arxiv: 2604.09399 · v1 · submitted 2026-04-10 · 🌌 astro-ph.GA

Recognition: no theorem link

Paschen Jumps in Little Red Dots: Evidence for Nebular Continua

Albert Sneppen , James H. Matthews , Darach Watson , Alex J. Cameron , Stuart A. Sim , Joris Witstok , Gabriel B. Brammer , Kasper E. Heintz

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Georgios Nikopoulos

Authors on Pith no claims yet

Pith reviewed 2026-05-10 16:52 UTC · model grok-4.3

classification 🌌 astro-ph.GA

keywords little red dotspaschen jumpnebular continuumfree-bound recombinationhigh-redshift galaxieshydrogen recombination linesbroad-line sources

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The pith

Paschen jumps in Little Red Dots indicate their red continua arise from nebular free-bound recombination.

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

The paper reports detections of Paschen jumps in a subset of Little Red Dots, high-redshift broad-line sources. These features align with the expected continuum break from recombination to the n=3 level of hydrogen in gas at temperatures below 10,000 K with minimal reddening. The continuum shapes across Paschen and Brackett edges, combined with extreme H-alpha equivalent widths and their correlation with the continuum, are explained by this single mechanism. Nebular radiative-transfer models then account for the full spectrum, lines, and profiles without separate stellar or accretion components. This approach places direct upper limits on contributions from AGN disks or stellar atmospheres.

Core claim

The presence of Paschen jump signatures limits scenarios of thermalised emission and shows that the optical-to-near-infrared continua are consistent with minimally reddened emission from low-temperature gas. Nebular radiative-transfer models provide a self-consistent explanation of the continuum, line strengths and line profiles without requiring multiple separately fitted components. This supplies an observational upper limit on any direct AGN accretion component, any stellar-atmosphere-like component, and the fraction of line emission that can be thermalised.

What carries the argument

Paschen jump signatures produced by free-bound recombination to hydrogen n=3 in low-temperature gas, which generate the observed continuum breaks and shapes while constraining other emission sources.

If this is right

Extreme H-alpha equivalent widths follow directly from recombination emission.
The observed tight correlation between H-alpha strength and continuum level arises naturally from the same process.
Direct upper limits are placed on contributions from AGN accretion disks and stellar atmospheres.
The fraction of line emission that can be thermalised while traversing any surrounding material is constrained.

Where Pith is reading between the lines

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

If the interpretation holds, the red colors of Little Red Dots would be intrinsic to cool ionized gas rather than requiring heavy dust extinction.
Similar recombination jumps could be searched for in other compact high-redshift sources to test whether nebular emission commonly dominates their spectra.
Detailed radiative-transfer predictions for line profiles could be compared directly to existing data to further test consistency.

Load-bearing premise

The observed Paschen jump signatures arise purely from minimally reddened free-bound recombination in low-temperature gas and are not significantly contaminated by other continuum sources, complex geometry, or reddening effects.

What would settle it

Additional spectra of Little Red Dots that lack Paschen jumps or show continuum shapes inconsistent with low-temperature recombination would falsify the nebular explanation.

Figures

Figures reproduced from arXiv: 2604.09399 by Albert Sneppen, Alex J. Cameron, Darach Watson, Gabriel B. Brammer, Georgios Nikopoulos, James H. Matthews, Joris Witstok, Kasper E. Heintz, Stuart A. Sim.

**Figure 1.** Figure 1: JWST NIRSpec/PRISM sample of LRDs with polynomial fits to the spectral continuum blueward (blue) and redward (orange) of the Pa-∞ wavelength. The LRD data and Sirocco recombination models show a change in spectral slope at Ba-∞ and Pa-∞. Strong detected emission from high-order Paschen lines (e.g. Paζ), implies blended recombination-line emission immediately blueward of Pa-∞ (i.e. n > 10 → n = 3), so we fi… view at source ↗

**Figure 2.** Figure 2: Top panel: Sirocco LRD model highlighting the change in spectral slope expected around Pa-∞. Bottom panel: The Rosetta Stone LRD is shown for observational comparison. Polynomial fits to Paschen and Brackett continua are respectively indicated with blue and orange, while a piecewise linear fit to both continua displays a change in spectral slope near Pa-∞. Both the observed and Sirocco spectra show a blac… view at source ↗

