Pith. sign in

REVIEW 3 major objections 4 minor 81 references

Chemical abundances and small-scale gas kinematics in the local star-forming galaxy NGC 2366

T0 review · 3 major / 4 minor · reviewed 2026-08-06 · deepseek-v4-flash

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

Pith's one-line read The starburst region Mrk 71 in NGC 2366 is richer in oxygen than the rest of the galaxy, a result the paper attributes to metal enrichment by the central cluster's outflow.

desk verdict Solid, honest survey paper with genuinely new Te abundances and kinematic candidates, but the Mrk 71 enrichment claim is weakened by an aperture-selection effect the authors do not quantify. read the letter →

arxiv 2507.08651 v1 pith:Y6U4DL5F submitted 2025-07-11 astro-ph.GA astro-ph.HEastro-ph.IM

Anastasiya D. Yarovova , Ivan S. Gerasimov , Oleg V. Egorov , Alexei V. Moiseev , Konstantin I. Vasiliev , Tatiana A. Lozinskaya This is my paper · ORCID
classification astro-ph.GAastro-ph.HEastro-ph.IM
keywords NGC2366Mrk71HIIregionabundancesdirectTemethoddwarfgalaxychemicalenrichmentstarburstoutflowsWolf-Rayetcandidatessupernovaremnants
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 measures gas-phase oxygen abundances and small-scale kinematics across the dwarf galaxy NGC 2366, a local Green Pea analogue, using long-slit spectroscopy and Fabry-Perot interferometry. The central result is that the starburst region Mrk 71 is richer in oxygen than the galaxy's other HII regions, with 12+log(O/H) up to 8.02 in its outer part against roughly 7.6–7.9 elsewhere, opposite to the flat gradient suggested by earlier photometric estimates. The authors interpret the excess, together with spatial abundance variations within Mrk 71, as evidence that the outflow from the central super star cluster has locally enriched the interstellar medium. They also identify 20 regions with elevated H-alpha velocity dispersion and argue that one object is a new Wolf–Rayet candidate and two are supernova remnants. If correct, the result shows that dwarf galaxies need not be chemically homogeneous and that stellar feedback can imprint small-scale abundance structure.

What carries the argument

The argument rests on the 'direct' electron-temperature method: detecting the auroral line [O iii] λ4363 in each region's integrated spectrum, deriving Te in the doubly ionized zone, and converting line fluxes to O/H with standard two-zone nebular relations (with a fixed Te(O+) relation for singly ionized oxygen). The kinematic classification uses an I–σ diagram built from Fabry-Perot Hα maps, which separates quiescent HII regions from diffuse gas, bubbles, and compact high-energy sources based on surface brightness and intrinsic velocity dispersion. The combination allows the authors to connect localized kinematic perturbations to candidate stars and remnants and to restrict abundance measurements to photoionized regions.

What would settle it

An integral-field map of NGC 2366 at roughly 30-pc resolution that measures Te and O/H in every HII region, with Mrk 71 resolved into knot A and the outflow cone, would settle the claim: if the apparent oxygen excess disappears when regions are compared at matched ionization parameter and Te sampling, the enrichment is a slit-selection artifact; if the excess persists with a radial peak near the cluster, outflow enrichment is confirmed. Searching for enhanced alpha-element abundances in the enriched gas would further distinguish supernova ejecta from photoionization biases.

Watch

Extended reading notes

Core claim

Using auroral-line electron temperatures measured from the [O iii] λ4363 line, the authors determine 12+log(O/H) for 15 HII regions in NGC 2366. Mrk 71 stands out: its central knot (region 65) has 7.83, the outflow and surrounding regions reach 7.90–8.02, while most other regions including NGC 2363 lie at 7.6–7.8. Within Mrk 71 the abundances and electron temperatures vary steeply along the slit (Te from about 13,500 K to 18,300 K), so the region is not chemically homogeneous. The paper rejects the earlier claim of a flat abundance gradient across the galaxy, attributing the discrepancy to the insensitivity and contamination problems of the earlier photometric calibrations, and interprets the localized oxygen excess as metal enrichment by the kiloparsec-scale outflow from the super star cluster at Mrk 71's center.

