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REVIEW 5 major objections 5 minor 1 cited by

Magnetic Field Structures In and Around Seyfert Galaxy Outflows

T0 review · 5 major / 5 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read This paper claims that kiloparsec-scale radio outflows in radio-quiet Seyfert and LINER galaxies are magnetic outflows whose power scales with black hole mass more than with Eddington ratio.

desk verdict The VLA polarization imaging is a genuine contribution; the MBH–jet-power correlation is a derived-quantity artifact that needs a robustness check before it carries the abstract's weight. read the letter →

arxiv 2501.08141 v1 pith:GATGPU7Y submitted 2025-01-14 astro-ph.GA

Salmoli Ghosh (NCRA-TIFR) , P. Kharb (NCRA-TIFR) , B. Sebastian (University of Manitoba , STScI) , J. Gallimore (Bucknell University) , A. Pasetto (IRyA-UNAM) , C. P. O'Dea (University of Manitoba) , T. Heckman (Johns Hopkins University)
show 1 more author
S. A. Baum (University of Manitoba)
This is my paper · ORCID
classification astro-ph.GA
keywords SeyfertgalaxiesLINERsradio-quietAGNkiloparsec-scaleoutflowsradiopolarimetrymagneticfieldstructurejetkineticpowerfeedback
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

This paper tries to establish that the kiloparsec-scale radio outflows seen in many radio-quiet Seyfert and LINER galaxies are magnetically driven AGN outflows, and that the power of those outflows is set primarily by the mass of the central black hole rather than by how fast the black hole is accreting. The evidence comes from new VLA polarimetric images of 12 such galaxies, which reveal organized magnetic fields in cores, jets, and lobes, with toroidal core fields suggesting a jet sheath or wind component around the jet. If the claim holds, radio-quiet AGN, which form the majority of active galaxies, can reshape their host environments in a way that depends mainly on black hole mass.

What carries the argument

The argument rests on two quantitative tools. First, VLA polarimetric imaging at 10 GHz (D-array) and 1.4 GHz (BnA to A array) yields electric vector position angle maps from which the projected magnetic field orientation is inferred, together with in-band spectral index maps obtained from multi-frequency synthesis. Second, jet kinetic and radiative powers are derived by inserting 10 GHz core peak flux densities into the Foschini (2014) and Merloni & Heinz (2007) core-luminosity to jet-power scaling relations, K-corrected to 15 or 5 GHz, and these jet powers are then tested against black hole mass and Eddington ratio using Kendall's tau and partial Spearman correlation tests. The toroidal core fields are interpreted through the expected distinction between toroidal fields in AGN winds and poloidal fields along jets.

What would settle it

Measure resolved lobe or cavity kinetic powers in a sample of radio-quiet Seyferts and LINERs using X-ray cavity or dynamical modeling, and check whether those powers still correlate with black hole mass when Eddington ratio is held fixed; alternatively, compare VLA 10 GHz core flux densities with simultaneous VLBI measurements at the frequencies used in the scaling relations to see whether diffuse VLA emission inflates the core luminosities that feed the jet power estimates.

Watch

Extended reading notes

Core claim

The paper's central claim is that Seyfert and LINER galaxies with kiloparsec-scale radio outflows are powered by magnetic fields anchored to the black hole and its accretion disk, and that these outflows significantly affect their surroundings. Concretely, it reports a strong partial correlation between jet kinetic power and supermassive black hole mass ($p = 0.0008$ with Eddington ratio held fixed), while correlations with Eddington ratio are weaker, and a marginal correlation between total equipartition energy and black hole mass. Polarization mapping shows ordered magnetic fields out to kiloparsec scales, fractional polarizations from a few per cent in cores up to $47 \pm 18$ per cent in lobes, and toroidal core fields in several sources, which the authors interpret as evidence for a jet sheath or wind component and for magnetically driven jet launching.

