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arxiv: 2606.04090 · v1 · pith:R3M6RK3Vnew · submitted 2026-06-02 · 🌌 astro-ph.GA

Mapping the nuclear environments of extreme coronal line emitting galaxies

Daniel Kynoch , Or Graur , Peter Clark , J.N. Aguilar , S. Ahlen , D. Bianchi , D. Brooks , T. Claybaugh
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A. de la Macorra P. Doel J.E. Forero-Romero S. Gontcho A Gontcho G. Gutierrez R. Joyce S. Juneau M. Landriau L. Le Guillou A. Meisner R. Miquel J. Moustakas S. Panda W.J. Percival F. Prada I. P\'erez-R\`afols G. Rossi E. Sanchez D. Schlegel J. Silber D. Sprayberry G. Tarl\'e B.A. Weaver R. Zhou H. Zou
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Pith reviewed 2026-06-28 09:05 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords extreme coronal line emittersblack hole massphotoionisationemission line profilestidal disruption eventsvirial motionionisation stratificationnarrow line region
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The pith

Gas distances in extreme coronal line galaxies correlate with black hole mass following a square-root dependence.

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

The paper compiles optical spectra of 33 extreme coronal line emitting galaxies, separating variable sources linked to tidal disruption events from non-variable AGN-linked systems. Using multi-epoch data, it measures emission line profiles and converts line widths to radial distances under the assumption of virial motion. This yields positive correlations between distance and black hole mass for both [O III] and [Fe VII], with slopes of 0.63 and 0.69 that align with a Mass to the power of 0.5 scaling, pointing to photoionisation as the main determinant of characteristic radii. The work also maps an ionisation stratification in which coronal lines arise at distances between the broad and narrow line regions, appearing similarly in both variable and non-variable objects.

Core claim

We find positive correlations between gas distance and black hole mass for both [O III] and [Fe VII]: the log(Distance)-log(Mass) relations have slopes 0.63±0.08 and 0.69±0.12, respectively, broadly consistent with a Mass^{0.5} dependence and with characteristic radii set primarily by photoionisation.

What carries the argument

Virial-motion assumption that converts measured emission-line widths into characteristic radial distances of the line-emitting gas.

If this is right

  • Coronal lines are emitted at radii intermediate between the broad line region and the low-ionisation narrow line region.
  • Ionisation stratification appears with similar incidence in both variable TDE-linked and non-variable AGN-linked ECLEs.
  • Characteristic radii are set primarily by photoionisation rather than dynamical or other effects.
  • Highest-ionisation lines fade first in variable sources, followed by [Fe VII] and brightening of [O III].

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The lack of difference in gas distributions between active and quiescent nuclei suggests that a recent TDE does not rearrange the circumnuclear material on observable scales.
  • If the mass-distance relation holds, it could be used to estimate black hole masses from single-epoch spectra of other high-ionisation sources.
  • Future monitoring of more ECLEs would test whether the observed stratification evolves differently in TDE versus steady AGN environments.

Load-bearing premise

The gas motions must be virial so that line widths can be converted directly into radial distances.

What would settle it

Finding no correlation, or slopes far from 0.5, between line-emitting gas distance and black hole mass in a larger sample of ECLEs would falsify the claimed scaling.

Figures

Figures reproduced from arXiv: 2606.04090 by A. de la Macorra, A. Meisner, B.A. Weaver, Daniel Kynoch, D. Bianchi, D. Brooks, D. Schlegel, D. Sprayberry, E. Sanchez, F. Prada, G. Gutierrez, G. Rossi, G. Tarl\'e, H. Zou, I. P\'erez-R\`afols, J.E. Forero-Romero, J. Moustakas, J.N. Aguilar, J. Silber, L. Le Guillou, M. Landriau, Or Graur, P. Doel, Peter Clark, R. Joyce, R. Miquel, R. Zhou, S. Ahlen, S. Gontcho A Gontcho, S. Juneau, S. Panda, T. Claybaugh, W.J. Percival.

