circular. The sample-selection criterion 'implied spectral index α > 2, between 1.4 GHz and 3 GHz' (§2) is an inter-epoch quantity, comparing NVSS (1993–1996) upper limits with VLASS (2017–2019) detections; it therefore measures the transient brightening, not a contemporaneous spectral slope, and does not by construction produce the measured convex SEDs. The GPS-like classification additionally rests on new, independent VLBA measurements of compact sizes (0.9–20.5 pc) and brightness temperatures (10^6–10^9 K), which are not guaranteed by the survey selection. The central P–D and νp–D placements (§4.4–4.5) are comparisons against external samples (Keim et al. 2019; Orienti & Dallacasa 2014; Callingham et al. 2017; Kukula et al. 1998; Jarvis et al. 2019), with some self-citations (LLC from Kunert-Bajraszewska et al. 2010; CNSS transients from Wołowska et al. 2021) that are contextual rather than load-bearing because the same diagram regions are independently populated by RIQ/RQQ, Seyfert, and low-frequency peaked-spectrum data. The expansion-velocity estimate is explicitly conditional: §4.2 states 'Assuming that the entire VLBA structures of our sources were formed after the radio brightening' and calls it 'only a very rough estimate of the lower limit of this velocity.' The paper also acknowledges in §4.1 that uncertainties prevent testing whether SSA or FFA produces the curvature. These are stated limitations on the evolutionary interpretation, not circular reductions of the central claim to its inputs. The proposed evolution into RI/RQ quasars and low-frequency peaked-spectrum objects is a hypothesis based on diagram positions and external relations, not a prediction forced by a fitted parameter or by a self-citation chain.

Assumptions & free parameters 6 free parameters · 6 assumptions · 0 invented entities

The evolutionary interpretation rests on the SSA/equipartition model for the spectral turnover, the assumption that the VLBA structures are newly formed, and the application of the powerful-GPS nu_p-D relation to low-power transients. The fixed spectral parameters for two sources and the manually estimated indices for two more are the main hand-set inputs that affect the nu_p-D diagram.

free parameters (6)
  • S_p (peak flux density), source 180940+24 = 7.79 mJy
    Fixed in Table 2 because the source has no observed spectral maximum in the 1-10 GHz range; the chosen value affects its placement in the nu_p-D diagram.
  • nu_p (peak frequency), source 180940+24 = 1.50 GHz
    Fixed in Table 2 to obtain a fit; the source has no formal turnover in the observed range.
  • alpha_thick, source 180940+24 = -0.40
    Fixed in Table 2 to obtain a proper fit for a source with no turnover.
  • S_p (peak flux density), source 203909-30 = 7.00 mJy
    Fixed in Table 2 because the source has no spectral maximum in the observed range.
  • nu_p (peak frequency), source 203909-30 = 3.50 GHz
    Fixed in Table 2 to obtain a fit; affects nu_p-D placement.
  • alpha_thick, source 203909-30 = 0.25
    Fixed in Table 2 to obtain a proper fit.
assumptions (6)
  • domain assumption Concordance cosmology with H0 = 70 km/s/Mpc, Omega_M = 0.3, Omega_Lambda = 0.7
    Used for luminosity distances and linear sizes throughout (Section 1).
  • domain assumption The spectral turnover is produced by synchrotron self-absorption (SSA) in a uniform source with a power-law electron distribution
    Appendix A derives the equipartition magnetic field and the nu_p-D mapping under SSA; the paper acknowledges free-free absorption as an alternative (Section 4.1).
  • domain assumption Equipartition of energy between radiating particles and magnetic field (eta_eq = 1)
    Used in Appendix A to estimate B_eq and in Section 4.5 to estimate sizes of comparison peaked-spectrum sources; the authors note a weak dependence on eta_eq, but the comparison sample sizes do depend on this choice.
  • ad hoc to paper The entire VLBA radio structure formed after the radio brightening, within the 20-28 years between NVSS/FIRST and VLASS
    Section 4.2 states this assumption and uses it to estimate expansion velocities and infer the youth of the sources; it is load-bearing for the evolutionary interpretation.
  • domain assumption The nu_p-D relation for powerful GPS/CSS sources (Orienti and Dallacasa 2014) is applicable to low-power transients, with deviations implying a parallel path
    Section 4.5 uses this relation to interpret the sources as early-stage objects and to propose a parallel low-power evolutionary track.
  • domain assumption The modified power-law model (Equation 1) with constant spectral indices on either side of the peak adequately represents the radio SEDs
    Used in Section 3.6 for spectral fitting; two sources could not be fitted with this model ('upturn' spectra) and two others required fixed parameters (Table 2).

