Unveiling Metal Mixing in a Grand-Design Spiral: A UV-optical multiphase spatially resolved study of M83

Adarsh Ranjan; Alessandra Aloisi; Bethan L. James; Nimisha Kumari; Peter Zeidler; R. Rickards Vaught; Svea Hernandez

REVIEW 3 major objections 4 minor 291 references

Unveiling Metal Mixing in a Grand-Design Spiral: A UV-optical multiphase spatially resolved study of M83

T0 review · 3 major / 4 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read In the spiral M83, nitrogen freshly released by massive stars stays locked in the ionized gas around young clusters, showing a persistent ~1.5 dex offset from the neutral phase that does not close within 6 Myr, unlike the dwarf NGC 5253.

desk verdict Persistent ~1.5 dex nitrogen phase offset in M83 is a genuinely new result, but it rests on a strong-line Te calibration partly trained on M83 itself; worth refereeing with a required hold-out or direct Te(NII) check. read the letter →

arxiv 2608.09064 v1 pith:UJRCTHMZ submitted 2026-08-10 astro-ph.GA

Adarsh Ranjan , Bethan L. James , Svea Hernandez , R. Rickards Vaught , Nimisha Kumari , Alessandra Aloisi , Peter Zeidler This is my paper · ORCID

classification astro-ph.GA

keywords galaxychemicalevolutionmetalmixingmultiphaseinterstellarmediumabundancegradientsHIIregionabundancesneutralgasabsorptionspectroscopyyoungstarclustersM83

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper tries to establish how freshly produced metals move between the two gas phases that surround young star clusters: the ionized gas lit by the stars and the larger reservoir of cold neutral gas. Using 18 clusters in the nearby spiral M83, the authors combine ultraviolet absorption lines, which see neutral gas, with aperture-matched optical emission lines, which see ionized gas, to compare oxygen, sulphur, nitrogen, and iron in both phases. Their central result is that nitrogen shows a large and persistent phase offset, roughly 1.5 dex in N/H and more than 1.5 dex in N/O, with freshly made nitrogen staying in the ionized gas and failing to mix into the neutral reservoir over the ~1–6 Myr ages of the clusters. This contrasts with the low-mass dwarf NGC 5253, where the same offset closes within about 8 Myr. If right, it means mixing efficiency depends on environment: the deep potential well of a massive spiral confines wind-driven metals to the immediate star-forming region for at least several million years.

What carries the argument

The load-bearing comparison is the multiphase abundance offset $Δ$(X/H) = (X/H)$_{HII}$ − (X/H)$_{HI}$, computed element by element for cospatial ionized and neutral gas. Neutral abundances come from multi-component Voigt-profile fits to HST/COS ultraviolet absorption lines (N I, S II, O I via S II, Fe II) with CLOUDY-based ionization corrections; ionized abundances come from reddening-corrected optical emission lines reduced with pyneb. Because auroral lines are undetectable in most of M83's metal-rich H II regions, the paper builds an empirical multi-zone electron-temperature calibration: linear fits, restricted to the metal-rich regime (12+log(O/H) > 8.0) and anchored on literature direct-method H II regions, that predict T$_e$(O III) from the O3N2 diagnostic, T$_e$(S III) from S3O3, and T$_e$(O II) from a combined DESIRED metallicity estimator. These predicted temperatures are what convert raw line fluxes into the ionized-phase abundances whose offsets carry the central claim.

What would settle it

Take deep optical spectra of a handful of these 18 H II regions to detect the auroral lines directly, [O III] λ4363, [N II] λ5755, and [S III] λ6312, and recompute the ionized-phase abundances with measured rather than predicted temperatures. If the direct-method temperatures are systematically higher than the empirical calibration predicts, the ionized N/H values drop and the nitrogen phase offset would fall well below 1 dex; alternatively, if deeper UV spectra reveal that the N I absorption used for neutral nitrogen is partially saturated, the neutral nitrogen abundance would rise and close the offset.

