FEAST: probing the stellar population of the starburst dwarf galaxy NGC4449 with JWST/NIRCam

Alex Pedrini; Ana Duarte-Cabral; Angela Adamo; Anne S. M. Buckner; Benjamin Gregg; Bruce G. Elmegreen; Daniela Calzetti; Drew Lapeer; Elena Sabbi; Elena Sacchi

REVIEW 3 major objections 5 minor 1 cited by

FEAST: probing the stellar population of the starburst dwarf galaxy NGC4449 with JWST/NIRCam

T0 review · 3 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

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

Pith's one-line read JWST star counts show NGC 4449's stars younger than 60 Myr arranged in an S-shaped pattern along the north–south axis, with the youngest stars in the north and progressively older stars to the south, implying sequential bursts possibly…

desk verdict Solid, honest JWST CMD paper: the S-shape is real but not new, the AGB gap and finger are genuinely new, and the Table 1 ratios are raw counts that need completeness correction or demotion. read the letter →

arxiv 2507.03420 v1 pith:CI36LNQU submitted 2025-07-04 astro-ph.GA

Matteo Correnti , Giacomo Bortolini , Flavia Dell'Agli , Angela Adamo , Michele Cignoni , Elena Sacchi , Monica Tosi , Alex Pedrini

show 17 more authors

Anne S. M. Buckner Daniela Calzetti Ana Duarte-Cabral Bruce G. Elmegreen Helena Faustino Vieira John S. Gallagher Kathryn Grasha Benjamin Gregg Kelsey E. Johnson Thomas S.-Y. Lai Drew Lapeer Sean T. Linden Matteo Messa Goran Ostlin Elena Sabbi Linda J. Smith Paolo Ventura

This is my paper

classification astro-ph.GA

keywords NGC4449JWST/NIRCamresolvedstellarpopulationsstarburstdwarfgalaxycolor-magnitudediagramsAGBstarsspatialdistributionofstarformationFEASTprogram

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 uses JWST/NIRCam images to resolve individual stars in the nearby starburst dwarf galaxy NGC 4449 and asks whether recent star formation is spread uniformly or structured in space and time. It claims that all stars younger than about 60 Myr follow an S-shaped distribution aligned with the galaxy's bar and H-alpha gas, with the youngest (≤10 Myr) stars concentrated in the north and the 30–60 Myr population shifted to the south; the same pattern appears in young star clusters. It further claims to resolve, for the first time in this galaxy, a clear gap between oxygen-rich and carbon-rich AGB stars and a vertical 'finger' of massive AGB stars, features that can constrain how AGB stars lose mass and produce dust. If correct, the results show that this dwarf starburst's most recent star formation is a sequence of spatially separated bursts, plausibly triggered by tidal interaction, rather than a single homogeneous event.

What carries the argument

The machinery is the NIR color–magnitude diagram (CMD) built from DOLPHOT PSF photometry of NIRCam data in F115W, F150W, F200W, and F444W, with ages assigned by matching each observed star to a synthetic CMD generated from PARSEC-COLIBRI isochrones and a Kroupa IMF. Age-stratified star-count maps and the ratios R1 = A/B, R2 = C/B, R3 = D/B, R4 = E/B between elliptical regions quantify the spatial shifts. For the AGB analysis, the ATON evolutionary tracks with dust production identify the O-rich vertical sequence, the carbon-star branch, and the massive-AGB 'finger'; the bifurcation point and the drops in the luminosity function are the observables that encode mass-loss and dust-production physics.

What would settle it

Recompute R1 and R2 using the paper's own artificial-star completeness functions, applied per tile and per magnitude bin for the same CMD selection box; if the corrected ratios no longer show a ≤10 Myr northern excess (R1 ≫ R2) followed by a 30–60 Myr southern excess (R2 > R1), the claimed sequential S-shaped bursts are not supported by the data.

Watch

Extended reading notes

Core claim

The central discovery is that NGC 4449's resolved stellar populations are not uniformly distributed: stars younger than 10 Myr form an S-shaped structure aligned with the north–south bar and following the H-alpha gas, while populations of 10–30 Myr and 30–60 Myr show a progressive shift of the concentration from the northern to the southern edge of the S-shape. Quantified through star-count ratios between northern, central, and southern regions, the youngest bin has R1 ≃ 0.45 and R2 ≃ 0.04, whereas by 30–60 Myr R2 ≃ 0.29 overtakes R1 ≃ 0.13. The paper interprets this as evidence that star formation was triggered in spatially distinct bursts, possibly by external interaction or accretion, and shows that clusters of comparable ages follow the field-star distributions, implying cluster and field stars form at the same pace. On the AGB side, the NIR CMDs reveal a clean gap between the oxygen-rich vertical sequence and the carbon-star branch, plus a bright 'finger' of massive AGB stars; the height and shape of these features are sensitive to the assumed mass-loss prescription, making them new constraints for AGB evolution and dust-production models.