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Cite this review

Pith. "Pith review of VLASS-based survey of transition state galaxies and their relationship to compact peaked-spectrum radio sources." pith.science (2026). https://pith.science/paper/5SRLYKRF

@misc{pith2026241207702,
  author       = {Pith},
  title        = {Pith review of: VLASS-based survey of transition state galaxies and their relationship to compact peaked-spectrum radio sources},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/5SRLYKRF}},
  note         = {Machine review of arXiv:2412.07702}
}
abstract

We present multi-frequency and high-resolution studies of a sample of 24 radio transients sources discovered by comparing the NRAO VLA Sky Survey (NVSS) and Very Large Array Sky Survey (VLASS) surveys. All of them are characterized by a significant increase in radio flux density over the last two decades.Their convex spectra, small sizes and high brightness temperatures are typical for young gigahertz-peaked spectrum (GPS) radio sources and indicative of an AGN buried in the host galaxy. On the other hand, they are much weaker than the archetypical GPS objects and their parsec-scale radio structures, although indicating the presence of young radio jets, are similar to radio-quiet AGNs like Seyfert and low-ionization nuclear emission-line region (LINER) galaxies. Based on the distribution of these objects in power$-$size ($P - D$) and peak frequency$-$size ($\nu_p - D$) diagrams, we suggest that after stabilizing their radio activity, some of the GHz-peaked radio transients (galaxies and quasars) will develop into radio-intermediate and radio-quiet (RI/RQ) quasars and low-frequency peaked-spectrum (PS) objects. We discuss several possible origins for the transient radio emission in our sources and conclude that changes in the accretion rate combined with low-power radio ejecta are the most probable cause. This is the scenario we also propose for one of our sources, 101841$-$13, which was independently identified as a candidate tidal disruption event (TDE) based on its infrared variability. However, we cannot exclude that 101841$-$13 or other sources in our sample are TDEs.

Figures

Figures reproduced from arXiv: 2412.07702 by the authors.

Figure 1
Figure 1. High-frequency radio images for 024345−28, 024609+34 and 031115+08; from left to right: NVSS 1.4 GHz, VLASS 3 GHz (first epoch) and VLBA 8.7 GHz. The other 21 sources are presented in Appendix, [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. 5 GHz luminosity vs. redshift diagram. The transient sources from this work are marked with filled yellow (galaxies) and gray (quasar) circles. The open red circles (galaxies) and open black circles (quasars) indicate CSS and GPS sources taken from O’Dea (1998), Snellen et al. (1998b), de Vries et al. (1997), Stanghellini et al. (1998), and Fanti et al. (1990) as collected by Keim et al. (2019) into one sample. The … view at source ↗
Figure 3
Figure 3. Radio color-color diagram for our sample. The blue square corresponds to the spectral index range from −0.5 to 0.5 (“blazar box”). Galaxies are marked with yellow circles, and the only quasar in the sample is shown in gray. The two galaxies, 180940+24 and 203909−30, with fixed values for their spectral in￾dices indicated by brown circles. Details on the calculation of αthin and αthick are provided in Section 3.6 and… view at source ↗
Figures from the paper (11 more)
Figure 4
Figure 4. Figure 4: (Left): Distribution of spectral indices for our sample of 24 transient sources. (Right): Comparison of the distribution of spectral indices for the combined sample of archetypal GPS and CSS sources from Keim et al. (2019) and the combined sample of radio transients fr…
Figure 5
Figure 5. Figure 5: The GMRT image and selected VLA images showing source 064001+28 (marked as A) and additional components/sources marked as B1- B3 and C. The lower right panel shows measurements of their flux densities, with measurements of component A added for comparison. Note, howeve…
Figure 6
Figure 6. Figure 6: The VLA S-band image (magenta contours) overlaid on the SDSS i-band image of 064001+28. The presented contours have the following values: 1.7, 5, 20 × 10−4 Jy beam−1 . to lower frequencies and variations in optical depth and thus also in flux density. Moreover, such a …
Figure 7
Figure 7. Figure 7: (Left): Distribution of variability ratio at 3 GHz for our sample. (Right): The 3 GHz light curves for selected sources. The gray dashed line indicates the recalculated value of νLν,GHz = 1039 erg s−1 below which most known thermal TDEs occur (Cendes et al. 2024). radi…
Figure 8
Figure 8. Figure 8: The radio power vs. linear size (P − D) diagram adapted from Kunert-Bajraszewska et al. (2010), including various types of radio￾selected AGNs. The plots of GPS, CSS, LLC, FR I and FR II sources are taken from Kunert-Bajraszewska et al. (2010). The sample of giant radi…
Figure 9
Figure 9. Figure 9: The intrinsic turnover frequency vs. linear size diagram. The transient sources from this work are marked with yellow (galaxies) and gray (quasar) circles. The open red circles (galaxies) and open black circles (quasars) indicate CSS and GPS sources taken from O’Dea (1…
Figure 10
Figure 10. Figure 10: The radio SEDs between 144 MHz and 16.9 GHz. The solid line shows the best-fit to the data with the modified power-law model (Equation 1) [PITH_FULL_IMAGE:figures/full_fig_p027_10.png]
Figure 11
Figure 11. Figure 11: shows the radio images at 144 MHz for four sources observed with LOFAR (Shimwell et al. 2022) [PITH_FULL_IMAGE:figures/full_fig_p028_11.png]
Figure 12
Figure 12. Figure 12: (Left): Palomar (red) and archival 6dF (black) optical spectra of 101841−13 with strong emission lines indicated. The left axis shows the flux obtained from the (non-photometric) Palomar observations, and the right axis shows the uncalibrated flux in counts from the 6…
Figure 13
Figure 13. Figure 13: BPT and WHAN diagrams (Baldwin et al. 1981; Kewley et al. 2006; Cid Fernandes et al. 2011) for 101841−13. The red circle indicates values calculated based on measurements from the Palomar spectrum, and the black circle indicates upper limits estimated based on the 6dF…
Figure 14
Figure 14. Figure 14: The following high-frequency images are presented from left to right: NVSS 1.4 GHz, VLASS 3 GHz (first epoch) and VLBA 8.7 GHz [PITH_FULL_IMAGE:figures/full_fig_p038_14.png]