Load-bearing premise

The jet power numbers come from empirical scaling relations calibrated on radio-loud, beamed AGN, and the paper itself notes that none of these relations were built for low-luminosity radio-quiet Seyferts and LINERs; if those calibrations do not transfer, the headline jet power versus black hole mass correlation is not quantitatively valid.

Editorial extensions

If this is right

  • If jet kinetic power is governed mainly by black hole mass, models of galaxy evolution can assign feedback strengths to radio-quiet AGN from black hole mass rather than from accretion rate.
  • The toroidal core magnetic fields imply that jet launching in these systems includes a sheath or wind component, which future VLBI and X-ray observations could test as the decollimated base of the jet.
  • The positive and negative feedback signatures seen in sources such as NGC 3079 and NGC 4388 imply that radio-quiet outflows can deplete or ionize gas and also trigger star formation in their hosts.
  • The bimodality between core spectral index and Eddington ratio provides a radio observable for distinguishing an active-jet phase from a radiatively dominated accretion phase.
  • The strong correlation between total and polarized core intensity indicates that more ordered magnetic fields produce both brighter and more polarized radio cores in these AGN.

Reading between the lines

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

  • Editorial extension: the jet power versus black hole mass correlation may be partly a sample-selection effect, because galaxies were chosen for having kiloparsec-scale outflows and black hole mass tracks host galaxy properties; repeating the analysis on the full 26-source parent sample, including compact point sources, would test this.
  • Editorial extension: comparing VLA 10 GHz core flux densities with simultaneous VLBI measurements at 15 GHz would directly test whether the adopted scaling relations overestimate jet power when diffuse VLA emission is included in the core measurement.
  • Editorial extension: if the weak Eddington-ratio dependence survives a larger sample, it would imply that accretion state controls the launching geometry while black hole mass controls the overall power, which is testable by mapping polarization structure across AGN that change accretion state.
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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

5 major / 5 minor

Summary. This paper reports VLA 10 GHz D-array and 1.4 GHz BnA-to-A polarimetric observations of 12 Seyfert and LINER galaxies with kiloparsec-scale radio outflows from the CfA+12 micron sample. The authors derive in-band spectral index maps, polarization fractions, and magnetic field orientations; they estimate jet radiative and kinetic powers using empirical core-luminosity scaling relations, compute equipartition field strengths and total energies, and run correlation analyses of outflow properties against SMBH mass and Eddington ratio. The central claim is that radio outflow power correlates strongly with SMBH mass while accretion rate plays a secondary role, suggesting magnetically driven outflows from the black hole-accretion disk system.

Significance. The observational material is genuinely valuable: 10 GHz polarimetric imaging of 12 KSR Seyferts at about 7 arcseconds, including sources without prior polarization data, gives new constraints on B-field geometry in radio-quiet AGN outflows. The paper also ships a reproducible Python calibration pipeline and is transparent about the scaling relations' limitations and the small sample size. If the SMBH-outflow correlation were robust, it would support a mass-dependent magnetic launching mechanism and would matter for AGN feedback models. However, the quantitative correlation analysis is not currently sufficient to carry the physical conclusion; the derived jet powers carry +/-6 dex uncertainties, the scaling relations are calibrated on radio-loud/beamed sources, and the headline p-value comes from a partial correlation with a collinear control variable. The paper's own caveats (small sample; 'none of these relations were estimated for low-luminosity radio-quiet AGN') are appropriate but are in tension with the strength of the abstract claims.

