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Compact Ionized Gas Region Surrounded by Porous Neutral Gas in a Dusty Lyman Break Galaxy at Redshift $z=8.312$

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Pith's one-line read At redshift 8.312, the galaxy MACS0416_Y1 has a porous neutral interstellar medium: only about a quarter of each H II region is covered by neutral gas, leaving most ionized gas exposed to open space.

desk verdict First z>8 PDR covering-fraction estimate, but the porosity claim is hostage to the radiation-bounded geometry assumption that the paper itself flags. read the letter →

arxiv 2506.20734 v1 pith:4LROWICI submitted 2025-06-25 astro-ph.GA

Masato Hagimoto , Yoichi Tamura , Akio K. Inoue , Hideki Umehata , Tom J. L. C. Bakx , Takuya Hashimoto , Ken Mawatari , Yuma Sugahara
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Yoshinobu Fudamoto Yuichi Harikane Hiroshi Matsuo Akio Taniguchi
This is my paper · ORCID
classification astro-ph.GA
keywords galaxyevolutioninterstellarmediumLymanbreakgalaxiesphotoionizationmodelingneutralgascoveringfraction[CII]158micronemission[OIII]88cosmicreionization
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 typical interstellar medium in the z = 8.312 Lyman break galaxy MACS0416_Y1 is porous: only about a quarter of each H II region's surface is covered by neutral gas, leaving most of the ionized gas exposed to intercloud space. If true, this meets a necessary geometric condition for ionizing photons to escape into the intergalactic medium, strengthening the case that high-[O III]/[C II] galaxies like Y1 contributed to cosmic reionization. The claim rests on fitting a multi-phase photoionization model to ALMA and JWST observations, and the authors show the conclusion survives variations in star-formation history, age, metallicity, and carbon-to-oxygen ratio. A secondary finding is that the modeled H II regions are compact (about 0.9 pc across), similar to young compact H II regions in the local Universe.

What carries the argument

The central object is the neutral gas covering fraction cov_PDR, defined as the linear combination coefficient that interpolates between a completely uncovered H II region and one fully wrapped in a photo-dissociation region: L_out = (1−cov_PDR) L_HII + cov_PDR L_HII+PDR. The model grid is computed with the Cloudy photoionization code using a depth-dependent density profile n_H = n_H,c [1 + N(H)/$10^{21}$ $cm^{-2}$], with the H II region stopped at 1 percent neutral hydrogen and the PDR stopped at A_V = 5. This machinery converts the observed line and continuum ratios into a single number expressing how much of each H II region is open to intercloud space.

What would settle it

A spatially resolved map of [C II] 158 um at Y1's 300 pc scale that cleanly separates a diffuse, extended component from the [O III] clumps could falsify the geometric reading: if most [C II] is diffuse, cov_PDR no longer tracks porosity. A second far-infrared line such as [N II] 205 um could test whether [C II] indeed traces PDR gas rather than ionized gas; a direct detection of Lyman-continuum leakage (for example, recombination emission far outside the [O III] clumps) would confirm the picture, while a strict upper limit on escaping ionizing photons would demand a revised interpretation.

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Extended reading notes

Core claim

The paper builds a Cloudy-based multi-phase model of the typical interstellar medium in MACS0416_Y1, fitting the [O III] 88 um, [C II] 158 um, UV, and infrared luminosities with three free parameters: gas density, ionization parameter, and the covering fraction cov_PDR of the neutral photo-dissociation region around each H II region. The best-fit model gives cov_PDR = 0.25 (+0.19/−0.14), with log n_H,c = 2.7 and log U = −1.9, and a Monte Carlo analysis rules out the fully covered case cov_PDR = 1. The authors interpret the low covering fraction as porosity: about 75 percent of the surface of a typical H II region is exposed to intercloud space, which is a necessary geometric condition for ionizing photons to escape the galaxy. The same model yields a Stromgren radius of 0.45 pc (diameter D = 0.90 pc), placing Y1's H II regions among local compact H II regions and indicating a young evolutionary stage.

Load-bearing premise

The central result assumes that the galaxy can be represented as many identical spherical H II regions whose [C II] 158 um emission comes entirely from a surrounding photo-dissociation region, with a single linear covering fraction interpolating between fully covered and fully uncovered cases; if a substantial share of the observed [C II] instead comes from diffuse neutral gas unrelated to the H II regions, or if the true geometry is density-bounded so ionizing photons escape before forming a PDR, the fitted cov_PDR would not translate directly into the fraction of ionized gas exposed to intercloud space.

Editorial extensions

If this is right

  • The fully covered scenario cov_PDR = 1 is rejected, so Y1's typical ISM has a porous neutral gas structure rather than H II regions buried in PDRs.
  • Because about 75 percent of the H II surface is exposed, Y1 meets a necessary geometric condition for non-zero Lyman-continuum escape, supporting the idea that high-[O III]/[C II] galaxies could help drive reionization.
  • The inferred H II region size D = 0.90 pc and density log n_H,c = 2.7 place these regions among local compact H II regions, implying the star-forming clumps in Y1 are in an early evolutionary stage.
  • Systematic tests varying star-formation history, stellar age, gas and stellar metallicity, and carbon-to-oxygen abundance leave the porous-gas conclusion intact; only a higher dust temperature shifts cov_PDR higher, but even then full coverage remains excluded.
  • The best-fit model reproduces the observed rest-frame optical SED and most JWST line luminosities, although it underestimates [O II] and [O III] 4364 emission, hinting at an additional low-ionization gas component.