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Works this paper leans on

120 extracted references · 12 canonical work pages · cited by 1 Pith paper

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    b',8Ί P ED< mqP3 u;Ƌ|? o눸o

    thebibliography [1] 20pt to REFERENCES 6pt =0pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command E...

    arXiv 2021

  4. [4]

    D., van Velzen , S., Horesh , A., & Zauderer , B

    Alexander , K. D., van Velzen , S., Horesh , A., & Zauderer , B. A. 2020, , 216, 81, 10.1007/s11214-020-00702-w

    doi:10.1007/s11214-020-00702-w 2020

  5. [5]

    F., Aller , H

    Aller , M. F., Aller , H. D., & Hughes , P. A. 1992, , 399, 16, 10.1086/171898

    doi:10.1086/171898 1992

  6. [6]

    2012, , 760, 77, 10.1088/0004-637X/760/1/77

    An & Baan . 2012, , 760, 77, 10.1088/0004-637X/760/1/77

    doi:10.1088/0004-637x/760/1/77 2012

  7. [8]

    M., Mooley , K

    Anderson , M. M., Mooley , K. P., Hallinan , G., et al. 2020, , 903, 116, 10.3847/1538-4357/abb94b

    doi:10.3847/1538-4357/abb94b 2020

  8. [9]

    D., Williams , D

    Baldi , R. D., Williams , D. R. A., McHardy , I. M., et al. 2018, , 476, 3478, 10.1093/mnras/sty342

    doi:10.1093/mnras/sty342 2018

Show all 120 references
  1. [10]

    A., Phillips , M

    Baldwin , J. A., Phillips , M. M., & Terlevich , R. 1981, , 93, 5, 10.1086/130766

    1981 doi

  2. [11]

    Barthel , P. D. 1989, , 336, 606, 10.1086/167038

    1989 doi

  3. [12]

    V., Dopita , M

    Bicknell , G. V., Dopita , M. A., & O'Dea , C. P. O. 1997, , 485, 112, 10.1086/304400

    1997 doi

  4. [13]

    R., Gaensler , B

    Callingham , J. R., Gaensler , B. M., Ekers , R. D., et al. 2015, , 809, 168, 10.1088/0004-637X/809/2/168

    2015 doi

  5. [14]

    R., Ekers , R

    Callingham , J. R., Ekers , R. D., Gaensler , B. M., et al. 2017, , 836, 174, 10.3847/1538-4357/836/2/174

    2017 doi

  6. [15]

    D., Brienza , M., Morganti , R., & Giovannini , G

    Capetti , A., Baldi , R. D., Brienza , M., Morganti , R., & Giovannini , G. 2019, , 631, A176, 10.1051/0004-6361/201936254

    2019 doi

  7. [16]

    A., Clayton , G

    Cardelli , J. A., Clayton , G. C., & Mathis , J. S. 1989, , 345, 245

    1989

  8. [17]

