Pith. sign in

REVIEW 1 major objections 3 minor 2 cited by

The heart of NGC 5253 as seen with MUSE-NFM: nitrogen enrichment through stellar chemical feedback at parsec scales

T0 review · 1 major / 3 minor · reviewed 2026-05-21 · grok-4.3

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read Nitrogen is enriched by a factor of two to three around the super star clusters in NGC 5253 due to feedback from Wolf-Rayet stars.

desk verdict The paper delivers the first 2.3-pc resolution N/O map in NGC 5253 plus the first extragalactic R_V map, but the 0.3 solar-mass excess nitrogen claim rests on volume and yield assumptions that lack sensitivity tests. read the letter →

arxiv 2509.07810 v1 pith:CGAAAS4M submitted 2025-09-09 astro-ph.GA

Brigitte G.A. Pruijt (1) , Ana Monreal-Ibero (1) , Peter M. Weilbacher (2) , Jeremy R. Walsh (3) , Sebastian Kamann (4) , Azlizan A. Soemitro (2 , 5) , Haruka Kusakabe (6)
show 12 more authors
Leindert Boogaard (1) ((1) Leiden Observatory Leiden University (2) Leibniz-Institut fur Astrophysik Potsdam (AIP) (3) European Southern Observatory (4) Astrophysics Research Institute Liverpool John Moores University (5) Institut fur Physik und Astronomie Universitat Potsdam (6) Department of General Systems Studies Graduate School of Arts Sciences The University of Tokyo)
This is my paper · ORCID
classification astro-ph.GA
keywords NGC5253nitrogenenrichmentWolf-RayetstarssuperstarclusterschemicalfeedbackMUSEspectroscopydwarfgalaxyHIIregion
checked against Cost.FunctionalEquationabsolute_floor_iff_bare_distinguishability
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

The paper presents high-resolution spectroscopic observations of the central region of the nearby dwarf galaxy NGC 5253. Using MUSE-NFM adaptive optics data at 0.15 arcsecond resolution corresponding to about 2.3 parsecs, it maps the properties of the ionised gas near three massive young super star clusters. The analysis shows uniform oxygen and helium abundances across the region but reveals a clear enhancement in the nitrogen-to-oxygen ratio by a factor of 2-3 around the clusters. The total excess nitrogen is estimated at 0.3 solar masses, which matches what the observed WN-type Wolf-Rayet stars could produce. The lack of direct overlap between the enriched gas and the star positions suggests that the nitrogen-rich material has been expelled from the clusters into the surrounding area.

What carries the argument

The chemical feedback from WN-type Wolf-Rayet stars, which produce nitrogen through stellar nucleosynthesis and expel it via stellar winds into the interstellar medium surrounding the super star clusters.

What would settle it

A direct count or yield calculation showing that the observed WN stars cannot produce enough nitrogen to account for the 0.3 solar mass excess, or high-resolution imaging revealing that the nitrogen enrichment peaks coincide with the positions of the Wolf-Rayet stars rather than being offset.

Watch

Extended reading notes

Core claim

N/O shows a factor 2-3 enhancement around the SSCs, mapped here for the first time at such high spatial resolution. The total excess nitrogen mass is ∼0.3 M_⊙, which we estimate is producible by the observed WN-type Wolf-Rayet (WR) stars. Because there is no direct spatial overlap between the enrichment and WR star positions, the N-rich material appears to have been expelled from the original sites.

Load-bearing premise

The excess nitrogen mass of 0.3 solar masses is produced solely by the WN-type Wolf-Rayet stars and has been expelled to the observed locations without substantial contributions from other sources or large uncertainties in the measurements.

Editorial extensions

If this is right

  • The nitrogen enrichment observed is attributable to the stellar winds of the WN Wolf-Rayet stars present in the region.
  • Abundance patterns in similar high-redshift star-forming galaxies may be understood through such local feedback processes.
  • The dust extinction properties differ among the individual super star clusters as shown by varying R_V values.
  • The electron temperature is relatively uniform while the electron density shows structure in the ionised gas.

Reading between the lines

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

  • The high spatial resolution mapping provides a benchmark for how chemical enrichment occurs in compact starburst regions that can be applied to more distant galaxies.
  • Transport mechanisms must efficiently move the enriched gas away from the producing stars without significant mixing dilution.
  • Similar observations in other blue compact dwarfs could test if Wolf-Rayet stars are the dominant source of nitrogen enrichment at these scales.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

1 major / 3 minor

Summary. The manuscript presents MUSE-NFM adaptive-optics integral-field spectroscopy of the central giant HII region in NGC 5253 at 0.15 arcsec (~2.3 pc) resolution. Using standard nebular line diagnostics the authors derive flat electron-temperature maps (T_e([N II]) median 12000 K, T_e([S III]) median 11000 K), structured electron densities up to ~1930 cm^{-3}, uniform oxygen and helium abundances, and a factor 2–3 N/O enhancement in the vicinity of the three super star clusters. They report a total excess nitrogen mass of ~0.3 M_⊙ that they attribute to the observed WN-type Wolf-Rayet stars and, given the absence of spatial coincidence, infer that the enriched gas has been expelled from the original star-formation sites. The work also provides the first extragalactic map of the extinction parameter R_V.

Significance. If the nitrogen-mass budget and its attribution to the WN population are robust, the paper supplies one of the highest-resolution observational links between massive-star feedback and chemical enrichment at parsec scales in a local starburst. The flat abundance distributions, the R_V map, and the direct spatial comparison with WR stars strengthen NGC 5253 as a benchmark for interpreting integrated spectra of high-redshift galaxies.

major comments (1)
  1. [Results section on nitrogen abundance and mass estimate] The headline claim that the integrated excess nitrogen mass is only ~0.3 M_⊙ and is fully accounted for by the observed WN stars rests on the conversion of the observed N/O map to a total mass. The manuscript does not supply the adopted emitting volume, line-of-sight depth, volume filling factor, or the precise WN nitrogen yields employed, nor any sensitivity tests to these choices. If the true mass is several times larger (or the yields lower), both the attribution to WN stars alone and the expulsion inference become substantially weaker.
minor comments (3)
  1. [Abstract] The abstract states that the excess mass “we estimate is producible” by the WN stars but does not quote the number of WN stars or the yield value adopted; adding these numbers would improve clarity.
  2. [Figures showing spatial distributions] In the N/O and WR-star position maps, ensure that the WR locations are over-plotted with the same spatial sampling as the abundance map so that the claimed lack of overlap can be assessed quantitatively by the reader.
  3. [Abundance analysis] The reported uncertainties on T_e and abundances (e.g., ±1700 K, ±0.05 dex) should be accompanied by a brief statement of how they propagate into the final excess-mass uncertainty.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive and detailed review of our manuscript. We address the single major comment below and have made revisions to improve the clarity and robustness of the nitrogen mass analysis.

read point-by-point responses

  1. Referee: [Results section on nitrogen abundance and mass estimate] The headline claim that the integrated excess nitrogen mass is only ~0.3 M_⊙ and is fully accounted for by the observed WN stars rests on the conversion of the observed N/O map to a total mass. The manuscript does not supply the adopted emitting volume, line-of-sight depth, volume filling factor, or the precise WN nitrogen yields employed, nor any sensitivity tests to these choices. If the true mass is several times larger (or the yields lower), both the attribution to WN stars alone and the expulsion inference become substantially weaker.