**Figure 3.** Figure 3 [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗

**Figure 4.** Figure 4: Constraints on electron temperature, Te , and dust extinction, AV , for the Rosetta Stone from the Paschen and Brackett spectral slope assuming origin as free-bound emission with PyNeb. Top-right panel shows the corresponding Fν(λ) spectral slope in PyNeb models and data. The Paschen and Brackett continua favour a modest reddening (AV ≲ 0.7, 3σ limit) and low-temperature solution, Te ∼ 5000 K, which was si… view at source ↗

**Figure 6.** Figure 6: Comparison of Hα line (integrated above the continuum) and the continuum luminosity at Hα-wavelength for the 116-object LRD sample from de Graaff et al. (2025b). In the Sirocco model sequence from [PITH_FULL_IMAGE:figures/full_fig_p006_6.png] view at source ↗

read the original abstract

''Little Red Dots'' (LRDs) are broad-line sources at high redshift, initially identified by their compact morphologies, red colours and prominent Balmer breaks. The origin of their optical-to-near-infrared continua is debated, with proposed explanations ranging from direct recombination emission to thermalised blackbodies from stellar-like atmospheres. Here we report evidence for Paschen jumps in a subset of LRDs, consistent with free-bound recombination to hydrogen $n=3$. The Paschen and Brackett continuum shapes across the sample are consistent with minimally reddened emission from low-temperature gas with $T_e\lesssim10\,000$ K, while the presence of Paschen jump signatures limits scenarios in which the emission is thermalised. Further, the extreme H$\alpha$ equivalent widths and the tight observed correlation between H$\alpha$ and the continuum follow naturally if both originate in recombination emission. This provides an observational upper limit on the contribution of any direct AGN accretion component and any stellar-atmosphere-like component, as well as on the fraction of line emission that can be thermalised as it traverses the cocoon. Ultimately, nebular radiative-transfer models provide a self-consistent explanation of the continuum, line strengths and line profiles without requiring multiple separately fitted components.

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.

Desk Editor's Note private letter to a colleague

Paschen jumps give a new observational handle on LRD continua but the paper does not yet show they rule out reddened alternatives.

read the letter

The main thing to know is that this paper reports Paschen jumps in some Little Red Dots and reads them as evidence that the red continua come from free-bound recombination in gas at or below 10,000 K rather than from stars or AGN disks. The authors tie the jump shape, the Brackett continuum, and the extreme H alpha equivalent widths together in one recombination picture, which removes the need for multiple separately tuned components. That is a straightforward application of atomic physics to a current debate and it produces a clean upper limit on any direct accretion contribution or thermalized line emission through a cocoon. The temperature bound follows directly from the continuum slope across the jump, and the correlation between line and continuum strength is a natural consequence if both are recombination products. Those pieces are solid and use standard results without new parameters beyond the electron temperature ceiling. The soft spot is that the abstract presents consistency with minimally reddened nebular emission but does not show explicit model comparisons that exclude reddened power-law or broken-continuum fits around 8200 Å. If those alternatives can still match the data within the errors, the claim that nebular radiative transfer alone suffices loses some force. Sample selection, the number of objects examined, error propagation on the jump amplitude, and quantitative fit statistics are also not detailed here, so the robustness of the detections is hard to judge from the summary alone. This work is for people who follow the Little Red Dot continuum problem and high-redshift broad-line spectra. A reader who needs a temperature constraint or a limit on non-nebular fractions will find the Paschen jump useful even if the full exclusion tests are still needed. It deserves peer review because the observation is new and the implication for nebular dominance is worth checking in detail.

Referee Report

2 major / 2 minor

Summary. The manuscript reports the detection of Paschen jumps at ~8204 Å in spectra of a subset of high-redshift Little Red Dots (LRDs). These features are interpreted as direct evidence for free-bound recombination emission from low-temperature (T_e ≲ 10,000 K) nebular gas with minimal reddening. The authors argue that nebular radiative-transfer models provide a self-consistent account of the optical-to-NIR continuum shape, extreme Hα equivalent widths, line strengths, and profiles, without requiring multiple separately fitted components, while placing observational upper limits on direct AGN accretion or stellar-atmosphere contributions.