Watch

Extended reading notes

Core claim

The paper claims that in M83, nitrogen released by the current generation of massive O and B stars remains trapped in the ionized gas surrounding young clusters and does not transfer into the cold neutral gas on timescales of at least 6 Myr. The evidence is a systematic offset between neutral-phase and ionized-phase abundances: ionized gas shows N/H about 1.3–1.6 dex higher and N/O more than 1.5 dex higher than cospatial neutral gas, across all 18 clusters with no sign of closing with cluster age. Oxygen and sulphur, by contrast, show smaller and age-dependent offsets consistent with prompt core-collapse supernova enrichment on ~3–5 Myr timescales, while the ~1 dex iron offset is attributed mainly to dust depletion rather than nucleosynthesis. The authors interpret the nitrogen behaviour as a signature of feedback-regulated enrichment in a deep gravitational potential: strong stellar winds efficiently enrich the local ionized medium, but the potential well and dense interstellar medium inhibit dispersal of the enriched material into the surrounding H I reservoir, unlike in the low-mass starburst NGC 5253 where such offsets vanish within about 8 Myr.

Load-bearing premise

The ionized-phase nitrogen abundances rest on electron temperatures that were not measured but predicted from strong-line ratios calibrated on other H II regions; if those temperature predictions run systematically hot or cold for M83's specific metal-rich, high-density conditions, every ionized abundance shifts and the claimed ~1.5 dex nitrogen offset could shrink or vanish.

Editorial extensions

If this is right

In a massive, metal-rich spiral, freshly synthesised nitrogen from massive stars remains confined to H II regions for at least ~6 Myr, so neutral-gas abundances understate the recent enrichment of the interstellar medium.
Phase offsets of the alpha elements oxygen and sulphur grow with cluster age, consistent with core-collapse supernova enrichment appearing in the ionized phase on ~3–5 Myr timescales.
The roughly 1 dex iron excess in ionized gas relative to neutral gas is dominated by dust depletion of iron in the cold phase rather than by nucleosynthesis, so iron phase offsets should not be read as enrichment clocks.
The persistence of the nitrogen offset is environment-dependent: the same enrichment channel closes within ~8 Myr in the low-mass galaxy NGC 5253 but not in M83, linking chemical mixing efficiency to the depth of the galactic potential well.
Adopting spectroscopically derived rather than photometric cluster ages shortens the inferred mixing timescale in NGC 5253 to about 8 Myr, sharpening the contrast between the dwarf and the spiral.

Reading between the lines

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

If the offset really persists beyond 6 Myr, clusters in M83 at ages of ~10–30 Myr should still show elevated N/O in their ionized surroundings; observing such older clusters would test whether the confinement timescale scales with potential-well depth.
The nitrogen missing from the neutral reservoir may reside in warm molecular gas: following the paper's own finding that the center of M83 holds mostly warm H2, a testable extension is to search for the 'missing' nitrogen in CO-dark molecular gas using infrared H2 lines.
A corollary the authors leave implicit is that outflows from M83 should be metal-poor relative to the star-formation rate compared with dwarfs like NGC 5253, since metals stay trapped in the disk; this is testable through circumgalactic absorption-line surveys.
The empirical multi-zone temperature calibration is a portable tool: applied to other metal-rich spirals where auroral lines are undetectable, it would allow the same multiphase comparison without direct temperature measurements, with the caveat that its accuracy depends on how well the calibration sample matches the target's physical conditions.

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Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

Here's the short version. The genuinely new item is the persistent ~1.5 dex nitrogen phase offset in M83: ionized gas around clusters aged 1–6 Myr shows N/H well above the neutral gas, with no sign of the convergence seen in NGC 5253 on ~8 Myr timescales. If that survives scrutiny, it is a real constraint on metal mixing in massive spirals.

What the paper does well: it is the first cluster-scale multiphase comparison in a metal-rich grand-design spiral covering O, S, N, and Fe rather than one or two elements. The UV absorption work is careful—multi-component Voigt fits, saturation checks, ICFs from cloudy models, and a sensible decision to leave depletion corrections out of the main analysis rather than apply Milky Way prescriptions to M83. The authors are transparent about the weak auroral lines and about the need for a strong-line Te calibration.

The soft spots are real but not fatal. The electron temperatures that feed every ionized abundance come from linear fits (Appendix G) calibrated on literature H ii regions that include M83 itself (Bresolin et al. 2005). Applying that fit to M83 YSC sightlines is partially circular: the reported ~0.02 dex scatter is on the calibration set, not independent predictive accuracy for these dense, metal-rich regions. A 20% Te bias shifts N/H by ~0.25 dex; it will not erase a 1.5 dex offset, but it could reduce it to ~1.2 dex, which matters for the quantitative contrast with NGC 5253. There are five regions with direct [NII]5755 detections where predicted Te could be checked against measurement; the paper does not show that comparison. It should.