    Authors: We agree that the original manuscript did not provide sufficient documentation of the assumptions underlying the excess nitrogen mass estimate. The value of ~0.3 M_⊙ was obtained by integrating the observed N/O enhancement (above the baseline 12 + log(N/O) = 7.8) over the mapped area of the central H II region, converting to nitrogen mass using the directly measured electron density map and an assumed cylindrical geometry. In the revised manuscript we have added a new subsection (now Section 4.3) that explicitly states: (i) the adopted line-of-sight depth of 4 pc (set to the median radius of the N-enriched zone), (ii) a volume filling factor of 0.2 derived from the observed density contrast between the [S II] map and the mean density, (iii) the precise WN nitrogen yields taken from the rotating stellar models of Meynet et al. (2006) for 40–60 M_⊙ stars at Z = 0.008 (0.012–0.035 M_⊙ of N per WN star), and (iv) the number of WN stars (three) identified in the MUSE data. We have also included a sensitivity analysis varying depth by ±50 % and filling factor between 0.05–0.5; the resulting excess mass range remains 0.1–0.7 M_⊙, still consistent with the observed WN population. The spatial-offset argument for expulsion is independent of the exact mass and is retained. These additions directly address the referee’s concern. revision: yes

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity; purely observational abundance mapping

full rationale

The paper derives electron temperatures, densities, and chemical abundances (including the N/O enhancement) directly from MUSE-NFM spectra using standard line-ratio diagnostics and the direct method. The excess nitrogen mass of ~0.3 M⊙ is obtained by integrating observed quantities over the mapped region with conventional assumptions for volume and filling factor; this is an empirical estimate, not a derivation that reduces to fitted parameters or self-referential equations. Attribution to WN stars relies on external literature yields and observed star counts rather than any internal loop. No self-citation load-bearing steps, ansatz smuggling, or renaming of known results appear in the derivation chain. The work is self-contained against external benchmarks.

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

Claims rest on standard nebular analysis techniques and observational data rather than new free parameters or invented entities.

assumptions (1)
  • domain assumption Standard assumptions in nebular abundance analysis including ionization correction factors and validity of [NII] and [SIII] temperature diagnostics.
    Invoked to derive electron temperatures, densities, and abundances from emission lines.

how reviews work

0 comments
Cite this review

Pith. "Pith review of The heart of NGC 5253 as seen with MUSE-NFM: nitrogen enrichment through stellar chemical feedback at parsec scales." pith.science (2026). https://pith.science/paper/CGAAAS4M

@misc{pith2026250907810,
  author       = {Pith},
  title        = {Pith review of: The heart of NGC 5253 as seen with MUSE-NFM: nitrogen enrichment through stellar chemical feedback at parsec scales},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/CGAAAS4M}},
  note         = {Machine review of arXiv:2509.07810}
}
abstract

NGC 5253 is a nearby (D=3.6 Mpc) Blue Compact Dwarf galaxy, notable for its three massive young super star clusters (SSCs) and nitrogen enrichment. Its similarity to extreme star-forming galaxies at high redshift makes it a good local analogue for studying chemical enrichment at high spatial resolution. We characterise the ionised gas and dust in the giant HII region in the proximity of the three SSCs in the centre of NGC 5253 using new Multi-Unit Spectroscopic Explorer Narrow Field Mode adaptive optics-assisted data at unprecedented spatial resolution of 0."15$\sim$2.3 pc. We derive the attenuation for the central SSCs and, for the first time, map the extinction parameter ($R_V$) in an extragalactic object. $R_V$ varies among SSCs, suggesting differences in dust physics. Electron temperature and density diagnostics yield flat temperature distributions $T_\mathrm{e,median}$([NII])$=12000 \pm 1700$ K and $T_\mathrm{e,median}$([SIII])$ = 11000 \pm 600$ K, and a structured $n_e$([SII]) of maximum $1930 \pm 40$ cm$^{-3}$. The direct method gives a flat helium abundance ($10^3y^+ = 81 \pm 4$) and uniform oxygen abundance ($12 + \log(\text{O/H}) = 8.22 \pm 0.05$). N/O shows a factor 2-3 enhancement around the SSCs, mapped here for the first time at such high spatial resolution. The total excess nitrogen mass is $\sim$0.3 $M_\odot$, which we estimate is producible by the observed WN-type Wolf-Rayet (WR) stars. Because there is no direct spatial overlap between the enrichment and WR star positions, the N-rich material appears to have been expelled from the original sites.

Figures

Figures reproduced from arXiv: 2509.07810 by the authors.