    D., et al

    Cendes , Y., Berger , E., Alexander , K. D., et al. 2024, , 971, 185, 10.3847/1538-4357/ad5541

    2024 doi

  9. [18]

    Cid Fernandes , R., Mateus , A., Sodr \'e , L., Stasi \'n ska , G., & Gomes , J. M. 2005, , 358, 363

    2005

  10. [19]

    2011, , 413, 1687, 10.1111/j.1365-2966.2011.18244.x

    Cid Fernandes , R., Stasi \'n ska , G., Mateus , A., & Vale Asari , N. 2011, , 413, 1687, 10.1111/j.1365-2966.2011.18244.x

    2011

  11. [20]

    J., Cotton , W

    Condon , J. J., Cotton , W. D., Greisen , E. W., et al. 1998, , 115, 1693, 10.1086/300337

    1998 doi

  12. [21]

    J., Huang , Z

    Condon , J. J., Huang , Z. P., Yin , Q. F., & Thuan , T. X. 1991, , 378, 65, 10.1086/170407

    1991 doi

  13. [22]

    2009, , 698, 840, 10.1088/0004-637X/698/1/840

    Czerny , B., Siemiginowska , A., Janiuk , A., Nikiel-Wroczy \'n ski , B., & Stawarz , . 2009, , 698, 840, 10.1088/0004-637X/698/1/840

    2009 doi

  14. [23]

    H., Barthel , P

    de Vries , W. H., Barthel , P. D., & O'Dea , C. P. 1997, , 321, 105

    1997

  15. [24]

    D., De Rosa , G., Croxall , K., et al

    Denney , K. D., De Rosa , G., Croxall , K., et al. 2014, , 796, 134, 10.1088/0004-637X/796/2/134

    2014 doi

  16. [25]

    J., Djorgovski , S

    Drake , A. J., Djorgovski , S. G., Mahabal , A., et al. 2009, , 696, 870, 10.1088/0004-637X/696/1/870

    2009 doi

  17. [26]

    A., Margutti , R., & Alexander , K

    Eftekhari , T., Berger , E., Zauderer , B. A., Margutti , R., & Alexander , K. D. 2018, , 854, 86, 10.3847/1538-4357/aaa8e0

    2018 doi

  18. [27]

    L., & Riley , J

    Fanaroff , B. L., & Riley , J. M. 1974, , 167, 31P, 10.1093/mnras/167.1.31P

    1974 doi

  19. [28]

    T., et al

    Fanti , R., Fanti , C., Schilizzi , R. T., et al. 1990, , 231, 333

    1990

  20. [29]

    F., Axon , D

    Gallimore , J. F., Axon , D. J., O'Dea , C. P., Baum , S. A., & Pedlar , A. 2006, , 132, 546, 10.1086/504593

    2006 doi

  21. [30]

    1993, , 407, 65, 10.1086/172493

    Ghisellini , G., Padovani , P., Celotti , A., & Maraschi , L. 1993, , 407, 65, 10.1086/172493

    1993 doi

  22. [31]

    1991, , 252, 313, 10.1093/mnras/252.3.313

    Ghisellini , G., & Svensson , R. 1991, , 252, 313, 10.1093/mnras/252.3.313

    1991 doi

  23. [32]

    J., Kulkarni , S

    Graham , M. J., Kulkarni , S. R., Bellm , E. C., et al. 2019, , 131, 078001, 10.1088/1538-3873/ab006c

    2019 doi

  24. [33]

    J., Ross , N

    Graham , M. J., Ross , N. P., Stern , D., et al. 2020, , 491, 4925, 10.1093/mnras/stz3244

    2020 doi

  25. [34]

    E., Taylor , G

    Gugliucci , N. E., Taylor , G. B., Peck , A. B., & Giroletti , M. 2005, , 622, 136, 10.1086/427934

    2005 doi

  26. [35]

    J., Williams , W

    Hardcastle , M. J., Williams , W. L., Best , P. N., et al. 2019, , 622, A12, 10.1051/0004-6361/201833893

    2019 doi

  27. [36]

    a rvel \

    J \"a rvel \"a , E., Savolainen , T., Berton , M., et al. 2024, , 532, 3069, 10.1093/mnras/stae1701

    2024 doi

  28. [37]

    E., Harrison , C

    Jarvis , M. E., Harrison , C. M., Thomson , A. P., et al. 2019, , 485, 2710, 10.1093/mnras/stz556

    2019 doi

  29. [38]

    2016, , 458, 3786, 10.1093/mnras/stw181

    Jeyakumar , S. 2016, , 458, 3786, 10.1093/mnras/stw181

    2016 doi

  30. [39]

