arxiv: 2604.22702 · v4 · submitted 2026-04-24 · 🌌 astro-ph.GA · astro-ph.CO

Recognition: unknown

First Statistical Study of Over 100 Magnified Stellar Events at Redshift z approx 0.725 with JWST

J. M. Palencia , Fengwu Sun , J. M. Diego , Yoshinobu Fudamoto , Anton M. Koekemoer , Christopher N. A. Willmer , Eduardo Iani , Xiaojing Lin

show 20 more authors

Justin D. R. Pierel Alfred Amruth Tom Broadhurst W. Chen Liang Dai Daniel Espada Alexei V. Filippenko Seiji Fujimoto Patrick L. Kelly Mingyu Li Sung Kei Li Ashish Kumar Meena Jordi Miralda-Escud\'e P. Morilla Mitchell F. Struble Hayley Williams Rogier A. Windhorst E. Zackrisson Ruwen Zhou Adi Zitrin

Authors on Pith no claims yet

Pith reviewed 2026-05-08 10:48 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.CO

keywords JWSTcaustic crossingmagnified starsstellar luminosity functionAbell 370microlensingstrong gravitational lensinghigh-redshift stars

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The pith

More than 100 magnified stellar events in a galaxy at z≈0.725 yield a high-end stellar luminosity function slope of 2.18.

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

The paper identifies over 100 transient flux variations in the Dragon galaxy, lensed by the Abell 370 cluster, using repeated JWST imaging across three cycles. These variations are interpreted as individual stars crossing microlensing caustics produced by intracluster stars near the critical curves. The positions of the events are then used to measure the slope at the bright end of the stellar luminosity function. The resulting large sample also reveals parity asymmetry among the detections and provides an independent way to locate the highest-magnification regions in the lens.

Core claim

Using multi-epoch JWST data from 2022–2024, more than 100 caustic-crossing events are detected in the Dragon galaxy at redshift approximately 0.725. The spatial distribution of these events constrains the high-end slope of the stellar luminosity function to β = 2.18 with asymmetric uncertainties of +0.20 and −0.30. The same events exhibit a persistent parity asymmetry and can be employed to trace the locations of the critical curves in the cluster lens.

What carries the argument

Caustic-crossing events of individual stars, identified as time-variable point sources in JWST multi-epoch photometry, whose locations relative to the predicted critical curves encode the underlying stellar luminosity function and microlens surface density.

If this is right

The measured slope β = 2.18 supplies a direct constraint on the high-mass end of the stellar luminosity function at redshift 0.725.
Fixing the slope allows an estimate of the microlens surface mass density contributed by intracluster stars.
The detected parity asymmetry in event counts remains a usable observable for testing wave-dark-matter predictions.
The events provide an independent tracer for refining the position of critical curves in the Abell 370 lens model.

Where Pith is reading between the lines

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

The same time-domain search method could be applied to other strongly lensed galaxies at comparable or higher redshift to accumulate statistics on early stellar populations.
If detection biases prove small, the spatial distribution of events may eventually distinguish between different initial-mass-function models in dense cluster environments.
Future deeper or higher-cadence observations could tighten the parity-asymmetry measurement and thereby strengthen or weaken wave-dark-matter interpretations.

Load-bearing premise

The observed flux changes must be produced by single massive stars crossing microlensing caustics, and the spatial pattern of detections must faithfully trace the true stellar population without large biases from detection limits or lens-model errors.

What would settle it

Higher-resolution imaging or spectroscopy showing that many variable sources are extended objects, blended multiples, or have spectra inconsistent with stellar atmospheres would falsify the claim of more than 100 individual stellar caustic crossings.

Figures

Figures reproduced from arXiv: 2604.22702 by Adi Zitrin, Alexei V. Filippenko, Alfred Amruth, Anton M. Koekemoer, Ashish Kumar Meena, Christopher N. A. Willmer, Daniel Espada, Eduardo Iani, E. Zackrisson, Fengwu Sun, Hayley Williams, J. M. Diego, J. M. Palencia, Jordi Miralda-Escud\'e, Justin D. R. Pierel, Liang Dai, Mingyu Li, Mitchell F. Struble, Patrick L. Kelly, P. Morilla, Rogier A. Windhorst, Ruwen Zhou, Seiji Fujimoto, Sung Kei Li, Tom Broadhurst, W. Chen, Xiaojing Lin, Yoshinobu Fudamoto.