Load-bearing premise

The abundance comparison assumes that the electron temperature measured from the [O III] 4363 line in a restricted integration window along each slit is representative of the whole HII region, and that the 15 regions with detected auroral lines fairly represent the galaxy's baseline metallicity.

Editorial extensions

If this is right

  • If Mrk 71's oxygen excess is real enrichment from the outflow, then star clusters can locally raise the metallicity of the ISM in dwarf galaxies on roughly hundred-parsec scales, making chemical inhomogeneity a common feature rather than a rarity.
  • The previously claimed flat radial gradient in NGC 2366 (Roy et al. 1996) is replaced by a non-uniform abundance floor of 12+log(O/H) ≈ 7.6–8.0, so future abundance studies of this galaxy must account for local scatter.
  • The new Wolf–Rayet candidate S1, identified by its triple-component Hα profile and He ii λ4686 emission, together with the new SNR candidates S2 and S11 and the confirmed candidate S3, adds to the census of mechanical feedback sources in the galaxy.
  • The similarity to the outflow-enriched galaxy J1044+0353 suggests that outflow-driven enrichment may be a general feature of compact starbursts, including Green Pea analogues.

Reading between the lines

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

  • A natural test: high-spatial-resolution integral-field maps of Mrk 71 that resolve knot A and the outflow cone could show whether the high O/H traces the outflow's metal-loaded gas as a spatial gradient falling with distance from the cluster, or instead mirrors the ionization structure; if the latter, part of the excess could be an excitation artifact.
  • The same method applied to other Green Pea analogues with known outflows could establish whether local metal enrichment near starbursts is a common precursor to the escaping Lyman continuum that Green Peas exhibit.
  • Because strong-line calibrations are calibrated on homogeneous HII regions, small-scale inhomogeneity of the type reported here could bias S-calibration or O3N2 estimates; the paper's S-calibration agrees with its Te values, but in more extreme cases the bias could be larger.
  • The absence of a clear N/O gradient between Mrk 71 and the rest of the galaxy may constrain the enrichment source: if oxygen was supplied by recent core-collapse supernovae, nitrogen might not yet have risen; this could be tested by comparing alpha-element abundances in the enriched gas.
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, and a circularity audit.

Referee Report

3 major / 4 minor

Summary. The paper presents new SCORPIO-2 Fabry-Perot interferometry and long-slit spectroscopy of the nearby dwarf galaxy NGC 2366, together with narrow-band imaging. It identifies 20 regions with elevated H-alpha velocity dispersion, classifies several as new Wolf-Rayet or supernova remnant candidates, and derives electron temperatures and oxygen/nitrogen abundances for 15 H ii regions using the direct Te method, supplemented by the S-calibration for additional regions. The central claim is that Mrk 71 and its associated outflow are more oxygen-rich than the other H ii regions in the galaxy, with 12+log(O/H) ranging from about 7.6 to 8.0, and that this difference, together with local spatial variations, indicates metal enrichment of the ISM by the outflow from the super star cluster in Mrk 71.

Significance. If the central claim holds, the paper provides direct evidence for small-scale chemical inhomogeneity and localized metal enrichment by stellar feedback in a dwarf galaxy, which is relevant to models of chemical evolution that assume instantaneous and homogeneous mixing. The paper's strengths include the homogeneous long-slit dataset, direct Te-based abundances for 15 regions, Monte Carlo random uncertainties, and the combination of kinematic and chemical diagnostics to identify new SNR and WR candidates. However, the significance of the abundance result is conditional on ruling out aperture-selection and other systematic biases in the Te measurements; the current analysis does not yet establish the claimed Mrk 71 enrichment as intrinsic.