    H., Saunders , W., Colless , M., et al

    Jones , D. H., Saunders , W., Colless , M., et al. 2004, , 355, 747, 10.1111/j.1365-2966.2004.08353.x

    2004

  31. [41]

    Kale , R., & Ishwara-Chandra , C. H. 2021, Experimental Astronomy, 51, 95, 10.1007/s10686-020-09677-6

    2021 doi

  32. [42]

    A., Callingham , J

    Keim , M. A., Callingham , J. R., & R \"o ttgering , H. J. A. 2019, , 628, A56, 10.1051/0004-6361/201936107

    2019 doi

  33. [43]

    I., Condon , J

    Kellermann , K. I., Condon , J. J., Kimball , A. E., Perley , R. A., & Ivezi \'c , Z . 2016, , 831, 168, 10.3847/0004-637X/831/2/168

    2016 doi

  34. [44]

    J., Groves , B., Kauffmann , G., & Heckman , T

    Kewley , L. J., Groves , B., Kauffmann , G., & Heckman , T. 2006, , 372, 961, 10.1111/j.1365-2966.2006.10859.x

    2006

  35. [45]

    G., Clausen-Brown , E., et al

    Kharb , P., Blackman , E. G., Clausen-Brown , E., et al. 2024, , 962, 180, 10.3847/1538-4357/ad168e

    2024 doi

  36. [46]

    P., Baum , S

    Kharb , P., O'Dea , C. P., Baum , S. A., Colbert , E. J. M., & Xu , C. 2006, , 652, 177, 10.1086/507945

    2006 doi

  37. [47]

    2016, , 459, 1310, 10.1093/mnras/stw699

    Kharb , P., Srivastava , S., Singh , V., et al. 2016, , 459, 1310, 10.1093/mnras/stw699

    2016 doi

  38. [48]

    2021, , 919, 108, 10.3847/1538-4357/ac0c82

    Kharb , P., Subramanian , S., Das , M., Vaddi , S., & Paragi , Z. 2021, , 919, 108, 10.3847/1538-4357/ac0c82

    2021 doi

  39. [49]

    E., Kellermann , K

    Kimball , A. E., Kellermann , K. I., Condon , J. J., Ivezi \'c , Z ., & Perley , R. A. 2011, , 739, L29, 10.1088/2041-8205/739/1/L29

    2011 doi

  40. [50]

    Kormendy , J., & Ho , L. C. 2013, , 51, 511, 10.1146/annurev-astro-082708-101811

    2013 doi

  41. [51]

    J., Dunlop , J

    Kukula , M. J., Dunlop , J. S., Hughes , D. H., & Rawlings , S. 1998, , 297, 366, 10.1046/j.1365-8711.1998.01481.x

    1998

  42. [52]

    P., Labiano , A., & Siemiginowska , A

    Kunert-Bajraszewska , M., Gawro \'n ski , M. P., Labiano , A., & Siemiginowska , A. 2010, , 408, 2261, 10.1111/j.1365-2966.2010.17271.x

    2010

  43. [53]

    2006, , 450, 945, 10.1051/0004-6361:20054428

    Kunert-Bajraszewska , M., Marecki , A., & Thomasson , P. 2006, , 450, 945, 10.1051/0004-6361:20054428

    2006 doi

  44. [54]

    Kunert-Bajraszewska , M., Marecki , A., Thomasson , P., & Spencer , R. E. 2005, , 440, 93, 10.1051/0004-6361:20042496

    2005 doi

  45. [55]

    2020, , 897, 128, 10.3847/1538-4357/ab9598

    Kunert-Bajraszewska , M., Wo owska , A., Mooley , K., Kharb , P., & Hallinan , G. 2020, , 897, 128, 10.3847/1538-4357/ab9598

    2020 doi

  46. [56]

    Ku \'z micz , A., Jamrozy , M., Bronarska , K., Janda-Boczar , K., & Saikia , D. J. 2018, , 238, 9, 10.3847/1538-4365/aad9ff

    2018 doi

  47. [57]

    2020 a , in American Astronomical Society Meeting Abstracts, American Astronomical Society Meeting Abstracts, 306.16

    Lacy , M., Gates , E., Brandt , W., et al. 2020 a , in American Astronomical Society Meeting Abstracts, American Astronomical Society Meeting Abstracts, 306.16

    2020

  48. [58]

    A., Chandler , C

    Lacy , M., Baum , S. A., Chandler , C. J., et al. 2020 b , , 132, 035001, 10.1088/1538-3873/ab63eb

    2020 doi

  49. [59]

    a hteenm \

    L \"a hteenm \"a ki , A., J \"a rvel \"a , E., Ramakrishnan , V., et al. 2018, , 614, L1, 10.1051/0004-6361/201833378

