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Observing Co-Located Neutral and Ionized Gas-Phase Iron Depletion in the Magellanic Clouds

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Pith's one-line read By comparing ultraviolet absorption through neutral gas with emission-line abundances in six neighboring H II regions in the Magellanic Clouds, this paper shows gas-phase iron is 0.3–2 dex lower in the ionized gas and attributes the…

desk verdict A genuinely new parsec-scale neutral/ionized Fe comparison in the Magellanic Clouds, with solid new column densities and honest treatment of systematics; the main caveat is the untested co-location assumption, which could inflate the headline offset. read the letter →

arxiv 2608.12557 v1 pith:GMOWQIJ5 submitted 2026-08-12 astro-ph.GA

Yun Qi Li , Jessica K. Werk , Caleb R. Choban , Julia Roman-Duval , Kirill Tchernyshyov , J. Xavier Prochaska , Doyeon A. Kim , Arianna S. Long This is my paper · ORCID
classification astro-ph.GA
keywords interstellardustgas-phaseabundancesirondepletionHIIregionsMagellanicCloudsultravioletspectroscopygrainsurvivalISMphases
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 asks whether dust grains survive the birth of massive stars. It measures gas-phase sulfur and iron in neutral interstellar gas along 33 ultraviolet sightlines in the Magellanic Clouds and compares them with the same elements in six adjacent H II regions, the ionized bubbles carved out by young stars. Sulfur matches between the two phases, but iron is 0.3 to 2 dex (roughly 2 to 100 times) less abundant in the H II gas. The authors argue this deficit is iron that has been accreted onto dust grains in the dense molecular clouds that preceded star formation, and that those iron-bearing grains are not destroyed during the first few million years after ionization. If correct, H II region iron depletion becomes a practical probe of dust in molecular clouds, where direct UV absorption measurements are difficult.

What carries the argument

The load-bearing comparison is the neutral-to-ionized pair: 33 Magellanic Cloud sightlines observed with HST/COS and HST/STIS, each within about 3 arcminutes (~50 pc) of one of six H II regions (ionized hydrogen bubbles around young hot stars). Neutral gas abundances of S and Fe are derived from Voigt-profile fits to UV absorption lines of S II and Fe II, with atomic hydrogen column densities from Ly-α fitting; the H II region values are adopted from optical emission-line studies, including Fe ionization corrections based on the O III/O II ratio. The measured quantity that carries the argument is the gas-phase Fe abundance offset, expressed as the fraction of Fe locked in dust, between the two phases.

What would settle it

Measure the 9.7 µm and 18 µm silicate absorption features toward the stars inside the H II regions and compare the inferred silicate column with what the gas-phase Fe deficit implies; if iron is genuinely locked in surviving grains, the silicate optical depth should be enhanced, not matched to the diffuse ISM dust-to-gas ratio, and a null result would indicate the Fe offset is an artifact of ionization corrections or sightline geometry.

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Extended reading notes

Core claim

The central discovery is that gas-phase iron abundances in H II regions can be lower than those of co-located neutral gas by 0.3 to 2 dex, while sulfur shows no such offset. The paper attributes the iron deficit to dust depletion: iron condensed onto grains in dense atomic or molecular clouds before star formation, and the grains survive destruction long enough that the ionized gas remains strongly depleted. It further shows that standard ionization corrections, sightline blending, and infall of metal-poor gas cannot explain the offset, and uses the measured neutral/ionized differences to place lower limits on the mixing timescale between H II regions and the diffuse ISM (~1–10 Myr) and upper limits on grain growth timescales in the precursor clouds (5–50 Myr for the adopted cloud lifetimes).

Load-bearing premise

The claim rests on assuming that neutral gas seen within about 50 parsecs of an H II region shares the same dust content as the gas that actually gave birth to that H II region; if dustiness varies by even a factor of three on that scale, the apparent iron deficit could be a mismatch of locations rather than surviving grains.

Editorial extensions

If this is right

  • If the offset is real, H II region Fe depletion can be used as a tracer of Fe depletion in dense molecular clouds, sidestepping the difficulty of UV absorption measurements through those clouds.
  • Fe-bearing grains must survive the harsh radiation and shocks inside H II regions for at least a few million years, so grain destruction in these environments is slower than the H II region lifetime.
  • The measured neutral/ionized differences set a lower limit of about 1–10 Myr on the mixing timescale between H II region gas and the surrounding diffuse ISM.
  • Under the paper's assumed 10–20 Myr molecular cloud lifetimes, the required grain growth timescale is between 5 and 50 Myr, consistent with theoretical growth rates for metallic iron grains of standard and nanoparticle sizes.
  • The larger SMC offsets point to a lower baseline Fe depletion in the low-metallicity SMC neutral ISM, and widening the sample beyond the single sightlines now available for three SMC regions could sharpen the comparison.

Reading between the lines

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

  • A direct consequence the paper does not draw fully: infrared spectroscopy of the 9.7 and 18 µm silicate features toward H II region stars should reveal silicate optical depths larger than expected from diffuse-ISM dust-to-gas ratios, because the depleted iron must reside in grains; this is a testable prediction of the dust-survival picture.
  • Better Fe ionization corrections—for example by directly detecting Fe IV in more H II regions—would likely increase the reported offsets rather than erase them, since the adopted ICFs tend to overestimate total Fe abundance; until then, the 0.3–2 dex range should be read as a lower bound.
  • The co-location assumption can be stress-tested by observing many neutral sightlines at even smaller separations around a single region; if the Fe offset is caused by spatial mismatch, it would shrink as sightlines approach the ionized bubble, whereas dust survival predicts it should persist for sightlines actually passing through H II region gas.
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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

2 major / 4 minor

Summary. This paper presents new measurements of neutral gas-phase S and Fe abundances along 33 UV absorption sightlines in the Magellanic Clouds and compares them with literature emission-line abundances for six co-located H II regions. The authors find that S is broadly consistent between the phases, whereas gas-phase Fe in four of the six H II regions is lower than in the neighboring neutral ISM by roughly 0.3 to 2 dex. They argue that the offset reflects stronger dust depletion inherited from the precursor molecular clouds and that Fe-bearing grains survive destruction for the first few Myr in H II regions. The paper includes a Cloudy-based reassessment of Fe ionization correction factors, a discussion of alternative explanations (sightline blending, metal-poor infall), and order-of-magnitude estimates of mixing and grain-growth timescales.