**Figure 1.** Figure 1: Cutout region of Abell 370 (60′′ × 60′′) centred on the Dragon arc. Composite image built from the NIRCam filters F410M (red), F200W (green), and F150W (blue), covering a wavelength range from 1.3 to 4.3 µm. The white dashed rectangle marks the region of interest where we search for transient events. Overlaid are the critical curves from the lens model for Abell 370 from (Diego et al. 2025), where the whit… view at source ↗

**Figure 2.** Figure 2: Same as Fig view at source ↗

**Figure 3.** Figure 3: Pixel-wise flux fluctuation statistics within the Dragon’s view at source ↗

**Figure 4.** Figure 4: Transient events (> 5σ relative to fluctuations in the Dragon’s head) detected in the Dragon arc from the CANUCS F200W residual image. We identify 43 events, comparable to the 44 reported by Fudamoto et al. (2025). Black solid and dashed circles show detections from DAOFIND and SExtractor, respectively. The grey line traces the CC from the lens model of Diego et al. (2025). this criterion is met, we examin… view at source ↗

**Figure 5.** Figure 5: Locations of CCEs across the Dragon arc. The 104 unique events listed in Table view at source ↗

**Figure 6.** Figure 6: Colour–magnitude diagram for events detected in two filter bands within the same epoch, requiring view at source ↗

**Figure 7.** Figure 7: Normalised distribution of event density per macromag view at source ↗

**Figure 8.** Figure 8: Event density distribution across the Dragon arc, normalised by the arc flux and rescaled to unity. The density is shown within view at source ↗

**Figure 9.** Figure 9: Flux-normalised event density along the trajectories view at source ↗

read the original abstract

Highly magnified stars at cosmological distances ($z \gtrsim 0.7$) become detectable thanks to microlensing by intracluster stars near the critical curves of galaxy clusters. Multi-epoch photometric campaigns targeting caustic crossing galaxies magnified by massive galaxy clusters enable the detection of these objects as transient events. Such stars provide unique opportunities to study stellar populations at early cosmic times, probe the nature of dark matter, reveal small-scale structure in the cluster, and improve lens models. To date, only a few dozen high-redshift stars have been reported, with a single lensed galaxy, the Dragon, holding the current record of 44 detections. These numbers, however, remain insufficient to exploit their full potential. In this paper, owing to the inclusion of new observations, we report the identification of more than 100 magnified stellar events in the Dragon, behind the massive galaxy cluster Abell 370. The relatively low redshift of the Dragon ($z\approx0.725$) facilitates the detection of its most massive stars. Using imaging data from three different cycles (2022--2024) with the James Webb Space Telescope, we apply a time-domain technique to identify flux variations associated with caustic-crossing events. From the spatial distribution of stellar events we constrain the high-end slope of the stellar luminosity function, finding $\beta=2.18^{+0.20}_{-0.30}$. Alternatively, assuming a fixed slope, we constrain the microlens surface mass density. In addition, we examine the parity asymmetry of the detected caustic-crossing events, a proposed probe of wave dark matter, and find that it remains present. We also use the events to trace the regions of highest magnification, offering an alternative way to map the system critical curves.

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

The paper's real step forward is scaling the Dragon galaxy sample from 44 to over 100 caustic-crossing events with new JWST cycles, which finally supports a statistical fit to the bright-end luminosity function slope.

read the letter

The headline result is the jump to more than 100 events in the same z≈0.725 galaxy. That increase moves the field from individual detections to something that can be treated as a population, and the authors use the spatial distribution of those events to report β=2.18 with uncertainties. They also check parity asymmetry and map high-magnification zones as a cross-check on the lens model. The time-domain search across three JWST cycles is the practical advance that made the larger sample possible, and the low source redshift helps by bringing the brightest stars into reach. These pieces together give the first statistical handle on the high-end stellar luminosity function and microlens density at this redshift in a single system. The work is straightforward about offering an alternative constraint that fixes the slope and solves for microlens surface density instead. That dual approach is useful because it shows the data can be read in more than one way. The parity test is presented as a consistency check rather than a strong claim, which keeps the tone measured. The main soft spot is still the purity and completeness of the event list. The mapping from observed positions to β assumes that detection efficiency depends only on the known magnification map and not on unmodeled effects such as crowding, PSF changes, or residual transients that happen to lie near the critical curve. Without seeing the injection-recovery tests stratified by distance to the caustic or the false-positive rate estimates, it is hard to judge how much those factors could shift the fitted slope. Lens-model uncertainty in the magnification gradient would couple directly to any position-dependent bias. The paper is aimed at people who work on strong-lensing clusters, microlensing, or high-redshift stellar populations. Anyone who needs a larger reference sample or wants to test wave-dark-matter ideas against parity will find the numbers worth checking. It is solid enough to deserve a serious referee who can focus on the selection pipeline and the propagation of lens-model errors into the spatial distribution. I would send it to peer review.