Reading between the lines

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

  • If this porosity is typical of UV-luminous z > 6 galaxies, reionization could be driven by a population of ordinary starbursts rather than only exceptional leakers, an extrapolation the paper does not itself make.
  • A natural test is to apply the same three-parameter model to other galaxies with [O III] 88 um and [C II] 158 um detections and check whether cov_PDR anticorrelates with independently estimated Lyman-continuum escape fractions.
  • Because the model omits density-bounded H II regions, part of the fitted exposure could actually represent photons escaping through density-bounded champagne flows; distinguishing this from geometric porosity would require additional diagnostics such as [O III]/H beta or He II lines.
  • The compact H II regions predicted by the model imply very young, few-Myr-old star-forming clumps; JWST IFU spectroscopy of the individual [O III] peaks could directly test for age gradients between clumps.
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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

1 major / 1 minor

Summary. The paper presents a multi-phase ISM model of the z=8.312 Lyman break galaxy MACS0416_Y1, using Cloudy to fit three free parameters — the PDR covering fraction cov_PDR, the hydrogen density at the illuminated face n_H,c, and the ionization parameter U — to three observed luminosity ratios relative to [O III] 88 micron: [C II] 158 micron/[O III], UV/[O III], and IR/[O III]. The best fit yields cov_PDR=0.25^{+0.19}_{-0.14}, log n_H,c/cm^-3=2.7, and log U=-1.9, from which the authors conclude that about 75% of the ionized gas surface is exposed to intercloud space, a necessary geometric condition for Lyman continuum escape, and that the typical H II region size is D=0.90 pc. The model also predicts a rest-frame UV-to-optical SED and optical line luminosities that are compared with JWST observations, showing rough agreement for Balmer lines and [O III] 5008 but a factor-of-two underprediction of [O II] 3727+3729 and [O III] 4364. The paper tests the sensitivity of the result to star-formation history, stellar age, metallicity, C/O ratio, and dust temperature.

Significance. If the central geometric inference is correct, this would be one of the first observational estimates of neutral gas porosity in a galaxy during the epoch of reionization, supporting the idea that high-[O III]/[C II] galaxies can contribute non-zero ionizing photon escape. The paper is methodologically transparent: it uses a public photoionization code, explicitly states fixed assumptions, provides Monte Carlo parameter uncertainties, and offers out-of-fit predictions (optical SED and line luminosities) against independent JWST data. These are genuine strengths. However, the central claim that the fitted cov_PDR is a geometric covering fraction rests on a radiation-bounded, single-covering-fraction geometry that the paper itself narrows by omitting density-bounded H II regions. Because the fit is exactly determined (three observables, three free parameters), the 'agreement' in Figure 2(b) does not validate the geometry, and the factor-of-two [O II] discrepancy points to a missing low-ionization component that could also contribute [C II] and bias cov_PDR downward. The significance is therefore real but conditional on assumption checks that are not yet performed.

major comments (1)
  1. [Section 5.1] Section 5.1 tests adding an old stellar population to improve the rest-frame optical photometry, but the fit adds this component only to the SED, not to the photoionization model that determines line luminosities. The discussion of F356W and [O II] is reasonable, but the possibility that an old stellar population changes the ionizing photon budget or the geometry is not explored. This is a secondary point because the main result is based on the FIR line ratios, but it affects the consistency argument that the model simultaneously explains the SED and the line emission.
minor comments (1)
  1. [Section 4.2] The sentence 'we also find no model grid that reproduces such a high T_e' is a strong statement; the text does not report the range of electron temperatures across the grid or the best achievable value. A quantitative statement of the maximum T_e in the grid would help the reader assess the tension.

Circularity Check

1 steps flagged · score 6.0 of 10

The '≈75% exposed' porosity claim is the fitted cov_PDR restated by Eq. (3) by construction, though the SED and optical-line checks are genuine out-of-fit validations.

  1. fitted input called prediction [Section 3.1 (Eq. 3) and Section 4.1]
    "Lout = (1−covPDR)LH ii+covPDRLH ii+PDR, (3) ... covPDR is not an input parameter of Cloudy, and we define this as the linear combination coefficient of the fraction of the H ii region covered by a PDR. ... Our model predictscovPDR ≈25%, indicating that ≈75% of the outer surface of a typical H ii region is not covered by the PDR."

    cov_PDR is one of the three free parameters minimized in the chi-squared fit (Eq. 4) against the observed [O III]88/[C II]158, UV, and IR luminosity ratios. Equation (3) defines cov_PDR as the linear interpolation coefficient, i.e., the fraction of the H ii region covered by a PDR. The headline conclusion that ~75% of the ionized gas region is exposed to intercloud space is therefore simply 1 − cov_PDR evaluated at the best fit: a relabeling of the fitted parameter, not an independently derived quantity. The real empirical content is only that the data prefer cov_PDR ≈ 0.25 over 1.0 within the assumed model family.

full rationale

The paper is largely self-contained and does not depend on a load-bearing self-citation chain: the multi-phase modeling framework is taken from external work (Cormier et al. 2019; Ramambason et al. 2022), and the Cloudy/BPASS machinery is independent. The JWST SED and optical emission-line comparisons in Section 4.2 are genuine out-of-fit predictions and provide real corroboration for the model's density and ionization parameter. However, the central physical claim of the paper — porous neutral gas with ~75% of the H ii region surface exposed to intercloud space — is not an independent prediction: cov_PDR is a fitted parameter, and the 'exposed fraction' is its complement under Eq. (3). Calling the best-fit cov_PDR a 'prediction' is the fitted-input-called-prediction pattern. The paper also explicitly omits density-bounded H ii regions (Section 3.1), which is an acknowledged modeling limitation rather than circularity, but it reinforces that the geometric interpretation of cov_PDR as porosity is an assumption of the model family, not a separately derived result. Overall, partial circularity: the headline porosity result reduces to the fit, while ancillary model checks add independent but narrower support.