Significance. If the central offset is robust, this is a valuable new observational constraint on dust destruction and survival in H II regions and provides an indirect probe of Fe depletion in dense molecular clouds, which are difficult to observe directly in UV absorption. The analysis benefits from a uniform re-measurement of all neutral-gas sightlines, cross-checks against earlier studies that agree within about 0.1 dex (Table 7), and an explicit Cloudy treatment of the main systematic, the ionization correction factors (Section 4.3). The comparison to CLASSY galaxies (James et al. 2026) places the result in a broader context. The main caveat is that the comparison relies on the assumption that neutral-gas sightlines within 3 arcminutes represent the precursor gas; this assumption is plausible but not yet quantitatively validated.

major comments (2)
  1. [Section 2.1.1, Figure 7, Table 5] The co-location assumption is load-bearing and currently untested. For SMC N66A, sightline A8 at 0.17 arcmin separation has 12+log(Fe/H)=5.49, only 0.23 dex above the adopted H II value of 5.26, while the mean of all 13 sightlines is 5.95, giving the quoted 0.69 dex offset. If neutral-gas Fe/H declines toward the H II region, the mean neutral baseline overestimates the precursor gas abundance and the offset is inflated. I request a quantitative test of a radial trend, for example a regression of 12+log(Fe/H) against projected separation, a jackknife excluding the innermost sightline, or a comparison of inner versus outer subsamples for N66A and N11B, together with a statement of how the quoted offsets change. With only one sightline each, N81, N88A, and N90 cannot constrain such a gradient, so the multi-sightline regions carry the weight of the claim.
  2. [Abstract and Section 5, Table 4] The headline range of 0.3 to 2 dex is not fully supported by the measured neutral-ionized comparison. For SMC N90, the H II Fe abundance is an upper limit (<4.68; Table 4) and only one neutral sightline is available (12+log(Fe/H)=6.07), so the offset is a lower limit of about 1.4 dex rather than a measured value of 2 dex; the upper end of the range appears to come from comparing with the SMC photospheric Fe abundance (6.89) rather than with the co-located neutral gas. Please quote the measured offsets and the lower limits separately, and avoid presenting the upper-limit-based value as part of the measured range.
minor comments (4)
  1. [Section 2.1.3] The treatment of molecular hydrogen for the 30 Doradus sightlines is internally inconsistent: the text states that H2 is "very likely present and not negligible" based on C I and C II detections, but then adopts log N(H2)=18.0±2.0 for all sightlines. Please clarify whether direct N(H2) constraints, such as the Welty et al. (2012) value for Brey 77, are used for the 30 Doradus targets, and quantify the resulting effect on 12+log(Fe/H) for those high-column sightlines.
  2. [General] General typographical cleanup is needed: "spacial" in Section 4.4, "traget" in the Figure 2 caption, and inconsistent spacing in "Hii region" throughout.
  3. [Figure 5 and Table 4] The N90 panel should be explicitly marked with an arrow or inequality sign in the figure, since the adopted H II value is an upper limit; as presented, the figure may be read as showing a measured abundance.
  4. [Section 4.7, Eq. (1)] Equation (1) is terse; please define f_Fe,gas(t) explicitly and state the assumed differential equation (df/dt = (f_HI - f)/tau_m) so that the integral and the resulting lower limits on the mixing timescale are unambiguous.

Circularity Check

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No significant circularity: the central neutral-versus-ionized Fe abundance offset is an independent comparison between new UV absorption measurements and literature emission-line abundances, and the interpretive timescale estimates are model-derived rather than fitted inputs.

full rationale

The central observational result—gas-phase Fe in H II regions can be lower than in co-located neutral gas—is a direct comparison of two independent datasets. Neutral gas S and Fe abundances are measured in this work from archival HST/COS and STIS spectra using Voigt profile and Ly-alpha fitting (Sections 2.1.2–2.1.3, Table 5). H II region S and Fe abundances are adopted from independent literature sources: Peimbert (2003), Toribio San Cipriano et al. (2017), Domínguez-Guzmán et al. (2022), and Rodríguez & Rubin (2005) (Section 2.2, Table 4). No parameter is fitted to the H II abundances and then used to predict them; the offset is read directly from the measurements. The grain-growth and mixing-timescale estimates in Sections 4.7–4.8 and Appendix B are interpretive integrations of the observed abundances under stated assumptions (initial depletion set equal to the surrounding diffuse ISM value, final depletion set equal to the H II region value), not independent predictions, so they do not constitute a fitted input called a prediction. The paper does cite prior work by overlapping authors (Jenkins & Wallerstein 2017; Roman-Duval et al. 2021) to characterize known neutral-ISM depletion variations, but the central offset does not reduce to those priors; it is measured from new column densities. The co-location assumption (sightline separation <3 arcminutes represents precursor gas) is a physical assumption that could affect the quantitative offset, but it is not a definitional or statistical circularity; it is a correctness and robustness concern. The paper also tests against an S abundance comparison and against independent Cloudy C25 ionization-correction modeling, which further demonstrates that the inference is not forced by its own inputs.

Assumptions & free parameters 1 free parameters · 7 assumptions · 0 invented entities

The paper's central observational result does not require many free parameters. The main adopted inputs are the co-location assumption, literature H II abundances with ICFs, and physical assumptions about grain growth and cloud lifetimes used for interpretive timescale estimates. The only hand-set parameter directly affecting the reported abundances is the Gaussian prior on unmeasured molecular hydrogen column densities.