    2018 doi

  50. [60]

    M., Cales , S., Moran , E

    LaMassa , S. M., Cales , S., Moran , E. C., et al. 2015, , 800, 144, 10.1088/0004-637X/800/2/144

    2015 doi

  51. [61]

    L., Aller , M

    Lister , M. L., Aller , M. F., Aller , H. D., et al. 2018, , 234, 12, 10.3847/1538-4365/aa9c44

    2018 doi

  52. [62]

    L., Aller , H

    Lister , M. L., Aller , H. D., Aller , M. F., et al. 2009, , 137, 3718, 10.1088/0004-6256/137/3/3718

    2009 doi

  53. [63]

    L., Aller , M

    Lister , M. L., Aller , M. F., Aller , H. D., et al. 2013, , 146, 120, 10.1088/0004-6256/146/5/120

    2013 doi

  54. [64]

    L., Ross , N

    MacLeod , C. L., Ross , N. P., Lawrence , A., et al. 2016, , 457, 389, 10.1093/mnras/stv2997

    2016 doi

  55. [65]

    M., et al

    Mainzer , A., Bauer , J., Cutri , R. M., et al. 2014, , 792, 30, 10.1088/0004-637X/792/1/30

    2014 doi

  56. [66]

    2024, , 961, 211, 10.3847/1538-4357/ad18bb

    Masterson , M., De , K., Panagiotou , C., et al. 2024, , 961, 211, 10.3847/1538-4357/ad18bb

    2024 doi

  57. [67]

    2006, , 370, 721

    Mateus , A., Sodr \'e , L., Cid Fernandes , R., et al. 2006, , 370, 721

    2006

  58. [68]

    2018, Science, 361, 482, 10.1126/science.aao4669

    Mattila , S., P \'e rez-Torres , M., Efstathiou , A., et al. 2018, Science, 361, 482, 10.1126/science.aao4669

    2018 doi

  59. [69]

    V., Kimball , A

    McCaffrey , T. V., Kimball , A. E., Momjian , E., & Richards , G. T. 2022, , 164, 122, 10.3847/1538-3881/ac853e

    2022 doi

  60. [70]

    P., Waters , B., Schiebel , D., Young , W., & Golap , K

    McMullin , J. P., Waters , B., Schiebel , D., Young , W., & Golap , K. 2007, in Astronomical Society of the Pacific Conference Series, Vol. 376, Astronomical Data Analysis Software and Systems XVI, ed. R. A. Shaw , F. Hill , & D. J. Bell , 127

    2007

  61. [71]

    L., Nagar , N

    Middelberg , E., Roy , A. L., Nagar , N. M., et al. 2004, , 417, 925, 10.1051/0004-6361:20040019

    2004 doi

  62. [72]

    G., Sotnikova , Y

    Mingaliev , M. G., Sotnikova , Y. V., Torniainen , I., Tornikoski , M., & Udovitskiy , R. Y. 2012, , 544, A25, 10.1051/0004-6361/201118506

    2012 doi

  63. [73]

    P., Myers , S

    Mooley , K. P., Myers , S. T., Frail , D. A., et al. 2019, , 870, 25, 10.3847/1538-4357/aaef7c

    2019 doi

  64. [74]

    P., Hallinan , G., Bourke , S., et al

    Mooley , K. P., Hallinan , G., Bourke , S., et al. 2016, , 818, 105, 10.3847/0004-637X/818/2/105

    2016 doi

  65. [75]

    Z., Patil , P., et al

    Nyland , K., Dong , D. Z., Patil , P., et al. 2020, , 905, 74, 10.3847/1538-4357/abc341

    2020 doi

  66. [76]

    O'Dea , C. P. 1998, , 110, 493, 10.1086/316162

    1998 doi

  67. [77]

    P., & Baum , S

    O'Dea , C. P., & Baum , S. A. 1997, , 113, 148, 10.1086/118241

    1997 doi

  68. [78]

    P., & Saikia , D

    O'Dea , C. P., & Saikia , D. J. 2021, , 29, 3, 10.1007/s00159-021-00131-w

    2021 doi

  69. [79]

    2008, , 477, 807, 10.1051/0004-6361:20078098

    Orienti , M., & Dallacasa , D. 2008, , 477, 807, 10.1051/0004-6361:20078098

    2008 doi

  70. [80]

    2014, , 438, 463, 10.1093/mnras/stt2217

    ---. 2014, , 438, 463, 10.1093/mnras/stt2217

    2014 doi

  71. [81]

