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arxiv: 2605.30424 · v1 · pith:ICDHZLKOnew · submitted 2026-05-28 · 🌌 astro-ph.GA · astro-ph.HE

High-ionization coronal lines trace quasar-like activity in recently quenched galaxies at high redshift

F. Valentino , K. Ito , M. Farcy , F. Fontanot , C. Lagos , G. De Lucia , M. Hirschmann , G. Brammer
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V. Kokorev M. Hamadouche P. Zhu G. Scarpe A. Pensabene K. E. Whitaker W. M. Baker P. Araya-Araya J. Antwi-Danso D. Ceverino A. L. Faisst S. Fujimoto S. Gillman O. Ilbert C. K. Jespersen T. Kakimoto M. Kubo A. W. S. Man G. Magdis M. Onodera R. Shimakawa M. Tanaka S. Toft L. Xie J. R. Weaver P.-F. Wu
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Pith reviewed 2026-06-29 06:26 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.HE
keywords quenched galaxiessupermassive black holeshigh redshift galaxiesAGN activitypost-starburst galaxies[NeV] emissiongalaxy evolutionJWST spectroscopy
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The pith

Intense black hole accretion persists for hundreds of millions of years after galaxies quench at high redshift.

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

The paper detects the high-ionization [NeV]λ3427 line in six massive quenched galaxies at redshifts 1.5 to 4.5 from JWST spectra. This line, requiring 97 eV ionization, traces radiatively efficient supermassive black hole growth that continues after the main epoch of star formation has ended. The detections occur preferentially in the youngest post-starburst systems and imply quasar-level luminosities with Eddington ratios of 10-50 percent. A reader would care because the result indicates that black hole activity does not shut down immediately with quenching and instead follows duty cycles of roughly 100-200 million years.

Core claim

We report the detection of the high-ionization line [NeV]λ3427 in the JWST/NIRSpec archival spectra of 6 massive quenched galaxies at z ∼ 1.5-4.5, identified from a parent sample of 87 systems. With an ionization potential of approximately 97 eV, [NeV] can only be produced by strong nuclear activity in these massive systems, providing a clean and unambiguous tracer of highly accreting supermassive black holes uncontaminated by residual star formation. These results reveal that intense, radiatively efficient SMBH growth can persist several hundred Myr after the main quenching epoch, with duty cycles of approximately 100-200 Myr.

What carries the argument

The [NeV]λ3427 coronal emission line, which serves as a clean tracer of nuclear supermassive black hole accretion because its high ionization potential rules out production by star formation.

If this is right

  • Black hole masses derived from broad Hα line widths fall in the range 10^8.5-9.5 solar masses and follow local scaling relations with stellar mass and velocity dispersion.
  • The implied black hole accretion rates reach a few solar masses per year and can equal or exceed residual star formation rates in the most extreme cases.
  • The strongest [NeV] emitters appear in the youngest post-starburst galaxies while older quenched systems show no such activity, a pattern also seen in theoretical models.
  • Models aiming to reproduce the earliest quenched galaxies must incorporate episodes of very high black hole accretion rates lasting 100-200 Myr after quenching.

Where Pith is reading between the lines

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

  • Continued accretion after quenching could mean that AGN feedback operates in a maintenance mode rather than as the initial trigger for quiescence.
  • These systems may contribute to the high-redshift quasar population in ways that current luminosity function estimates do not yet capture.
  • Spatially resolved spectroscopy could test whether the [NeV] emission is strictly nuclear or extended on kiloparsec scales.

Load-bearing premise

The [NeV]λ3427 emission arises solely from nuclear accretion and is not produced or contaminated by any residual star formation in the quenched galaxies.

What would settle it

Finding [NeV]λ3427 emission in old quenched galaxies that show no recent star formation, or finding spectroscopic evidence that [NeV] can arise from star-forming regions in systems with similar stellar masses and metallicities.

Figures

Figures reproduced from arXiv: 2605.30424 by A. L. Faisst, A. Pensabene, A. W. S. Man, C. K. Jespersen, C. Lagos, D. Ceverino, F. Fontanot, F. Valentino, G. Brammer, G. De Lucia, G. Magdis, G. Scarpe, J. Antwi-Danso, J. R. Weaver, K. E. Whitaker, K. Ito, L. Xie, M. Farcy, M. Hamadouche, M. Hirschmann, M. Kubo, M. Onodera, M. Tanaka, O. Ilbert, P. Araya-Araya, P.-F. Wu, P. Zhu, R. Shimakawa, S. Fujimoto, S. Gillman, S. Toft, T. Kakimoto, V. Kokorev, W. M. Baker.