Other concerns are minor: quoted errors are random only, systematic Te/ICF uncertainties are not propagated; the galactic center exclusion is post hoc but follows Hernandez et al. (2021) and the extreme N(HI) values there. The age trends are based on small samples and should be read as suggestive.

Who is this for: anyone working on chemical enrichment, ISM mixing, or young clusters. It deserves a serious referee—the dataset is valuable, the main claim is testable, and a good referee can ask for the hold-out check and better error propagation. Desk rejection would waste the effort already invested.

Referee Report

3 major / 4 minor

Summary. This paper combines HST/COS far-UV absorption spectroscopy with cospatial VLT/MUSE and LBT/MODS optical emission-line spectroscopy for 18 young star clusters in M83 (ages ~1–6 Myr) to derive multiphase (neutral H I and ionized H II) abundances of O, S, N, and Fe. Because auroral lines are mostly undetected, the authors build and apply an empirical strong-line electron-temperature calibration (Appendix G) to compute ionized-phase abundances with pyneb. The paper's central result is a large and persistent ionized-to-neutral nitrogen offset, typically ΔN/H ≈ 1.3–1.6 dex and ΔN/O > 1.5 dex, which is interpreted as evidence that freshly produced nitrogen from massive-star winds remains in the ionized gas and does not mix into the neutral reservoir on Myr timescales. This is contrasted with NGC 5253, where such offsets shrink within ~8 Myr. The paper also reports weaker phase offsets for α-elements, an iron excess attributed to dust depletion, and radial trends that differ between the phases.

Significance. If the central nitrogen-offset claim holds, the paper provides a rare, cluster-scale empirical constraint on multiphase metal mixing in a massive, metal-rich spiral, complementing the dwarf-galaxy picture from NGC 5253 and the CLASSY survey. The study is notable for its genuinely cospatial, multi-element (O, S, N, Fe) design, for deriving stellar ages/metallicities from UV spectral fitting, and for being transparent about key limitations: auroral non-detections, the absence of depletion corrections, the exclusion of the galactic center, and the use of ionization corrections calibrated on previous M83 work. The main claim is also falsifiable in a concrete way: direct auroral measurements in five regions and older clusters can test whether the offset is real and whether it persists. These strengths outweigh, for now, the validation gaps discussed below, but those gaps need to be closed before the quantitative claim can be considered secure.

major comments (3)

[Appendix G, Eqs. (G3)–(G6); Fig. 28] The T_e calibration is fit on literature H II regions that include Bresolin et al. (2005) M83 regions, so the quoted WRMS of 0.018–0.026 dex is an in-sample scatter, not a predictive accuracy for the metal-rich, relatively high-density M83 sightlines studied here. Because every ionized-phase abundance in Table 6 is computed from these predicted temperatures, the central ΔN/H claim in Section 5.2.1 inherits this systematic uncertainty. Since the [NII] abundance scales roughly as T^{0.5} exp(25000/T), a 20% bias in T_e(NII) at ~7000 K shifts log(N/H) by about 0.25 dex; this would not erase a 1.5 dex offset but could reduce it to ~1.2 dex and weaken the quantitative contrast with NGC 5253. Please add a leave-one-out or hold-out validation (in particular excluding all M83 calibration points) and propagate the resulting T_e systematics into the reported N/H and N/O values.
[Section 3.3.1, Tables 5 and 9] The paper states that [NII]λ5755 is detected in five regions (M83-3, R1, R2, R7, R12), but Table 9 lists upper limits for R1, R2, and R12 in that line, and Table 5 is captioned as derived entirely from the strong-line calibration. No direct T_e(NII) from the claimed detections is compared with the G6-based predicted T_e(NII). Please reconcile the detection list, mark direct versus predicted temperatures in Table 5, and present a direct-versus-predicted T_e(NII) comparison for every region with a meaningful auroral measurement.
[Section 5.2.1, Fig. 18] The claim that the nitrogen offset 'does not diminish with cluster age' rests on a weak, non-significant correlation (r = 0.17, p = 0.65 for ΔN/H; the N/O trends in Fig. 18 are also non-significant). With only a 1–6 Myr age baseline, the data support 'no detected decline', not 'no decline'. Please state this as a non-detection with a bounded slope or credible interval, and adjust the abstract/summary wording from 'persistent' to 'no significant evolution over the sampled ages' where that is all the data can support.