free parameters (1)
  • log N(H2) prior parameters = mean 18.0, sigma 2.0 dex
    Chosen by hand for sightlines without H2 measurements (Section 2.1.3). Affects the N(H) denominator uncertainty and therefore the abundance error bars, but not the central values.
assumptions (7)
  • domain assumption Sightlines within 3 arcmin (<=50 pc) of an H II region trace gas with depletion representative of the region's precursor gas, and neutral ISM depletion varies slowly on this scale.
    Used to justify comparing neutral absorption and ionized emission measurements. The paper cites Jenkins (2009) and others for 100 pc-scale variations, but this is an adopted premise, not a measured property of the specific sightlines.
  • domain assumption H II region Fe abundances from the literature, including ionization correction factors (Eq. 2 of Rodríguez & Rubin 2005), are accurate enough to infer the offset.
    Four H II regions rely on model-based ICFs; the paper's Cloudy modeling suggests ICFs overestimate Fe, which would not erase the offset, but the literature abundances are adopted as input.
  • domain assumption The gas parcel that formed the H II region was initially chemically homogeneous with the surrounding diffuse neutral gas, so the observed neutral Fe depletion is the initial condition.
    Stated in Section 4.8; used to estimate grain growth timescales. This assumption directly enables the timescale derivation but is not required for the observed offset.
  • domain assumption Grain growth by accretion is negligible in H II region gas; sticking efficiency approaches zero at temperatures above ~1000 K.
    Quoted from Bossion et al. (2024); central to the conclusion that the missing Fe was depleted before star formation and later survived.
  • domain assumption Molecular cloud lifetimes are 10-20 Myr, and H II region ages are 1-3 Myr for the two regions used in the mixing timescale estimate.
    Adopted from Hartmann et al. (2001), Vázquez-Semadeni et al. (2007), Walborn et al. (1999), and Heydari-Malayeri & Selier (2010). These ages set the derived timescale limits.
  • domain assumption Photospheric Fe abundances for the SMC (6.89) and LMC (7.32) from Tchernyshyov et al. (2015) represent the total (gas + dust) Fe reservoir.
    Used to convert gas-phase abundances into depletion fractions (Figures 6 and Tables 8-10). If these are systematically off, the depletion fractions shift, though the neutral/ionized offset is unaffected.
  • standard math Standard Bayesian statistical methods used for computing means and intrinsic spreads (Ivezić et al. 2014) are valid for this dataset.
    Section 3.1 applies their Section 5.6 scheme; a standard statistical treatment.

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Pith. "Pith review of Observing Co-Located Neutral and Ionized Gas-Phase Iron Depletion in the Magellanic Clouds." pith.science (2026). https://pith.science/paper/GMOWQIJ5

@misc{pith2026260812557,
  author       = {Pith},
  title        = {Pith review of: Observing Co-Located Neutral and Ionized Gas-Phase Iron Depletion in the Magellanic Clouds},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/GMOWQIJ5}},
  note         = {Machine review of arXiv:2608.12557}
}
abstract

Depletion is the observed phenomenon where gas-phase elemental abundances are reduced through accretion onto dust grains. We measure neutral gas-phase elemental abundances (S, Fe) in the Magellanic Clouds along 33 sightlines using high-resolution UV spectroscopy (HST/COS and HST/STIS), and compare them to ionized gas-phase abundances (S, Fe) adopted from the literature for six co-located H\,\textsc{ii} regions (with the furthest separation of $\lesssim3'$, 50 pc). Comparing S abundances show that S is minimally depleted in the H\,\textsc{ii} regions and surrounding diffuse ISM. However, we find that the gas-phase Fe abundances in H\,\textsc{ii} regions can be lower than those of the neighboring neutral ISM by 0.3 to 2 dex. This difference is likely an offset in the amount of Fe depleted into dust grains. As accretion of gas-phase Fe is likely not effective at the temperatures of the H\,\textsc{ii} regions, Fe depletion into solid form would have occurred in the dense atomic or molecular clouds prior to star formation. Stronger depletion in the H\,\textsc{ii} regions shows that Fe-bearing grains survive destruction in the first few million years following ionization. Our observations highlight that Fe depletion in H\,\textsc{ii} regions can be a useful tracer of Fe depletion in dense molecular clouds, which are challenging to observe directly via UV absorption.

Figures

Figures reproduced from arXiv: 2608.12557 by the authors.

Figure 1
Figure 1. The location of H ii regions and sightlines included in this study relative to the Small Magellanic Cloud (SMC) and the Large Magellanic Cloud (LMC). The Australia Telescope Compact Array (ATCA) and Parkes HI survey peak 21 cm brightness temperature images (Stanimirovic et al. 1999; Kim et al. 2003) are shown in grayscale, while the Southern H𝛼 Sky Survey Atlas (SHASSA) (Gaustad et al. 2001) images are shown in purp… view at source ↗
Figure 2
Figure 2. Examples of Voigt profile fitting for the Fe and S lines in this work. The Fe ii 𝜆𝜆𝜆 1142, 1143, 1144 Å and the S ii 𝜆𝜆 1250, 1253 Å lines are measured in the COS spectra for LMC target BAT 99 114 (corresponding to 30 Doradus) and SMC target 2dFS 3694 (corresponding to SMC N88A). The Fe ii (𝜆𝜆 1608, 1611, 2249, 2260 Å) and the S ii 𝜆𝜆 1250, 1253 Å lines are measured in the STIS spectra for LMC target BI 42 (PGMW 322… view at source ↗
Figure 3
Figure 3. Fitting two convolved Lorentzian profiles to the Ly𝛼 absorption feature, using the SMC sightline SK 80 as an example. The linear continuum is shown in the solid yellow line. The parameters for the linear continuum fit are found by performing a least squares polynomial fit to the cyan regions of the spectra. The velocities to the Milky Way and the SMC/LMC components are estimated from fitting Voigt profiles to the S … view at source ↗
Figures from the paper (9 more)
Figure 4
Figure 4. Figure 4: A side-by-side comparison of 12 + log(S/H) in neutral gas and adjacent H ii regions. The two left panels show the LMC H ii regions, while the four right panels show the SMC H ii regions. The left column of each panel shows the literature H ii S region abundance detaile…
Figure 5
Figure 5. Figure 5: A side-by-side comparison of 12 + log(Fe/H) in neutral gas and adjacent H ii regions. The two left panels show the LMC H ii regions, while the four right panels show the SMC H ii regions. As in the previous Figure for S, the left column of each panel shows the adopted …
Figure 6
Figure 6. Figure 6: A side-by-side comparison of the fraction of Fe depleted into dust in neutral gas and adjacent H ii regions. The two left panels show the LMC H ii regions, while the four right panels show the SMC H ii regions. The left and right columns respectively show the percentag…
Figure 7
Figure 7. Figure 7: The spatial location of the SMC sightlines relative to the H ii regions. The large top panel shows the compact H ii region SMC N66A and neutral gas sightlines toward targets in the associated open cluster NGC 346. The bottom three panels show three H ii region slits ea…
Figure 8
Figure 8. Figure 8: The spacial location of the LMC sightlines relative to 30 Doradus. Sightlines are indicated by squares (standard) and circles (where necessary to avoid obstructing data features). The slit is indicated by the rectangle. The large numbers within the squares or pointed a…
Figure 9
Figure 9. Figure 9: The spacial location of the LMC sightlines relative to LMC N11B. Sightlines are indicated by squares. The slit is indicated by the rectangle. The large numbers within the squares denote the 12 + log(Fe/H), while the uncertainty and the sightline ID are respectively lab…
Figure 10
Figure 10. Figure 10: log(Fe/Fe iii), or log ICF(Fe iii) as a function of log(O iii/O ii) for all Cloudy input parameters (black and gray bands). In the Cloudy simulations, at different metallicities the ICF for Fe can be different by up to ∼ 0.6 dex, while at the same metallicity the ICF …
Figure 11
Figure 11. Figure 11: A schematic of the evolution of the Fe fraction depleted into dust grains ( 𝑓Fe, dust). The vertical axis denotes the dust depletion fraction, while the horizontal axis indicates the evolutionary stage of the local ISM, labeled with the hydrogen column density. The ho…
Figure 12
Figure 12. Figure 12: Change of the inferred 𝜏g, observed relative to the initial and final fraction of Fe in dust for an assumed molecular cloud lifetime of 10 Myr. The horizontal axis denotes the initial depleted Fe fraction, which we assume is represented by the Fe depletion measured fr…