major comments (3)
  1. [Section 3.4] The Te for each region is measured from the area where [O III] lambda4363 is detected above 3-sigma per pixel, and this Te is then assumed to represent the entire O2+ zone. For faint comparison regions (1, 2, 61, 63, 69, and the NGC 2363 components), this sub-aperture selects the hottest, highest-ionization gas, biasing Te high and O/H low, while Mrk 71, being much brighter, is integrated over a larger and less extreme fraction of its volume. The paper provides no test of the sensitivity of Te and 12+log(O/H) to the integration aperture, and the Monte Carlo errors in Table 3 propagate only line-flux noise. Given the paper's own caveat in Section 3.3 that the slits cross only the outskirts of regions 1, 44, 45, and 63, the Mrk 71 versus rest-of-galaxy contrast could be produced by the measurement procedure rather than by true enrichment. Please re-derive the abundances using a homogeneous aperture definition, for example matching S/N or physical radius, and report the resulting contrast.
  2. [Section 4.2 and Table 3] The spatial abundance pattern does not cleanly match the proposed outflow enrichment. The highest oxygen abundance in the Mrk 71 complex, 12+log(O/H) = 8.02, is in region 65C, which Section 3.3 places further than the outflow area, whereas region 65B at the outflow tip has 7.90 and the central knot A (region 65) has 7.83. If metals are being transported by the outflow, the peak enrichment would be expected in or immediately downstream of the detected cone, not beyond it. The authors should address this tension, for example by discussing projection effects or an alternative geometry, or by explicitly stating that the enrichment pattern is not spatially correlated with the outflow.
  3. [Section 3.4 and Table 3] No systematic error budget is given for the Te method. The calculation fixes ne = 30 cm^-3 for all non-Mrk 71 regions, adopts the empirical relation Te(O+) = 0.7 Te(O2+) + 3000 K, and uses the Fitzpatrick (1999) reddening law without varying these choices. The claimed 0.1-0.4 dex excess of Mrk 71 relative to the rest of the galaxy is small compared to the plausible range of such systematics, so the quoted uncertainties substantially understate the error budget. Please provide systematic-error estimates, or show explicitly that the Mrk 71 versus rest-of-galaxy contrast is insensitive to each of these assumptions.
minor comments (4)
  1. [Section 3.4] The sentence describing the density measurement, 'based on [S ii] lambda6731/[S ii] lambda6731 ratio', should read '[S ii] lambda6717/[S ii] lambda6731' or '[S ii] 6717/6731' to be meaningful.
  2. [Section 4.3] The phrase 'Broad outflow component remain over-resolved in our FPI data' should be 'remains over-resolved' or, more clearly, 'was not resolved' to convey the intended meaning.
  3. [Figure 6 caption] The caption says 'The bottom panels (j,k,i) show...' but the panels are labelled j, k, and l; this should be corrected to '(j,k,l)'.
  4. [Table A1] The region labels '57PA=87' and '57PA=32' are confusing; the authors should use distinct names for the two spectra of region 57, for example '57 (PA=87)' and '57 (PA=32)', to match the text.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the Te-based abundances are outputs of measured line ratios, not fitted inputs; the enrichment claim is an interpretation, and the self-citations are not load-bearing.

full rationale

The paper's central abundance result is derived from independently measured emission-line fluxes: electron temperatures come from the [O III] λ4363/λ5007 ratio via pyneb, and oxygen abundances follow from the temperature plus [O II] and [O III] line ratios. These quantities are not supplied into the derivation as assumed values; they are produced by it. The claim that Mrk 71 is more oxygen-rich than the other H II regions is a comparison of these independently derived outputs, not a recovered input. The self-citations in the paper (Moiseev 2002; Moiseev & Egorov 2008; Egorov et al. 2018, 2021, 2023; Yarovova et al. 2023) concern data reduction and the I-sigma classification scheme, none of which is used to define or force the abundance values. The stated caveat that slits cross only the outskirts of regions 1, 44, 45, and 63, and the 3σ-window integration for [O III] λ4363, are potential systematic and aperture-selection limitations; they may bias the comparison, but they do not make the derivation circular, because the comparison regions' abundances are not constructed from Mrk 71's abundance or from a parameter fitted to it. No equation in the paper reduces a predicted quantity to an input by construction, and no load-bearing premise is established solely by a self-citation.