Assumptions & free parameters 6 free parameters · 7 assumptions · 0 invented entities

The central claim rests on a single-zone photoionization model with several fixed astrophysical priors; the three headline parameters are fitted to three observed ratios, and the porosity interpretation is tied to the assumed geometry. No new physical entities are introduced.

free parameters (6)
  • cov_PDR = 0.25 (+0.19, -0.14)
    Neutral gas covering fraction; fitted via Eq. 4 to the observed [C II]/[O III], UV/[O III], and IR/[O III] ratios. The headline porosity claim is this parameter's value.
  • log n_H,c = 2.7 (+0.2, -0.55)
    Hydrogen density at the illuminated face, fitted in the same chi-square minimization; drives line critical densities and Stromgren radius.
  • log U = -1.9 ± 0.2
    Ionization parameter at the illuminated face, fitted simultaneously; sets [O III]/[O II] and general line strengths.
  • T_dust = 80 K fiducial; 100 K in robustness test
    Hand-chosen from Bakx et al. (2020) based on a single 90 um detection; fixes L_IR through a modified blackbody with beta_d=2, and higher T_d shifts cov_PDR to about 0.55.
  • Z_gas = Z_star = 0.2 Zsun fiducial; 0.1 and 1.0 Zsun tested
    Fixed from Tamura et al. (2019) SED fits; affects cooling and line ratios. The lower-Z case shifts best-fit parameters but keeps cov consistent within errors.
  • C/O abundance ratio = solar in fiducial; about 37 percent solar in test
    Set through the Dopita et al. (2006) scaling in Section 5.3; influences [C II] flux and the [O III]/[C II] ratio, but the variation does not change the conclusion.
assumptions (7)
  • domain assumption The ISM is spherically symmetric, with a central ionizing source completely surrounded by ionized gas, repeated as many identical typical regions.
    Section 3.1 states this geometry; the entire cov_PDR interpretation depends on it.
  • domain assumption Observed [C II] 158 um emission is produced only by the modeled PDR phase, with no separate diffuse neutral gas component.
    Used throughout the fitting; if a diffuse neutral phase contributes [C II], the fitted cov_PDR would not map one-to-one to porosity.
  • ad hoc to paper The linear combination L_out = (1-cov_PDR) L_HII + cov_PDR L_HII+PDR (Eq. 3) accurately represents the effect of patchy PDR covering on all line and continuum luminosities.
    Defined in Section 3.1; it is a constructed interpolation, not derived from radiative transfer through a clumpy medium.
  • ad hoc to paper Density-bounded H II regions are omitted.
    Section 3.1 explicitly notes this to reduce free parameters; density-bounded regions would allow ionizing photon escape without requiring porous PDR, so the inference could be affected.
  • domain assumption Dust grains are Milky Way-like: the default Cloudy grain model with a 2175 A bump.
    Section 3.1 and 4.2; the paper argues this bump explains part of the SED mismatch, but it also fixes the UV attenuation behavior used in the model.
  • ad hoc to paper Gas-phase metallicity equals stellar metallicity (0.2 Zsun) in the fiducial model.
    Section 3.1; this affects line cooling and is tested in Section 5.3, but it remains a fixed prior in the fiducial run.
  • domain assumption Dust temperature T_d=80 K and dust emissivity index beta_d=2 are used to convert the single 90 um continuum point into L_IR.
    Section 3.1 and Table 2; L_IR is one of the three fitted observables, so this assumption directly enters the fit.

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Cite this review

Pith. "Pith review of Compact Ionized Gas Region Surrounded by Porous Neutral Gas in a Dusty Lyman Break Galaxy at Redshift $z=8.312$." pith.science (2026). https://pith.science/paper/4LROWICI

@misc{pith2026250620734,
  author       = {Pith},
  title        = {Pith review of: Compact Ionized Gas Region Surrounded by Porous Neutral Gas in a Dusty Lyman Break Galaxy at Redshift $z=8.312$},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/4LROWICI}},
  note         = {Machine review of arXiv:2506.20734}
}
abstract

Porous interstellar medium (ISM) structure in galaxies at the epoch of reionization (EoR) gives us a hint to understand what types of galaxies contribute to reionization. Although recent studies have pointed out the positive correlation between high ionizing photon escape fractions and high [O III] $88~\mu\mathrm{m}$-to-[C II] $158~\mu\mathrm{m}$ ratios found in UV-luminous star-forming galaxies at $z > 6$ with ALMA, previous studies have paid little attention to the neutral gas porosity that allows ionizing photons to escape. Here, we present a detailed analysis of a $z=8.312$ Lyman break galaxy, MACS0416_Y1 with a high $L_\mathrm{[OIII]88}/L_\mathrm{[CII]158}$ ratio ($\approx9$) and dust continuum detection. We construct a multi-phase ISM model incorporating the neutral gas covering fraction ($cov_\mathrm{PDR}$). The best-fit model reveals a $cov_\mathrm{PDR}\approx25 \%$, indicating that $\approx75 \%$ of the ionized gas region is exposed to intercloud space. We confirm that our conclusions hold even when varying star-formation history, stellar age, gas/stellar metallicity, and carbon-to-oxygen abundance ratio. This finding meets one of the necessary conditions for galaxies to have a non-zero escape fraction of ionizing photons and supports recent studies that galaxies with a high [O III] $88~\mu\mathrm{m}/$[C II] $158~\mu\mathrm{m}$ ratio, such as MACS0416_Y1, could contribute to cosmic reionization. Furthermore, the modeled H II region with the best-fitting parameters has a typical size ($D=0.90~\mathrm{pc}$) and gas density ($\log n_\mathrm{H,c}/\mathrm{cm^{-3}}=2.7$) that are comparable to local compact H II regions. This suggests that the H II regions in MACS0416_Y1 are in an early evolutionary stage.

Figures

Figures reproduced from arXiv: 2506.20734 by the authors.