Figure 1
Figure 1. Figure 1: Optical spectra of SDSS J0748. The upper panel shows the full spectra plotted as a function of rest-frame wavelength. Key emission lines are indicated with vertical lines: H α 𝜆6565 and H β 𝜆4863 (dotted green lines); [O iii] 𝜆𝜆4960, 5007, [N ii] 𝜆𝜆6549, 6585, and [S ii] 𝜆𝜆6718, 6732 (red dot-dashed lines); and [Fe x] 𝜆6374 and [Fe xi] 𝜆7891 (magenta solid lines). The lower panels show cut-outs of key emis… view at source ↗
Figure 2
Figure 2. Figure 2: DESI spectra of the ECLEs in our sample. The left-hand panel shows the spectra of the v-ECLEs (cyan) and the CL-TDEs (purple); the right-hand plot shows the spectra of the nv-ECLEs (grey). The spectra have been smoothed for clarity. The locations of key emission lines are indicated by vertical dotted and dashed lines for the coronal and low-ionisation lines, respectively. follow-up spectrum, taken nearly 8… view at source ↗
Figure 3
Figure 3. Figure 3: Emission line maps for v-ECLEs. We show the FWHM-inferred distances of emission line gas versus ionisation potential for each emission line. Transitions are ordered by increasing ionisation potential along the x-axis. Permitted transitions are coloured grey, low-ionisation forbidden lines purple, and coronal lines cyan. Where multiple epochs are available, measurements are grouped by line and plotted left … view at source ↗
Figure 3
Figure 3. Figure 3: Emission line maps for v-ECLEs (continued). we are still able to measure the width of broad H α. Consistent with the analysis performed by Wang et al. (2024), we observe a broad component to H α that decreases in both flux and width as time progresses. Its width in the earliest spectrum is 3671 ± 359 km s−1 and in the latest is just 1784 ± 72 km s−1 . The luminosity of this component peaks at log(𝐿) = 41.0… view at source ↗
Figure 4
Figure 4. Figure 4: Emission line maps for CL-TDEs. We show the FWHM-inferred distances of emission line gas versus ionisation potential for each emission line. Transitions are ordered by increasing ionisation potential along the x-axis. Permitted transitions are coloured grey, low-ionisation forbidden lines purple, and coronal lines cyan. Where multiple epochs are available, measurements are grouped by line and plotted left … view at source ↗
Figure 4
Figure 4. Figure 4: Emission line maps for CL-TDEs (continued). is only obtained from the MMT spectrum. There is little evolution of the source across the three epochs. The low-ionisation lines and [Fe vii] coronal lines appear narrower in the later spectra, whereas [Fe x] 𝜆6374 and [Fe xi] 𝜆7891 have consistent widths between SDSS and DESI. Similar to many other ECLEs, the emission line gas is stratified, with coronal lines … view at source ↗
Figure 5
Figure 5. Figure 5: Emission line maps for nv-ECLEs. We show the FWHM-inferred distances of emission line gas versus ionisation potential for each emission line. Transitions are ordered by increasing ionisation potential along the x-axis. Permitted transitions are coloured grey, low-ionisation forbidden lines purple, and coronal lines cyan. Where multiple epochs are available, measurements are grouped by line and plotted left… view at source ↗
Figure 5
Figure 5. Figure 5: Emission line maps for nv-ECLEs (continued). and BH mass. Performing a simple, unweighted, linear regression of the form log(𝑅vir/pc) = 𝛼 log(𝑀BH/M⊙) + 𝛽, we find slopes 𝛼[Oiii] = 0.63 ± 0.08 and 𝛼[Fevii] = 0.71 ± 0.12. Since the measure￾ment uncertainties on the virial radii are small compared to the scatter in the relation, the simple regression yields a chi-squared per degree of freedom of 𝜒 2 𝜈 ∼ 100-2… view at source ↗
Figure 5
Figure 5. Figure 5: Emission line maps for nv-ECLEs (continued). at ≳ 5𝜎, confirming that the distance–mass correlation is statistically significant for both emission lines. In the right-hand panel of [PITH_FULL_IMAGE:figures/full_fig_p025_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Representative emission line gas distances, inferred from the FWHM of [O iii] 𝜆5007 (purple) and an [Fe vii] coronal line (cyan) for sources in our sample. On the left we show the absolute distances in pc and on the right mass-scaled distances in gravitational radii. The different source classifications are represented by different markers, as indicated in the legend. Best-fitting linear relations between … view at source ↗
read the original abstract

Extreme coronal line emitters (ECLEs) are a rare class of galactic nuclei exhibiting unusually strong high-ionisation forbidden emission lines, and several ECLEs have been linked to tidal disruption events (TDEs). In this work, we compile and analyse optical spectra of 33 ECLEs, dividing them into variable, TDE-linked sources and non-variable, AGN-linked systems. Using multi-epoch spectroscopy from the Sloan Digital Sky Survey, Dark Energy Spectroscopic Instrument, and other facilities, we investigate the evolution of the emission line spectra and measure emission line profiles. Many variable ECLEs have changing spectra in which the highest-ionisation lines (e.g., [Fe X]-[Fe XIV]) appear and fade first, followed by [Fe VII], accompanied by brightening of [O III]. These changes may reflect a softening ionising continuum, the outward propagation of the ionisation front following the TDE flare, or both. Assuming virial motion, we translate line widths into characteristic radial distances, reconstructing the spatial distribution of line-emitting gas. Coronal lines are generally emitted at radii intermediate between the broad line region and the low-ionisation narrow line region. This ionisation stratification is seen in many sources, with similar incidence in variable and non-variable ECLEs, suggesting no apparent difference in circumnuclear gas distributions between active and quiescent nuclei. We find positive correlations between gas distance and black hole mass for both [O III] and [Fe VII]: the log(Distance)-log(Mass) relations have slopes $0.63\pm0.08$ and $0.69\pm0.12$, respectively, broadly consistent with a Mass$^{0.5}$ dependence and with characteristic radii set primarily by photoionisation.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript compiles and analyzes optical spectra of 33 extreme coronal line emitters (ECLEs), separating variable TDE-linked sources from non-variable AGN-linked systems. It examines multi-epoch spectral evolution of high-ionization lines, measures emission-line profiles, derives characteristic radial distances for the emitting gas by assuming virial motion from observed line widths, and reports positive correlations between these distances and black-hole mass with fitted slopes of 0.63±0.08 ([O III]) and 0.69±0.12 ([Fe VII]), interpreted as consistent with a photoionization origin and M^{0.5} scaling.