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Works this paper leans on

126 extracted references · 16 canonical work pages

  1. [1]

    L., Aloisi, A., et al

    Abril-Melgarejo, V., James, B. L., Aloisi, A., et al. 2024, The Astrophysical Journal, 973, 173, 10.3847/1538-4357/ad5e79

    doi:10.3847/1538-4357/ad5e79 2024

  2. [2]

    1996, Astronomy and Astrophysics, 305, 616

    Allain, T., Leach, S., & Sedlmayr, E. 1996, Astronomy and Astrophysics, 305, 616. https://ui.adsabs.harvard.edu/abs/1996A&A...305..616A/abstract

    1996

  3. [3]

    M., et al

    Aloisi, A., Savaglio, S., Heckman, T. M., et al. 2003, The Astrophysical Journal, 595, 760, 10.1086/377496

    doi:10.1086/377496 2003

  4. [4]

    2021, Monthly Notices of the Royal Astronomical Society, 505, 2361, 10.1093/mnras/stab1467

    Amayo, A., Delgado-Inglada, G., & Stasińska, G. 2021, Monthly Notices of the Royal Astronomical Society, 505, 2361, 10.1093/mnras/stab1467

    doi:10.1093/mnras/stab1467 2021

  5. [5]

    M., Lim, P

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

    doi:10.3847/1538-4357/ac7c74 2022

  6. [6]

    S., & Wenger, T

    Balser, D. S., & Wenger, T. V. 2024, The Astrophysical Journal, 964, 47, 10.3847/1538-4357/ad2458

    doi:10.3847/1538-4357/ad2458 2024

  7. [7]

    2024, Annual Review of Astronomy and Astrophysics, 62, 157, 10.1146/annurev-astro-071221-052705

    Birnstiel, T. 2024, Annual Review of Astronomy and Astrophysics, 62, 157, 10.1146/annurev-astro-071221-052705

    doi:10.1146/annurev-astro-071221-052705 2024

  8. [8]

    2000, Astronomy and Astrophysics Supplement Series, 143, 33, 10.1051/aas:2000331

    Bonnarel, F., Fernique, P., Bienaymé, O., et al. 2000, Astronomy and Astrophysics Supplement Series, 143, 33, 10.1051/aas:2000331

    doi:10.1051/aas:2000331 2000

Show all 126 references
  1. [9]

    2024, Astronomy and Astrophysics, 692, A249, 10.1051/0004-6361/202452362

    Bossion, D., Sarangi, A., Aalto, S., et al. 2024, Astronomy and Astrophysics, 692, A249, 10.1051/0004-6361/202452362

    2024 doi

  2. [10]

    L., Sloan, G

    Boyer, M. L., Sloan, G. C., Nanni, A., et al. 2025, The Astrophysical Journal, 991, 10.3847/1538-4357/adf06a

    2025 doi

  3. [11]

    2024, the Veeper , 10.5281/zenodo.10993984

    Burchett, J. 2024, the Veeper , 10.5281/zenodo.10993984

    2024 doi

  4. [12]

    2019, The Astrophysical Journal, 876, 62, 10.3847/1538-4357/ab16cf

    Chastenet, J., Sandstrom, K., Chiang, I.-D., et al. 2019, The Astrophysical Journal, 876, 62, 10.3847/1538-4357/ab16cf

    2019 doi

  5. [13]

    Chevance, M., Kruijssen, J. M. D., Vazquez-Semadeni, E., et al. 2020, Space Science Reviews, 216, 10.1007/s11214-020-00674-x

    2020 doi

  6. [14]

    R., Kereš, D., Hopkins, P

    Choban, C. R., Kereš, D., Hopkins, P. F., et al. 2022, Monthly Notices of the Royal Astronomical Society, 514, 4506, 10.1093/mnras/stac1542

    2022 doi

  7. [15]

    R., Salim, S., Kereš, D., Roman-Duval, J., & Sandstrom, K

    Choban, C. R., Salim, S., Kereš, D., Roman-Duval, J., & Sandstrom, K. M. 2026, Monthly Notices of the Royal Astronomical Society, 549, stag1020, 10.1093/mnras/stag1020

    2026 doi

  8. [16]

    2024, Astronomy & Astrophysics, 685, A75, 10.1051/0004-6361/202346662

    Chown, R., Sidhu, A., Peeters, E., et al. 2024, Astronomy & Astrophysics, 685, A75, 10.1051/0004-6361/202346662

    2024 doi

  9. [17]

    Clark, C. J. R., Roman-Duval, J. C., Gordon, K. D., et al. 2023, The Astrophysical Journal, 946, 42, 10.3847/1538-4357/acbb66

    2023 doi

  10. [18]

    W., Sankrit, R., Blair, W

    Danforth, C. W., Sankrit, R., Blair, W. P., Howk, J. C., & Chu, Y.-H. 2003, The Astrophysical Journal, 586, 1179, 10.1086/367959

    2003 doi

  11. [19]

    2024, Astronomy & Astrophysics, 683, A216, 10.1051/0004-6361/202346611

    De Cia, A., Roman-Duval, J., Konstantopoulou, C., et al. 2024, Astronomy & Astrophysics, 683, A216, 10.1051/0004-6361/202346611

    2024 doi

  12. [20]

    D., Misselt, K

    Decleir, M., Gordon, K. D., Misselt, K. A., et al. 2025, The Astronomical Journal, 169, 99, 10.3847/1538-3881/ada147