major comments (5)
  1. [Section 4.2, Tables 4 and 6] The headline Pjet,kin-MBH correlation rests on point estimates whose quoted uncertainties (+/-6 dex in Table 4) far exceed the roughly 2 dex sample spread, so the rank-based p-values in Table 6 ignore a dominant error term and cannot establish the correlation. Moreover, because Eq. (3) is a deterministic increasing function of Lcore, the Kendall's tau test on Pjet,kin (p=0.0209) is essentially a restatement of the Lcore-MBH test (p=0.0311, Table 6); the much smaller partial Spearman p=0.0008 is obtained while controlling for lambda_Edd, which is strongly anti-correlated with MBH (p=0.0001), and is likely unstable. The authors should propagate the uncertainties, including the scatter in the Foschini and Merloni-Heinz relations, in a Monte Carlo analysis and should also report the correlation of the directly measured Lcore,10GHz with MBH.
  2. [Section 4.2, Eqs. (1)-(3)] The jet-power scaling relations were calibrated on radio-loud and often relativistically beamed AGN, as the authors acknowledge; the 10 GHz VLA D-array core peak flux is not the same observational quantity as the 15 GHz or 5 GHz core luminosities used to fit those relations. Since the authors state that none of these relations were estimated for low-luminosity radio-quiet AGN like Seyferts and LINERs, the absolute values of Pjet,kin and Pjet,rad in Table 4 are uncertain beyond the quoted random errors. The consistency check with the Willott et al. (1999) relation is only described qualitatively; the paper should present those alternative jet-power values and demonstrate that the MBH correlation survives, or it should refrain from quantitative jet-power versus MBH claims.
  3. [Section 4.4, Figure 18] The claimed bimodality in core spectral index versus Eddington ratio is obtained only after excluding NGC 4593, an exclusion that is disclosed in the text. With 11 points, Figure 18 can be read as a continuous trend rather than two separated groups. The authors should include NGC 4593 using its integrated spectral index of -0.48 (Rao et al. 2023) and test statistically whether a two-group model is preferred over a single trend. Without this, the abstract statement that radio cores with flatter spectra have lower Eddington ratios while steeper cores have higher overstates the current evidence.
  4. [Table 6] The table reports about 20 rank or partial correlations on a sample of 10-12 objects without any multiple-testing correction. With this many tests, p-values around 0.01-0.05 (e.g., fp,core-lambda_Edd p=0.0251, fp,extended-lambda_Edd p=0.0133, Etotal-MBH p=0.0210) are expected by chance. The authors should apply a false-discovery-rate control, for example the Benjamini-Hochberg procedure, or explicitly label these correlations as exploratory; the current presentation invites over-interpretation of borderline results in Sections 5.3 and 5.5.
  5. [Section 4.3, Table 5] The equipartition estimates of Bmin, Etotal, and tau depend on unconstrained assumptions: the ratio of ion to electron energy k, the filling factor phi, the frequency cutoffs nu_l and nu_u, the assumed source volume geometry, and the value of c12. The Etotal-MBH correlation (Table 6, p=0.021) is used to support the conclusion that outflow energy scales with black hole mass, but no sensitivity analysis is shown. The authors should demonstrate that this correlation persists under a plausible range of equipartition parameters before using it in the physical interpretation.
minor comments (5)
  1. [Section 1, first paragraph] The word 'Seyeferts' is a typo and should be 'Seyferts'.
  2. [Table 4] The column header uses 'W Hz^-1 sr^-1' while the table note uses 'erg s^-1 Hz^-1 Sr^-1'; these are dimensionally equivalent but the notation should be unified for clarity.
  3. [Table 3, NGC 1320 row] The notation '5 x 10^-3(5)' for the core polarized intensity is unclear; please specify the error convention explicitly (for example, 5 +/- 5 or a similar format).
  4. [Section 4.4 and Figure 17] The text says Figure 17 (left panel) demonstrates a significant correlation, but the p-values quoted in the text (p=0.019 for I_p,extended versus I_core) are inconsistent with the figure caption values (p=0.0041 for the left panel and p=0.0466 for the right panel); please align the wording and the values.
  5. [Section 4.4, Figure 18] The definitions of a flat core (alpha > -0.3) and a steep core (alpha < -0.3) are introduced without justification; please provide a reference for this threshold or show that the qualitative results are insensitive to its exact value.

Circularity Check

1 steps flagged · score 2.0 of 10

No self-citation circularity; one derived correlation relabels the core-luminosity–MBH correlation as a jet-power–MBH correlation.