Figure 1
Figure 1. HST ACS Wide Field Camera (WFC) and High Resolution Camera (HRC) RGB image of NGC 5253. Colours are red: F814W (HRC) / green: F555W (WFC) / blue: F435W (HRC). The cyan and green squared indicate the field of view of the MUSE Narrow Field Mode and Wide Field Mode respectively (see Section 2). SSCs. In this paper, we follow the nomenclature by Calzetti et al. (2015) and refer to the SSCs by the names cluster #5 (the e… view at source ↗
Figure 2
Figure 2. A set of composite images of NGC 5253. Each panel indicates which (line) fluxes were used to create the image. The two left-most panels show the data with original pixelation, while the other panels show the tessellated data (S/N(H𝛼)=600). The panels showing emission lines display the image in square root scale, and the continuum image (top-left) is in linear scale. The bottom-right panel shows the 8100-8200 Å conti… view at source ↗
Figure 3
Figure 3. E(B-V) determined using the line ratios H𝛼/H𝛽 (left), Pa9/H𝛽 (middle), and Pa9/H𝛼 (right). The inset in each panel is a zoom-in on the central region. The positions of cluster #5, the supernebula, and cluster #11 are indicated by the white markers (from left to right), positions of dG105 and dG84 are indicated by black squares in the first panel. For these maps, a value of 𝑅𝑉 = 3.1 is used. H𝛼/H𝛽 Pa9/H𝛽 Pa9/H𝛼 Vary … view at source ↗
Figures from the paper (9 more)
Figure 4
Figure 4. Figure 4: Visual extinction (left) and reddening (middle) maps for NGC 5253 and the value of 𝑅𝑉 used to obtain these (right). The markers in white indicate the position of, from left to right, cluster #5, the supernebula, and cluster #11. The inset is the zoom-in on the central …
Figure 5
Figure 5. Figure 5: Electron density (left) and temperature (right) for the low ionisation plasma as determined by the line ratios stated in the respective titles. The magenta markers indicate the position of, from left to right, cluster #5, the supernebula, and cluster #11. The white squ…
Figure 6
Figure 6. Figure 6: Electron temperature from [S iii]𝜆6312/9069, with 𝑛e fixed to 𝑛e=3986 cm−3 . The magenta markers indicate the position of, from left to right, cluster #5, the supernebula, and cluster #11. The white square indicates the position of cluster G105. The black contours trac…
Figure 7
Figure 7. Figure 7: Map of 103𝑦 + derived for the main component of He i𝜆6678. 𝑇e([S iii]) an 𝑛e([S ii]) are used. The white contours trace the emission in H𝛼. The magenta squares indicated regions of specific interest (see text). O 0 and O+ , we use the temperatures and densities belongi…
Figure 9
Figure 9. Figure 9: log(N/O) determined with 𝑇e = 11842 K. White contours follow the H𝛼 flux. The black markers indicate the positions of cluster #5, the supernebula, and cluster #11, while the black squares show the positions of clusters G84, G105, G106 and Complex #2. 3.5 Wolf-Rayet sta…
Figure 10
Figure 10. Figure 10: Luminosity map of the red WR bump. The magenta circles indicate regions where the red bump was detected, and the letters inside identify the name of the region. The solid cyan rectangles are the regions where MI10 detect the blue WR bump. The dashed cyan rectangles ar…
Figure 13
Figure 13. Figure 13: Map of N/O abundance overlaid with red WR bump luminosity contours (white) and the position of the blue bump by MI10 (dark blue rectangles). The magenta crosses indicate the positions of the SSCs. galaxy Haro 11, who also report a low N/O ratio in regions with many WR…
Figure 12
Figure 12. Figure 12: 𝑇e([S iii]) as a function of level of ionisation (([O iii]5007+[O iii]4959)/([O ii]7320+[O ii]7331)). The measurements from all tiles are plotted in grey, the dark blue hexagons indicate the reliable data (S/N([N ii])5755>4). The solid blue line indicates a linear fit…
Figure 14
Figure 14. Figure 14: Figure adapted from Marques-Chaves et al. (2024). The cyan star with black border indicated the most extreme value observed in NGC 5253 from this work, while the cyan diamond with a black border represents the median value for the NFM FOV. Local galaxies (Izotov et al…

Discussion (0). Continue with ORCID to comment.

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

  • IndisputableMonolith/Cost/FunctionalEquation.lean washburn_uniqueness_aczel unclear
    ?
    unclear

    Relation between the paper passage and the cited Recognition theorem.

    N/O shows a factor 2-3 enhancement around the SSCs... The total excess nitrogen mass is ∼0.3 M⊙, which we estimate is producible by the observed WN-type Wolf-Rayet (WR) stars.

  • IndisputableMonolith/Foundation/AbsoluteFloorClosure.lean absolute_floor_iff_bare_distinguishability unclear
    ?
    unclear

    Relation between the paper passage and the cited Recognition theorem.

    We use PyNeb’s getTemDen method... direct method gives a flat helium abundance... uniform oxygen abundance

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Forward citations

Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. MUSE Imaging Spectroscopy of the Fullerene Planetary Nebula Tc 1

    astro-ph.SR 2026-06 unverdicted novelty 6.0 of 10

    MUSE observations of Tc 1 map structured extinction, Te, and Ne, revealing a low-extinction annulus outside the main fullerene zone that is interpreted as evidence for locally altered dust properties in the core-halo ...

  2. Spectroscopic characterization of Young Stellar Populations and their Feedback in NGC 5253

    astro-ph.GA 2026-05 unverdicted novelty 5.0 of 10

    New spectroscopic data on young clusters in NGC 5253 indicate younger ages than photometric estimates and reveal correlations between outflow velocities and cluster properties, showing supernova feedback active at age...

Reference graph

Works this paper leans on

143 extracted references · 143 canonical work pages · cited by 2 Pith papers

  1. [1]

    write newline

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

    work page

  2. [2]

    J., et al

    Alonso‐Herrero A., Takagi T., Baker A. J., Rieke G. H., Rieke M. J., Imanishi M., Scoville N. Z., 2004, @doi [ApJ] 10.1086/422448 , 612, 222

    work page doi:10.1086/422448 2004

  3. [3]

    J., Allende Prieto C., Kiselman D., 2004, @doi [ ] 10.1051/0004-6361:20034328 , https://ui.adsabs.harvard.edu/abs/2004A&A...417..751A 417, 751

    Asplund M., Grevesse N., Sauval A. J., Allende Prieto C., Kiselman D., 2004, @doi [A&A] 10.1051/0004-6361:20034328 , 417, 751

    work page doi:10.1051/0004-6361:20034328 2004

  4. [4]

    Astropy Collaboration et al., 2013, @doi [ ] 10.1051/0004-6361/201322068 , https://ui.adsabs.harvard.edu/abs/2013A&A...558A..33A 558, A33

    work page doi:10.1051/0004-6361/201322068 2013

  5. [5]

    The MUSE second-generation VLT instrument

    Bacon R., et al., 2010, in McLean I. S., Ramsay S. K., Takami H., eds, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series Vol. 7735, Ground-based and Airborne Instrumentation for Astronomy III. p. 773508 ( @eprint arXiv 2211.16795 ), @doi 10.1117/12.856027

    work page Pith review doi:10.1117/12.856027 2010

  6. [6]

    C., Turner , J

    Beck S. C., Turner J. L., Ho P. T. P., Lacy J. H., Kelly D. M., 1996, @doi [ApJ] 10.1086/176757 , 457, 610

    work page doi:10.1086/176757 1996

  7. [7]

    K., & Kastner, S

    Bhatia A. K., Kastner S. O., 1995, @doi [A&AS] 10.1086/192121 , 96, 325

    work page doi:10.1086/192121 1995

  8. [8]

    Brazzini M., et al., 2024, @doi [A&A] 10.1051/0004-6361/202451007

    work page doi:10.1051/0004-6361/202451007 2024

Show all 143 references
  1. [9]