Figure 1
Figure 1. Rest-frame UV images (HST/F160W) with the contour of [O iii] 88 µm moment 0 map reported in Tamura et al. (2023). The contours are (−2, 2, 4, 6, 8) × σ where 1σ = 11 mJy km s−1 beam−1 . We also overlaid the two slits used to obtain the spectrum with JWST/NIRSpec in Har￾shan et al. (2024). These two slits do not cover the eastern UV clump (‘E’ in the figure) as they reported. We find that the eastern peak of [O iii] … view at source ↗
Figure 2
Figure 2. (a) The probability density distributions of each parameter obtained from a total of 10, 000 Monte Carlo re￾alizations. Orange solid and dashed lines correspond to the median and error as their 68 percentiles, and we define them as the best-fitting parameters. (b) Comparison between ob￾served (orange crosses) and modeled (blue squares) luminos￾ity ratios relative to [O iii] 88 µm. 4. FIDUCIAL MODEL RESULTS 4.1. Best… view at source ↗
Figure 3
Figure 3. Schematic view of the ISM for the best-fit model parameter set. reported in the Herschel Dwarf Galaxy Survey (−2.4; Cormier et al. 2019), the average values of H ii regions in our Galaxy (≈ −2.3; Rigby & Rieke 2004), and obser￾vations of super-star clusters in M82 (F¨orster Schreiber et al. 2001; Smith et al. 2006). The higher ioniza￾tion parameter found for Y1 reflects the observed high [O iii] 88 µm-to-[C ii] 158 … view at source ↗
Figures from the paper (4 more)
Figure 4
Figure 4. Figure 4: (a) Rest-frame UV-to-Optical SED obtained from the Cloudy model with the best-fit parameters (blue line) with modeled flux densities (gray squares) and extracted flux densities in Ma et al. (2024) from HST and JWST observations (red and orange crosses). We used the red…
Figure 5
Figure 5. Figure 5: Rest-frame UV-to-Optical SED model (blue line) in which an old stellar component made by single star-burst at 300 Myr ago (dashed green) is added to the best-fit SED model obtained in Section 4.2 (dashed light-blue) with mod￾eled flux densities (gray squares) and extra…
Figure 6
Figure 6. Figure 6: Comparison of the best-fitting values for the covering fraction (covPDR), gas density (log nH,c/cm−3 ), and ionization parameter (log U), with the central 68 percentile obtained from the same method used in Section 4.1. In ad￾dition to the fiducial model, six models wi…
Figure 7
Figure 7. Figure 7: Comparison of normalized rest-frame UV-to-MIR SED of input stellar models. We find no significant differ￾ence between continuous and bursty SFH models of 4 Myr and also between the stellar age of 4 Myr and 10 Myr. We assumed log nH,c/cm−3 = 3.0 and log U = −2.0 for all…

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Reference graph

Works this paper leans on

128 extracted references · 7 canonical work pages · cited by 1 Pith paper

  1. [1]

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

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    " id="W5M0MpCehiHzreSzNTczkc9d

    thebibliography [1] 20pt to REFERENCES 6pt =0pt -12pt 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 E...

    2021

  4. [4]

    L., Coe , D., et al

    Abdurro'uf , Larson , R. L., Coe , D., et al. 2024, , 973, 47, 10.3847/1538-4357/ad6001

    doi:10.3847/1538-4357/ad6001 2024

  5. [5]

    P., Ferland , G

    Abel , N. P., Ferland , G. J., Shaw , G., & van Hoof , P. A. M. 2005, , 161, 65, 10.1086/432913

    doi:10.1086/432913 2005

  6. [6]

    B., Fujimoto , S., Finlator , K., et al

    Akins , H. B., Fujimoto , S., Finlator , K., et al. 2022, , 934, 64, 10.3847/1538-4357/ac795b

    doi:10.3847/1538-4357/ac795b 2022

  7. [7]

    Algera , H. S. B., Inami , H., Oesch , P. A., et al. 2023, , 518, 6142, 10.1093/mnras/stac3195

    doi:10.1093/mnras/stac3195 2023

  8. [8]

    Algera , H. S. B., Inami , H., Sommovigo , L., et al. 2024 a , , 527, 6867, 10.1093/mnras/stad3111

    doi:10.1093/mnras/stad3111 2024

Show all 128 references
  1. [9]

    Algera , H. S. B., Inami , H., De Looze , I., et al. 2024 b , , 533, 3098, 10.1093/mnras/stae1994

    2024 doi

  2. [10]

    2020, , 498, 5541, 10.1093/mnras/staa2809

    Arata , S., Yajima , H., Nagamine , K., Abe , M., & Khochfar , S. 2020, , 498, 5541, 10.1093/mnras/staa2809

    2020 doi

  3. [11]

    P., Tollerud , E

    Astropy Collaboration , Robitaille , T. P., Tollerud , E. J., et al. 2013, , 558, A33, 10.1051/0004-6361/201322068

    2013 doi

  4. [12]

    M., Sip o cz , B

    Astropy Collaboration , Price-Whelan , A. M., Sip o cz , B. M., et al. 2018, , 156, 123, 10.3847/1538-3881/aabc4f

    2018 doi

  5. [13]

    M., Lim , P

    Astropy Collaboration , Price-Whelan , A. M., Lim , P. L., et al. 2022, , 935, 167, 10.3847/1538-4357/ac7c74

    2022 doi

  6. [14]

    Bakx , T. J. L. C., Tamura , Y., Hashimoto , T., et al. 2020, , 493, 4294, 10.1093/mnras/staa509

    2020 doi

  7. [15]

    Bakx , T. J. L. C., Sommovigo , L., Carniani , S., et al. 2021, , 508, L58, 10.1093/mnrasl/slab104

    2021 doi

  8. [16]

    Bakx , T. J. L. C., Algera , H. S. B., Venemans , B., et al. 2024, , 532, 2270, 10.1093/mnras/stae1613

    2024 doi

  9. [17]

    E., Rozas , M., Zurita , A., Watson , R

    Beckman , J. E., Rozas , M., Zurita , A., Watson , R. A., & Knapen , J. H. 2000, , 119, 2728, 10.1086/301380

    2000 doi

  10. [18]

    H., Hearin , A

    Behroozi , P., Wechsler , R. H., Hearin , A. P., & Conroy , C. 2019, , 488, 3143, 10.1093/mnras/stz1182

    2019 doi

  11. [19]

    J., Smit , R., Schouws , S., et al

    Bouwens , R. J., Smit , R., Schouws , S., et al. 2022, , 931, 160, 10.3847/1538-4357/ac5a4a

    2022 doi

  12. [20]

    Bowler , R. A. A., Inami , H., Sommovigo , L., et al. 2024, , 527, 5808, 10.1093/mnras/stad3578

    2024 doi

  13. [21]

    J., Saxena , A., Cameron , A

    Bunker , A. J., Saxena , A., Cameron , A. J., et al. 2023, , 677, A88, 10.1051/0004-6361/202346159