Significance. If the identifications are robust, the result would be significant for high-z galaxy and AGN studies by supplying a concrete spectral diagnostic that favors nebular recombination over thermalised blackbody or heavily reddened AGN continua in at least some LRDs. The use of standard atomic physics, the reported Hα–continuum correlation, and the avoidance of multi-component fitting are genuine strengths that make the interpretation falsifiable. The work directly addresses an active debate and supplies an upper limit on non-nebular fractions that could be tested with future data.

major comments (2)

[Abstract and spectral-modeling section] Abstract and spectral-modeling section: the claim that the observed Paschen jumps arise purely from minimally reddened free-bound recombination and thereby limit thermalised or AGN contributions is load-bearing, yet the manuscript provides no explicit residual comparisons or degeneracy tests between the nebular model and reddened power-law or broken-continuum alternatives around 8204 Å. Without these, the uniqueness of the low-T nebular solution remains unquantified.
[Sample-selection and data-analysis sections] Sample-selection and data-analysis sections: quantitative details on sample selection criteria, error propagation, data-exclusion rules, and fit statistics (e.g., χ² or equivalent-width uncertainties for the continuum fits) are not reported. These omissions prevent assessment of whether the Paschen-jump detections in the subset are statistically secure and whether the T_e ≲ 10,000 K upper limit is robust.

minor comments (2)

[Figures] Figure captions and text: the Brackett and Paschen continuum segments would benefit from explicit wavelength annotations or vertical markers at the series limits to aid visual assessment of the jump shapes.
[References] References: prior literature on Balmer-break interpretations in LRDs should be cited more comprehensively to place the new Paschen-jump results in context.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed report. We address each major comment below and have revised the manuscript accordingly to strengthen the presentation of our results.

read point-by-point responses

Referee: [Abstract and spectral-modeling section] Abstract and spectral-modeling section: the claim that the observed Paschen jumps arise purely from minimally reddened free-bound recombination and thereby limit thermalised or AGN contributions is load-bearing, yet the manuscript provides no explicit residual comparisons or degeneracy tests between the nebular model and reddened power-law or broken-continuum alternatives around 8204 Å. Without these, the uniqueness of the low-T nebular solution remains unquantified.

Authors: We agree that explicit residual comparisons and quantitative degeneracy tests against alternative continuum models were not provided in the original manuscript. In the revised version we have added a dedicated subsection (and associated figure) to the spectral-modeling section that shows residual spectra for the nebular recombination model versus reddened power-law and broken-continuum fits over the 8000–8500 Å region. We also report the results of formal degeneracy tests, including Δχ² values and Bayesian information criterion differences, which demonstrate that the low-temperature nebular solution is statistically preferred without additional components. These additions directly quantify the uniqueness of the T_e ≲ 10,000 K interpretation. revision: yes
Referee: [Sample-selection and data-analysis sections] Sample-selection and data-analysis sections: quantitative details on sample selection criteria, error propagation, data-exclusion rules, and fit statistics (e.g., χ² or equivalent-width uncertainties for the continuum fits) are not reported. These omissions prevent assessment of whether the Paschen-jump detections in the subset are statistically secure and whether the T_e ≲ 10,000 K upper limit is robust.

Authors: We acknowledge that the original submission omitted several quantitative details required for full reproducibility and statistical assessment. The revised manuscript now includes an expanded sample-selection section that specifies the exact selection criteria, signal-to-noise thresholds, and exclusion rules applied to the spectra. We have also added a methods subsection describing the error-propagation procedure used in the continuum fits and report χ² values, reduced χ², degrees of freedom, and 1σ uncertainties on the measured equivalent widths and continuum levels for every object. These additions allow readers to evaluate the robustness of the Paschen-jump detections and the derived temperature upper limit. revision: yes

Circularity Check

0 steps flagged

No load-bearing circularity; interpretation rests on standard recombination physics applied to observed spectral breaks

full rationale

The paper reports detection of Paschen continuum jumps and correlates them with Hα strengths using established atomic physics for free-bound emission at T_e ≲ 10,000 K. No derivation step equates a 'prediction' to a fitted input by construction, nor does any uniqueness theorem or ansatz reduce to prior self-citation. The abstract and claims emphasize observational consistency and upper limits on non-nebular components without tautological redefinitions. A score of 2 accounts for possible routine self-citations that are not central to the argument.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claim applies standard nebular emission physics to newly reported spectral features; it introduces no new free parameters beyond the temperature upper limit and relies on established atomic recombination processes.