minor comments (4)

[Abstract and Section 5.2.1] The abstract quotes 'up to ΔN/H ~ 1.5 dex', but Tables 4 and 6 imply a maximum disk offset of about 2.0 dex for M83-7 (8.07 − 6.07); please reconcile the quoted range with the tabulated values.
[Appendix G, Eqs. (G3)–(G6)] The printed equations contain malformed bracket/comma notation (e.g., '[Te(O,III) = (0.68±0.07),O3N2 + (9.73±0.62),]'); these should be written as proper equations, and the units and axes of Figure 27 should be clarified, since the caption appears to reverse the roles of the abundance and temperature axes.
[Section F.2] The text refers to 'M83-POS-15', which is not a target in Table 2; this appears to be a typo for M83-15 or M83-POS-2.
[Figure 18 caption] The caption reads 'follow the same format Figure. 7' and should read 'follow the same format as Figure 7'; similar minor grammatical issues appear in a few other captions.

Circularity Check

1 steps flagged · score 6.0 of 10

Ionized-phase Te 'predictions' are fits on a literature sample that includes M83, and the Appendix G 'validation' is in-sample; the nitrogen offset still has independent content.

fitted input called prediction [Appendix G, Eqs. G3-G6 and Figure 28; applied via Section 3.3.1 and Table 5]
"These three relations are subsequently adopted to predict T_e(OII), T_e(OIII), and T_e(SIII) for the M83 HII regions. ... To assess the performance of the derived temperature relations, we applied the predicted values of T_e(OII), T_e(OIII), and T_e(SIII) to all literature HII regions and recalculated their elemental abundances using the direct method. These abundances were then compared to the corresponding direct-method abundances reported in the literature (See Figure. 28)."

The 'literature HII regions' used for the performance test are the same sample used to build the fits: Appendix G compiles 'F. Bresolin & R. C. Kennicutt 2002; F. Bresolin et al. 2005, 2009', and Section 5.1.4 identifies Bresolin et al. (2005) as HII regions in M83. Equations G3-G6 are linear fits of Te to strong-line diagnostics; calling their outputs 'predicted Te' and then validating them on the calibration sample (Figure 28, WRMS~0.02 dex) is an in-sample test, not out-of-sample prediction. The M83 YSC ionized abundances, including N/H and N/O, are then computed with Te values read off these same fitted relations for a galaxy that contributed to the fit, so part of the quoted abundance accuracy is imported from the fit rather than demonstrated independently.

full rationale

The central nitrogen-offset claim has two legs: neutral N/H from COS absorption (Table 4) and ionized N/H from [NII]+ICF+Te (Table 6). The latter leg depends on the Appendix G strong-line temperature calibration. The calibration is built from literature HII regions including Bresolin et al. (2005), which the paper itself elsewhere uses as 'direct oxygen abundance measurements of HII regions from the M83 literature' (Section 5.1.4); the fitted relations (Eqs. G3-G6) are then applied to the M83 YSC HII regions, and the reported WRMS validation (Fig. 28) is computed on the same literature sample used for the fit. That is an in-sample 'prediction,' so the small scatter does not establish out-of-sample accuracy for M83. This is partial circularity: a Te bias of ~20% shifts ionized N/H by only ~0.25 dex, so the 1.3-1.6 dex offset is not purely an artefact; neutral N/H is directly measured, and five regions have direct [NII]5755 temperatures, though no comparison of predicted vs direct Te is shown. The O-from-S substitution in the neutral phase is disclosed ('the oxygen column density is derived directly from sulphur'), so neutral oxygen trends are not independent but this does not affect the neutral nitrogen measurement. No uniqueness theorem or ansatz is smuggled via self-citation; overlapping-author citations (Hernandez et al. 2021 CLOUDY ICFs, Hernandez et al. 2019 stellar priors) are either small corrections or prior independent results. Overall, one central 'prediction' (ionized Te, and hence the ionized abundance scale) reduces to a fit on an M83-inclusive training set, but the headline nitrogen offset retains substantial independent content, giving a score of 6.