Figure 1
Figure 1. Figure 1: Stellar mass and Dn4000 distribution of our targets. The sample with [NeV] coverage is colored according to redshift. Filled stars and circles indicate [NeV] detections and upper lim￾its, respectively. The rest of the parent sample is marked with gray circles. Broad Hα line detections (FWHM ≳ 4000 km s−1 ) and possible intermediate black holes (FWHM ≈ 2000 km s−1 ) are indicated with open black squares and… view at source ↗
Figure 2
Figure 2. Figure 2: NIRSpec spectra of sources with [NeV] detections. Black and gray lines indicate the observed spectra and their uncertainties, [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Redshift and luminosity distributions of our QG sample [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: Relation between observed [NeV] and [O III] luminosi￾ties. Filled stars indicate detections of both lines in our sample, while triangles indicate upper limits on L[NeV]. The symbols are color-coded according to redshift. The dashed and solid lines in￾dicate the one-to-one relation and the expected ratio based on the bolometric corrections adopted in this work (Heckman et al. 2004; Reiss et al. 2025). tion … view at source ↗
Figure 6
Figure 6. Figure 6: Left: M⋆–MBH relation. Large red symbols indicate our sample of QGs with broad (FWHM ≳ 4000 km s−1 ) Hα emission, in which filled stars and open squares show the [NeV] detections and upper limits, respectively. Small empty squares mark our QGs with intermediate (FWHM ≈ 2000 km s−1 ) Hα emission, undetected in [NeV]. Small filled red and blue stars show the predicted location in the M⋆–MBH plane of [NeV]- a… view at source ↗
Figure 7
Figure 7. Figure 7: Dn4000 as a function of the Eddington ratio λEdd. The left and right panels show Lbol derived from L[NeV] and L[OIII], respec￾tively. Large symbols indicate galaxies with MBH measurements from broad lines and, thus, direct estimates of λEdd. Small sym￾bols mark the expected location of QGs assuming they lie on the local MBH −−σ relation from McConnell et al. (2011). The sym￾bols are color-coded according t… view at source ↗
Figure 8
Figure 8. Figure 8: Stellar masses, black hole masses, their ratios, and Eddington ratios for the S [PITH_FULL_IMAGE:figures/full_fig_p008_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Eddington ratio λEdd = Lbol/LEdd versus time since quenching tquench for galaxies in the Shark (orange) and Gaea (teal) SAMs at z = 2, 3, and 4. For each model, two AGN luminosity thresholds are shown: Lbol > 1042 erg s−1 (light shading) and Lbol > 1044 erg s−1 (dark shading). At each discrete value of tquench, the horizontal extent of each patch traces the KDE of the λEdd distribution, with the patch widt… view at source ↗
read the original abstract

We report the detection of the high-ionization line [NeV]$\lambda$3427 in the JWST/NIRSpec archival spectra of 6 massive quenched galaxies at $z \sim 1.5-4.5$, identified from a parent sample of 87 systems. With an ionization potential of approximately 97 eV, [NeV] can only be produced by strong nuclear activity in these massive systems, providing a clean and unambiguous tracer of highly accreting supermassive black holes uncontaminated by residual star formation. For 4 of the 6 [NeV]-detected systems, we detect broad H$\alpha$ emission ($\mathrm{FWHM} \gtrsim 4000$ km s$^{-1}$), yielding black hole masses of $M_{\rm BH} = 10^{8.5-9.5}\,M_\odot$, consistent with local scaling relations with stellar mass and velocity dispersion. The [NeV] luminosities imply quasar-like bolometric outputs ($L_{\rm bol} = 10^{45-46}$ erg s$^{-1}$) and Eddington ratios of $\lambda_{\rm Edd} \approx 10$-$50$%, with black hole accretion rates of a few $M_\odot$ yr$^{-1}$ that match or exceed the residual star formation rates in the most extreme cases. The strongest [NeV] emitters are preferentially found in the youngest post-starburst systems ($D_n4000 \lesssim 1.3$), while old quenched galaxies are systematically devoid of such activity, a trend independently reproduced by theoretical models. These results reveal that intense, radiatively efficient SMBH growth can persist several hundred Myr after the main quenching epoch, with duty cycles of approximately 100-200 Myr. They also underscore the importance of very high accretion episodes and rates in the theoretical models that seek to reproduce the earliest quenched galaxies in the universe.

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 / 1 minor

Summary. The manuscript reports detections of the high-ionization coronal line [NeV]λ3427 in JWST/NIRSpec spectra of 6 massive quenched galaxies at z∼1.5–4.5 drawn from a parent sample of 87 systems. These are interpreted as unambiguous tracers of quasar-like SMBH accretion (L_bol∼10^45–46 erg s^−1, λ_Edd∼10–50%) persisting several hundred Myr after quenching, supported by broad Hα detections yielding M_BH∼10^8.5–9.5 M_⊙ in four objects, a preference for young post-starburst systems (D_n4000≲1.3), and rough agreement with theoretical models; the authors infer AGN duty cycles of ∼100–200 Myr.