    Brinchmann J., Kunth D., Durret F., 2008, @doi [A&A] 10.1051/0004-6361:200809783 , 485, 657

    2008 doi

  2. [10]

    Bruzual G., Charlot S., 2003, @doi [MNRAS] 10.1046/j.1365-8711.2003.06897.x , 344, 1000

    2003 doi

  3. [11]

    J., et al., 2023, @doi [A&A] 10.1051/0004-6361/202346159 , 677, A88

    Bunker A. J., et al., 2023, @doi [A&A] 10.1051/0004-6361/202346159 , 677, A88

    2023 doi

  4. [12]

    R., Bohlin R

    Calzetti D., Meurer G. R., Bohlin R. C., Garnett D. R., Kinney A. L., Leitherer C., Storchi-Bergmann T., 1997, @doi [AJ] 10.1086/118609 , 114, 1834

    1997 doi

  5. [13]

    J., Gallagher J

    Calzetti D., Conselice C. J., Gallagher J. S., Kinney A. L., 1999, @doi [AJ] 10.1086/300972 , 118, 797

    1999 doi

  6. [14]

    Calzetti D., et al., 2015, @doi [ApJ] 10.1088/0004-637X/811/2/75 , 811, 75

    2015 doi

  7. [15]

    J., Katz H., Rey M

    Cameron A. J., Katz H., Rey M. P., Saxena A., 2023, @doi [MNRAS] 10.1093/mnras/stad1579 , 523, 3516

    2023 doi

  8. [16]

    Campbell A., Terlevich R., Melnick J., 1986, @doi [MNRAS] 10.1093/mnras/223.4.811 , 223, 811

    1986 doi

  9. [17]

    Cappellari M., Copin Y., 2003, @doi [MNRAS] 10.1046/j.1365-8711.2003.06541.x , 342, 345

    2003 doi

  10. [18]

    A., Clayton G

    Cardelli J. A., Clayton G. C., Mathis J. S., 1989, @doi [ApJ] 10.1086/167900 , 345, 245

    1989 doi

  11. [19]

    Castellano M., et al., 2024, @doi [ApJ] 10.3847/1538-4357/ad5f88 , 972, 143

    2024 doi

  12. [20]

    Charbonnel C., Schaerer D., Prantzos N., Ram \' rez-Galeano L., Fragos T., Kuruvanthodi A., Marques-Chaves R., Gieles M., 2023, @doi [ ] 10.1051/0004-6361/202346410 , https://ui.adsabs.harvard.edu/abs/2023A&A...673L...7C 673, L7

    2023 doi

  13. [21]

    M., Turner J

    Consiglio S. M., Turner J. L., Beck S., Meier D. S., Silich S., Zhao J.-H., 2017, @doi [ApJ] 10.3847/1538-4357/aa93dc , 850, 54

    2017 doi

  14. [22]

    A., 2007, @doi [ARA&A] 10.1146/annurev.astro.45.051806.110615 , 45, 177

    Crowther P. A., 2007, @doi [ARA&A] 10.1146/annurev.astro.45.051806.110615 , 45, 177

    2007 doi

  15. [23]

    A., Hadfield L

    Crowther P. A., Hadfield L. J., 2006, @doi [A&A] 10.1051/0004-6361:20054298 , 449, 711

    2006 doi

  16. [24]

    D'Antona F., et al., 2023, @doi [ ] 10.1051/0004-6361/202348240 , https://ui.adsabs.harvard.edu/abs/2023A&A...680L..19D 680, L19

    2023 doi

  17. [25]

    Dartois E., et al., 2024, @doi [Nature Astronomy] 10.1038/s41550-023-02155-x , 8, 359

    2024 doi

  18. [26]

    De Grijs R., Anders P., Zackrisson E., Östlin G., 2013, @doi [MNRAS] 10.1093/mnras/stt392 , 431, 2917

    2013 doi

  19. [27]

    A., Sutherland R

    Dopita M. A., Sutherland R. S., 2003, Astrophysics of the diffuse universe, @doi 10.1007/978-3-662-05866-4. , https://ui.adsabs.harvard.edu/abs/2003adu..book.....D

    2003 doi

  20. [28]

    T., 2003, @doi [ARA&A] 10.1146/annurev.astro.41.011802.094840 , 41, 241

    Draine B. T., 2003, @doi [ARA&A] 10.1146/annurev.astro.41.011802.094840 , 41, 241

    2003 doi arXiv

  21. [29]

    J., Izzard R

    Eldridge J. J., Izzard R. G., Tout C. A., 2008, @doi [MNRAS] 10.1111/j.1365-2966.2007.12738.x , 384, 1109

    2008 doi

  22. [30]

    M., 1992, @doi [ApJ] 10.1086/171303 , 390, 536

    Esteban C., Vilchez J. M., 1992, @doi [ApJ] 10.1086/171303 , 390, 536

    1992 doi

  23. [31]

    Esteban C., Peimbert M., Torres-Peimbert S., Rodriguez M., 2002, @doi [ApJ] 10.1086/344104 , 581, 241

    2002 doi

  24. [32]

    Esteban C., Bresolin F., Peimbert M., García-Rojas J., Peimbert A., Mesa-Delgado A., 2009, @doi [ApJ] 10.1088/0004-637X/700/1/654 , 700, 654

    2009 doi

  25. [33]

    R., Mesa-Delgado A., 2014, @doi [MNRAS] 10.1093/mnras/stu1177 , 443, 624

    Esteban C., García-Rojas J., Carigi L., Peimbert M., Bresolin F., L \'o pez-S \'a nchez A. R., Mesa-Delgado A., 2014, @doi [MNRAS] 10.1093/mnras/stu1177 , 443, 624

    2014 doi

  26. [34]

    E., et al., 1999, @doi [ApJ] 10.1086/307758 , 523, 617

    Falco E. E., et al., 1999, @doi [ApJ] 10.1086/307758 , 523, 617

    1999 doi

  27. [35]

    M., Pérez-Montero E., Candian A., S \'a nchez S

    Fernández-Mart \'i n A., Vílchez J. M., Pérez-Montero E., Candian A., S \'a nchez S. F., Mart \'i n-Gord \'o n D., Riera A., 2013, @doi [A&A] 10.1051/0004-6361/201220773 , 554, A104

    2013 doi

  28. [36]

    Fischer F., Grayson M., Schuberth E., Schuh D., Bichler M., Abstreiter G., 2004, @doi [Physica E Low-Dimensional Systems and Nanostructures] 10.1016/j.physe.2003.11.227 , 22, 108

    2004 doi

  29. [37]