    2025 doi

  13. [21]

    Delgado-Inglada, G., Rodríguez, M., García-Rojas, J., Peña, M., & Ruiz, M. T. 2011, Revista Mexicana de Astronomia y Astrofisica Conference Series, 40, 165, 10.48550/arXiv.1103.2158

    2011 doi arXiv

  14. [22]

    Diplas, A., & Savage, B. D. 1994, The Astrophysical Journal Supplement Series, 93, 211, 10.1086/192052

    1994 doi

  15. [23]

    2022, Monthly Notices of the Royal Astronomical Society, 517, 4497, 10.1093/mnras/stac2974

    Domínguez-Guzmán, G., Rodríguez, M., García-Rojas, J., Esteban, C., & Toribio San Cipriano, L. 2022, Monthly Notices of the Royal Astronomical Society, 517, 4497, 10.1093/mnras/stac2974

    2022 doi

  16. [24]

    Draine, B. T. 2011, Physics of the Interstellar and Intergalactic Medium , 1st edn., Princeton Series in Astrophysics Series No. v.19 (Princeton: Princeton University Press)

    2011

  17. [25]

    T., & Bertoldi, F

    Draine, B. T., & Bertoldi, F. 1996, The Astrophysical Journal, 468, 269, 10.1086/177689

    1996 doi

  18. [26]

    T., & Salpeter, E

    Draine, B. T., & Salpeter, E. E. 1979, The Astrophysical Journal, 231, 77, 10.1086/157165

    1979 doi

  19. [27]

    2023, Protostars and Planets VII, 534, 717, 10.48550/arXiv.2203.09759

    Drążkowska, J., Bitsch, B., Lambrechts, M., et al. 2023, Protostars and Planets VII, 534, 717, 10.48550/arXiv.2203.09759

    2023 doi arXiv

  20. [28]

    1998, The Astrophysical Journal, 501, 643, 10.1086/305829

    Dwek, E. 1998, The Astrophysical Journal, 501, 643, 10.1086/305829

    1998 doi

  21. [29]

    2016, The Astrophysical Journal, 825, 136, 10.3847/0004-637X/825/2/136

    ---. 2016, The Astrophysical Journal, 825, 136, 10.3847/0004-637X/825/2/136

    2016 doi

  22. [30]

    G., Kim, S., & Staveley-Smith, L

    Elmegreen, B. G., Kim, S., & Staveley-Smith, L. 2001, The Astrophysical Journal, 548, 749, 10.1086/319021

    2001 doi

  23. [31]

    1998, The Astrophysical Journal, 500, 280, 10.1086/305727

    Faison, M., Churchwell, E., Hofner, P., et al. 1998, The Astrophysical Journal, 500, 280, 10.1086/305727

    1998 doi

  24. [32]

    Field, G. B. 1974, The Astrophysical Journal, 187, 453, 10.1086/152654

    1974 doi

  25. [33]

    W., Lang, D., & Goodman, J

    Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J. 2013, Publications of the Astronomical Society of the Pacific, 125, 306, 10.1086/670067

    2013 doi

  26. [34]

    Galliano, F., Galametz, M., & Jones, A. P. 2018, Annual Review of Astronomy and Astrophysics, 56, 673, 10.1146/annurev-astro-081817-051900

    2018 doi

  27. [35]

    Garnett, D. R. 1989, The Astrophysical Journal, 345, 282, 10.1086/167904

    1989 doi

  28. [36]

    E., McCullough, P

    Gaustad, J. E., McCullough, P. R., Rosing, W., & Van Buren, D. 2001, Publications of the Astronomical Society of the Pacific, 113, 1326, 10.1086/323969

    2001 doi

  29. [37]

    D., Bot, C., Boyer, M

    Gordon, K. D., Bot, C., Boyer, M. L., et al. 2024, JWST Proposal. Cycle 3, 5168. https://ui.adsabs.harvard.edu/abs/2024jwst.prop.5168G/abstract

    2024

  30. [38]

    J., & Salpeter, E

    Gould, R. J., & Salpeter, E. E. 1963, The Astrophysical Journal, 138, 393, 10.1086/147654

    1963 doi

  31. [39]

    C., Froning, C

    Green, J. C., Froning, C. S., Osterman, S., et al. 2011, The Astrophysical Journal, 744, 60, 10.1088/0004-637X/744/1/60

    2011 doi

  32. [40]

    M., van Hoof, P

    Gunasekera, C. M., van Hoof, P. a. M., Dehghanian, M., et al. 2025, Revista Mexicana de Astronomia y Astrofisica, 61, 120, 10.22201/ia.01851101p.2025.61.03.01

    2025 doi

  33. [41]

    2019, Astronomy and Astrophysics, 621, A85, 10.1051/0004-6361/201833787

    Hainich, R., Ramachandran, V., Shenar, T., et al. 2019, Astronomy and Astrophysics, 621, A85, 10.1051/0004-6361/201833787

    2019 doi

  34. [42]

    2024, The Astrophysical Journal, 966, 80, 10.3847/1538-4357/ad307b

    Hamanowicz, A., Tchernyshyov, K., Roman-Duval, J., et al. 2024, The Astrophysical Journal, 966, 80, 10.3847/1538-4357/ad307b

    2024 doi

  35. [43]

    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

  36. [44]

    Hartmann, L., Ballesteros-Paredes, J., & Bergin, E. A. 2001, The Astrophysical Journal, 562, 852, 10.1086/323863

    2001 doi

  37. [45]

    Henry, R. B. C., Speck, A., Karakas, A. I., Ferland, G. J., & Maguire, M. 2012, The Astrophysical Journal, 749, 61, 10.1088/0004-637X/749/1/61

    2012 doi

  38. [46]

    S., & Draine, B

    Hensley, B. S., & Draine, B. T. 2017, The Astrophysical Journal, 834, 134, 10.3847/1538-4357/834/2/134

    2017 doi

  39. [47]

    2023, The Astrophysical Journal, 948, 55, 10.3847/1538-4357/acc4c2

    ---. 2023, The Astrophysical Journal, 948, 55, 10.3847/1538-4357/acc4c2

    2023 doi

  40. [48]

    L., et al

    Hernandez, S., Aloisi, A., James, B. L., et al. 2021, The Astrophysical Journal, 908, 226, 10.3847/1538-4357/abd6c4

    2021 doi

  41. [49]