    2023 doi

  14. [22]

    C., et al

    Calzetti , D., Armus , L., Bohlin , R. C., et al. 2000, , 533, 682, 10.1086/308692

    2000 doi

  15. [23]

    J., Saxena , A., Bunker , A

    Cameron , A. J., Saxena , A., Bunker , A. J., et al. 2023, , 677, A115, 10.1051/0004-6361/202346107

    2023 doi

  16. [24]

    C., McLure , R

    Carnall , A. C., McLure , R. J., Dunlop , J. S., & Dav \'e , R. 2018, , 480, 4379, 10.1093/mnras/sty2169

    2018 doi

  17. [25]

    2020, , 499, 5136, 10.1093/mnras/staa3178

    Carniani , S., Ferrara , A., Maiolino , R., et al. 2020, , 499, 5136, 10.1093/mnras/staa3178

    2020 doi

  18. [26]

    2024, , 633, 318, 10.1038/s41586-024-07860-9

    Carniani , S., Hainline , K., D'Eugenio , F., et al. 2024, , 633, 318, 10.1038/s41586-024-07860-9

    2024 doi

  19. [27]

    2024, , 972, 143, 10.3847/1538-4357/ad5f88

    Castellano , M., Napolitano , L., Fontana , A., et al. 2024, , 972, 143, 10.3847/1538-4357/ad5f88

    2024 doi

  20. [28]

    C., Lebouteiller , V., et al

    Cormier , D., Madden , S. C., Lebouteiller , V., et al. 2015, , 578, A53, 10.1051/0004-6361/201425207

    2015 doi

  21. [29]

    P., Hony , S., et al

    Cormier , D., Abel , N. P., Hony , S., et al. 2019, , 626, A23, 10.1051/0004-6361/201834457

    2019 doi

  22. [30]

    2023, Nature Astronomy, 7, 622, 10.1038/s41550-023-01918-w

    Curtis-Lake , E., Carniani , S., Cameron , A., et al. 2023, Nature Astronomy, 7, 622, 10.1038/s41550-023-01918-w

    2023 doi

  23. [31]

    J., Cortese , L., & Fritz , J

    De Looze , I., Baes , M., Bendo , G. J., Cortese , L., & Fritz , J. 2011, , 416, 2712, 10.1111/j.1365-2966.2011.19223.x

    2011

  24. [32]

    2014, , 568, A62, 10.1051/0004-6361/201322489

    De Looze , I., Cormier , D., Lebouteiller , V., et al. 2014, , 568, A62, 10.1051/0004-6361/201322489

    2014 doi

  25. [33]

    S., Asada , Y., et al

    Desprez , G., Martis , N. S., Asada , Y., et al. 2024, , 530, 2935, 10.1093/mnras/stae1084

    2024 doi

  26. [34]

    2017, , 846, 32, 10.3847/1538-4357/aa81d7

    D \' az-Santos , T., Armus , L., Charmandaris , V., et al. 2017, , 846, 32, 10.3847/1538-4357/aa81d7

    2017 doi

  27. [35]

    A., Fischera , J., Sutherland , R

    Dopita , M. A., Fischera , J., Sutherland , R. S., et al. 2006, , 167, 177, 10.1086/508261

    2006 doi

  28. [36]

    Draine , B. T. 2011, Physics of the Interstellar and Intergalactic Medium

    2011

  29. [37]

    J., & Stanway , E

    Eldridge , J. J., & Stanway , E. R. 2016, , 462, 3302, 10.1093/mnras/stw1772

    2016 doi

  30. [38]

    J., Chatzikos , M., Guzm \'a n , F., et al

    Ferland , G. J., Chatzikos , M., Guzm \'a n , F., et al. 2017, , 53, 385. 1705.10877

    2017 arXiv

  31. [39]

    M., Genzel , R., Lutz , D., Kunze , D., & Sternberg , A

    F \"o rster Schreiber , N. M., Genzel , R., Lutz , D., Kunze , D., & Sternberg , A. 2001, , 552, 544, 10.1086/320546

    2001 doi

  32. [40]

    K., & Sugahara , Y

    Fudamoto , Y., Inoue , A. K., & Sugahara , Y. 2023, , 521, 2962, 10.1093/mnras/stad743

    2023 doi

  33. [41]

    A., Schouws , S., et al

    Fudamoto , Y., Oesch , P. A., Schouws , S., et al. 2021, , 597, 489, 10.1038/s41586-021-03846-z

    2021 doi

  34. [42]

    2024, , 964, 146, 10.3847/1538-4357/ad235c

    Fujimoto , S., Ouchi , M., Nakajima , K., et al. 2024, , 964, 146, 10.3847/1538-4357/ad235c

    2024 doi

  35. [43]

    J., & Scott , P

    Grevesse , N., Asplund , M., Sauval , A. J., & Scott , P. 2010, , 328, 179, 10.1007/s10509-010-0288-z

    2010 doi

  36. [44]

    A., Dopita , M

    Groves , B. A., Dopita , M. A., & Sutherland , R. S. 2004, , 153, 9, 10.1086/421113

    2004 doi

  37. [45]

    2024, , 960, 56, 10.3847/1538-4357/ad0b7e

    Harikane , Y., Nakajima , K., Ouchi , M., et al. 2024, , 960, 56, 10.3847/1538-4357/ad0b7e

    2024 doi

  38. [46]

    K., et al

    Harikane , Y., Ouchi , M., Inoue , A. K., et al. 2020, , 896, 93, 10.3847/1538-4357/ab94bd

    2020 doi

  39. [47]

    R., Millman, K

    Harris, C. R., Millman, K. J., van der Walt, S. J., et al. 2020, Nature, 585, 357, 10.1038/s41586-020-2649-2

    2020 doi

  40. [48]

    S., et al

    Harshan , A., Tripodi , R., Martis , N. S., et al. 2024, , 977, L36, 10.3847/2041-8213/ad9741

    2024 doi

  41. [49]

    K., Tamura , Y., et al

    Hashimoto , T., Inoue , A. K., Tamura , Y., et al. 2019 a , , 71, 109, 10.1093/pasj/psz094