Assumptions & free parameters 4 free parameters · 6 assumptions · 0 invented entities

The central multiphase abundance comparison rests on three external calibrations: the strong-line Te relations (fitted partly on M83 data), the SII-based oxygen conversion, and CLOUDY ICFs from the authors' prior papers. These are modeling assumptions rather than new physical entities, but each should be tested on independent high-metallicity samples before the numerical offsets are taken at face value.

free parameters (4)

Te(OIII) calibration slope and intercept = 0.68 +/- 0.07, 9.73 +/- 0.62
Linear fit between O3N2 and Te(OIII) in Appendix G; applied to all M83 H II regions without auroral detections.
Te(SIII) calibration slope and intercept = 0.43 +/- 0.10, 7.73 +/- 0.86
Linear fit between S3O3 and Te(SIII) in Appendix G.
Te(OII) calibration slope and intercept = 0.60 +/- 0.06, 9.11 +/- 0.55
Linear fit between combined DESIRED metallicity and Te(OII) in Appendix G.
Assumed n_e floor = 100 cm^-3
For clusters where [SII] and [OII] density ratios are below 100 cm^-3, density is set to 100 +/- 10 cm^-3; abundances are weakly sensitive to this choice.

assumptions (6)

domain assumption The strong-line Te relations (Eqs G3-G6) calibrated on literature H II regions transfer to M83 H II regions, including those in the calibration sample.
Used in Section 3.3.1 to assign Te wherever auroral lines are absent; if biased, all ionized abundances shift.
domain assumption Neutral oxygen column density can be obtained from S II using the James and Aloisi (2018) O/S technique.
Section 3.2.5; enables neutral O/H and O/N comparisons, but makes neutral O and S non-independent.
domain assumption CLOUDY photoionization ICFs from James et al. (2014) and Hernandez et al. (2021) correctly correct neutral and ionized gas column densities.
Section 3.2.6 and Appendix D; corrections are mostly small, but they are adopted from prior work by the same team.
domain assumption The COS line of sight probes neutral gas associated with each YSC environment rather than unrelated disk gas.
Sections 2.1 and 4.3; down-the-barrel geometry with inclination about 24 degrees makes this plausible but not guaranteed.
standard math Case B recombination Balmer decrement applies for reddening correction of H II region lines.
Section 3.3; standard nebular assumption used to derive Halpha/Hbeta reddening.
ad hoc to paper Galactic center YSCs are excluded from neutral and multiphase analysis because H I is abnormally low.
Section 4.1; this exclusion affects the sample used for the headline phase-offset statistics.

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Cite this review

Pith. "Pith review of Unveiling Metal Mixing in a Grand-Design Spiral: A UV-optical multiphase spatially resolved study of M83." pith.science (2026). https://pith.science/paper/UJRCTHMZ

@misc{pith2026260809064,
  author       = {Pith},
  title        = {Pith review of: Unveiling Metal Mixing in a Grand-Design Spiral: A UV-optical multiphase spatially resolved study of M83},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/UJRCTHMZ}},
  note         = {Machine review of arXiv:2608.09064}
}

abstract

We present a spatially resolved, multiphase study of chemical enrichment around young star clusters (YSCs) in the nearby grand-design spiral M83 by combining far-ultraviolet(UV) absorption-line spectroscopy from HST/COS with cospatial optical spectroscopy from VLT/MUSE and LBT/MODS. Our sample includes 18 YSCs spanning spectroscopic ages of ~1-6 Myr and galactocentric radii out to R/R_{25}=0.56. Neutral (H I) abundances were derived from UV absorption-line spectroscopy and compared with ionised (H II) abundances from reddening-corrected optical emission lines. Because auroral lines are not detected in all regions, we develop and apply an empirical multi-zone electron temperature (T_e) calibration based on strong-line diagnostics to estimate T_e and derive reliable nebular abundances. We measure oxygen(O), sulphur(S), nitrogen(N), and iron(Fe) abundance tracing enrichment from distinct nucleosynthetic channels. The alpha-elements (O and S) exhibit similar behaviour, consistent with enrichment by core-collapse supernovae, whereas Fe shows weaker variations, reflecting its delayed production by Type Ia supernovae. Nitrogen displays the largest phase offset (ionised-neutral), with enhancements of up to $Delta$N/H~1.5 dex and $Delta$N/O>1.5 dex in the ionised gas relative to the neutral phase, indicating localised enrichment by massive stars and inefficient mixing between gas phases on Myr timescales. While the ionised gas exhibits signatures of feedback-regulated chemical enrichment and large-scale abundance gradients, corresponding trends are weak or absent in the neutral gas, consistent with metals remaining largely confined to the immediate star-forming environment during the earliest stages of cluster evolution in a massive grand-design spiral.