    2010, Astronomy and Astrophysics, 517, A39, 10.1051/0004-6361/201014230

    Heydari-Malayeri, M., & Selier, R. 2010, Astronomy and Astrophysics, 517, A39, 10.1051/0004-6361/201014230

    2010 doi

  42. [50]

    1999, Astronomy and Astrophysics, 344, L87, 10.48550/arXiv.astro-ph/9903259

    Hirashita, H. 1999, Astronomy and Astrophysics, 344, L87, 10.48550/arXiv.astro-ph/9903259

    1999 doi arXiv

  43. [51]

    2012, Monthly Notices of the Royal Astronomical Society, 422, 1263, 10.1111/j.1365-2966.2012.20702.x

    ---. 2012, Monthly Notices of the Royal Astronomical Society, 422, 1263, 10.1111/j.1365-2966.2012.20702.x

    2012

  44. [52]

    Hollenbach, D., & Salpeter, E. E. 1971, The Astrophysical Journal, 163, 155, 10.1086/150754

    1971 doi

  45. [53]

    C., & Savage, B

    Howk, J. C., & Savage, B. D. 1999, The Astrophysical Journal, 517, 746, 10.1086/307211

    1999 doi

  46. [54]

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

    2007 doi

  47. [55]

    T., & Gray, A., eds

    Ivezić, Z., Connolly, A., VanderPlas, J. T., & Gray, A., eds. 2014, Statistics, data mining, and machine learning in astronomy: a practical Python guide for the analysis of survey data, Princeton series in modern observational astronomy (Princeton, N.J: Princeton University Press)

    2014

  48. [56]

    I., Stasińska, G., Meynet, G., Guseva, N

    Izotov, Y. I., Stasińska, G., Meynet, G., Guseva, N. G., & Thuan, T. X. 2006, Astronomy and Astrophysics, 448, 955, 10.1051/0004-6361:20053763

    2006 doi

  49. [57]

    2018, The Astrophysical Journal, 853, 124, 10.3847/1538-4357/aa9ffb

    James, B., & Aloisi, A. 2018, The Astrophysical Journal, 853, 124, 10.3847/1538-4357/aa9ffb

    2018 doi

  50. [58]

    L., Aloisi, A., Heckman, T., Sohn, S

    James, B. L., Aloisi, A., Heckman, T., Sohn, S. T., & Wolfe, M. A. 2014, The Astrophysical Journal, 795, 109, 10.1088/0004-637X/795/2/109

    2014 doi

  51. [59]

    L., Abril-Melgarejo, V., Arellano-Córdova, K

    James, B. L., Abril-Melgarejo, V., Arellano-Córdova, K. Z., et al. 2026, The Astrophysical Journal, 1002, 82, 10.3847/1538-4357/ae5056

    2026 doi

  52. [60]

    Jenkins, E. B. 2009, The Astrophysical Journal, 700, 1299, 10.1088/0004-637X/700/2/1299

    2009 doi

  53. [61]

    B., & Wallerstein, G

    Jenkins, E. B., & Wallerstein, G. 2017, The Astrophysical Journal, 838, 85, 10.3847/1538-4357/aa64d4

    2017 doi

  54. [62]

    A., et al

    Kim, S., Staveley-Smith, L., Dopita, M. A., et al. 2003, The Astrophysical Journal Supplement Series, 148, 473, 10.1086/376980

    2003 doi

  55. [63]

    A., Woodgate, B

    Kimble, R. A., Woodgate, B. E., Bowers, C. W., et al. 1997, The Astrophysical Journal, 492, L83, 10.1086/311102

    1997 doi

  56. [64]

    2001, The Astronomical Journal, 121, 267, 10.1086/318043

    Koenigsberger, G., Georgiev, L., Peimbert, M., et al. 2001, The Astronomical Journal, 121, 267, 10.1086/318043

    2001 doi

  57. [65]

    2022, Astronomy & Astrophysics, 666, A12, 10.1051/0004-6361/202243994

    Konstantopoulou, C., De Cia, A., Krogager, J.-K., et al. 2022, Astronomy & Astrophysics, 666, A12, 10.1051/0004-6361/202243994

    2022 doi

  58. [66]

    A., et al

    Kreckel, K., Ho, I.-T., Blanc, G. A., et al. 2020, Monthly Notices of the Royal Astronomical Society, 499, 193, 10.1093/mnras/staa2743

    2020 doi

  59. [67]

    R., & Ting, Y.-S

    Krumholz, M. R., & Ting, Y.-S. 2018, Monthly Notices of the Royal Astronomical Society, 475, 2236, 10.1093/mnras/stx3286

    2018 doi

  60. [68]

    Kunth, D., & Sargent, W. L. W. 1986, The Astrophysical Journal, 300, 496, 10.1086/163828

    1986 doi

  61. [69]

    C., Nigoche-Netro, A., et al

    Lagos, P., Scott, T. C., Nigoche-Netro, A., et al. 2018, Monthly Notices of the Royal Astronomical Society, 477, 392, 10.1093/mnras/sty601

    2018 doi

  62. [70]

    2003, The Astrophysical Journal Supplement Series, 146, 417, 10.1086/374373

    Lanz, T., & Hubeny, I. 2003, The Astrophysical Journal Supplement Series, 146, 417, 10.1086/374373

    2003 doi

  63. [71]

    2013, Astronomy & Astrophysics, 553, A16, 10.1051/0004-6361/201220948

    Lebouteiller, V., Heap, S., Hubeny, I., & Kunth, D. 2013, Astronomy & Astrophysics, 553, A16, 10.1051/0004-6361/201220948

    2013 doi

  64. [72]

    2004, Astronomy and Astrophysics, 415, 55, 10.1051/0004-6361:20034592

    Lebouteiller, V., Kunth, D., Lequeux, J., et al. 2004, Astronomy and Astrophysics, 415, 55, 10.1051/0004-6361:20034592

    2004 doi

  65. [73]

    2012, Astronomy and Astrophysics, 537, A72, 10.1051/0004-6361/201117867

    Lelli, F., Verheijen, M., Fraternali, F., & Sancisi, R. 2012, Astronomy and Astrophysics, 537, A72, 10.1051/0004-6361/201117867

    2012 doi

  66. [74]

    M., et al

    Martín-Doménech, R., Jiménez-Serra, I., Muñoz Caro, G. M., et al. 2016, Astronomy and Astrophysics, 585, A112, 10.1051/0004-6361/201526271

    2016 doi

  67. [75]