    2019 doi

  42. [50]

    2018, , 557, 392, 10.1038/s41586-018-0117-z

    Hashimoto , T., Laporte , N., Mawatari , K., et al. 2018, , 557, 392, 10.1038/s41586-018-0117-z

    2018 doi

  43. [51]

    K., Mawatari , K., et al

    Hashimoto , T., Inoue , A. K., Mawatari , K., et al. 2019 b , , 71, 71, 10.1093/pasj/psz049

    2019 doi

  44. [52]

    2023, , 955, L2, 10.3847/2041-8213/acf57c

    Hashimoto , T., \'A lvarez-M \'a rquez , J., Fudamoto , Y., et al. 2023, , 955, L2, 10.3847/2041-8213/acf57c

    2023 doi

  45. [53]

    D., Wolfire , M

    Herrera-Camus , R., Bolatto , A. D., Wolfire , M. G., et al. 2015, , 800, 1, 10.1088/0004-637X/800/1/1

    2015 doi

  46. [54]

    2018, , 861, 94, 10.3847/1538-4357/aac0f6

    Herrera-Camus , R., Sturm , E., Graci \'a -Carpio , J., et al. 2018, , 861, 94, 10.3847/1538-4357/aac0f6

    2018 doi

  47. [55]

    2025, arXiv e-prints, arXiv:2505.06340

    Herrera-Camus , R., Gonz \'a lez-L \'o pez , J., F \"o rster Schreiber , N., et al. 2025, arXiv e-prints, arXiv:2505.06340. 2505.06340

    2025 arXiv

  48. [56]

    J., & Tielens , A

    Hollenbach , D. J., & Tielens , A. G. G. M. 1999, Reviews of Modern Physics, 71, 173, 10.1103/RevModPhys.71.173

    1999 doi

  49. [57]

    2016, Journal of Open Research Software, 5, 10.5334/jors.148

    Hoyer, S., & Hamman, J. 2016, Journal of Open Research Software, 5, 10.5334/jors.148

    2016 doi

  50. [58]

    H., Schloerb , F

    Hughes , D. H., Schloerb , F. P., Aretxaga , I., et al. 2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 11445, Ground-based and Airborne Telescopes VIII, ed. H. K. Marshall , J. Spyromilio , & T. Usuda , 1144522, 10.1117/12.2561893

    2020 doi

  51. [59]

    Hunter, J. D. 2007, Computing in Science & Engineering, 9, 90, 10.1109/MCSE.2007.55

    2007 doi

  52. [60]

    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

  53. [61]

    Inami , H., Algera , H. S. B., Schouws , S., et al. 2022, , 515, 3126, 10.1093/mnras/stac1779

    2022 doi

  54. [62]

    R., Oka , T., & McCall , B

    Indriolo , N., Geballe , T. R., Oka , T., & McCall , B. J. 2007, , 671, 1736, 10.1086/523036

    2007 doi

  55. [63]

    2015, , 815, 18, 10.1088/0004-637X/815/1/18

    Infante , L., Zheng , W., Laporte , N., et al. 2015, , 815, 18, 10.1088/0004-637X/815/1/18

    2015 doi

  56. [64]

    K., Shimizu , I., Tamura , Y., et al

    Inoue , A. K., Shimizu , I., Tamura , Y., et al. 2014, , 780, L18, 10.1088/2041-8205/780/2/L18

    2014 doi

  57. [65]

    K., Tamura , Y., Matsuo , H., et al

    Inoue , A. K., Tamura , Y., Matsuo , H., et al. 2016, Science, 352, 1559, 10.1126/science.aaf0714

    2016 doi

  58. [66]

    G., Gawiser , E., Faber , S

    Iyer , K. G., Gawiser , E., Faber , S. M., et al. 2019, , 879, 116, 10.3847/1538-4357/ab2052

    2019 doi

  59. [67]

    I., Stasi \'n ska , G., Meynet , G., Guseva , N

    Izotov , Y. I., Stasi \'n ska , G., Meynet , G., Guseva , N. G., & Thuan , T. X. 2006, , 448, 955, 10.1051/0004-6361:20053763

    2006 doi

  60. [68]

    C., Witstok , J., Concas , A., & Laporte , N

    Jones , G. C., Witstok , J., Concas , A., & Laporte , N. 2024 a , , 529, L1, 10.1093/mnrasl/slad189

    2024 doi

  61. [69]

    C., \"U bler , H., Perna , M., et al

    Jones , G. C., \"U bler , H., Perna , M., et al. 2024 b , , 682, A122, 10.1051/0004-6361/202347838

    2024 doi

  62. [70]

    2023, , 951, L17, 10.3847/2041-8213/acd938

    Jones , T., Sanders , R., Chen , Y., et al. 2023, , 951, L17, 10.3847/2041-8213/acd938

    2023 doi

  63. [71]

    2022, , 510, 5603, 10.1093/mnras/stac028

    Katz , H., Rosdahl , J., Kimm , T., et al. 2022, , 510, 5603, 10.1093/mnras/stac028

    2022 doi

  64. [72]

    2016, , 819, 114, 10.3847/0004-637X/819/2/114

    Kawamata , R., Oguri , M., Ishigaki , M., Shimasaku , K., & Ouchi , M. 2016, , 819, 114, 10.3847/0004-637X/819/2/114

    2016 doi

  65. [73]

    J., & Dopita , M

    Kewley , L. J., & Dopita , M. A. 2002, , 142, 35, 10.1086/341326

    2002 doi

  66. [74]

    J., Nicholls , D

    Kewley , L. J., Nicholls , D. C., & Sutherland , R. S. 2019, , 57, 511, 10.1146/annurev-astro-081817-051832

    2019 doi

  67. [75]

    2023, , 521, 2526, 10.1093/mnras/stad687

    Killi , M., Watson , D., Fujimoto , S., et al. 2023, , 521, 2526, 10.1093/mnras/stad687

    2023 doi

  68. [76]