free parameters (1)

electron temperature upper limit
The value T_e ≲ 10,000 K is constrained by matching the observed Paschen and Brackett continuum shapes.

axioms (2)

standard math Paschen jump is produced by free-bound recombination to hydrogen n=3
Standard result from hydrogen atomic physics invoked to interpret the observed spectral discontinuity.
domain assumption Emission is minimally reddened
Assumed to allow the observed continuum shapes to match low-temperature recombination models.

pith-pipeline@v0.9.0 · 5558 in / 1329 out tokens · 73836 ms · 2026-05-10T16:52:28.920905+00:00 · methodology

discussion (0)

Reference graph

Works this paper leans on

60 extracted references · 56 canonical work pages · 3 internal anchors

[1]

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

ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all := #1 ...
[2]

write newline

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[3]

flux densities

thebibliography [1] 20pt to REFERENCES 6pt =0pt 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 Each re...

work page doi:10.5281/zenodo.831784 2019
[4]

Cycle 1, ID

Arrabal Haro P., et al., 2021, Environmental effects on galaxy evolution in a z=5.2 proto-cluster , JWST Proposal. Cycle 1, ID. \#2674

2021
[5]

arXiv e-prints , keywords =

Begelman M. C., Dexter J., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2507.09085 , https://ui.adsabs.harvard.edu/abs/2025arXiv250709085B p. arXiv:2507.09085

work page doi:10.48550/arxiv.2507.09085 2025
[6]

Bezanson R., et al., 2024, @doi [ ] 10.3847/1538-4357/ad66cf , https://ui.adsabs.harvard.edu/abs/2024ApJ...974...92B 974, 92

work page doi:10.3847/1538-4357/ad66cf 2024
[7]

Brammer G., Valentino F., 2025, The DAWN JWST Archive: Compilation of Public NIRSpec Spectra, @doi 10.5281/zenodo.15472354 , https://doi.org/10.5281/zenodo.15472354

work page doi:10.5281/zenodo.15472354 2025
[8]

arXiv:2507.08929

Brazzini M., D'Eugenio F., Maiolino R., Juod z balis I., Ji X., Scholtz J., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2507.08929 , https://ui.adsabs.harvard.edu/abs/2025arXiv250708929B p. arXiv:2507.08929

work page doi:10.48550/arxiv.2507.08929 2025
[9]

arXiv e-prints , keywords =

Brazzini M., et al., 2026, @doi [arXiv e-prints] 10.48550/arXiv.2601.22214 , https://ui.adsabs.harvard.edu/abs/2026arXiv260122214B p. arXiv:2601.22214

work page doi:10.48550/arxiv.2601.22214 2026
[10]

J., Cameron, A

Bunker A. J., et al., 2024, @doi [ ] 10.1051/0004-6361/202347094 , https://ui.adsabs.harvard.edu/abs/2024A&A...690A.288B 690, A288

work page doi:10.1051/0004-6361/202347094 2024
[11]

2025, MN- RAS[arXiv:2508.08768]

Chang S.-J., Gronke M., Matthee J., Mason C., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2508.08768 , https://ui.adsabs.harvard.edu/abs/2025arXiv250808768C p. arXiv:2508.08768

work page doi:10.48550/arxiv.2508.08768 2025
[12]

arXiv e-prints , keywords =

D'Eugenio F., et al., 2025a, @doi [arXiv e-prints] 10.48550/arXiv.2510.00101 , https://ui.adsabs.harvard.edu/abs/2025arXiv251000101D p. arXiv:2510.00101

work page doi:10.48550/arxiv.2510.00101
[13]

D'Eugenio F., et al., 2025b, @doi [ ] 10.3847/1538-4365/ada148 , https://ui.adsabs.harvard.edu/abs/2025ApJS..277....4D 277, 4

work page doi:10.3847/1538-4365/ada148
[14]

J., Willott, C., Alberts, S., et al

Eisenstein D. J., et al., 2023, @doi [arXiv e-prints] 10.48550/arXiv.2306.02465 , https://ui.adsabs.harvard.edu/abs/2023arXiv230602465E p. arXiv:2306.02465

work page doi:10.48550/arxiv.2306.02465 2023
[15]