    S., Rumpl, W., & Nordsieck, K

    Mathis, J. S., Rumpl, W., & Nordsieck, K. H. 1977, The Astrophysical Journal, 217, 425, 10.1086/155591

    1977 doi

  68. [76]

    C., Zijlstra, A

    McDonald, I., Sloan, G. C., Zijlstra, A. A., et al. 2010, The Astrophysical Journal, 717, L92, 10.1088/2041-8205/717/2/L92

    2010 doi

  69. [77]

    1989, Interstellar Dust, 135, 431

    McKee, C. 1989, Interstellar Dust, 135, 431. https://ui.adsabs.harvard.edu/abs/1989IAUS..135..431M/abstract

    1989

  70. [78]

    2010, SciPy 2010, 10.25080/Majora-92bf1922-00a

    McKinney, W. 2010, SciPy 2010, 10.25080/Majora-92bf1922-00a

    2010 doi

  71. [79]

    J., Greene, G

    McLean, B. J., Greene, G. R., Lattanzi, M. G., & Pirenne, B. 2000, Astronomical Data Analysis Software and Systems IX, 216, 145. https://ui.adsabs.harvard.edu/abs/2000ASPC..216..145M/abstract

    2000

  72. [80]

    E., Hasselquist, S., Peek, J

    Murray, C. E., Hasselquist, S., Peek, J. E. G., et al. 2024, The Astrophysical Journal, 962, 120, 10.3847/1538-4357/ad1591

    2024 doi

  73. [81]

    E., Kreckel, K., Esteban, C., et al

    Méndez-Delgado, J. E., Kreckel, K., Esteban, C., et al. 2024, Astronomy and Astrophysics, 690, A248, 10.1051/0004-6361/202450928

    2024 doi

  74. [82]

    2012, The Astrophysical Journal, 760, 149, 10.1088/0004-637X/760/2/149

    Paladini, R., Umana, G., Veneziani, M., et al. 2012, The Astrophysical Journal, 760, 149, 10.1088/0004-637X/760/2/149

    2012 doi

  75. [83]

    2003, The Astrophysical Journal, 584, 735, 10.1086/345793

    Peimbert, A. 2003, The Astrophysical Journal, 584, 735, 10.1086/345793

    2003 doi

  76. [84]

    X., Tejos, N., Crighton, N., et al

    Prochaska, J. X., Tejos, N., Crighton, N., et al. 2016, linetools/linetools: Second major release, 10.5281/zenodo.168270

    2016 doi

  77. [85]

    X., Tejos, N., cwotta, et al

    Prochaska, J. X., Tejos, N., cwotta, et al. 2017, pyigm/pyigm: Initial release for publications. https://zenodo.org/records/1045480

    2017

  78. [86]

    2002, The Astrophysical Journal, 564, 704, 10.1086/324286

    Relaño, M., Peimbert, M., & Beckman, J. 2002, The Astrophysical Journal, 564, 704, 10.1086/324286

    2002 doi

  79. [87]

    2016, Astronomy & Astrophysics, 595, A43, 10.1051/0004-6361/201628139

    Relaño, M., Kennicutt, R., Lisenfeld, U., et al. 2016, Astronomy & Astrophysics, 595, A43, 10.1051/0004-6361/201628139

    2016 doi

  80. [88]

    M., Jenkins, E

    Ritchey, A. M., Jenkins, E. B., Shull, J. M., et al. 2023, The Astrophysical Journal, 952, 57, 10.3847/1538-4357/acda25

    2023 doi

  81. [89]

    2003, The Astrophysical Journal, 590, 296, 10.1086/374925

    Rodríguez, M. 2003, The Astrophysical Journal, 590, 296, 10.1086/374925

    2003 doi

  82. [90]

    Rodríguez, M., & Rubin, R. H. 2005, The Astrophysical Journal, 626, 900, 10.1086/429958

    2005 doi

  83. [91]

    D., Meixner, M., et al

    Roman-Duval, J., Gordon, K. D., Meixner, M., et al. 2014, The Astrophysical Journal, 797, 86, 10.1088/0004-637X/797/2/86

    2014 doi

  84. [92]

    B., Williams, B., et al

    Roman-Duval, J., Jenkins, E. B., Williams, B., et al. 2019, The Astrophysical Journal, 871, 151, 10.3847/1538-4357/aaf8bb

    2019 doi

  85. [93]

    B., Tchernyshyov, K., et al

    Roman-Duval, J., Jenkins, E. B., Tchernyshyov, K., et al. 2021, The Astrophysical Journal, 910, 95, 10.3847/1538-4357/abdeb6

    2021 doi

  86. [94]

    2022 a , The Astrophysical Journal, 928, 90, 10.3847/1538-4357/ac5248

    ---. 2022 a , The Astrophysical Journal, 928, 90, 10.3847/1538-4357/ac5248

    2022 doi

  87. [95]

    2022 b , The Astrophysical Journal, 935, 105, 10.3847/1538-4357/ac7713

    ---. 2022 b , The Astrophysical Journal, 935, 105, 10.3847/1538-4357/ac7713

    2022 doi

  88. [96]

    J., Fullerton, A

    Roman-Duval, J., Fischer, W. J., Fullerton, A. W., et al. 2025, The Astrophysical Journal, 985, 109, 10.3847/1538-4357/adc45b

    2025 doi

  89. [97]

    1995, Astronomy and Astrophysics, 294, 432, 10.48550/arXiv.astro-ph/9410023

    Roy, J.-R., & Kunth, D. 1995, Astronomy and Astrophysics, 294, 432, 10.48550/arXiv.astro-ph/9410023

    1995 doi arXiv

  90. [99]

    2012, Astronomy & Astrophysics, 540, A144, 10.1051/0004-6361/201117830

    Sander, A., Hamann, W.-R., & Todt, H. 2012, Astronomy & Astrophysics, 540, A144, 10.1051/0004-6361/201117830

    2012 doi

  91. [100]

    D., & Sembach, K

    Savage, B. D., & Sembach, K. R. 1996, Annual Review of Astronomy and Astrophysics, 34, 279, 10.1146/annurev.astro.34.1.279

    1996 doi

  92. [101]

    M., Christensen, L., et al

    Schady, P., Yates, R. M., Christensen, L., et al. 2024, Monthly Notices of the Royal Astronomical Society, 529, 2807, 10.1093/mnras/stae677

    2024 doi

  93. [102]

    A., McGee, R

    Shaver, P. A., McGee, R. X., Newton, L. M., Danks, A. C., & Pottasch, S. R. 1983, Monthly Notices of the Royal Astronomical Society, 204, 53, 10.1093/mnras/204.1.53