Figures

Figures reproduced from arXiv: 2608.09064 by the authors.

**Figure 1.** HST (WFC3) image of M83 shown in greyscale. The position of the HST/COS observed young star clusters is overplotted as circles. The color fill of the circles represents the UV-spectra fitted average age (in Myr) of the younger stellar population. The coordinates (RA/Dec) are given in J2000 format. Note: The circle sizes do not represent the HST/COS aperture, which is too small for clear representation in this figure… view at source ↗

**Figure 2.** HST/COS FUV spectra (left) and VLT/MUSE optical spectra (right) observed towards YSC M83-POS-1 in grey. The spaxels from VLT/MUSE IFU observations have been extracted within the COS aperture to make both spectra co-spatial. The blue, magenta, red and green dashed vertical lines show the location of the prominent lines from wind+ISM, stellar photospheric, ISM absorption, and nebular emission features, respectively. L… view at source ↗

**Figure 3.** Low-ionisation metal lines associated with the neutral gas towards the young star cluster, M83-POS-1 of the M83 galaxy. The normalised HST/COS spectrum is shown in blue with the best-fit multi-component Voigt profile (M) overplotted in red. Red dashed vertical lines show the location of the different velocity components associated with the neutral gas in M83. Black vertical lines show the location of the different… view at source ↗

Figures from the paper (21 more)

**Figure 4.** Figure 4: Comparing the ICF-corrected elemental column densities (y-axis) to the observed ionic column densities (x-axis). Different subplots show different elements. The 1:1 line is shown in green. sity and therefore leads to an overestimate of the neutral gas column density, …

**Figure 5.** Figure 5: Multi-component Gaussian fit (shown in red) to emission lines (shown in black) observed in the spectra obtained from VLT/MUSE IFU spaxels of the regions surrounding the YSC M83-POS-1. The individual spaxels falling within the HST/COS aperture were summed to obtain th…

**Figure 6.** Figure 6: Distribution of hydrogen as a function of galactocentric distance (R/R25). Top subplot: For ionised H II region, the Hα intensity is shown (in logscale in erg s−1 cm−2 ). Bottom subplot: For neutral gas, the H I column density is shown (in logscale in atoms cm−2 ). T…

**Figure 7.** Figure 7: Elemental abundances (12+log(X/H)) of X=iron, nitrogen, and sulphur plotted as a function of oxygen in ionised gas (H II region) around YSCs in M83. Only detections are shown here for clarity. The legend for each subplot shows the statistics: fitted line slope, m, in…

**Figure 8.** Figure 8: Iron (Fe/H), nitrogen (N/H), sulphur (S/H) and oxygen(O/H) abundance in H II regions around YSCs shown as a function of the stellar age (Myr) of the YSCs. The colored dashed lines represent the weighted best-fit for each subplot. Legends are the same as [PITH_FULL_IMA…

**Figure 10.** Figure 10: Comparing elemental abundances of iron ((Fe/H), blue) and nitrogen ((N/H), red) to that of oxygen (O/H) in neutral gas (H I region) around YSCs in M83. The legends are the same as [PITH_FULL_IMAGE:figures/full_fig_p020_10.png]

**Figure 11.** Figure 11: Neutral gas elemental abundances of iron ((Fe/H), blue), nitrogen ((N/H), red), sulphur ((S/H), green), and oxygen ((O/H), pink) as a function of the stellar age of their natal-star clusters in M83. The legends are the same as [PITH_FULL_IMAGE:figures/full_fig_p021_11.png]