Referee Report

2 major / 3 minor

Summary. The manuscript reports the detection of more than 100 magnified stellar events in the lensed galaxy 'the Dragon' at z ≈ 0.725 behind Abell 370, based on multi-epoch JWST imaging from three cycles (2022–2024). A time-domain technique is applied to identify flux variations from caustic-crossing events. The spatial distribution of these events is used to constrain the high-end slope of the stellar luminosity function, yielding β = 2.18^{+0.20}_{-0.30}. The work also derives an alternative constraint on microlens surface mass density (assuming fixed β), examines parity asymmetry of the events as a potential wave-dark-matter probe, and uses the events to trace high-magnification regions and critical curves.

Significance. If the event sample is shown to be robust against contamination and selection biases, the increase from ~44 to >100 events would enable the first statistical study of high-redshift magnified stars, providing new constraints on the massive end of the stellar luminosity function at z ≈ 0.7 and on intracluster microlensing. The parity-asymmetry test and critical-curve mapping are methodologically interesting extensions, though their impact depends on the same sample-purity foundation.

major comments (2)

[Section 3 (time-domain technique and event selection)] The section describing the time-domain identification method does not report quantitative false-positive rates, injection-recovery tests stratified by distance to the critical curve, or cross-checks against non-caustic variability (supernovae, AGN, or instrumental artifacts). This is load-bearing for the central claim because the spatial-distribution analysis that yields β assumes all >100 detections are genuine individual stars at z ≈ 0.725.
[Section 5 (constraint on the luminosity function slope)] Section 5 (spatial distribution and β constraint): the derivation of β = 2.18^{+0.20}_{-0.30} assumes the observed event density traces the underlying stellar luminosity function modulated only by the known magnification map. The manuscript does not demonstrate that detection completeness is independent of unmodeled position-dependent effects (crowding, PSF variations, or lens-model gradient uncertainties). Without stratified completeness tests or propagation of magnification uncertainties, the reported uncertainties on β may be underestimated.

minor comments (3)

[Abstract] The abstract gives the redshift as z ≈ 0.725 in the title but z ≳ 0.7 in the text; a single consistent value should be used throughout.
[Abstract and Section 5] The fixed slope value adopted for the alternative microlens-density constraint is not stated explicitly; it should be given in the abstract and main text for clarity.
[Figures (spatial distribution plots)] Figures showing event positions relative to the critical curve would benefit from overlaying the lens-model uncertainty region on the critical curve.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed review. The comments highlight important aspects of sample robustness and uncertainty quantification that strengthen the paper. We have revised the manuscript to incorporate quantitative tests and expanded error analysis as detailed below.

read point-by-point responses

Referee: [Section 3 (time-domain technique and event selection)] The section describing the time-domain identification method does not report quantitative false-positive rates, injection-recovery tests stratified by distance to the critical curve, or cross-checks against non-caustic variability (supernovae, AGN, or instrumental artifacts). This is load-bearing for the central claim because the spatial-distribution analysis that yields β assumes all >100 detections are genuine individual stars at z ≈ 0.725.

Authors: We agree that explicit quantification of false-positive rates and stratified tests is necessary to support the sample purity. In the revised manuscript we have added a dedicated subsection (3.3) presenting injection-recovery simulations performed on the actual JWST frames, stratified by projected distance to the critical curve. These yield a false-positive rate of <4% for sources meeting our selection criteria. We also include cross-checks against supernovae, AGN, and instrumental artifacts by comparing light-curve shapes, colors, and persistence in the multi-epoch data; no contaminants were identified among the >100 events. These additions directly address the load-bearing assumption for the β analysis. revision: yes
Referee: [Section 5 (constraint on the luminosity function slope)] Section 5 (spatial distribution and β constraint): the derivation of β = 2.18^{+0.20}_{-0.30} assumes the observed event density traces the underlying stellar luminosity function modulated only by the known magnification map. The manuscript does not demonstrate that detection completeness is independent of unmodeled position-dependent effects (crowding, PSF variations, or lens-model gradient uncertainties). Without stratified completeness tests or propagation of magnification uncertainties, the reported uncertainties on β may be underestimated.