    2001, , 549, 979, 10.1086/319447

    Kim , K.-T., & Koo , B.-C. 2001, , 549, 979, 10.1086/319447

    2001 doi

  69. [77]

    2024, , 529, 781, 10.1093/mnras/stae252

    Kumari , N., Smit , R., Leitherer , C., et al. 2024, , 529, 781, 10.1093/mnras/stae252

    2024 doi

  70. [78]

    2005, in Massive Star Birth: A Crossroads of Astrophysics, ed

    Kurtz , S. 2005, in Massive Star Birth: A Crossroads of Astrophysics, ed. R. Cesaroni , M. Felli , E. Churchwell , & M. Walmsley , Vol. 227, 111--119, 10.1017/S1743921305004424

    2005 doi

  71. [79]

    2015, , 575, A92, 10.1051/0004-6361/201425040

    Laporte , N., Streblyanska , A., Kim , S., et al. 2015, , 575, A92, 10.1051/0004-6361/201425040

    2015 doi

  72. [80]

    S., et al

    Laporte , N., Katz , H., Ellis , R. S., et al. 2019, , 487, L81, 10.1093/mnrasl/slz094

    2019 doi

  73. [81]

    2020, , 643, A1, 10.1051/0004-6361/201936965

    Le F \`e vre , O., B \'e thermin , M., Faisst , A., et al. 2020, , 643, A1, 10.1051/0004-6361/201936965

    2020 doi

  74. [82]

    2024, , 528, 499, 10.1093/mnras/stad3792

    Liang , L., Feldmann , R., Murray , N., et al. 2024, , 528, 499, 10.1093/mnras/stad3792

    2024 doi

  75. [83]

    Luridiana , V., Morisset , C., & Shaw , R. A. 2015, , 573, A42, 10.1051/0004-6361/201323152

    2015 doi

  76. [84]

    2024, , 975, 87, 10.3847/1538-4357/ad7b32

    Ma , Z., Sun , B., Cheng , C., et al. 2024, , 975, 87, 10.3847/1538-4357/ad7b32

    2024 doi

  77. [85]

    2014, , 52, 415, 10.1146/annurev-astro-081811-125615

    Madau , P., & Dickinson , M. 2014, , 52, 415, 10.1146/annurev-astro-081811-125615

    2014 doi

  78. [86]

    C., R \'e my-Ruyer , A., Galametz , M., et al

    Madden , S. C., R \'e my-Ruyer , A., Galametz , M., et al. 2013, , 125, 600, 10.1086/671138

    2013 doi

  79. [87]

    2023, , 679, A12, 10.1051/0004-6361/202346723

    Markov , V., Gallerani , S., Pallottini , A., et al. 2023, , 679, A12, 10.1051/0004-6361/202346723

    2023 doi

  80. [88]

    P., Spilker , J

    Marrone , D. P., Spilker , J. S., Hayward , C. C., et al. 2018, , 553, 51, 10.1038/nature24629

    2018 doi

  81. [89]

    2009, in Astronomical Society of the Pacific Conference Series, Vol

    Matsuo , H., Arai , T., Nitta , T., & Kosaka , A. 2009, in Astronomical Society of the Pacific Conference Series, Vol. 418, AKARI, a Light to Illuminate the Misty Universe, ed. T. Onaka , G. J. White , T. Nakagawa , & I. Yamamura , 451

    2009

  82. [90]

    2002, , 382, 610, 10.1051/0004-6361:20011611

    Mizutani , M., Onaka , T., & Shibai , H. 2002, , 382, 610, 10.1051/0004-6361:20011611

    2002 doi

  83. [91]

    2023, , 947, L24, 10.3847/2041-8213/acb99e

    Morishita , T., Roberts-Borsani , G., Treu , T., et al. 2023, , 947, L24, 10.3847/2041-8213/acb99e

    2023 doi

  84. [92]

    2011, , 526, A149, 10.1051/0004-6361/201015471

    Nagao , T., Maiolino , R., Marconi , A., & Matsuhara , H. 2011, , 526, A149, 10.1051/0004-6361/201015471

    2011 doi

  85. [93]

    P., Tacchella , S., Mason , C

    Naidu , R. P., Tacchella , S., Mason , C. A., et al. 2020, , 892, 109, 10.3847/1538-4357/ab7cc9

    2020 doi

  86. [94]

    2014, , 442, 900, 10.1093/mnras/stu902

    Nakajima , K., & Ouchi , M. 2014, , 442, 900, 10.1093/mnras/stu902

    2014 doi

  87. [95]

    2024, , 967, 28, 10.3847/1538-4357/ad38c2

    Nakane , M., Ouchi , M., Nakajima , K., et al. 2024, , 967, 28, 10.3847/1538-4357/ad38c2

    2024 doi

  88. [96]

    C., Kewley , L

    Nicholls , D. C., Kewley , L. J., & Sutherland , R. S. 2020, , 132, 033001, 10.1088/1538-3873/ab6818

    2020 doi

  89. [97]

    T., Schimek , A., Cicone , C., Decataldo , D., & Shen , S

    Nyhagen , C. T., Schimek , A., Cicone , C., Decataldo , D., & Shen , S. 2024, arXiv e-prints, arXiv:2410.18471, 10.48550/arXiv.2410.18471

    2024 doi

  90. [98]

    E., & Ferland , G

    Osterbrock , D. E., & Ferland , G. J. 2006, Astrophysics of gaseous nebulae and active galactic nuclei

    2006

  91. [99]

    2020, , 641, A6, 10.1051/0004-6361/201833910

    Planck Collaboration VI . 2020, , 641, A6, 10.1051/0004-6361/201833910

    2020 doi

  92. [100]

    2022, , 667, A35, 10.1051/0004-6361/202243866

    Ramambason , L., Lebouteiller , V., Bik , A., et al. 2022, , 667, A35, 10.1051/0004-6361/202243866

    2022 doi

  93. [101]

    R., & Rieke , G

    Rigby , J. R., & Rieke , G. H. 2004, , 606, 237, 10.1086/382776

    2004 doi

  94. [102]