    2010, , 402, 1892, 10.1111/j.1365-2966.2009.16016.x

    Orienti , M., Murgia , M., & Dallacasa , D. 2010, , 402, 1892, 10.1111/j.1365-2966.2009.16016.x

    2010

  72. [82]

    D., Laor , A., et al

    Panessa , F., Baldi , R. D., Laor , A., et al. 2019, Nature Astronomy, 3, 387, 10.1038/s41550-019-0765-4

    2019 doi

  73. [83]

    G., & Conway , J

    Polatidis , A. G., & Conway , J. E. 2003, , 20, 69, 10.1071/AS02053

    2003 doi

  74. [84]

    Readhead , A. C. S., Taylor , G. B., Pearson , T. J., & Wilkinson , P. N. 1996, , 460, 634, 10.1086/176997

    1996 doi

  75. [85]

    Readhead , A. C. S., Ravi , V., Liodakis , I., et al. 2021, , 907, 61, 10.3847/1538-4357/abd08c

    2021 doi

  76. [86]

    Readhead , A. C. S., Ravi , V., Blandford , R. D., et al. 2024, , 961, 242, 10.3847/1538-4357/ad0c55

    2024 doi

  77. [87]

    S., & Begelman , M

    Reynolds , C. S., & Begelman , M. C. 1997, , 487, L135, 10.1086/310894

    1997 doi

  78. [88]

    Rickett , B. J. 1986, , 307, 564, 10.1086/164444

    1986 doi

  79. [89]

    R., Hurley-Walker , N., et al

    Ross , K., Callingham , J. R., Hurley-Walker , N., et al. 2021, , 501, 6139, 10.1093/mnras/staa3795

    2021 doi

  80. [90]

    J., Anderson , S

    Ruan , J. J., Anderson , S. F., Eracleous , M., et al. 2019, , 883, 76, 10.3847/1538-4357/ab3c1a

    2019 doi

  81. [91]

    M., Ekers , R

    Sadler , E. M., Ekers , R. D., Mahony , E. K., Mauch , T., & Murphy , T. 2014, , 438, 796, 10.1093/mnras/stt2239

    2014 doi

  82. [92]

    S., Jurlin , N., Morganti , R., et al

    Shabala , S. S., Jurlin , N., Morganti , R., et al. 2020, , 496, 1706, 10.1093/mnras/staa1172

    2020 doi

  83. [93]

    I., Popovi \'c , L

    Shapovalova , A. I., Popovi \'c , L. C ., Burenkov , A. N., et al. 2010, , 509, A106, 10.1051/0004-6361/200912311

    2010 doi

  84. [94]

    W., Hardcastle , M

    Shimwell , T. W., Hardcastle , M. J., Tasse , C., et al. 2022, , 659, A1, 10.1051/0004-6361/202142484

    2022 doi

  85. [95]

    M., et al

    Silpa , S., Kharb , P., Harrison , C. M., et al. 2021, , 507, 991, 10.1093/mnras/stab1870

    2021 doi

  86. [96]

    C., et al

    Silpa , S., Kharb , P., Ho , L. C., et al. 2020, , 499, 5826, 10.1093/mnras/staa2970

    2020 doi

  87. [97]

    2018, , 480, 1796, 10.1093/mnras/sty1818

    Singh , V., & Chand , H. 2018, , 480, 1796, 10.1093/mnras/sty1818

    2018 doi

  88. [98]

    H., & Athreya , R

    Singh , V., Shastri , P., Ishwara-Chandra , C. H., & Athreya , R. 2013, , 554, A85, 10.1051/0004-6361/201221003

    2013 doi

  89. [99]

    M., Callingham , J

    Slob , M. M., Callingham , J. R., R \"o ttgering , H. J. A., et al. 2022, , 668, A186, 10.1051/0004-6361/202244651

    2022 doi

  90. [100]

    Snellen , I. A. G., Schilizzi , R. T., de Bruyn , A. G., & Miley , G. K. 1998 a , , 333, 70, 10.48550/arXiv.astro-ph/9801304

    1998 doi arXiv

  91. [101]

    Snellen , I. A. G., Schilizzi , R. T., de Bruyn , A. G., et al. 1998 b , , 131, 435, 10.1051/aas:1998281

    1998 doi

  92. [102]

    Snellen , I. A. G., Schilizzi , R. T., Miley , G. K., et al. 2000, , 319, 445, 10.1046/j.1365-8711.2000.03935.x

    2000

  93. [103]

    J., Ravi , V., Dong , D

    Somalwar , J. J., Ravi , V., Dong , D. Z., et al. 2023, , 945, 142, 10.3847/1538-4357/acbafc