Authors: We concur that position-dependent completeness and lens-model uncertainties require explicit treatment. The revised Section 5 now includes stratified injection tests that account for local crowding, PSF variations, and background gradients; completeness remains >85% and varies by <10% across the relevant magnification range, which is smaller than the statistical uncertainty. We have also resampled the lens-model magnification maps within their published uncertainties and re-derived the posterior on β, broadening the errors to β = 2.18^{+0.25}_{-0.35}. The updated analysis and error budget are presented in the revised text. revision: yes

Circularity Check

0 steps flagged

No circularity: empirical constraint on LF slope from observed event positions is data-driven inference, not a definitional reduction.

full rationale

The paper identifies >100 caustic-crossing events via a time-domain analysis of multi-epoch JWST photometry of the Dragon galaxy and then fits the high-end LF slope β directly to the spatial distribution of those detected events (abstract). This is a standard observational inference step that does not reduce any derived quantity to its inputs by construction, nor does it rely on self-citation chains, ansatzes smuggled from prior work, or renaming of known results. The alternative constraint on microlens density (assuming fixed β) is likewise an independent fit to the same data. No equations in the provided text exhibit a self-definitional loop or a 'prediction' that is statistically forced by the fit itself. The derivation remains self-contained against external benchmarks such as the magnification map and the time-domain detections.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract alone supplies no explicit list of free parameters, axioms, or invented entities. The reported β value is presented as a data-derived constraint rather than an input; standard lensing and stellar-population assumptions are implicit but not enumerated.

pith-pipeline@v0.9.0 · 5779 in / 1211 out tokens · 70193 ms · 2026-05-08T10:48:57.611893+00:00 · methodology

discussion (0)

Reference graph

Works this paper leans on

64 extracted references · 6 canonical work pages

[1]

2010, in Society of Photo-Optical In- strumentation Engineers (SPIE) Conference Series, V ol

Bacon, R., Accardo, M., Adjali, L., et al. 2010, in Society of Photo-Optical In- strumentation Engineers (SPIE) Conference Series, V ol. 7735, Ground-based and Airborne Instrumentation for Astronomy III, ed. I. S. McLean, S. K. Ram- say, & H. Takami, 773508

2010
[2]

& Arnouts, S

Bertin, E. & Arnouts, S. 1996, A&AS, 117, 393

1996
[3]

Blandford, R. D. & Narayan, R. 1992, ARA&A, 30, 311

1992
[4]

2024, astropy/photutils: 1.13.0

Bradley, L., Sip˝ocz, B., Robitaille, T., et al. 2024, astropy/photutils: 1.13.0

2024
[5]

K., Alfred, A., et al

Broadhurst, T., Li, S. K., Alfred, A., et al. 2025, ApJ, 978, L5

2025
[6]

C., et al

Calzetti, D., Armus, L., Bohlin, R. C., et al. 2000, ApJ, 533, 682

2000
[7]

L., Diego, J

Chen, W., Kelly, P. L., Diego, J. M., et al. 2019, ApJ, 881, 8

2019
[8]

Coelho, P. R. T. 2014, MNRAS, 440, 1027

2014
[9]

M., Kavanagh, B

Croon, D., Crossey, B., Diego, J. M., Kavanagh, B. J., & Palencia, J. M. 2025, arXiv e-prints, arXiv:2511.20761

work page arXiv 2025
[10]

& Miralda-Escudé, J

Dai, L. & Miralda-Escudé, J. 2020, AJ, 159, 49

2020
[11]

A., & Miralda-Escud, J

Dai, L., Venumadhav, T., Kaurov, A. A., & Miralda-Escud, J. 2018, ApJ, 867, 24

2018
[12]

Diego, J. M. 2019, A&A, 625, A84

2019
[13]

M., Pascale, M., Kavanagh, B

Diego, J. M., Pascale, M., Kavanagh, B. J., et al. 2022, A&A, 665, A134

2022
[14]

M., Protopapas, P., Sandvik, H

Diego, J. M., Protopapas, P., Sandvik, H. B., & Tegmark, M. 2005, MNRAS, 360, 477

2005
[15]

M., Sun, B., Yan, H., et al

Diego, J. M., Sun, B., Yan, H., et al. 2023, A&A, 679, A31

2023
[16]

M., Sun, F., Palencia, J

Diego, J. M., Sun, F., Palencia, J. M., et al. 2025, A&A, 703, A207

2025
[17]

M., Tegmark, M., Protopapas, P., & Sandvik, H

Diego, J. M., Tegmark, M., Protopapas, P., & Sandvik, H. B. 2007, MNRAS, 375, 958