Significance. If the derived distances prove reliable, the results would map ionization stratification in ECLE nuclei, demonstrate that coronal lines arise at radii intermediate between the BLR and NLR, and provide empirical support for photoionization setting characteristic radii in both TDE and AGN environments.

major comments (2)
  1. [distance derivation and correlation analysis] The central Distance–Mass correlations (Abstract and the section on reconstruction of spatial distribution) are obtained by converting measured line widths directly into radii via the virial relation R = f G M_BH / v². No cross-check against reverberation-mapping lags, resolved imaging, or kinematic modeling that could test the pure-gravitational assumption is presented; coronal-line kinematics in other AGN samples often show non-virial contributions, which would render the reported slopes (0.63±0.08 and 0.69±0.12) and the claimed consistency with M^{0.5} photoionization scaling dependent on an unverified premise.
  2. [results on stratification and correlations] The sample is divided into variable and non-variable ECLEs, yet the incidence of ionization stratification is stated to be similar in both subsets. The manuscript does not quantify how the virial-derived radii for the two subsets separately affect the overall log D–log M fits or whether the slope uncertainties incorporate possible systematic differences in line-profile measurement between the subsets.
minor comments (2)
  1. [Abstract] The abstract states the slopes are “broadly consistent with a Mass^{0.5} dependence” but does not show the formal statistical test or the exact functional form assumed for the comparison.
  2. [methods] Notation for the geometric factor f in the virial relation is introduced without a table of adopted values or discussion of its range across sources.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thoughtful comments on our manuscript. We respond point-by-point to the major comments below, acknowledging limitations where appropriate and outlining planned revisions.

read point-by-point responses

  1. Referee: The central Distance–Mass correlations (Abstract and the section on reconstruction of spatial distribution) are obtained by converting measured line widths directly into radii via the virial relation R = f G M_BH / v². No cross-check against reverberation-mapping lags, resolved imaging, or kinematic modeling that could test the pure-gravitational assumption is presented; coronal-line kinematics in other AGN samples often show non-virial contributions, which would render the reported slopes (0.63±0.08 and 0.69±0.12) and the claimed consistency with M^{0.5} photoionization scaling dependent on an unverified premise.

    Authors: We agree that the virial assumption is fundamental to our distance estimates and that no direct cross-checks (e.g., reverberation mapping or resolved imaging) are presented, as such data are unavailable for this rare sample of ECLEs. This method follows standard practice in AGN emission-line studies where independent radius measurements are lacking. We will revise the manuscript to include an expanded discussion of possible non-virial contributions to coronal-line widths, citing relevant AGN literature, and will qualify the interpretation of the slopes as indirect support for photoionization rather than definitive proof. The observed slopes near 0.5 remain consistent with the expected scaling under the assumption, but we acknowledge the premise is unverified. revision: partial

  2. Referee: The sample is divided into variable and non-variable ECLEs, yet the incidence of ionization stratification is stated to be similar in both subsets. The manuscript does not quantify how the virial-derived radii for the two subsets separately affect the overall log D–log M fits or whether the slope uncertainties incorporate possible systematic differences in line-profile measurement between the subsets.

    Authors: We will add a quantitative analysis separating the variable (TDE-linked) and non-variable (AGN-linked) subsets, including separate log(D)–log(M) fits for each to show their individual slopes, contributions to the combined relation, and any differences. This will also address potential systematic differences in line-profile measurements between subsets and clarify how they impact the reported uncertainties. The statement on similar incidence of stratification was qualitative; the new analysis will provide the requested quantification. revision: yes

Circularity Check

0 steps flagged

No significant circularity; distances from standard virial method yield empirical correlations

full rationale

The paper derives characteristic gas radii from measured line widths via the standard virial relation R = f G M_BH / v^2 (abstract and methods). The reported log(Distance)-log(Mass) slopes of 0.63±0.08 and 0.69±0.12 are direct empirical fits to these independently measured quantities. The slopes are not forced by construction, as they depend on the observed velocity dispersions; a slope near 0.5 emerges only if the data exhibit a specific v-M relation, which is not assumed. No self-citations, uniqueness theorems, or ansatzes from prior author work are invoked as load-bearing steps. The central claims rest on external benchmarks (standard AGN virial methods and photoionization scaling) rather than reducing to the paper's own inputs.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Analysis rests on the standard virial assumption for radius estimation and implicit photoionization equilibrium; no new entities or ad-hoc parameters beyond the reported empirical fits.

axioms (1)
  • domain assumption Virial motion of line-emitting gas allows line widths to be converted to characteristic radii
    Explicitly stated when reconstructing spatial distribution from emission line profiles.

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