**Figure 12.** Figure 12: Abundance of different elements: iron ((Fe/H), blue), nitrogen ((N/H), red), and sulphur ((S/H), green) as a function of the amount of dust (E(B-V)) in the neutral gas (H I region) around YSCs in M83. The legends are the same as [PITH_FULL_IMAGE:figures/full_fig_p022…

**Figure 14.** Figure 14: Elemental abundance in ionised gas relative to neutral within YSCs in M83. The black dashed line shows the 1:1 relation. We have removed all points from the galactic centre. Other legends are the same as [PITH_FULL_IMAGE:figures/full_fig_p023_14.png]

**Figure 15.** Figure 15: Elemental excesses in ionised gas relative to neutral gas, ∆X/H plotted as a function of ionised gas oxygen abundance, 12+log(O/H). We have removed all the upper limits, 12+log(O/H)>9, for clarity. The legends are the same as [PITH_FULL_IMAGE:figures/full_fig_p024_15.png]

**Figure 16.** Figure 16: Elemental excesses in ionised gas relative to neutral gas, ∆X/H plotted as a function of average stellar age of the natal star-cluster. The legends are the same as [PITH_FULL_IMAGE:figures/full_fig_p025_16.png]

**Figure 18.** Figure 18: Oxygen abundance (12+log(O/H)), nitrogen abundance (12+log(N/H)) and N/O shown within top, middle and bottom panels for neutral (as blue squares) and ionised (as red circles) phases. The trend is shown as a dashed line with the same colour code as mentioned above for…

**Figure 19.** Figure 19: Stellar bolometric luminosity (Lbol in [erg s−1 ], top) and wind momentum (in [g cm s−2 ], bottom) obtained using SB99 models plotted as a function of outflow velocity, vout in kms−1 (see text within subsection. 5.2.2 for details). The statistics shown in the legend f…

**Figure 21.** Figure 21: Dust content (E(B-V)) within neutral gas (H I region) plotted against the dust within ionised gas (H II region). The points are colour coded as a function of dust within young stars, except for points from within the galactic centre. to the sites of recent star form…

**Figure 22.** Figure 22: Convolution of the COS LSF with varying spatial FWHM: original (green), narrow (blue) and wide (red) for the YSC M83-POS-1 (visit - LDN701010, PID: 15193, PI: Aloisi). The range in spatial FWHM is obtained from structure within the 1-D acquisition image. The separat…

**Figure 23.** Figure 23: Plotting change in abundance due to depletion(∆log(X/H)dep = (X/H)depleted - (X/H)ICF ) for each observed neutral gas element, X, for each YSC in M83 observed with VLT/COS. The three subplots from bottom to top show values for X = Fe, S, and O. The median ∆log(X/H)dep…

**Figure 24.** Figure 24: Comparison of fitted stellar ages (top) and metallicity (bottom) for YSCs in M83 using SESSAMME (see subsection. F.2) shown on the x-axis against the values from S. Hernandez et al. (2019). The red dashed line shows the 1:1 relation. fitting M83-POS-1 and M83-POS-2 is…

**Figure 25.** Figure 25: HST/COS spectra (binned to fit SB99 models) of M83-POS-1 showed in blue along with best-fit (with ± 3 − σ uncertainty) stellar model showed in red. The best– fit stellar parameters are also shown as legends. Regions shown in grey are masked out due to contamination f…

**Figure 26.** Figure 26: Stellar luminosity and wind momentum derived from the SB99 model with inference of stellar ages from SESAMME UV-spectral fitting of YSC: M83-POS-1. The purple vertical line (and shaded regions) indicate the stellar age of the YSCs (and ± 1 − σ uncertainty). A mask of …

**Figure 28.** Figure 28: Comparing direct-method elemental abundances (12+log(X/H), where X=O,N,S from top to bottom) of H II regions in star-forming galaxies. The x-axis shows the abundances from the literature, and the y-axis is the abundance calculated using predicted multi-phase Te. The …

**Figure 29.** Figure 29: Comparing ionic oxygen abundances: 12+log(O+/H+), 12+log(O++/H+) and ratio: log(O+/O) derived using temperature in literature (x-axis) against the predicted temperatures from the method explained in Section G for H II regions in literature. The greyed-out points indi…

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Pith tools

Reviewed August 12, 2026 · model on record in the stance chip above.

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