Load-bearing premise

The age-resolved maps and Table 1 ratios are computed from raw star counts, assuming photometric completeness is roughly the same across the northern, central, and southern regions; the paper's own artificial-star tests show 50% completeness varies by 1–2 magnitudes between inner and outer tiles, so if incompleteness varies in the same sense as the S-shape, the north-to-south age progression could be partly an artifact.

Editorial extensions

If this is right

NGC 4449's recent star formation is better described as sequential, spatially separated bursts than as a single central starburst, with the north–south age gradient favoring an external trigger such as the interaction with DDO 125.
Field stars and young clusters trace the same large-scale distribution, supporting the idea that most stars form in clustered environments and that cluster and field formation are coeval in each galaxy region.
The orientation shift of the oldest sampled populations (160–250 Myr) from north–south to east–west supports a picture of multiple, decoupled dynamical components, consistent with the counter-rotating H I gas.
The AGB gap and massive-star finger turn JWST CMDs of a resolved dwarf into quantitative tests of AGB mass-loss prescriptions and dust-production timescales.
The central RGB density dip, shown to coincide with a crowding- and saturation-driven completeness drop, demonstrates that apparent morphological features in dense dwarf centers must be checked against completeness maps.

Reading between the lines

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

The same completeness corrections already computed with artificial stars could be applied to the young-star maps; if the corrected R1/R2 ratios flatten, the S-shape age gradient would weaken or vanish, so a completeness-corrected version of Table 1 is the natural next check.
The external-trigger interpretation can be tested beyond the current field of view: if tidal interaction is the cause, the age gradients should connect to the large-scale H I streamer morphology and the stellar tidal stream already detected in the halo.
The AGB gap, if caused by a rapid spectral transition from M-type to carbon-star spectra, should appear in any JWST-resolved massive dwarf with a rich carbon-star population; the Magellanic Clouds should show it at fainter magnitudes once crowding is matched.
The massive-AGB 'finger' height could serve as a distance-independent diagnostic of recent (30–200 Myr) star formation intensity in starburst dwarfs, complementing integrated star-formation-history fitting.

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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

This is a competent, transparent JWST/NIRCam resolved-population paper. The genuinely new items are the NIR CMDs, the age-resolved spatial maps, and the detection of an O-rich/C-rich AGB gap plus a massive AGB "finger" in NGC 4449. The S-shape itself was already reported by Sacchi et al. (2018) from HST data, and the authors say so explicitly, which is the right way to handle it.

The photometry is carefully done: DOLPHOT with the JWST NIRCam module, AST with 1M stars per tile, diagnostic cuts shown and described, and completeness maps presented and used where they matter. The paper is honest about what is preliminary: the SFH derivation and the cluster analysis are explicitly deferred to future papers, and the authors flag their own selection effects, e.g., the conservative field-star selection in Sect. 4.2 and the incompleteness of the manually selected AGB sample in Sect. 5. The AGB analysis is thoughtful, overplotting ATON tracks with C/O ratios and discussing the gap as a spectral or dust-production transition, and the gap and finger are plausible new constraints for AGB mass-loss and dust models.

The soft spot is quantitative, not qualitative. The age-progression ratios in Table 1 are raw star counts with no completeness correction, even though the paper applies exactly such a correction to the RGB central dip and attributes that dip to crowding. Their own AST shows the 50% completeness limit in F200W varies by about a magnitude between outer and inner tiles, and the young-star box reaches mF200W ~ 24, within about a magnitude of the central limit. Since region B (the central denominator) is the most crowded, differential incompleteness could bias the R1 and R2 ratios and possibly the apparent north-to-south age shift. The authors call the test "preliminary" and defer the rigorous SFH analysis, so this is a weakness in a supporting test, not the core result. The S-shape and the qualitative age-dependent shifts in the spatial maps are likely robust, and the cluster-field comparison is properly hedged.

I would send this to peer review. The data are public, the reduction is reproducible, and the AGB gap and finger are new and interesting. The main request to the authors should be to either completeness-correct the Table 1 ratios or demote them further to a qualitative illustration. Anyone working on resolved stellar populations in nearby dwarfs, AGB evolution, or interaction-triggered star formation will want to read this.