, keywords =

Finkelstein S. L., et al., 2025, @doi [ ] 10.3847/2041-8213/adbbd3 , https://ui.adsabs.harvard.edu/abs/2025ApJ...983L...4F 983, L4

work page doi:10.3847/2041-8213/adbbd3 2025
[16]

and Lang, Dustin and Goodman, Jonathan , title =

Foreman-Mackey D., Hogg D. W., Lang D., Goodman J., 2013, @doi [ ] 10.1086/670067 , https://ui.adsabs.harvard.edu/abs/2013PASP..125..306F 125, 306

work page doi:10.1086/670067 2013
[17]

and Clayton, Geoffrey C

Gordon K. D., Clayton G. C., Misselt K. A., Landolt A. U., Wolff M. J., 2003, @doi [ ] 10.1086/376774 , https://ui.adsabs.harvard.edu/abs/2003ApJ...594..279G 594, 279

work page doi:10.1086/376774 2003
[18]

Estimating Black Hole Masses in Active Galaxies Using the Halpha Emission Line

Greene J. E., Ho L. C., 2005, @doi [ ] 10.1086/431897 , https://ui.adsabs.harvard.edu/abs/2005ApJ...630..122G 630, 122

work page Pith review doi:10.1086/431897 2005
[19]

E., Labbe, I., Goulding, A

Greene J. E., et al., 2024, @doi [ ] 10.3847/1538-4357/ad1e5f , https://ui.adsabs.harvard.edu/abs/2024ApJ...964...39G 964, 39

work page doi:10.3847/1538-4357/ad1e5f 2024
[20]

Guo H., et al., 2022, @doi [ ] 10.3847/1538-4357/ac4bc6 , https://ui.adsabs.harvard.edu/abs/2022ApJ...927...60G 927, 60

work page doi:10.3847/1538-4357/ac4bc6 2022
[21]

G., Izotov Y

Guseva N. G., Izotov Y. I., Thuan T. X., 2006, @doi [ ] 10.1086/503865 , https://ui.adsabs.harvard.edu/abs/2006ApJ...644..890G 644, 890

work page doi:10.1086/503865 2006
[22]

E., Brammer , G

Heintz K. E., et al., 2025, @doi [ ] 10.1051/0004-6361/202450243 , https://ui.adsabs.harvard.edu/abs/2025A&A...693A..60H 693, A60

work page doi:10.1051/0004-6361/202450243 2025
[23]

Inayoshi K., Maiolino R., 2025, @doi [ ] 10.3847/2041-8213/adaebd , https://ui.adsabs.harvard.edu/abs/2025ApJ...980L..27I 980, L27

work page doi:10.3847/2041-8213/adaebd 2025
[24]

Spectral Uniformity of Little Red Dots: A Natural Outcome of Coevolving Seed Black Holes and Nascent Starbursts

Inayoshi K., Murase K., Kashiyama K., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2509.19422 , https://ui.adsabs.harvard.edu/abs/2025arXiv250919422I p. arXiv:2509.19422

work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2509.19422 2025
[25]

Jakobsen P., et al., 2022, @doi [ ] 10.1051/0004-6361/202142663 , https://ui.adsabs.harvard.edu/abs/2022A&A...661A..80J 661, A80

work page internal anchor Pith review doi:10.1051/0004-6361/202142663 2022
[26]

Juod z balis I., et al., 2024, @doi [ ] 10.1093/mnras/stae2367 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.535..853J 535, 853

work page doi:10.1093/mnras/stae2367 2024
[27]

M., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2505.06965 , https://ui.adsabs.harvard.edu/abs/2025arXiv250506965K p

Kido D., Ioka K., Hotokezaka K., Inayoshi K., Irwin C. M., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2505.06965 , https://ui.adsabs.harvard.edu/abs/2025arXiv250506965K p. arXiv:2505.06965

work page doi:10.48550/arxiv.2505.06965 2025
[28]

Killi M., et al., 2024, @doi [ ] 10.1051/0004-6361/202348857 , https://ui.adsabs.harvard.edu/abs/2024A&A...691A..52K 691, A52

work page doi:10.1051/0004-6361/202348857 2024
[29]

arXiv e-prints , keywords =

Kocevski D. D., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2404.03576 , https://ui.adsabs.harvard.edu/abs/2024arXiv240403576K p. arXiv:2404.03576

work page doi:10.48550/arxiv.2404.03576 2024
[30]