    1983 doi

  94. [103]

    H., Hopkins, P

    Soliman, N. H., Hopkins, P. F., & Grudić, M. Y. 2024, The Astrophysical Journal, 974, 136, 10.3847/1538-4357/ad6ddd

    2024 doi

  95. [104]

    Spitzer, L., & Jenkins, E. B. 1975, Annual Review of Astronomy and Astrophysics, 13, 133, 10.1146/annurev.aa.13.090175.001025

    1975

  96. [105]

    M., Sault, R

    Stanimirovic, S., Staveley-Smith, L., Dickey, J. M., Sault, R. J., & Snowden, S. L. 1999, Monthly Notices of the Royal Astronomical Society, 302, 417, 10.1046/j.1365-8711.1999.02013.x

    1999

  97. [106]

    W., Evans, J

    Stephens, I. W., Evans, J. M., Xue, R., et al. 2014, The Astrophysical Journal, 784, 147, 10.1088/0004-637X/784/2/147

    2014 doi

  98. [107]

    2024, The Astrophysical Journal, 971, 178, 10.3847/1538-4357/ad54bd

    Sutter, J., Sandstrom, K., Chastenet, J., et al. 2024, The Astrophysical Journal, 971, 178, 10.3847/1538-4357/ad54bd

    2024 doi

  99. [108]

    G., Muñoz-Tuñón, C., et al

    Sánchez Almeida, J., Elmegreen, B. G., Muñoz-Tuñón, C., et al. 2015, The Astrophysical Journal, 810, L15, 10.1088/2041-8205/810/2/L15

    2015 doi

  100. [109]

    2015, The Astrophysical Journal, 811, 78, 10.1088/0004-637X/811/2/78

    Tchernyshyov, K., Meixner, M., Seale, J., et al. 2015, The Astrophysical Journal, 811, 78, 10.1088/0004-637X/811/2/78

    2015 doi

  101. [110]

    K., & Roman-Duval, J

    Tchernyshyov, K., Werk, J. K., & Roman-Duval, J. 2025, The Astronomical Journal, 170, 10.3847/1538-3881/adf33a

    2025 doi

  102. [111]

    2015, The Astrophysical Journal, 799, 158, 10.1088/0004-637X/799/2/158

    Temim, T., Dwek, E., Tchernyshyov, K., et al. 2015, The Astrophysical Journal, 799, 158, 10.1088/0004-637X/799/2/158

    2015 doi

  103. [112]

    2026, pandas-dev/pandas: Pandas , Zenodo, 10.5281/zenodo.21500199

    The pandas development team . 2026, pandas-dev/pandas: Pandas , Zenodo, 10.5281/zenodo.21500199

    2026 doi

  104. [113]

    2015, Astronomy and Astrophysics, 579, A75, 10.1051/0004-6361/201526253

    Todt, H., Sander, A., Hainich, R., et al. 2015, Astronomy and Astrophysics, 579, A75, 10.1051/0004-6361/201526253

    2015 doi

  105. [114]

    2017, Monthly Notices of the Royal Astronomical Society, 467, 3759, 10.1093/mnras/stx328

    Toribio San Cipriano, L., Domínguez-Guzmán, G., Esteban, C., et al. 2017, Monthly Notices of the Royal Astronomical Society, 467, 3759, 10.1093/mnras/stx328

    2017 doi

  106. [115]

    C., & Varoquaux, G

    Van Der Walt, S., Colbert, S. C., & Varoquaux, G. 2011, Computing in Science and Engineering, 13, 22, 10.1109/MCSE.2011.37

    2011 doi

  107. [116]

    E., et al

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

    2020 doi

  108. [117]

    C., Jappsen, A

    Vázquez-Semadeni, E., Gómez, G. C., Jappsen, A. K., et al. 2007, The Astrophysical Journal, 657, 870, 10.1086/510771

    2007 doi

  109. [118]

    R., Drissen, L., Parker, J

    Walborn, N. R., Drissen, L., Parker, J. W., et al. 1999, The Astronomical Journal, 118, 1684, 10.1086/301038

    1999 doi

  110. [119]

    C., & Draine, B

    Weingartner, J. C., & Draine, B. T. 2001, The Astrophysical Journal, 548, 296, 10.1086/318651

    2001 doi

  111. [120]

    E., Sonnentrucker, P., Snow, T

    Welty, D. E., Sonnentrucker, P., Snow, T. P., & York, D. G. 2020, The Astrophysical Journal, 897, 36, 10.3847/1538-4357/ab8f8e

    2020 doi

  112. [121]

    E., Xue, R., & Wong, T

    Welty, D. E., Xue, R., & Wong, T. 2012, The Astrophysical Journal, 745, 173, 10.1088/0004-637X/745/2/173

    2012 doi

  113. [122]

    2000, Astronomy and Astrophysics Supplement Series, 143, 9, 10.1051/aas:2000332

    Wenger, M., Ochsenbein, F., Egret, D., et al. 2000, Astronomy and Astrophysics Supplement Series, 143, 9, 10.1051/aas:2000332

    2000 doi

  114. [123]

    E., Kimble, R

    Woodgate, B. E., Kimble, R. A., Bowers, C. W., et al. 1998, Publications of the Astronomical Society of the Pacific, 110, 1183, 10.1086/316243

    1998 doi

  115. [124]

    T., Marshall, J

    Zeegers, S. T., Marshall, J. P., Gordon, K. D., et al. 2025, The Astrophysical Journal, 987, 25, 10.3847/1538-4357/add73b

    2025 doi

  116. [125]

    B., & Klessen, R

    Zhukovska, S., Dobbs, C., Jenkins, E. B., & Klessen, R. S. 2016, The Astrophysical Journal, 831, 147, 10.3847/0004-637X/831/2/147

    2016 doi

  117. [126]

    2008, Astronomy and Astrophysics, 479, 453, 10.1051/0004-6361:20077789

    Zhukovska, S., Gail, H.-P., & Trieloff, M. 2008, Astronomy and Astrophysics, 479, 453, 10.1051/0004-6361:20077789

    2008 doi

  118. [127]

    2018, The Astrophysical Journal, 857, 94, 10.3847/1538-4357/aab438

    Zhukovska, S., Henning, T., & Dobbs, C. 2018, The Astrophysical Journal, 857, 94, 10.3847/1538-4357/aab438

    2018 doi

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