Referee Report

3 major / 5 minor

Summary. The paper presents JWST/NIRCam resolved stellar photometry of the starburst dwarf galaxy NGC 4449 from the FEAST program, using F115W, F150W, F200W, and F444W images reduced with DOLPHOT in 18 tiles. The authors construct CMDs, assign stellar ages via a synthetic CMD built from PARSEC-COLIBRI isochrones and a constant SFH, and study the spatial distributions of six young age intervals, of RGB stars, and of candidate O-rich and C-rich AGB stars. The main claims are: (i) stars younger than about 60 Myr trace an S-shaped structure aligned with the bar and H-alpha morphology; (ii) the youngest stars concentrate in the north while the 30-60 Myr population shifts to the south, suggesting sequential, possibly externally triggered bursts; (iii) young clusters broadly follow the field-star distributions; and (iv) the NIR CMDs reveal a gap between O-rich and carbon stars and a massive AGB star 'finger'. The analysis is explicitly preliminary, with a detailed SFH paper announced as forthcoming.

Significance. If the results hold, the paper provides a rare resolved-NIR view of a local starburst dwarf and offers a concrete, testable picture of spatially and temporally structured star formation, while also demonstrating JWST's ability to separate AGB evolutionary phases in crowded extragalactic fields. The photometric reduction is carefully described, including per-tile DOLPHOT runs, sharpness/crowding cuts, and large-scale artificial star tests (18 million injected stars), and the main quantitative claims are appropriately hedged as preliminary. These strengths make the paper a useful first step for the FEAST program. The central quantitative support for the north-to-south age progression, however, rests on raw star-count ratios that are not corrected for spatially varying completeness, and the age assignment assumes a constant SFH; both issues are addressable with data already in hand.

major comments (3)

[Section 4.1, Table 1, Fig. 3] The ratios R1=A/B and R2=C/B (and R3, R4) in Table 1 are computed from raw star counts in the selected young-star CMD box, with no completeness correction, despite the paper's own AST results (Fig. 3) showing that the 50% completeness limit varies by roughly 1 mag in mF200W between outer tiles (~26 mag) and the crowded inner tiles (~25 mag). Because the young-star box extends to mF200W ~ 24 mag, within about 1 mag of the central completeness limit, and because older age bins are systematically fainter within the same box, differential incompleteness is age-dependent and can bias the reported ratios, potentially producing or amplifying the apparent R2 overtaking R1 at 30-60 Myr. The paper applies completeness reasoning to the RGB central dip (Sect. 4.1, Fig. 10) but not to the young-star maps or Table 1; the ratios should be recomputed using the per-tile completeness functions for the same CMD box, or an equivalent robustness test should be supplied. The text also calls these quantities 'relative stellar densities' while the table caption reports raw star counts; if the three elliptical regions differ in area, area normalization is needed as well.
[Section 4.1] The age assignment for observed stars uses a synthetic CMD generated with an assumed constant SFH (Sect. 4.1), and the uncertainties quoted in Table 1 are Poisson only. If the true SFH of NGC 4449 is bursty, as the paper itself argues, the relative weights of different age populations in the CMD box change, and the ages assigned to individual stars can be systematically biased; the claimed north-to-south progression therefore depends partly on the assumed prior. The authors should test the sensitivity of the Table 1 ratios and the age-bin maps to the choice of SFH in the synthetic CMD (e.g., by using a bursty or declining SFH) and report whether the R2/R1 crossover at 30-60 Myr survives. This is a load-bearing point because the sequential-burst conclusion is the paper's central astrophysical claim.
[Section 4.2 and Abstract] The abstract states that clusters and field stars 'form at the same pace in each galaxy region,' but the supporting comparison in Sect. 4.2 is qualitative, and the authors themselves note that the field-star selection samples only about 1% of the youngest population, leading to 0-1 selected stars in some regions (Sect. 4.2). This statement should either be quantified with a completeness- and selection-corrected field-to-cluster comparison or explicitly softened in the abstract and conclusions to match the level of evidence presented.

minor comments (5)