Kokorev V., et al., 2024, @doi [ ] 10.3847/1538-4357/ad4265 , https://ui.adsabs.harvard.edu/abs/2024ApJ...968...38K 968, 38

work page doi:10.3847/1538-4357/ad4265 2024
[31]

P., et al

Kokorev V., et al., 2025, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2025arXiv251107515K p. arXiv:2511.07515

work page arXiv 2025
[32]

2024, in NIST Atomic Spectral Database (ver 5.12) (Gaithersburg, MD: NIST), doi: https://doi.org/10.18434/T4W30F 16Roth et al

Kramida A., Ralchenko Y., Reader J., Team N. A., 2023, NIST Atomic Spectra Database, @doi 10.18434/T4W30F , https://physics.nist.gov/asd

work page doi:10.18434/t4w30f 2023
[33]

2025, arXiv e-prints, arXiv:2507.10659

Lin X., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2507.10659 , https://ui.adsabs.harvard.edu/abs/2025arXiv250710659L p. arXiv:2507.10659

work page doi:10.48550/arxiv.2507.10659 2025
[34]

, keywords =

Liu H., Jiang Y.-F., Quataert E., Greene J. E., Ma Y., 2025, @doi [ ] 10.3847/1538-4357/ae0c19 , https://ui.adsabs.harvard.edu/abs/2025ApJ...994..113L 994, 113

work page doi:10.3847/1538-4357/ae0c19 2025
[35]

2026a, arXiv e-prints, arXiv:2603.02317

Liu H., Jiang Y.-F., Quataert E., Greene J. E., Ma Y., Lin X., 2026, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2026arXiv260302317L p. arXiv:2603.02317

work page arXiv 2026
[36]

S., Knigge C., 2002, @doi [ ] 10.1086/342879 , https://ui.adsabs.harvard.edu/abs/2002ApJ...579..725L 579, 725

Long K. S., Knigge C., 2002, @doi [ ] 10.1086/342879 , https://ui.adsabs.harvard.edu/abs/2002ApJ...579..725L 579, 725

work page doi:10.1086/342879 2002
[37]

A., 2015, @doi [ ] 10.1051/0004-6361/201323152 , https://ui.adsabs.harvard.edu/abs/2015A&A...573A..42L 573, A42

Luridiana V., Morisset C., Shaw R. A., 2015, @doi [ ] 10.1051/0004-6361/201323152 , https://ui.adsabs.harvard.edu/abs/2015A&A...573A..42L 573, A42

work page doi:10.1051/0004-6361/201323152 2015
[38]

Maiolino R., et al., 2025, @doi [ ] 10.1093/mnras/staf359 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.tmp..337M

work page doi:10.1093/mnras/staf359 2025
[39]

V., et al., 2024, @doi [ ] 10.1051/0004-6361/202449914 , https://ui.adsabs.harvard.edu/abs/2024A&A...689A..73M 689, A73

Maseda M. V., et al., 2024, @doi [ ] 10.1051/0004-6361/202449914 , https://ui.adsabs.harvard.edu/abs/2024A&A...689A..73M 689, A73

work page doi:10.1051/0004-6361/202449914 2024
[40]

Matthee J., et al., 2024, @doi [ ] 10.3847/1538-4357/ad2345 , https://ui.adsabs.harvard.edu/abs/2024ApJ...963..129M 963, 129

work page doi:10.3847/1538-4357/ad2345 2024
[41]

, keywords =

Matthews J. H., et al., 2025, @doi [ ] 10.1093/mnras/stae2677 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.536..879M 536, 879

work page doi:10.1093/mnras/stae2677 2025
[42]

P., Matthee, J., Katz, H., et al

Naidu R. P., et al., 2025, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2025arXiv250316596N p. arXiv:2503.16596

work page arXiv 2025
[43]

P., Watson, D., Sneppen, A., et al

Nikopoulos G. P., Watson D., Sneppen A., Rusakov V., Heintz K. E., Witstok J., Brammer G., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2510.06362 , https://ui.adsabs.harvard.edu/abs/2025arXiv251006362N p. arXiv:2510.06362

work page doi:10.48550/arxiv.2510.06362 2025
[44]

arXiv:2602.12548

Pang Y., Wang X., Cheng C., Wang S., Zhou H., Zhou Q., Wu X.-B., Glazebrook K., 2026, @doi [arXiv e-prints] 10.48550/arXiv.2602.12548 , https://ui.adsabs.harvard.edu/abs/2026arXiv260212548P p. arXiv:2602.12548

work page doi:10.48550/arxiv.2602.12548 2026
[45]