  1. renaming known result [Section 4.2 (Eq. 3) and Section 4.4 / Table 6]
    "log Pjet,kin = (0.81 ± 0.11) logLcore,5GHz + 11.9+4.1−4.4 (3) ... we found a strong correlation (p = 0.0008 with partial SR test, see Table 6) between the jet kinetic power, derived using the method of Merloni & Heinz (2007), and black hole mass."

    The jet kinetic power used in the headline correlation is not measured independently; it is computed from the same 10 GHz core peak flux via Eq. 3. Table 6 reports both Lcore,10GHz–MBH (KT p=0.0311) and Pjet,kin–MBH (KT p=0.0209) from the same underlying core flux. Because Eq. 3 is a monotone function of Lcore (with only mild dependence on the core spectral index), the rank correlation between Pjet,kin and MBH is statistically inherited from the Lcore–MBH correlation. Presenting the Pjet,kin–MBH correlation as evidence that black-hole mass drives jet power is therefore a relabeling of the core-luminosity–MBH correlation rather than an independent confirmation from outflow energetics.

full rationale

The paper is primarily an observational study: it presents new VLA polarimetric images, derives B-field geometries, spectral indices, fractional polarizations, and equipartition energetics from the data. The central claim that radio outflow properties correlate with SMBH mass is partly supported by the Pjet,kin–MBH correlation, but Pjet,kin is obtained by inserting the measured 10 GHz core peak flux into the external Merloni & Heinz (2007) scaling relation (Eq. 3). The paper explicitly acknowledges that these scaling relations were not calibrated for low-luminosity radio-quiet AGN and that the jet powers could be overestimates. This is a correctness risk, not circularity, because the calibration is external and cross-checked against Willott et al. (1999) using 151 MHz lobe luminosities. The only mild circular step is that the Pjet,kin–MBH correlation is a monotone transform of the Lcore–MBH correlation already reported in Table 6, so it does not provide independent statistical evidence for a mass-driven jet-power relation. Other parts of the paper, such as the Etotal–MBH correlation from equipartition and the polarization/spectral-index results, are independent of this transform. Self-citations are present (e.g., Sebastian et al. 2020; Ghosh et al. 2023) but are contextual and not load-bearing for the main derivation. Overall, the paper is not significantly circular; the derived-correlation issue is a caveat rather than a collapse of the argument.

Assumptions & free parameters 6 free parameters · 5 assumptions · 0 invented entities

The paper introduces no new particles, forces, or physical entities. Its quantitative outputs rely on standard but tunable assumptions: equipartition parameters, assumed source volumes, chosen spectral index thresholds for bimodality, a modified radio loudness definition, and external jet power scaling relations not calibrated for the target population. These are the main degrees of freedom that determine the absolute jet powers, energies, and the claimed correlation strengths.