[Abstract] The sentence 'These results confirms NGC 4449 status' contains a subject-verb agreement error and should read 'These results confirm NGC 4449's status.'
[Abstract] The abstract refers to 'stars aged 10 - 60 Myr,' but the analysis in Sect. 4.1 uses two separate bins, 10-30 Myr and 30-60 Myr; the wording should be aligned with the actual bin definitions.
[Author list] The author list contains 'F austino Vieira' with a stray space; this should be corrected to 'Faustino Vieira.'
[Section 5] The name 'Del'Agli' in 'Del'Agli et al., in prep.' is inconsistent with 'Dell'Agli' used elsewhere in the text and references; the spelling should be unified.
[Section 2, Fig. 3] In the discussion of Fig. 3, the text says the drop in completeness at bright magnitudes is 'due to the choice of how the quality cuts are applied,' but it would be clearer to state explicitly that the conservative sharpness/crowding cuts remove some bright saturated or blended sources, since this behavior is visible in Fig. 2.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: this is an observational mapping paper whose claims are descriptive, with no fitted quantity renamed as a prediction and no load-bearing self-citation chain.

full rationale

This is an observational mapping paper, not a derivation with predicted outputs. The central age-dependent spatial distributions are obtained from observed NIRCam photometry, a synthetic CMD age-assignment procedure using PARSEC isochrones and a Kroupa IMF, and direct star-count ratios computed in fixed elliptical regions (Table 1). None of these steps fits a target result and then reports it as a prediction. The only fitted quantity, E(B-V)=0.05, is optimized on the blue edge of the upper main sequence and used as a global reddening calibration for the synthetic CMD; the age assignments and spatial morphology claims are not defined in terms of that fit. The S-shaped distribution is independently visible in the actual spatial maps (Fig. 7) and is consistent with the H-alpha morphology from earlier external work; the prior note by Sacchi et al. (2018) is corroborated rather than load-bearing. The AGB claims are direct CMD identifications with evolutionary tracks used for interpretation, not results derived from the tracks by construction. The genuine weakness flagged by the skeptic—the R1=A/B and R2=C/B ratios in Table 1 are raw counts computed without applying the AST completeness corrections that the paper does apply to the RGB central dip (Fig. 10)—is a completeness and bias concern, not a circularity: the ratios are counts, not fitted predictions, so the derivation does not reduce to its own inputs. Self-citations (e.g., Sacchi et al. 2018, Cignoni et al. 2018, Pedrini et al. in preparation) provide external, independently obtained, or forthcoming data and are not the mathematical engine of the claims.

Assumptions & free parameters 3 free parameters · 5 assumptions · 0 invented entities

The central claims rest on the adopted distance, isochrone models, and the synthetic CMD; these are standard tools but not independently verified here.

free parameters (3)

Reddening E(B-V) = 0.05 mag
Derived by optimizing the isochrone fit of the blue edge of the upper MS (Sect. 3); used in all CMD comparisons and age assignments.
Age interval boundaries = <=10, 10-30, 30-60, 60-100, 100-160, 160-250 Myr
Chosen by hand after trials (Sect. 4.1) to balance age resolution and number statistics; defines the spatial maps and Table 1 ratios.
Young-star CMD selection box = 17 <= mF200W <= 24 mag; color 0.1-0.75 mag, widening with brightness
Hand-defined color-magnitude region to isolate stars younger than ~250 Myr (Sect. 4.1); affects which stars enter the age-assignment step.

assumptions (5)

domain assumption PARSEC-COLIBRI isochrones accurately represent stellar evolution at the adopted metallicities
Used in Sect. 3 to interpret CMDs and in Sect. 4.1 to build the synthetic CMD for age assignments.
domain assumption Synthetic CMD with constant SFH and Kroupa (2001) IMF provides unbiased age assignments
Sect. 4.1: observed star ages are the mean age of synthetic stars within 0.25 mag in the CMD; if the true SFH is strongly bursty, the age-color mapping may be less representative.
domain assumption Adopted distance modulus (m-M)0 = 28.15 mag
Taken from Annibali et al. (2008) and Tully et al. (2013) (Sect. 3); sets the absolute magnitude scale for all comparisons.
domain assumption ATON AGB+dust models with Z=0.008 and Bloecker (1995) mass loss represent the AGB population
Used in Sect. 5 to explain the C-rich/O-rich gap and the massive AGB finger; the paper notes the height of the finger depends on the mass-loss prescription.
domain assumption AST completeness accurately reflects the true recovery fraction
Sect. 2: AST injection of 1 million stars per tile is used to quantify completeness; the RGB dip interpretation (Fig. 10) rests on this.