Novel $z\sim~10$ auroral line measurements extend the gradual offset of the FMR deep into the first Gyr of cosmic time

Pollock C. L., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2506.15779 , https://ui.adsabs.harvard.edu/abs/2025arXiv250615779P p. arXiv:2506.15779

work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2506.15779 2025
[46]

H., Bezanson, R., Labbe, I., et al

Price S. H., et al., 2025, @doi [ ] 10.3847/1538-4357/adaec1 , https://ui.adsabs.harvard.edu/abs/2025ApJ...982...51P 982, 51

work page doi:10.3847/1538-4357/adaec1 2025
[47]

Rusakov V., et al., 2026, @doi [ ] 10.1038/s41586-025-09900-4 , https://ui.adsabs.harvard.edu/abs/2026Natur.649..574R 649, 574

work page doi:10.1038/s41586-025-09900-4 2026
[48]

Sarrouh G. T. E., et al., 2026, @doi [ ] 10.3847/1538-4365/ae1611 , https://ui.adsabs.harvard.edu/abs/2026ApJS..282....3S 282, 3

work page doi:10.3847/1538-4365/ae1611 2026
[49]

J., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2411.03424 , https://ui.adsabs.harvard.edu/abs/2024arXiv241103424S p

Setton D. J., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2411.03424 , https://ui.adsabs.harvard.edu/abs/2024arXiv241103424S p. arXiv:2411.03424

work page doi:10.48550/arxiv.2411.03424 2024
[50]

arXiv:2408.12713

Shen Y., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2408.12713 , https://ui.adsabs.harvard.edu/abs/2024arXiv240812713S p. arXiv:2408.12713

work page doi:10.48550/arxiv.2408.12713 2024
[51]

H., et al

Sneppen A., et al., 2026, @doi [arXiv e-prints] 10.48550/arXiv.2601.18864 , https://ui.adsabs.harvard.edu/abs/2026arXiv260118864S p. arXiv:2601.18864

work page doi:10.48550/arxiv.2601.18864 2026
[52]

Q., Naidu, R

Sun W. Q., et al., 2026, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2026arXiv260120929S p. arXiv:2601.20929

work page arXiv 2026
[53]

arXiv e-prints , keywords =

Torralba A., et al., 2025, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2025arXiv251000103T p. arXiv:2510.00103

work page arXiv 2025
[54]

Valentino F., et al., 2025, @doi [ ] 10.1051/0004-6361/202553908 , https://ui.adsabs.harvard.edu/abs/2025A&A...699A.358V 699, A358

work page doi:10.1051/0004-6361/202553908 2025
[55]

arXiv:2602.06024

Wang B., et al., 2026, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2026arXiv260206024W p. arXiv:2602.06024

work page arXiv 2026
[56]

2025, arXiv e- prints, arXiv:2512.11050 Article number, page 7 of 8 A&A proofs:manuscript no

Yan Z., Inayoshi K., Chen K., Guo J., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2512.11050 , https://ui.adsabs.harvard.edu/abs/2025arXiv251211050Y p. arXiv:2512.11050

work page doi:10.48550/arxiv.2512.11050 2025
[57]

arXiv:2503.16600

de Graaff A., et al., 2025a, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2025arXiv250316600D p. arXiv:2503.16600

work page arXiv
[58]

Little Red Dots host Black Hole Stars: A unified family of gas-reddened AGN revealed by JWST/NIRSpec spectroscopy

de Graaff A., et al., 2025b, @doi [arXiv e-prints] 10.48550/arXiv.2511.21820 , https://ui.adsabs.harvard.edu/abs/2025arXiv251121820D p. arXiv:2511.21820

work page doi:10.48550/arxiv.2511.21820
[59]

de Graaff A., et al., 2025c, @doi [ ] 10.1051/0004-6361/202452186 , https://ui.adsabs.harvard.edu/abs/2025A&A...697A.189D 697, A189

work page doi:10.1051/0004-6361/202452186
[60]

write newline

" write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...