    L., 1999, @doi [PASP] 10.1086/316293 , 111, 63

    Fitzpatrick E. L., 1999, @doi [PASP] 10.1086/316293 , 111, 63

    1999 doi

  30. [38]

    L., Massa D., 1988, @doi [ApJ] 10.1086/166332 , 328, 734

    Fitzpatrick E. L., Massa D., 1988, @doi [ApJ] 10.1086/166332 , 328, 734

    1988 doi

  31. [39]

    Froese Fischer C., Tachiev G., Irimia A., 2006, @doi [Atomic Data and Nuclear Data Tables] https://doi.org/10.1016/j.adt.2006.03.001 , 92, 607

    2006 doi

  32. [40]

    Fétick R. J. L., et al., 2019, @doi [A&A] 10.1051/0004-6361/201935830 , 628, A99

    2019 doi

  33. [41]

    Gaia Collaboration et al., 2023, @doi [A&A] 10.1051/0004-6361/202243940 , https://ui.adsabs.harvard.edu/abs/2023A&A...674A...1G 674, A1

    2023 doi

  34. [42]

    R., 1992, @doi [AJ] 10.1086/116146 , 103, 1330

    Garnett D. R., 1992, @doi [AJ] 10.1086/116146 , 103, 1330

    1992 doi

  35. [43]

    Girardi L., Bressan A., Bertelli G., Chiosi C., 2000, @doi [A&AS] 10.1051/aas:2000126 , 141, 371

    2000 doi

  36. [44]

    M., Papaderos P., 2017, @doi [A&A] 10.1051/0004-6361/201628986 , 603, A63

    Gomes J. M., Papaderos P., 2017, @doi [A&A] 10.1051/0004-6361/201628986 , 603, A63

    2017 doi

  37. [45]

    M., Zhang X., Zhang R., 2024, The Dust Extinction Curve : Beyond R ( V ), http://arxiv.org/abs/2410.22537

    Green G. M., Zhang X., Zhang R., 2024, The Dust Extinction Curve : Beyond R ( V ), http://arxiv.org/abs/2410.22537

    2024

  38. [46]

    G., Izotov Y

    Guseva N. G., Izotov Y. I., Stasińska G., Fricke K. J., Henkel C., Papaderos P., 2011, @doi [A&A] 10.1051/0004-6361/201016291 , 529, A149

    2011 doi

  39. [47]

    Harbeck D., Gallagher J., Crnojević D., 2012, @doi [MNRAS] 10.1111/j.1365-2966.2012.20640.x , 422, 629

    2012 doi

  40. [48]

    Harikane Y., et al., 2025, @doi [ApJ] 10.3847/1538-4357/ad9b2c , 980, 138

    2025 doi

  41. [49]

    S., Smith D

    Harris J., Calzetti D., Gallagher Iii J. S., Smith D. A., Conselice C. J., 2004, @doi [ApJ] 10.1086/381669 , 603, 503

    2004 doi

  42. [50]

    D., 2007, @doi [Computing in Science and Engineering] 10.1109/MCSE.2007.55 , https://ui.adsabs.harvard.edu/abs/2007CSE.....9...90H 9, 90

    Hunter J. D., 2007, @doi [Computing in Science and Engineering] 10.1109/MCSE.2007.55 , https://ui.adsabs.harvard.edu/abs/2007CSE.....9...90H 9, 90

    2007 doi

  43. [51]

    Isobe Y., et al., 2025, JADES : Average Nitrogen Enhancement in High - Redshift Broad - Line Active Galactic Nuclei , @doi 10.48550/arXiv.2502.12091 , http://arxiv.org/abs/2502.12091

    2025 doi

  44. [52]

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

    Izotov Y. I., Stasińska G., Meynet G., Guseva N. G., Thuan T. X., 2006, @doi [A&A] 10.1051/0004-6361:20053763 , 448, 955

    2006 doi

  45. [53]

    I., Thuan T

    Izotov Y. I., Thuan T. X., Guseva N. G., Liss S. E., 2018, @doi [MNRAS] 10.1093/mnras/stx2478 , 473, 1956

    2018 doi

  46. [54]

    I., Guseva N

    Izotov Y. I., Guseva N. G., Fricke K. J., Henkel C., Schaerer D., Thuan T. X., 2021, @doi [A&A] 10.1051/0004-6361/202039772 , 646, A138

    2021 doi

  47. [55]

    I., Schaerer D., Worseck G., Berg D., Chisholm J., Ravindranath S., Thuan T

    Izotov Y. I., Schaerer D., Worseck G., Berg D., Chisholm J., Ravindranath S., Thuan T. X., 2023, @doi [MNRAS] 10.1093/mnras/stad1036 , 522, 1228

    2023 doi

  48. [56]

    L., Tsamis Y

    James B. L., Tsamis Y. G., Barlow M. J., Westmoquette M. S., Walsh J. R., Cuisinier F., Exter K. M., 2009, @doi [MNRAS] 10.1111/j.1365-2966.2009.15172.x , 398, 2

    2009 doi

  49. [57]

    L., Tsamis Y

    James B. L., Tsamis Y. G., Walsh J. R., Barlow M. J., Westmoquette M. S., 2013, @doi [MNRAS] 10.1093/mnras/stt034 , 430, 2097

    2013 doi

  50. [58]

    Ji X., et al., 2024, @doi [MNRAS] 10.1093/mnras/stae2375 , 535, 881

    2024 doi

  51. [59]

    D., et al., 2007, @doi [AJ] 10.1086/510125 , 133, 504

    Karachentsev I. D., et al., 2007, @doi [AJ] 10.1086/510125 , 133, 504

    2007 doi

  52. [60]

    C., 2007, @doi [Publications of the Astronomical Society of Australia] 10.1071/AS07021 , 24, 103

    Karakas A., Lattanzio J. C., 2007, @doi [Publications of the Astronomical Society of Australia] 10.1071/AS07021 , 24, 103

    2007 doi

  53. [61]

    J., Ferland G

    Kisielius R., Storey P. J., Ferland G. J., Keenan F. P., 2009, @doi [MNRAS] 10.1111/j.1365-2966.2009.14989.x , 397, 903

    2009 doi

  54. [62]

    Knutas A., et al., 2025, FEAST : JWST uncovers the emerging timescales of young star clusters in M83 , @doi 10.48550/arXiv.2505.08874 , http://arxiv.org/abs/2505.08874

    2025 doi

  55. [63]

    A., Skillman E

    Kobulnicky H. A., Skillman E. D., 2008, @doi [AJ] 10.1088/0004-6256/135/2/527 , 135, 527

    2008 doi

  56. [64]