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Cite this review

Pith. "Pith review of FEAST: probing the stellar population of the starburst dwarf galaxy NGC4449 with JWST/NIRCam." pith.science (2026). https://pith.science/paper/CI36LNQU

@misc{pith2026250703420,
  author       = {Pith},
  title        = {Pith review of: FEAST: probing the stellar population of the starburst dwarf galaxy NGC4449 with JWST/NIRCam},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/CI36LNQU}},
  note         = {Machine review of arXiv:2507.03420}
}

read the original abstract

We present new JWST/NIRCam observations of the starburst irregular galaxy NGC 4449, obtained in Cycle 1 as part of the Feedback in Emerging extrAgalactic Star clusTers (FEAST) program, which we use to investigate its resolved stellar populations and their spatial distributions. NGC4449 NIR color-magnitude diagrams reveal a broad range of stellar populations, spanning different evolutionary phases, from young main sequence stars, to old red giant branch stars and asymptotic giant branch (AGB) stars. The analysis of their spatial distributions shows that younger (< 10 Myr) populations form an S-shaped distribution aligned with the galaxy's north-south axis, while stars aged 10 - 60 Myr show shifting concentrations from the north to the south, consistent with the possibility that external interactions or tidal effects may have triggered star formation in spatially distinct bursts. Clusters of comparable ages generally follow these distributions, suggesting that cluster and field stars form at the same pace in each galaxy region. Thanks to the unprecedented high-spatial resolution and sensitivity of the JWST data we recover a clear gap between Oxygen-rich and the carbon star branch of the AGB population and the presence of a massive AGB star "finger". The analysis of these stars can provide constraints on AGB evolution models and dust production in this galaxy. These results confirms NGC 4449 status as a compelling example of a local dwarf starburst galaxy undergoing complex and possibly external driven star formation and underscore the power of JWST in probing the full lifecycle of stars in nearby starburst systems.

Figures

Figures reproduced from arXiv: 2507.03420 by the authors.

**Figure 1.** NIRCam F200W NGC 4449 field of view (FoV), corresponding to ∼ 2.9 × 6.35 kpc at the adopted distance. To facilitate the data reduction process we divided the image in 18 tiles (with approximate size of 0.95 × 1.05 kpc) as indicated by the white dashed lines and numbers in the figure. Angular scale (30′′, corresponding to ∼ 550 pc) and North and East directions are also reported. sub-solar [α/Fe] ratios, with a peak … view at source ↗

**Figure 2.** DOLPHOT sharpness (top panels) and crowding (bottom panels) as a function of mF 115W for a tile in the galaxy outskirt (tile 1, left panels) and for a tile covering the central region (tile 11, right panels). Light gray dots represent all the sources passing the preliminary selection cuts (i.e., Object Type, quality flag, and SNR) while black points indicate the sources that pass sharpness and crowding cuts. For eac… view at source ↗

**Figure 3.** Completeness vs magnitudes (mF 115W , blue dots; mF 200W , orange dots) as a function of spatial position in the galaxy (i.e., for each tile), displayed on top of the F200W NGC 4449 image. The number of recovered stars in each tile, out of the 1 million injected, is reported in each panel. 50% completeness is indicated by the red dashed line, whereas the corresponding mF 115W and mF 200W are indicated by the blue an… view at source ↗

Figures from the paper (11 more)

**Figure 4.** Figure 4: mF 200W vs mF 115W - mF 200W CMDs, plotted as 2D hexagonal bins, as a function of their spatial position, displayed on top of the F200W NGC 4449 image. In each CMD we reported the number of stars. The CMDs of the different tiles clearly show how the presence and densit…

**Figure 5.** Figure 5: mF 200W vs mF 115W - mF 200W CMDs, plotted as 2D hexagonal bins, for four selected tiles, representative of different regions of the galaxy (Tile 1, outer region, top-left panel; Tile 6 and Tile 13, intermediate regions, right panels; Tile 11, inner region, bottom-left…

**Figure 6.** Figure 6: Left panel: Synthetic mF 200W vs mF 115W - mF 200W CMD, obtained as described in Sect. 4.1, with stars color-coded according to their age. The region adopted to analyze the young populations is reported in light-red. Right panel: mF 200W vs mF 115W - mF 200W observed c…

**Figure 7.** Figure 7: Left panels: mF 200W vs mF 115W - mF 200W composite CMDs, with overplotted in red, color-coded following the star count density, the stars in each specific age intervals (top panel: age ≤ 10 Myr; middle panel: 10 Myr < age ≤ 30 Myr; bottom panel: 30 Myr < age ≤ 60 Myr)…