free parameters (6)
  • Equipartition assumption parameters (k, phi, nu_l, nu_u) = k=1, phi=1, 100 MHz to 15 GHz
    Section 4.3: assumed ion/electron energy ratio and filling factor unity, and frequency cutoffs 100 MHz and 15 GHz in equipartition estimates of Bmin, Etotal, and tau. These choices directly set the absolute B-field and energy scales.
  • Assumed source volume geometry = cylindrical or spherical
    Section 4.3: volumes chosen by morphology, affecting Bmin and Etotal estimates.
  • Flat/steep core spectral index threshold = alpha = -0.3
    Section 4.4 and Figure 18: sources with alpha greater than -0.3 are classified flat, lower values steep. Chosen by hand and drives the claimed bimodality.
  • Eddington ratio bimodality split = 2.5e-3
    Section 4.4 and Figure 18: vertical dashed line at the central value of lambda_Edd (minimum plus maximum divided by two). This choice affects the bimodality claim.
  • Radio loudness R definition = ratio of 8.4 GHz to [OIV] 25.89 micron flux density
    Section 2: adopted from Melendez et al. (2010), differing from the Kellermann definition, though the authors state it does not change the RL/RQ classification. The R versus MBH correlation depends on this definition.
  • Jet power scaling relations = Foschini (2014) and Merloni & Heinz (2007) coefficients
    Section 4.2, Equations 1 to 3: external empirical relations calibrated on radio-loud and relativistic jet sources, applied here to radio-quiet Seyferts and LINERs. The authors acknowledge that none of the relations were derived for these objects.
assumptions (5)
  • standard math Standard synchrotron radiation theory maps EVPA to B-field orientation: perpendicular for optically thin emission, parallel for optically thick cores with tau greater than about 6 and alpha greater than about 0.5.
    Section 3: used throughout to infer B-field geometries from polarization angle measurements.
  • domain assumption Equipartition between relativistic particles and magnetic fields holds in these sources.
    Section 4.3: used to estimate Bmin, Etotal, and tau; a standard but unverified assumption in radio astrophysics.
  • domain assumption The empirical Pjet versus core luminosity relations (Foschini 2014; Merloni and Heinz 2007; Willott et al. 1999) transfer to radio-quiet Seyferts and LINERs.
    Section 4.2, Equations 1 to 4. The authors explicitly note that none of these relations were derived for radio-quiet AGN. If this transfer fails, the Pjet,kin versus MBH correlation is compromised.
  • domain assumption Literature black hole masses and bolometric luminosities (mostly from Woo and Urry 2002, Dong and De Robertis 2006, and related references) are accurate enough for the correlation analyses.
    Section 4.4 and Table 1: the authors note systematic differences between mass estimates for type 1 and type 2 AGN, which could bias correlations.
  • domain assumption The kiloparsec-scale radio outflows are predominantly AGN-driven rather than starburst-driven.
    Section 5.2: the authors use the radio-FIR correlation and star formation rate estimates to argue AGN dominance, but this is a premise when interpreting B-fields as AGN outflow tracers.

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Cite this review

Pith. "Pith review of Magnetic Field Structures In and Around Seyfert Galaxy Outflows." pith.science (2026). https://pith.science/paper/GATGPU7Y

@misc{pith2026250108141,
  author       = {Pith},
  title        = {Pith review of: Magnetic Field Structures In and Around Seyfert Galaxy Outflows},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/GATGPU7Y}},
  note         = {Machine review of arXiv:2501.08141}
}
abstract

We present radio polarimetric images of 12 Seyfert and Low-Ionization Nuclear Emission-line Region (LINER) galaxies belonging to the Centre for Astrophysics (CfA)+12 micron sample exhibiting kiloparsec-scale radio outflows (KSRs). These observations have been carried out at 10 GHz with Karl G. Jansky Very Large Array (VLA) in D-array and at 1.4 GHz with the BnA$\rightarrow$A array configurations. We find signatures of organized magnetic (B-) field structures in the cores, jets and lobes of these galaxies. The linear polarization fraction varies from a few per cent in the cores to $47\pm18$ per cent in the lobes. The inferred B-fields are toroidal in the cores of several sources making them consistent with the presence of either a sheath-like or a wind-like component surrounding the jet. The in-band spectral index images typically show the presence of flat/inverted spectrum cores and steep spectrum lobes. Radio cores with flatter spectra are found to have lower Eddington ratios while the steeper ones have higher. A strong correlation is observed between the Seyfert/LINER radio outflow properties and the mass of the supermassive black holes (SMBHs); correlations with Eddington ratios are weaker. We find signatures of jet-medium interaction and both positive and negative AGN feedback in these sources. Overall, our study indicates that radio-quiet (RQ) AGN with KSRs possess radio outflows driven by magnetic fields anchored to their black holes - accretion disks, which significantly impact their environments.

Figures

Figures reproduced from arXiv: 2501.08141 by the authors.