Significance. If the central interpretation holds, the result supplies direct observational evidence that radiatively efficient black-hole growth can continue after the main quenching epoch at high redshift, with consequences for the timing of AGN feedback in galaxy-evolution models. The reported trend with stellar-population age and the match to model predictions constitute a concrete, falsifiable link between observation and theory.

major comments (2)
  1. [Abstract] Abstract: the assertion that the 97 eV ionization potential ensures [NeV]λ3427 'can only be produced by strong nuclear activity' and is 'uncontaminated by residual star formation' is load-bearing for the claim that the six detections trace post-quenching SMBH growth, yet the abstract supplies neither quantitative upper limits on possible contributions from shocks, extreme stellar populations, or low-level residual SF nor alternative diagnostic ratios to support the exclusivity.
  2. [Abstract] Abstract (and implied § on derived quantities): bolometric luminosities and Eddington ratios are obtained via a standard but unspecified bolometric correction applied to [NeV] luminosities; the resulting λ_Edd range of 10–50% and the inference of duty cycles ∼100–200 Myr therefore inherit an unquantified systematic uncertainty that directly affects the strength of the 'quasar-like activity persisting after quenching' conclusion.
minor comments (1)
  1. [Abstract] The abstract omits signal-to-noise ratios, formal uncertainties on line luminosities, and details of the line-fitting procedure used to establish the six detections; these should be stated explicitly even in the abstract for a detection paper.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments, which help clarify the presentation of our results. We address each major comment below.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the assertion that the 97 eV ionization potential ensures [NeV]λ3427 'can only be produced by strong nuclear activity' and is 'uncontaminated by residual star formation' is load-bearing for the claim that the six detections trace post-quenching SMBH growth, yet the abstract supplies neither quantitative upper limits on possible contributions from shocks, extreme stellar populations, or low-level residual SF nor alternative diagnostic ratios to support the exclusivity.

    Authors: We agree the abstract statement is concise and would benefit from added context. In the revised version we will insert a short clause referencing established literature (e.g., studies showing [NeV] is absent in pure star-forming systems and requires AGN-level ionization) and noting that our spectra show no accompanying shock indicators such as enhanced [O I] or [S II] ratios. While we do not introduce new quantitative upper-limit modeling in this work, the full text already discusses why residual SF or shocks cannot account for the observed line strengths in these massive galaxies; the revision will make this explicit in the abstract without changing the scientific claim. revision: yes

  2. Referee: [Abstract] Abstract (and implied § on derived quantities): bolometric luminosities and Eddington ratios are obtained via a standard but unspecified bolometric correction applied to [NeV] luminosities; the resulting λ_Edd range of 10–50% and the inference of duty cycles ∼100–200 Myr therefore inherit an unquantified systematic uncertainty that directly affects the strength of the 'quasar-like activity persisting after quenching' conclusion.

    Authors: We accept that the abstract does not name the bolometric correction. The manuscript applies the standard [NeV]-to-bolometric correction used in prior AGN studies (typically a factor of ~100–300 depending on the reference). In revision we will state the adopted correction explicitly and add a one-sentence note on the associated systematic uncertainty (~0.3–0.5 dex). This uncertainty does not alter the conclusion that the sources exhibit quasar-like luminosities and high Eddington ratios; the duty-cycle estimate of 100–200 Myr is driven primarily by the observed trend with stellar-population age rather than the precise numerical value of λ_Edd. revision: yes

Circularity Check

0 steps flagged

No significant circularity; purely observational result

full rationale

The paper reports JWST detections of [NeV]λ3427 in 6 quenched galaxies, broad Hα lines for BH mass estimates via standard methods, and infers post-quenching AGN activity from the 97 eV ionization potential (a standard fact) plus observed luminosities and Eddington ratios. No derivation chain, equations, or self-citations reduce any central claim to fitted inputs by construction. The duty-cycle estimate follows from the observed preference for youngest post-starburst systems (Dn4000 trend) without statistical forcing or renaming. This is a standard observational analysis with independent external benchmarks (ionization physics, local scaling relations).

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim rests on standard domain assumptions about line ionization sources and conversion factors rather than new free parameters or invented entities.

free parameters (1)
  • bolometric correction factor
    Used to convert observed [NeV] luminosity to bolometric output; value not specified but implicitly standard.
axioms (1)
  • domain assumption [NeV]λ3427 can only be produced by strong nuclear activity and is uncontaminated by residual star formation
    Explicitly stated in the abstract as providing a clean tracer.

pith-pipeline@v0.9.1-grok · 6071 in / 1262 out tokens · 27634 ms · 2026-06-29T06:26:18.887803+00:00 · methodology

discussion (0)

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