**Figure 8.** Figure 8: Same as [PITH_FULL_IMAGE:figures/full_fig_p010_8.png]

**Figure 9.** Figure 9: Same as [PITH_FULL_IMAGE:figures/full_fig_p012_9.png]

**Figure 10.** Figure 10: Map of the mean photometric completeness across the FoV, computed in 50×50 px regions within the selected RGB magnitude range. The map reveals a significant drop in completeness coinciding with the central density dip observed in the stellar distribution. The location…

**Figure 11.** Figure 11: Young star clusters (eYSC1, orange squares; eYSC2, green diamonds, optical YSC, blue dots) spatial distributions as a function of four age intervals (top-left panel: age ≤ 10 Myr; top-right panel: 10 Myr < age ≤ 50 Myr; bottom-left panel: 50 Myr < age ≤ 100 Myr; botto…

**Figure 12.** Figure 12: Stellar spatial distributions as a function of the same age intervals adopted in [PITH_FULL_IMAGE:figures/full_fig_p014_12.png]

**Figure 13.** Figure 13: NGC 4449 data in the mF150W vs mF150W − mF200W (left panel) and mF444W vs mF200W − mF444W (right panel) CMDs, with AGB stars candidates overplotted in red. ATON evolutionary tracks of MS masses 2 M⊙ (triangles) and 4 M⊙ (pentagons) at Z=0.008 are shown in both the pan…

**Figure 14.** Figure 14: Same as [PITH_FULL_IMAGE:figures/full_fig_p017_14.png]

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Forward citations

Cited by 1 Pith paper

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

FEAST: JWST/NIRCam view of the Resolved Stellar Populations of the Interacting Dwarf Galaxies NGC~4485/NGC~4490
astro-ph.GA 2025-09 conditional novelty 6.0 of 10

JWST/NIRCam resolves stellar populations in the interacting dwarf pair NGC 4485/NGC 4490, revealing star formation bursts roughly 30 and 200 Myr ago and a metallicity gradient across the tidal bridge.

Reference graph

Works this paper leans on

72 extracted references · 62 canonical work pages · cited by 1 Pith paper

[1]

?b: FMųE ;܂6wӁr 33 NgĵX/ ưK _<oo /w?ܡؿ V7o o8`uu+W ^k +ǃ X O)/]? 0g;;i6/2_K g 06 _Wt: >Opi W w w; ;W^ᥗ^ݻ<| _

thebibliography [1] 20pt to REFERENCES 6pt =0pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command E...

2021
[2]

Ai, M., Zhu, M., Xu, J., et al.\ 2023, , 524, 2911

work page 2023
[3]

2008, , 135, 1900

Annibali, F., Aloisi, A., Mack, J., et al. 2008, , 135, 1900

work page 2008
[4]

2018, , 476, 1942

Annibali, F., Morandi, E., Watkins, L.L., et al. 2018, , 476, 1942

work page 2018
[5]

2011, , 142, 129

Annibali, F., Tosi, M., Aloisi, A., et al. 2011, , 142, 129

work page 2011
[6]

2012, , 745, L1

Annibali, F., Tosi, M., Aloisi, A., et al. 2012, , 745, L1

work page 2012
[7]

2017, , 843, 20

Annibali, F., Tosi, M., Romano, D., et al. 2017, , 843, 20

work page 2017
[9]

K., & Klein, U., 1994, , 285, 385

Bajaja, E., Huchtmeier, W. K., & Klein, U., 1994, , 285, 385

work page 1994

Show all 72 references

[10]

Bl\"ocker, T.\ 1995, , 297, 727

1995
[11]

P., Mazzuca, L., at al

Boker, T., van der Marel, R. P., Mazzuca, L., at al. 2001, , 121, 1473

2001
[12]

2019, , 622, A103

Boquien, M., Burgarella, D., Roehlly, Y., et al. 2019, , 622, A103

2019
[13]

Bothun, G. D. 1986, , 91, 507

1986
[14]

2003, , 408, 493

B\"ottner, C., Klein, U., & Heithausen, A. 2003, , 408, 493

2003
[15]

2012, , 427, 127

Bressan, A., Marigo, P., Girardi, L., et al. 2012, , 427, 127

2012
[16]

C., Sabbi, E., et al

Calzetti, D., Lee, J. C., Sabbi, E., et al. 2015, , 149, 51

2015
[17]

W., Draine, B

Calzetti, D., Wilson, G. W., Draine, B. T., et al. 2018, , 852, 106

2018
[18]

doi:10.1051/0004-6361/201936612

Chen, Y., Girardi, L., Fu, X., et al.\ 2019, , 632, A105. doi:10.1051/0004-6361/201936612