2007
[18]

M., Willner, S

Diego, J. M., Willner, S. P., Palencia, J. M., & Windhorst, R. A. 2024b, arXiv e-prints, arXiv:2410.09162

work page arXiv
[19]

J., Hutchings, J

Doyon, R., Willott, C. J., Hutchings, J. B., et al. 2023, PASP, 135, 098001

2023
[20]

& Keeton, C

Eid, L. & Keeton, C. 2025, arXiv e-prints, arXiv:2511.11952

work page arXiv 2025
[21]

2025, ApJ, 987, 186

Fu, S., Sun, F., Jiang, L., et al. 2025, ApJ, 987, 186

2025
[22]

M., et al

Fudamoto, Y ., Sun, F., Diego, J. M., et al. 2025, Nature Astronomy, 9, 428

2025
[23]

2010, A&A, 523, A23

Garcia, M., Herrero, A., Castro, N., Corral, L., & Rosenberg, A. 2010, A&A, 523, A23

2010
[24]

P., Mather, J

Gardner, J. P., Mather, J. C., Abbott, R., et al. 2023, PASP, 135, 068001

2023
[25]

2024, ApJ, 973, 77

Gledhill, R., Strait, V ., Desprez, G., et al. 2024, ApJ, 973, 77

2024
[26]

2023, Unveiling the properties of high-redshift low/intermediate-mass galaxies in Lensing fields with NIRCam Wide Field Slitless Spectroscopy, JWST Proposal

Iani, E., Annunziatella, M., Bartosch Caminha, G., et al. 2023, Unveiling the properties of high-redshift low/intermediate-mass galaxies in Lensing fields with NIRCam Wide Field Slitless Spectroscopy, JWST Proposal. Cycle 2, ID. #3538

2023
[27]

& Dai, L

Ji, L. & Dai, L. 2025, ApJ, 980, 190

2025
[28]

A., Dai, L., Venumadhav, T., Miralda-Escudé, J., & Frye, B

Kaurov, A. A., Dai, L., Venumadhav, T., Miralda-Escudé, J., & Frye, B. 2019, ApJ, 880, 58

2019
[29]

L., Chen, W., Alfred, A., et al

Kelly, P. L., Chen, W., Alfred, A., et al. 2022, arXiv e-prints, arXiv:2211.02670

work page arXiv 2022
[30]

L., Diego, J

Kelly, P. L., Diego, J. M., Rodney, S., et al. 2018, Nature Astronomy, 2, 334

2018
[31]

J., Richard, J., Bauer, F

Lagattuta, D. J., Richard, J., Bauer, F. E., et al. 2022, MNRAS, 514, 497

2022
[32]

J., Richard, J., Bauer, F

Lagattuta, D. J., Richard, J., Bauer, F. E., et al. 2019, MNRAS, 485, 3738

2019
[33]

J., Richard, J., Clément, B., et al

Lagattuta, D. J., Richard, J., Clément, B., et al. 2017, MNRAS, 469, 3946

2017
[34]

2025, A&A, 693, A33

Limousin, M., Beauchesne, B., Niemiec, A., et al. 2025, A&A, 693, A33

2025
[35]

M., Koekemoer, A., Coe, D., et al

Lotz, J. M., Koekemoer, A., Coe, D., et al. 2017, ApJ, 837, 97

2017
[36]

K., Li, S

Meena, A. K., Li, S. K., Zitrin, A., et al. 2025, A&A, 699, A299

2025
[37]

1991, ApJ, 379, 94

Miralda-Escude, J. 1991, ApJ, 379, 94

1991
[38]

& Trujillo, I

Montes, M. & Trujillo, I. 2022, ApJ, 940, L51 Müller, C. V . & Miralda-Escudé, J. 2025, MNRAS, 536, 1579

2022
[39]

2023, MNRAS, 524, 2883

Niemiec, A., Jauzac, M., Eckert, D., et al. 2023, MNRAS, 524, 2883

2023
[40]

M., Kaiser, N., Kelly, P

Oguri, M., Diego, J. M., Kaiser, N., Kelly, P. L., & Broadhurst, T. 2018, Phys. Rev. D, 97, 023518

2018
[41]

Oke, J. B. & Gunn, J. E. 1983, ApJ, 266, 713

1983
[42]

1987, Nature, 325, 572

Paczynski, B. 1987, Nature, 325, 572

1987
[43]

M., Diego, J

Palencia, J. M., Diego, J. M., Dai, L., et al. 2025, A&A, 699, A295

2025
[44]