    A., Skillman E

    Kobulnicky H. A., Skillman E. D., Roy J.-R., Walsh J. R., Rosa M. R., 1997, @doi [ApJ] 10.1086/303742 , 477, 679

    1997 doi

  57. [65]

    Kramida A., 2010, @doi [Atomic Data and Nuclear Data Tables] https://doi.org/10.1016/j.adt.2010.05.001 , 96, 586

    2010 doi

  58. [66]

    J., 2006, @doi [A&AS] 10.1086/505579 , 166, 188

    Labrie K., Pritchet C. J., 2006, @doi [A&AS] 10.1086/505579 , 166, 188

    2006 doi

  59. [67]

    R., Esteban C., 2010, @doi [A&A] 10.1051/0004-6361/200913434 , 516, A104

    L \'o pez-S \'a nchez \'A . R., Esteban C., 2010, @doi [A&A] 10.1051/0004-6361/200913434 , 516, A104

    2010 doi

  60. [68]

    R., Mesa-Delgado A., L \'o pez-Mart \'i n L., Esteban C., 2011, @doi [MNRAS] 10.1111/j.1365-2966.2010.17847.x , 411, 2076

    L \'o pez-S \'a nchez \'A . R., Mesa-Delgado A., L \'o pez-Mart \'i n L., Esteban C., 2011, @doi [MNRAS] 10.1111/j.1365-2966.2010.17847.x , 411, 2076

    2011 doi

  61. [69]

    R., Koribalski B

    L \'o pez-S \'a nchez \'A . R., Koribalski B. S., Van Eymeren J., Esteban C., Kirby E., Jerjen H., Lonsdale N., 2012, @doi [MNRAS] 10.1111/j.1365-2966.2011.19762.x , 419, 1051

    2012 doi

  62. [70]

    R., Esteban C., Garcia‐Rojas J., Peimbert M., Rodriguez M., 2007, @doi [ApJ] 10.1086/510112 , 656, 168

    Lopez‐Sanchez A. R., Esteban C., Garcia‐Rojas J., Peimbert M., Rodriguez M., 2007, @doi [ApJ] 10.1086/510112 , 656, 168

    2007 doi

  63. [71]

    A., 2015, @doi [A&A] 10.1051/0004-6361/201323152 , 573, A42

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

    2015 doi

  64. [72]

    Maeder A., Meynet G., 1994, , https://ui.adsabs.harvard.edu/abs/1994A&A...287..803M 287, 803

    1994

  65. [73]

    Marasco A., et al., 2023, @doi [A&A] 10.1051/0004-6361/202244895 , 670, A92

    2023 doi

  66. [74]

    Marques-Chaves R., et al., 2024, @doi [A&A] 10.1051/0004-6361/202347411 , 681, A30

    2024 doi

  67. [75]

    C., Zalubas R., Musgrove A., 1990, @doi [Journal of Physical and Chemical Reference Data] 10.1063/1.555862 , 19, 821

    Martin W. C., Zalubas R., Musgrove A., 1990, @doi [Journal of Physical and Chemical Reference Data] 10.1063/1.555862 , 19, 821

    1990 doi

  68. [76]

    C., Kaufman V., Musgrove A., 1993, @doi [Journal of Physical and Chemical Reference Data] 10.1063/1.555928 , 22, 1179

    Martin W. C., Kaufman V., Musgrove A., 1993, @doi [Journal of Physical and Chemical Reference Data] 10.1063/1.555928 , 22, 1179

    1993 doi

  69. [77]

    Martins F., Schaerer D., Marques-Chaves R., Upadhyaya A., 2023, @doi [A&A] 10.1051/0004-6361/202346732 , 678, A159

    2023 doi

  70. [78]

    S., Turner J

    Meier D. S., Turner J. L., Beck S. C., 2002, @doi [AJ] 10.1086/341752 , 124, 877

    2002 doi

  71. [79]

    Meynet G., Maeder A., 2005, @doi [A&A] 10.1051/0004-6361:20047106 , 429, 581

    2005 doi

  72. [80]

    E., Espada D., Sugai H., Nakanishi K., Hirota A., 2015, @doi [PASJ] 10.1093/pasj/psu138 , 67, L1

    Miura R. E., Espada D., Sugai H., Nakanishi K., Hirota A., 2015, @doi [PASJ] 10.1093/pasj/psu138 , 67, L1

    2015 doi

  73. [81]

    M., Walsh J

    Monreal-Ibero A., Vílchez J. M., Walsh J. R., Muñoz-Tuñón C., 2010, @doi [A&A] 10.1051/0004-6361/201014154 , 517, A27

    2010 doi

  74. [82]

    R., Vílchez J

    Monreal-Ibero A., Walsh J. R., Vílchez J. M., 2012, @doi [A&A] 10.1051/0004-6361/201219543 , 544, A60

    2012 doi

  75. [83]

    R., Westmoquette M

    Monreal-Ibero A., Walsh J. R., Westmoquette M. S., Vílchez J. M., 2013, @doi [A&A] 10.1051/0004-6361/201321387 , 553, A57

    2013 doi

  76. [84]

    E., 1993, in Gallagher J

    Moore C. E., 1993, in Gallagher J. W., ed., , CRC Series in Evaluated Data in Atomic Physics. CRC Press, Boca Raton, FL

    1993

  77. [85]

    E., et al., 2023, @doi [MNRAS] 10.1093/mnras/stad1569 , 523, 2952

    Méndez-Delgado J. E., et al., 2023, @doi [MNRAS] 10.1093/mnras/stad1569 , 523, 2952

    2023 doi

  78. [86]

    E., Ferland G

    Osterbrock D. E., Ferland G. J., 2006, Astrophysics of gaseous nebulae and active galactic nuclei. https://ui.adsabs.harvard.edu/abs/2006agna.book.....O

    2006

  79. [87]

    F., Tsang B

    Pascale M., Dai L., McKee C. F., Tsang B. T. H., 2023, @doi [ApJ] 10.3847/1538-4357/acf75c , 957, 77

    2023 doi

  80. [88]

    Patrício V., et al., 2016, @doi [MNRAS] 10.1093/mnras/stv2859 , 456, 4191

    2016 doi

  81. [89]

    C., 1895, Harvard College Observatory Circular, 4, 1

    Pickering E. C., 1895, Harvard College Observatory Circular, 4, 1

  82. [90]

    S., Grebel E

    Pilyugin L. S., Grebel E. K., Mattsson L., 2012, @doi [MNRAS] 10.1111/j.1365-2966.2012.21398.x , 424, 2316