2019 doi
[19]

2018, , 856, 62

Cignoni, M., Sacchi, E., Aloisi, A., et al. 2018, , 856, 62

2018
[20]

Dell'Agli, F., Ventura, P., Schneider, R., et al.\ 2015a, , 447, 2992
[21]

Dell'Agli, F., Di Criscienzo, M., Ventura, P., et al.\ 2018, , 479, 5035

2018
[22]

Dolphin, A. E. \ 2000, , 112, 776, doi:10.1086/316630

2000 doi
[23]

Dolphin, A. E. \ 2016, Astrophysics Source Code Library, record ascl:1608.013

2016
[24]

E., Hunter, D

Gelatt, A. E., Hunter, D. A., & Gallagher, J. S., 2001, , 113, 142

2001
[25]

Genzel, R., Lutz, D., & Tacconi, L., 1998, Nature, 395, 859

1998
[26]

Giavalisco, M., 2002, , 40, 579

2002
[27]

2024, , 971, 115

Gregg, B., Calzetti, D., Adamo, A., et al. 2024, , 971, 115

2024
[28]

doi:10.1046/j.1365-8711.2001.04022.x

Kroupa, P.\ 2001, , 322, 231. doi:10.1046/j.1365-8711.2001.04022.x

2001
[29]

Hunter, J. D. 2007, Computing in Science Engineering, 9, 90

2007
[30]

A., Gallagher, J

Hunter, D. A., Gallagher, J. S., & Rautenkranz, D., 1982, , 49, 53

1982
[31]

A., & Gallagher, J

Hunter, D. A., & Gallagher, J. S., 1990, , 362, 480

1990
[32]

A., & Thronson, H

Hunter, D. A., & Thronson, H. A., Jr., 1996, , 461, 202

1996
[33]

A., & Gallagher, J

Hunter, D. A., & Gallagher, J. S., 1997, , 475, 65

1997
[34]

A., Wilcots, E

Hunter, D. A., Wilcots, E. M., van Woerden, H., et al., 1998, , 495, L47

1998
[35]

A., van Woerden, H., & Gallagher, J

Hunter, D. A., van Woerden, H., & Gallagher, J. S. 1999, , 118, 2184

1999
[36]

I., Lattanzio J

Karakas A. I., Lattanzio J. C.\ 2014, PASA, 31, e030

2014
[37]

B., & Tinsley, B

Larson, R. B., & Tinsley, B. M. 1978, , 219, 46

1978
[38]

Le Fevre, O., et al., 2005, , 439, 877

2005
[39]

2014, , 445, 1694

Lelli, F., Verheijen, M., & Fraternali, F. 2014, , 445, 1694

2014
[40]

doi:10.1093/mnras/stt1034

Marigo, P., Bressan, A., Nanni, A., et al.\ 2013, , 434, 488. doi:10.1093/mnras/stt1034

2013 doi
[41]

2017, , 835, 77

Marigo, P., Girardi, L., Bressan, A., et al. 2017, , 835, 77

2017
[42]

A., et al., 2023, A&A, 670, A97

Marini E., Dell'Agli F., Kamath D., Ventura P., Mattsson L., Marchetti T., Garc \' a-Hern \'a ndez D. A., et al., 2023, A&A, 670, A97

2023
[43]

2012, , 748, 24

Martinez-Delgado, D., et al. 2012, , 748, 24

2012
[44]

T., et al

McQuaid, T., Calzetti, D., Linden, S. T., et al. 2024, , 967, 102

2024
[45]

McQuinn, K. B. W., Skillman, E. D., Cannon, J. M., et al., 2010, , 721, 297

2010
[46]

Nanni A., Bressan A., Marigo P., et al.\ 2013, , 434, 2390

2013
[47]

Stationary Shell Sources, 20, 287

Paczy \'n ski, B.\ 1970, , Evolution of Single Stars III. Stationary Shell Sources, 20, 287

1970
[48]

2020, , 498, 3283

Pastorelli, G., Marigo, P., Girardi, L., et al. 2020, , 498, 3283

2020
[49]

2024, , 971, 32

Pedrini, A., Adamo, A., Calzetti, D., et al. 2024, , 971, 32

2024
[50]

E., Steidel, C

Pettini, M., Shapley, A. E., Steidel, C. C., 2001, , 554, 981

2001
[51]

S., Grebel, E

Pilyugin, L. S., Grebel, E. K., & Zinchenko, I. A., 2015, , 450, 3254

2015
[52]