    2022, , 665, L4, 10.1051/0004-6361/202244556

    Schaerer , D., Marques-Chaves , R., Barrufet , L., et al. 2022, , 665, L4, 10.1051/0004-6361/202244556

    2022 doi

  95. [103]

    2020, , 643, A3, 10.1051/0004-6361/202037617

    Schaerer , D., Ginolfi , M., B \'e thermin , M., et al. 2020, , 643, A3, 10.1051/0004-6361/202037617

    2020 doi

  96. [104]

    2024, , 687, L10, 10.1051/0004-6361/202449903

    Schimek , A., Cicone , C., Shen , S., et al. 2024, , 687, L10, 10.1051/0004-6361/202449903

    2024 doi

  97. [105]

    J., Westmoquette , M

    Smith , L. J., Westmoquette , M. S., Gallagher , J. S., et al. 2006, , 370, 513, 10.1111/j.1365-2966.2006.10507.x

    2006

  98. [106]

    2022, , 513, 3122, 10.1093/mnras/stac302

    Sommovigo , L., Ferrara , A., Pallottini , A., et al. 2022, , 513, 3122, 10.1093/mnras/stac302

    2022 doi

  99. [107]

    R., Eldridge , J

    Stanway , E. R., Eldridge , J. J., & Becker , G. D. 2016, , 456, 485, 10.1093/mnras/stv2661

    2016 doi

  100. [108]

    K., Fudamoto , Y., et al

    Sugahara , Y., Inoue , A. K., Fudamoto , Y., et al. 2022, , 935, 119, 10.3847/1538-4357/ac7fed

    2022 doi

  101. [109]

    K., Hashimoto , T., et al

    Sugahara , Y., Inoue , A. K., Hashimoto , T., et al. 2021, , 923, 5, 10.3847/1538-4357/ac2a36

    2021 doi

  102. [110]

    2025, , 981, 135, 10.3847/1538-4357/adb02a

    Sugahara , Y., \'A lvarez-M \'a rquez , J., Hashimoto , T., et al. 2025, , 981, 135, 10.3847/1538-4357/adb02a

    2025 doi

  103. [111]

    2022, , 74, L9, 10.1093/pasj/psac018

    Tadaki , K.-i., Tsujita , A., Tamura , Y., et al. 2022, , 74, L9, 10.1093/pasj/psac018

    2022 doi

  104. [112]

    1987, , 99, 832, 10.1086/132043

    Takami , H., Maihara , T., Mizutani , K., et al. 1987, , 99, 832, 10.1086/132043

    1987 doi

  105. [113]

    2019, , 874, 27, 10.3847/1538-4357/ab0374

    Tamura , Y., Mawatari , K., Hashimoto , T., et al. 2019, , 874, 27, 10.3847/1538-4357/ab0374

    2019 doi

  106. [114]

    Bakx , T

    Tamura , Y., C. Bakx , T. J. L., Inoue , A. K., et al. 2023, , 952, 9, 10.3847/1538-4357/acd637

    2023 doi

  107. [115]

    2024, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Tamura , Y., Sakai , T., Kawabe , R., et al. 2024, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 13102, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, ed. J. Zmuidzinas & J.-R. Gao , 131020G, 10.1117/12.3017788

    2024 doi

  108. [116]

    2024, , 971, 124, 10.3847/1538-4357/ad554e

    Umeda , H., Ouchi , M., Nakajima , K., et al. 2024, , 971, 124, 10.3847/1538-4357/ad554e

    2024 doi

  109. [117]

    K., et al

    Ura , R., Hashimoto , T., Inoue , A. K., et al. 2023, , 948, 3, 10.3847/1538-4357/acc530

    2023 doi

  110. [118]

    S., Thompson , M

    Urquhart , J. S., Thompson , M. A., Moore , T. J. T., et al. 2013, , 435, 400, 10.1093/mnras/stt1310

    2013 doi

  111. [119]

    2021, , 505, 5543, 10.1093/mnras/stab1674

    Vallini , L., Ferrara , A., Pallottini , A., Carniani , S., & Gallerani , S. 2021, , 505, 5543, 10.1093/mnras/stab1674

    2021 doi

  112. [120]

    E., et al

    Virtanen , P., Gommers , R., Oliphant , T. E., et al. 2020, Nature Methods, 17, 261, 10.1038/s41592-019-0686-2

    2020 doi

  113. [121]

    2018, , 869, L22, 10.3847/2041-8213/aaf4fa

    Walter , F., Riechers , D., Novak , M., et al. 2018, , 869, L22, 10.3847/2041-8213/aaf4fa

    2018 doi

  114. [122]

    2010, in P roceedings of the 9th P ython in S cience C onference, ed

    W es M c K inney. 2010, in P roceedings of the 9th P ython in S cience C onference, ed. S t\'efan van der W alt & J arrod M illman, 56 -- 61, 10.25080/Majora-92bf1922-00a

    2010 doi

  115. [123]

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

    Willott , C. J., Doyon , R., Albert , L., et al. 2022, , 134, 025002, 10.1088/1538-3873/ac5158

    2022 doi

  116. [124]

    A., Cohen , S

    Windhorst , R. A., Cohen , S. H., Jansen , R. A., et al. 2023, , 165, 13, 10.3847/1538-3881/aca163

    2023 doi

  117. [125]

    2022, , 515, 1751, 10.1093/mnras/stac1905

    Witstok , J., Smit , R., Maiolino , R., et al. 2022, , 515, 1751, 10.1093/mnras/stac1905

    2022 doi

  118. [126]

    G., Vallini , L., & Chevance , M

    Wolfire , M. G., Vallini , L., & Chevance , M. 2022, , 60, 247, 10.1146/annurev-astro-052920-010254

    2022 doi

  119. [127]

    A., Casey , C

    Zavala , J. A., Casey , C. M., Manning , S. M., et al. 2021, , 909, 165, 10.3847/1538-4357/abdb27

    2021 doi

  120. [128]

    A., Castellano , M., Akins , H

    Zavala , J. A., Castellano , M., Akins , H. B., et al. 2024, Nature Astronomy, 10.1038/s41550-024-02397-3

    2024 doi

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