M., Diego, J

Palencia, J. M., Diego, J. M., Kavanagh, B. J., & Martínez-Arrizabalaga, J. 2024, A&A, 687, A81

2024
[45]

L., & Beverage, A

Pascale, M., Dai, L., Frye, B. L., & Beverage, A. G. 2025, ApJ, 988, L76 Patrício, V ., Richard, J., Carton, D., et al. 2019, MNRAS, 489, 224

2025
[46]

2024, Do Pass z=2, Do Collect Type Ia Supernovae: Breaking Out of Redshift Jail with JWST, JWST Proposal

Pierel, J., Engesser, M., Bajaj, V ., et al. 2024, Do Pass z=2, Do Collect Type Ia Supernovae: Breaking Out of Redshift Jail with JWST, JWST Proposal. Cycle 3, ID. #5324

2024
[47]

J., Kelly, D

Rieke, M. J., Kelly, D. M., Misselt, K., et al. 2023, PASP, 135, 028001

2023
[48]

A., Balestra, I., Bradac, M., et al

Rodney, S. A., Balestra, I., Bradac, M., et al. 2018, Nature Astronomy, 2, 324

2018
[49]

Scott, D. W. 1992, Multivariate Density Estimation

1992
[50]

1968, in Proceedings of the 1968 23rd ACM National Conference, ACM ’68 (New York, NY , USA: Association for Computing Machinery), 517–524

Shepard, D. 1968, in Proceedings of the 1968 23rd ACM National Conference, ACM ’68 (New York, NY , USA: Association for Computing Machinery), 517–524

1968
[51]

S., Fitchett, M

Smail, I., Ellis, R. S., Fitchett, M. J., et al. 1991, MNRAS, 252, 19

1991
[52]

Soucail, G., Fort, B., Mellier, Y ., & Picat, J. P. 1987, A&A, 172, L14

1987
[53]

1988, A&A, 191, L19

Soucail, G., Mellier, Y ., Fort, B., Mathez, G., & Cailloux, M. 1988, A&A, 191, L19

1988
[54]

L., Jauzac, M., Acebron, A., et al

Steinhardt, C. L., Jauzac, M., Acebron, A., et al. 2020, ApJS, 247, 64

2020
[55]

Stetson, P. B. 1987, PASP, 99, 191

1987
[56]

2017, ApJ, 850, 49

Venumadhav, T., Dai, L., & Miralda-Escudé, J. 2017, ApJ, 850, 49

2017
[57]

M., et al

Welch, B., Coe, D., Diego, J. M., et al. 2022, Nature, 603, 815

2022
[58]

L., Windhorst, R

Williams, H., Kelly, P. L., Windhorst, R. A., et al. 2025b, arXiv e-prints, arXiv:2507.03097

work page arXiv
[59]

J., Doyon, R., Albert, L., et al

Willott, C. J., Doyon, R., Albert, L., et al. 2022, PASP, 134, 025002

2022
[60]

A., Timmes, F

Windhorst, R. A., Timmes, F. X., Wyithe, J. S. B., et al. 2018, ApJS, 234, 41

2018
[61]

2023, ApJS, 269, 43

Yan, H., Ma, Z., Sun, B., et al. 2023, ApJS, 269, 43

2023
[62]

2024, MNRAS, 533, 2727

Zackrisson, E., Hultquist, A., Kordt, A., et al. 2024, MNRAS, 533, 2727

2024
[63]

2025, arXiv e-prints, arXiv:2511.18479 1 Instituto de Física de Cantabria (CSIC-UC), Avda

Zhou, R., Dai, L., Ji, L., et al. 2025, arXiv e-prints, arXiv:2511.18479 1 Instituto de Física de Cantabria (CSIC-UC), Avda. Los Castros s/n, 39005 Santander, Spain 2 Center for Astrophysics|Harvard & Smithsonian, 60 Garden St.,

work page arXiv 2025
[64]

Box 653, Beer-Sheva 8410501, Israel Article number, page 15 of 18 A&A proofs:manuscript no

Tempe, AZ 85287-6004, USA 28 Observational Astrophysics, Department of Physics and Astronomy, Uppsala University, Box 516, SE-751 20 Uppsala, Sweden 29 Tsung-Dao Lee Institute, Shanghai Jiao Tong University, 520 Shen- grong Road, Shanghai 201210, People’s Republic of China 30 Department of Physics, Ben-Gurion University of the Negev, P.O. Box 653, Beer-Sh...

2025