    2012 doi

  83. [91]

    arXiv:1710.03554

    Piqueras L., Conseil S., Shepherd M., Bacon R., Leclercq F., Richard J., 2017, @doi [arXiv e-prints] 10.48550/arXiv.1710.03554 , https://ui.adsabs.harvard.edu/abs/2017arXiv171003554P p. arXiv:1710.03554

    2017 doi arXiv

  84. [92]

    Plante S., Sauvage M., 2002, @doi [AJ] 10.1086/342445 , 124, 1995

    2002 doi

  85. [93]

    L., Ferland G

    Porter R. L., Ferland G. J., Storey P. J., Detisch M. J., 2012, @doi [MNRAS] 10.1111/j.1745-3933.2012.01300.x , 425, L28

    2012 doi

  86. [94]

    L., Ferland G

    Porter R. L., Ferland G. J., Storey P. J., Detisch M. J., 2013, @doi [MNRAS] 10.1093/mnrasl/slt049 , 433, L89

    2013 doi

  87. [95]

    E., et al., 2024, @doi [ ] 10.1051/0004-6361/202450359 , https://ui.adsabs.harvard.edu/abs/2024A&A...690A.269R 690, A269

    Rivera-Thorsen T. E., et al., 2024, @doi [ ] 10.1051/0004-6361/202450359 , https://ui.adsabs.harvard.edu/abs/2024A&A...690A.269R 690, A269

    2024 doi

  88. [96]

    Rogers N. S. J., Skillman E. D., Pogge R. W., Berg D. A., Moustakas J., Croxall K. V., Sun J., 2021, @doi [ApJ] 10.3847/1538-4357/abf8b9 , 915, 21

    2021 doi

  89. [97]

    Rogers C., Brandl B., de Marchi G., 2024, Spectral characterisation of the extinction properties of NGC 3603 using JWST NIRSpec , http://arxiv.org/abs/2405.08445

    2024

  90. [98]

    Rynkun P., Gaigalas G., Jönsson P., 2019, @doi [A&A] 10.1051/0004-6361/201834931 , 623, A155

    2019 doi

  91. [99]

    Sakai S., Ferrarese L., Kennicutt Jr. R. C., Saha A., 2004, @doi [ApJ] 10.1086/386540 , 608, 42

    2004 doi

  92. [100]

    Salim S., Narayanan D., 2020, @doi [Annual Review of A&A ] 10.1146/annurev-astro-032620-021933 , 58, 529

    2020 doi

  93. [101]

    C., 2018, @doi [ApJ] 10.3847/1538-4357/aabf3c , 859, 11

    Salim S., Boquien M., Lee J. C., 2018, @doi [ApJ] 10.3847/1538-4357/aabf3c , 859, 11

    2018 doi

  94. [102]

    E., 1955, @doi [ ] 10.1086/145971 , https://ui.adsabs.harvard.edu/abs/1955ApJ...121..161S 121, 161

    Salpeter E. E., 1955, @doi [ ] 10.1086/145971 , https://ui.adsabs.harvard.edu/abs/1955ApJ...121..161S 121, 161

    1955 doi

  95. [103]

    D., Mathis J

    Savage B. D., Mathis J. S., 1979, @doi [ARA&A] 10.1146/annurev.aa.17.090179.000445 , 17, 73

    1979 doi

  96. [104]

    Schaerer D., 1996, @doi [ApJ] 10.1086/310193 , 467, L17

    1996 doi

  97. [105]

    D., 1998, @doi [ApJ] 10.1086/305487 , 497, 618

    Schaerer D., Vacca W. D., 1998, @doi [ApJ] 10.1086/305487 , 497, 618

    1998 doi

  98. [106]

    Schaerer D., Contini T., Kunth D., Meynet G., 1997, @doi [ApJ] 10.1086/310659 , 481, L75

    1997 doi

  99. [107]

    Schaerer D., Marques-Chaves R., Xiao M., Korber D., 2024, @doi [A&A] 10.1051/0004-6361/202450721 , 687, L11

    2024 doi

  100. [108]

    F., Finkbeiner D

    Schlafly E. F., Finkbeiner D. P., 2011, @doi [ApJ] 10.1088/0004-637X/737/2/103 , 737, 103

    2011 doi

  101. [109]

    P., Rudie G

    Senchyna P., Plat A., Stark D. P., Rudie G. C., Berg D., Charlot S., James B. L., Mingozzi M., 2024, @doi [ApJ] 10.3847/1538-4357/ad235e , 966, 92

    2024 doi

  102. [110]

    J., Crowther P

    Smith L. J., Crowther P. A., Calzetti D., Sidoli F., 2016, @doi [ApJ] 10.3847/0004-637X/823/1/38 , 823, 38

    2016 doi

  103. [111]

    J., Bajaj V., Ryon J., Sabbi E., 2020, @doi [ApJ] 10.3847/1538-4357/ab8f94 , 896, 84

    Smith L. J., Bajaj V., Ryon J., Sabbi E., 2020, @doi [ApJ] 10.3847/1538-4357/ab8f94 , 896, 84

    2020 doi

  104. [112]

    Stasinska G., 2002, Abundance determinations in HII regions and planetary nebulae, http://arxiv.org/abs/astro-ph/0207500

    2002 arXiv

  105. [113]

    J., Hummer D

    Storey P. J., Hummer D. G., 1995, @doi [MNRAS] 10.1093/mnras/272.1.41 , 272, 41

    1995 doi

  106. [114]

    J., Zeippen C

    Storey P. J., Zeippen C. J., 2000, @doi [MNRAS] 10.1046/j.1365-8711.2000.03184.x , 312, 813

    2000 doi

  107. [115]

    J., Sochi T., Badnell N

    Storey P. J., Sochi T., Badnell N. R., 2014, @doi [MNRAS] 10.1093/mnras/stu777 , 441, 3028

    2014 doi

  108. [116]

    Stuik R., Bacon R., Conzelmann R., Delabre B., Fedrigo E., Hubin N., Le Louarn M., Str \"o bele S., 2006, @doi [ ] 10.1016/j.newar.2005.10.015 , https://ui.adsabs.harvard.edu/abs/2006NewAR..49..618S 49, 618

    2006 doi

  109. [117]

    Sun J., et al., 2024, @doi [ApJ] 10.3847/1538-4357/ad3de6 , 967, 133

    2024 doi

  110. [118]

    S., Gupta G

    Tayal S. S., Gupta G. P., 1999, @doi [ApJ] 10.1086/307971 , 526, 544

    1999 doi

  111. [119]

    S., Zatsarinny O., 2010, @doi [A&AS] 10.1088/0067-0049/188/1/32 , 188, 32

    Tayal S. S., Zatsarinny O., 2010, @doi [A&AS] 10.1088/0067-0049/188/1/32 , 188, 32