Figure 1
Figure 1. Redshift distribution of the sample presented in this paper with their corresponding VLA NVSS 1.4 GHz radio luminosities. Each Seyfert and LINER galaxy has been assigned a coloured marker that is preserved in the subsequent plots. pendicular to the observed EVPAs (Pacholczyk 1970; Contopoulos et al. 2015). Conversely, in optically thick regions (with optical depth τ ≳ 6 and spectral index α ≳ 0.5), inferred B-field … view at source ↗
Figure 2
Figure 2. (Top left) NGC 1068 image at 1.52 GHz with the VLA BnA→A array at a resolution of ∼ 2 ′′. The contour levels in all the panels are at 3σ × (−1, 1, 2, 4, 8, 16, 32, 64, 128, 256, 512, 1024) with σ = 250 µJy beam−1 . Similarly, the synthesized beam size is 4.57′′ × 1.23′′ at a position angle (PA) of 63.8 ◦ . The tick lengths are proportional to fractional polarization with 5 arcsec = 15.6%. Radio emission is detected … view at source ↗
Figure 3
Figure 3. (Left) NGC 1320 image at 1.46 GHz with the VLA BnA→A array. For all the panels the contour levels are at 3σ × (−1, 1, 1.414, 2, 2.828, 4, 5.657, 8, 11.31, 16) with σ = 40 µJy beam−1 . Similarly, the synthesized beam size is 2.11′′ × 1.59′′ at a PA of −77.0 ◦ . The tick lengths are proportional to fractional polarization; 3′′ = 1%. Fractional polarization of errors > 35% have been blanked. (Right) The VLA in-band spe… view at source ↗
Figures from the paper (18 more)
Figure 4
Figure 4. Figure 4: (Left) NGC 2639 image at 10 GHz with the VLA D-array. For all the panels the contour levels are at 3σ × (−0.4, 1, 2, 4, 8, 16, 32, 64, 128, 256) with σ = 15 µJy beam−1 . Similarly, the synthesized beam size is 6.33′′ × 4.26′′ at a PA of 69.7 ◦ .The tick lengths are pro…
Figure 5
Figure 5. Figure 5: (Top left) Seyfert galaxy NGC 2992 image at 10 GHz with the VLA D array. For all the panels the contour levels are at 3σ × (−1, 1, 2, 4, 8, 16, 32, 64, 128, 256, 512) with σ = 12 µJy beam−1 . Similarly, the synthesized beam size is 8.81′′ × 4.71′′ at a PA of −6.5 ◦ . T…
Figure 6
Figure 6. Figure 6: (Top left) NGC 3079 image at 10 GHz with the VLA D-array. Galactic radio emission is detected along with the KSR in this galaxy. For all the panels the contour levels are at 3σ × (−1, 1, 2, 4, 8, 16, 32, 64, 128, 256, 512) with σ = 50 µJy beam−1 . Similarly, the synthe…
Figure 7
Figure 7. Figure 7: (Left) NGC 3516 at 10 GHz with the VLA D-array. For all the panels the contour levels are at 3σ × (−1, 1, 2, 4, 8, 16, 32, 64) with σ = 16 µJy beam−1 . The synthesized beam size is 7.38′′ × 4.71′′ at a PA of 26.29◦ . The tick lengths are proportional to fractional pola…
Figure 8
Figure 8. Figure 8: (Left) NGC 4051 image at 10 GHz with the VLA D array. For all the panels the contour levels are at 3σ × (−1, 1, 2, 4, 8, 16, 32, 64) with σ = 15 µJy beam−1 . Similarly, the synthesized beam size is 6.40′′ × 4.51′′ at a PA of 69◦ . The tick lengths are proportional to f…
Figure 9
Figure 9. Figure 9: (Top) NGC 4235 image at 10 GHz with the VLA D array. For all the panels the contour levels are at 3σ × (−1, 1, 2, 4, 8, 16, 32, 64, 128) with σ = 10 µJy beam−1 . Similarly, the synthesized beam size is 9.24′′ × 7.60′′ at a PA of −17.18◦ . The tick lengths are proportio…
Figure 10
Figure 10. Figure 10: (Top) NGC 4388 image at 10 GHz with the VLA D array. Galactic radio emission is detected along with the KSR in this galaxy. For all the panels the contour levels are at 3σ × (−1, 1, 2, 4, 8, 16, 32, 64, 128) with σ = 20 µJy beam−1 . Similarly, the synthesized beam siz…