E., Johnson, K

Reines, A. E., Johnson, K. E., & Goss, W. M., 2008, , 135, 2222

2008
[53]

Sabbi, E., Calzetti, D., Ubeda, L., et al., 2018, , 235, 23

2018
[54]

2018, , 857, 63

Sacchi, E., Cignoni, M., Aloisi, A., et al. 2018, , 857, 63

2018
[55]

R., Johnson, K

Sokal, K. R., Johnson, K. E., Indebetouw, R., et al. 2015, , 149, 115

2015
[56]

P., Topping M

Stark D. P., Topping M. W., Endsley R., Tang M., 2025, arXiv, arXiv:2501.17078

2025 arXiv
[57]

C., Giavalisco, M., Pettini, M., et al., 1996, , 462, L17

Steidel, C. C., Giavalisco, M., Pettini, M., et al., 1996, , 462, L17

1996
[58]

K., Stevens, I

Summers, L. K., Stevens, I. R., Strickland, D. K., & Heckman, T. M., 2003, , 342, 690

2003
[59]

L., 1980, Ph.D

Talent, D. L., 1980, Ph.D. Thesis, Rice Univ., Houston, TX

1980
[60]

2001, , 370, 365

Theis, C., & Kohle, S. 2001, , 370, 365

2001
[61]

A., Jr., Hunter, D

Thronson, H. A., Jr., Hunter, D. A., Telesco, C. M., et al., 1987, , 317, 180

1987
[62]

B., Courtois, H

Tully, R. B., Courtois, H. M., Dolphin, A. E., et al.\ 2013, , 146, 86. doi:10.1088/0004-6256/146/4/86

2013 doi
[63]

Valdez-Gutierrez, M., Rosado, M., Puerari, I., et al., 2002, , 124, 3157

2002
[64]

C., & Varoquax, G

van der Walt, S., Colbert, S. C., & Varoquax, G. 2011, Computing in Science Engineering, 13, 22

2011
[65]

& Wood, P

Vassiliadis, E. & Wood, P. R.\ 1993, , 413, 641, VW93

1993
[66]

Ventura, P., Zeppieri, A., Mazzitelli, I., D'Antona, F., 1998, A&A, 334, 953

1998
[67]

Ventura P., Di Criscienzo M., Schneider R., et al.\ 2012, , 420, 1442

2012
[68]

Ventura P., Dell'Agli F., Schneider R., et al.\ 2014, , 439, 977

2014
[69]

Ventura, P., Karakas, A., Dell'Agli, F., et al.\ 2018, , 475, 2282

2018
[70]

Ventura, P., Dell'Agli, F., Tailo, M., et al.\ 2022, Universe, 8, 45

2022
[72]

R., Dolphin, A

Weisz, D. R., Dolphin, A. E., Savino, A., et al, 2024, , 271, 47

2024
[73]

St\'efan van der Walt & Jarrod Millman, 56 -- 61, doi:10.1051/0004-6361/201322068

Wes McKinney, 2010, in Proceedings of the 9th Python in Science Conference, ed. St\'efan van der Walt & Jarrod Millman, 56 -- 61, doi:10.1051/0004-6361/201322068

2010 doi
[74]

D., Chandar, R., Lee, J., et al., 2020, , 889, 154

Whitmore, B. D., Chandar, R., Lee, J., et al., 2020, , 889, 154

2020

Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.

[1] [1]

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thebibliography [1] 20pt to REFERENCES 6pt =0pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command E...

2021

[2] [2]

Ai, M., Zhu, M., Xu, J., et al.\ 2023, , 524, 2911

work page 2023

[3] [3]

2008, , 135, 1900

Annibali, F., Aloisi, A., Mack, J., et al. 2008, , 135, 1900

work page 2008

[4] [4]

2018, , 476, 1942

Annibali, F., Morandi, E., Watkins, L.L., et al. 2018, , 476, 1942

work page 2018

[5] [5]

2011, , 142, 129

Annibali, F., Tosi, M., Aloisi, A., et al. 2011, , 142, 129

work page 2011

[6] [6]

2012, , 745, L1

Annibali, F., Tosi, M., Aloisi, A., et al. 2012, , 745, L1

work page 2012

[7] [7]

2017, , 843, 20

Annibali, F., Tosi, M., Romano, D., et al. 2017, , 843, 20

work page 2017

[8] [9]

K., & Klein, U., 1994, , 285, 385

Bajaja, E., Huchtmeier, W. K., & Klein, U., 1994, , 285, 385

work page 1994