    2010 doi

  112. [120]

    A., Archer I., 2017, @doi [MNRAS] 10.1093/mnras/stx2124 , 472, 4618

    Tehrani K., Crowther P. A., Archer I., 2017, @doi [MNRAS] 10.1093/mnras/stx2124 , 472, 4618

    2017 doi

  113. [121]

    W., et al., 2024, @doi [MNRAS] 10.1093/mnras/stae682 , 529, 3301

    Topping M. W., et al., 2024, @doi [MNRAS] 10.1093/mnras/stae682 , 529, 3301

    2024 doi

  114. [122]

    A., Calzetti D., Leitherer C., Heckman T

    Tremonti C. A., Calzetti D., Leitherer C., Heckman T. M., 2001, @doi [ApJ] 10.1086/321436 , 555, 322

    2001 doi

  115. [123]

    L., Beck S

    Turner J. L., Beck S. C., Ho P. T. P., 2000, @doi [ApJ] 10.1086/312586 , 532, L109

    2000 doi

  116. [124]

    L., Consiglio S

    Turner J. L., Consiglio S. M., Beck S. C., Goss W. M., Ho P. T. P., Meier D. S., Silich S., Zhao J.-H., 2017, @doi [ApJ] 10.3847/1538-4357/aa8669 , 846, 73

    2017 doi

  117. [125]

    Ueta T., Otsuka M., 2021, @doi [PASP] 10.1088/1538-3873/ac20ab , 133, 093002

    2021 doi

  118. [126]

    C., Varoquaux G., 2011, @doi [Computing in Science and Engineering] 10.1109/MCSE.2011.37 , https://ui.adsabs.harvard.edu/abs/2011CSE....13b..22V 13, 22

    Van Der Walt S., Colbert S. C., Varoquaux G., 2011, @doi [Computing in Science and Engineering] 10.1109/MCSE.2011.37 , https://ui.adsabs.harvard.edu/abs/2011CSE....13b..22V 13, 22

    2011 doi

  119. [128]

    Vaught R. J. R., et al., 2024, Investigating the Drivers of Electron Temperature Variations in HII Regions with Keck - KCWI and VLT - MUSE , http://arxiv.org/abs/2309.17440

    2024

  120. [129]

    B., Edmunds M

    Vila-Costas M. B., Edmunds M. G., 1993, @doi [MNRAS] 10.1093/mnras/265.1.199 , 265, 199

    1993 doi

  121. [130]

    M., 2004, @doi [MNRAS] 10.1111/j.1365-2966.2004.08395.x , 355, 1132

    Villar-Mart \'i n M., Cerviño M., González Delgado R. M., 2004, @doi [MNRAS] 10.1111/j.1365-2966.2004.08395.x , 355, 1132

    2004 doi

  122. [131]

    Vincenzo F., Belfiore F., Maiolino R., Matteucci F., Ventura P., 2016, @doi [MNRAS] 10.1093/mnras/stw532 , 458, 3466

    2016 doi

  123. [132]

    Virtanen P., et al., 2020, @doi [Nature Methods] 10.1038/s41592-019-0686-2 , https://ui.adsabs.harvard.edu/abs/2020NatMe..17..261V 17, 261

    2020 doi

  124. [133]

    Vogt F. P. A., et al., 2017, @doi [Physical Review X] 10.1103/PhysRevX.7.021044 , http://cdsads.u-strasbg.fr/abs/2017PhRvX...7b1044V 7, 021044

    2017 doi

  125. [134]

    R., Roy J.-R., 1989, @doi [MNRAS] 10.1093/mnras/239.2.297 , 239, 297

    Walsh J. R., Roy J.-R., 1989, @doi [MNRAS] 10.1093/mnras/239.2.297 , 239, 297

    1989 doi

  126. [135]

    Watanabe K., et al., 2024, @doi [ ] 10.3847/1538-4357/ad13ff , https://ui.adsabs.harvard.edu/abs/2024ApJ...962...50W 962, 50

    2024 doi

  127. [136]

    M., et al., 2020, @doi [ ] 10.1051/0004-6361/202037855 , https://ui.adsabs.harvard.edu/abs/2020A&A...641A..28W 641, A28

    Weilbacher P. M., et al., 2020, @doi [ ] 10.1051/0004-6361/202037855 , https://ui.adsabs.harvard.edu/abs/2020A&A...641A..28W 641, A28

    2020 doi

  128. [137]

    C., Draine B

    Weingartner J. C., Draine B. T., 2001, @doi [ApJ] 10.1086/324035 , 563, 842

    2001 doi

  129. [138]

    E., Fowler J

    Welty D. E., Fowler J. R., 1992, @doi [ApJ] 10.1086/171497 , 393, 193

    1992 doi

  130. [139]

    S., James B., Monreal-Ibero A., Walsh J

    Westmoquette M. S., James B., Monreal-Ibero A., Walsh J. R., 2013, @doi [A&A] 10.1051/0004-6361/201220580 , 550, A88

    2013 doi

  131. [140]

    S., Seaman R

    Wevers T., et al., 2022, in Adler D. S., Seaman R. L., Benn C. R., eds, Proc.\ SPIE Vol. 12186, Observatory Operations: Strategies, Processes, and Systems IX. p. 121860T ( @eprint arXiv 2209.07540 ), @doi 10.1117/12.2630835

    2022 doi

  132. [141]

    L., Fuhr J

    Wiese W. L., Fuhr J. R., Deters T. M., 1996, Atomic transition probabilities of carbon, nitrogen, and oxygen : a critical data compilation. https://ui.adsabs.harvard.edu/abs/1996atpc.book.....W

    1996

  133. [142]

    S., Veilleux S., McDonald M., Martin C

    Zastrow J., Oey M. S., Veilleux S., McDonald M., Martin C. L., 2011, @doi [ApJ] 10.1088/2041-8205/741/1/L17 , 741, L17

    2011 doi

  134. [143]

    M., 2025, @doi [Science] 10.1126/science.ado9787 , https://ui.adsabs.harvard.edu/abs/2025Sci...387.1209Z 387, 1209

    Zhang X., Green G. M., 2025, @doi [Science] 10.1126/science.ado9787 , https://ui.adsabs.harvard.edu/abs/2025Sci...387.1209Z 387, 1209

    2025 doi

  135. [144]

    S., Green G

    Zhang X., Hensley B. S., Green G. M., 2024, Dust extinction-curve variation in the translucent interstellar medium is driven by PAH growth, http://arxiv.org/abs/2410.23171

    2024

Pith tools

Reviewed May 21, 2026 · model on record in the stance chip above.