Figure 11
Figure 11. Figure 11: (Top) NGC 4388 image at 5.3 GHz with the VLA D array. Galactic radio emission is detected along with the KSR in this galaxy. For all the panels the contour levels are at 3σ×(−1, 1, 2, 4, 8, 16, 32, 64, 128, 256) with σ = 17 µJy beam−1 . Similarly, the synthesized beam…
Figure 12
Figure 12. Figure 12: (Top) NGC 4593 image at 10 GHz with the VLA D array. For all the panels the contour levels are at 3σ × (−1, 1, 2, 4, 8, 16) with σ = 45 µJy beam−1 . Similarly, the synthesized beam size is 8.77′′ × 7.09′′ at a PA of 59.74◦ . The ticks are proportional to fractional po…
Figure 13
Figure 13. Figure 13: (Top) NGC 4594 image at 10 GHz with the VLA D array. Galactic radio emission is detected along with the KSR in this galaxy. For all the panels the contour levels are at 3σ × (−1, 1, 2, 4, 8, 16, 32, 64, 128, 256, 512) with σ = 22 µJy beam−1 . Similarly, the synthesize…
Figure 14
Figure 14. Figure 14: (Left) NGC 5506 image at 10 GHz with the VLA D array. For all the panels the contour levels are at 3σ × (−1, 1, 2, 4, 8, 16, 32, 64, 128, 256, 512, 1024, 2048) with σ = 9 µJy beam−1 . Similarly, the synthesized beam size is 7.25′′ × 5.42′′ at a PA of −31.47◦ . The tic…
Figure 15
Figure 15. Figure 15: Radio loudness parameter versus black hole masses for 11 out of 12 sources in the selected sample. We did not have a proper estimate of radio loudness for NGC 4594 due to large uncertainties in the [OIV]λ25.89 µm line luminosity and has thus been excluded. A strong co…
Figure 16
Figure 16. Figure 16: (Left) Total luminosity versus core luminosity at 10 GHz. The black dashed line indicates the slope equal to unity. (Right) Core luminosity at 10 GHz versus black hole mass. A marginal correlation is observed with KT test p = 0.0311. Error bars are noted along with th…
Figure 17
Figure 17. Figure 17: (Left) Logarithm of polarized flux density versus logarithm of total flux density in the core at 10 GHz. The errors on log10y-value have been calculated as (errors on y-value)/(y-value× loge10) using error propagation methods. The generalized KT test indicates a signi…
Figure 18
Figure 18. Figure 18: In-band core spectral indices versus the Eddington ratios. The horizontal black dashed line indicates a spectral index of −0.3. The vertical dashed line indicates the central value ([minimum+maximum]/2)of λEdd. Values greater than α = −0.3 are considered flat while lo…
Figure 19
Figure 19. Figure 19: (Left) Total energy (particle + fields) versus the black hole mass in log-log scale. The KT test indicates a marginal correlation (p = 0.0210). A linear regression model has been fit here to obtain the best-fit line shown in black. The 1σ, 3σ and 5σ standard deviation…
Figure 20
Figure 20. Figure 20: (Top left) Log-log plot of the core polarized flux density versus the Eddington ratios. The generalized KT test indicates a strong correlation (p = 0.0072). A linear regression model has been fit here to obtain the best-fit line shown in black. The 1σ and 3σ deviation…
Figure 21
Figure 21. Figure 21 [PITH_FULL_IMAGE:figures/full_fig_p036_21.png]

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Cited by 1 Pith paper

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