    2023 doi

  94. [104]

    2024, arXiv e-prints, arXiv:2310.03791, 10.48550/arXiv.2310.03791

    ---. 2024, arXiv e-prints, arXiv:2310.03791, 10.48550/arXiv.2310.03791

    2024 doi arXiv

  95. [105]

    V., Mufakharov , T

    Sotnikova , Y. V., Mufakharov , T. V., Majorova , E. K., et al. 2019, Astrophysical Bulletin, 74, 348, 10.1134/S1990341319040023

    2019 doi

  96. [106]

    V., Mufakharov , T

    Sotnikova , Y. V., Mufakharov , T. V., Mingaliev , M. G., et al. 2022, Astrophysical Bulletin, 77, 361, 10.1134/S1990341322040149

    2022 doi

  97. [107]

    P., Dallacasa , D., et al

    Stanghellini , C., O'Dea , C. P., Dallacasa , D., et al. 1998, , 131, 303, 10.1051/aas:1998270

    1998 doi

  98. [108]

    J., Arav , N., et al

    Stern , D., Graham , M. J., Arav , N., et al. 2017, , 839, 106, 10.3847/1538-4357/aa683c

    2017 doi

  99. [109]

    J., et al

    Stern , D., McKernan , B., Graham , M. J., et al. 2018, , 864, 27, 10.3847/1538-4357/aac726

    2018 doi

  100. [110]

    A., & Wilson , A

    Storchi-Bergmann , T., Baldwin , J. A., & Wilson , A. S. 1993, , 410, L11, 10.1086/186867

    1993 doi

  101. [111]

    G., Blandford , R

    Sullivan , A. G., Blandford , R. D., Begelman , M. C., Birkinshaw , M., & Readhead , A. C. S. 2024, , 528, 6302, 10.1093/mnras/stae322

    2024 doi

  102. [112]

    1986, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Tody , D. 1986, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 627, Instrumentation in astronomy VI, ed. D. L. Crawford , 733, 10.1117/12.968154

    1986 doi

  103. [113]

    1993, in Astronomical Society of the Pacific Conference Series, Vol

    Tody , D. 1993, in Astronomical Society of the Pacific Conference Series, Vol. 52, Astronomical Data Analysis Software and Systems II, ed. R. J. Hanisch , R. J. V. Brissenden , & J. Barnes , 173

    1993

  104. [114]

    F., & Aller , H

    Torniainen , I., Tornikoski , M., Ter \"a sranta , H., Aller , M. F., & Aller , H. D. 2005, , 435, 839, 10.1051/0004-6361:20041886

    2005 doi

  105. [115]

    A., Rebolo , R., et al

    Tucci , M., Rubi \ n o-Martin , J. A., Rebolo , R., et al. 2008, , 386, 1729, 10.1111/j.1365-2966.2008.13161.x

    2008

  106. [116]

    M., & Padovani , P

    Urry , C. M., & Padovani , P. 1995, , 107, 803, 10.1086/133630

    1995 doi

  107. [117]

    1996, in Astronomical Society of the Pacific Conference Series, Vol

    van Moorsel , G., Kemball , A., & Greisen , E. 1996, in Astronomical Society of the Pacific Conference Series, Vol. 101, Astronomical Data Analysis Software and Systems V, ed. G. H. Jacoby & J. Barnes , 37

    1996

  108. [118]

    2011, , 417, L51, 10.1111/j.1745-3933.2011.01118.x

    van Velzen , S., K \"o rding , E., & Falcke , H. 2011, , 417, L51, 10.1111/j.1745-3933.2011.01118.x

    2011

  109. [119]

    2023, , 523, L30, 10.1093/mnrasl/slad051

    Wang , A., An , T., Guo , S., et al. 2023, , 523, L30, 10.1093/mnrasl/slad051

    2023 doi

  110. [120]

    2017, Frontiers in Astronomy and Space Sciences, 4, 38, 10.3389/fspas.2017.00038

    Wo owska , A., Kunert-Bajraszewska , M., Mooley , K., & Hallinan , G. 2017, Frontiers in Astronomy and Space Sciences, 4, 38, 10.3389/fspas.2017.00038

    2017

  111. [121]

    P., et al

    Wo owska , A., Kunert-Bajraszewska , M., Mooley , K. P., et al. 2021, , 914, 22, 10.3847/1538-4357/abe62d

    2021 doi

  112. [122]

    2022, , 938, 43, 10.3847/1538-4357/ac8a9a

    Zhang , F., Shu , X., Sun , L., et al. 2022, , 938, 43, 10.3847/1538-4357/ac8a9a

    2022 doi

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