Assumptions & free parameters 1 free parameters · 5 assumptions · 0 invented entities

The central claims rely on standard astrophysical calibrations and on the representativeness of sparse slit sampling; no new particles, forces, or fitted constants are introduced. The fixed low-density value and the empirical T(O+) relation are inherited from prior work and could shift abundances systematically.

free parameters (1)
  • Fixed electron density for low-density HII regions = 30 cm^-3 (assumed, not fitted)
    The [S II] ratio is degenerate near the low-density limit for most regions, so n_e is fixed at 30 cm^-3. Abundances are nearly insensitive to this choice, but it is an input parameter.
assumptions (5)
  • domain assumption The electron temperature of the O2+ zone, measured from [O III] 4363/5007, can be converted to the O+ zone temperature with T_e(O+) = 0.7 T_e(O2+) + 3000 K.
    Used in Sec 3.4; no direct measurement of the O+ auroral line is made, so the empirical Garnett (1992) relation is load-bearing for oxygen abundance.
  • domain assumption The Balmer decrement reddening correction, using the Fitzpatrick (1999) curve and negligible underlying stellar absorption, is adequate for all regions.
    Invoked in Sec 3.3; absorption is cited as small from Chen et al. (2023), but no per-region absorption correction is applied.
  • domain assumption The line ratios from the selected HII regions are dominated by photoionization, so shocks and DIG do not significantly bias the Te-based abundances.
    The BPT analysis in Sec 3.3 places most regions in the photoionization zone, but the authors note that some objects lie outside the model envelope and could have shock contributions.
  • domain assumption The 15 regions with [O III] 4363 detections from three slit positions are representative enough to compare Mrk 71 with the rest of NGC 2366.
    Sec 3.1 and Sec 3.4 use only 15 of 74 HII regions; slit positions are limited and some slits cross only region outskirts, making sampling bias a possible issue for the galaxy-wide comparison.
  • domain assumption Standard pyneb atomic data and the Pilyugin & Grebel (2016) S-calibration are applicable at NGC 2366's metallicity.
    Used in Sec 3.4; systematic calibration uncertainties are not propagated into the final abundance errors.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Chemical abundances and small-scale gas kinematics in the local star-forming galaxy NGC 2366." pith.science (2026). https://pith.science/paper/Y6U4DL5F

@misc{pith2026250708651,
  author       = {Pith},
  title        = {Pith review of: Chemical abundances and small-scale gas kinematics in the local star-forming galaxy NGC 2366},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/Y6U4DL5F}},
  note         = {Machine review of arXiv:2507.08651}
}
read the original abstract

We present a detailed spectroscopic study of ionised gas in the nearby (~3.3Mpc) dwarf galaxy NGC 2366, a local analogue of Green Pea galaxies, based on observations with the SCORPIO-2 instrument at the Russian 6-m BTA telescope. Using scanning Fabry-Perot interferometry and long-slit spectroscopy, we examine the gas kinematics, excitation mechanisms, and chemical abundances across the disc of NGC 2366, including its prominent starburst region Mrk 71 and the companion region NGC 2363. We identified 20 regions with locally elevated Ha velocity dispersion, only four of which correspond to known high-energy sources. We argue that one of the remaining objects can be a previously unidentified Wolf-Rayet star and two - supernova remnants. For 15 HII regions, we measure electron temperatures, oxygen and nitrogen abundances via the `direct' Te method, with 12 + log(O/H) ranging from 7.6 to 8.0 in most of the regions. We show that Mrk 71 has higher oxygen abundance compared to the other \HII regions in the galaxy, contrary to the previous indirect estimates suggesting flat gradient throughout the galaxy. Together with the localized spatial variations of metallicity in the area, it is indicative of metal enrichment by the outflow from the super star cluster in the centre of Mrk 71.

Figures

Figures reproduced from arXiv: 2507.08651 by the authors.

Figure 1
Figure 1. The image of NGC 2366 (left-hand panel) and zoom-in to its central part (middle panel) and Mrk 71 (right-hand panel). Left panel shows H𝛼+continuum narrow-band image (red; this paper) combined with the stellar continuum (grey; DECaLS; Dey et al. 2019). Middle panel shows combination of images in H𝛼 (red; this paper) and [O iii] (green; this paper) emission lines tracing ionized gas, far-UV (blue; GALEX; Hunter et al… view at source ↗
Figure 2
Figure 2. Maps of NGC 2366 obtained from narrow-band images in H𝛼, [S ii] and [O iii] emission lines. Panel ‘a’ shows a map of NGC 2366 in H𝛼 line with overlapped H ii region positions defined in this work. Panels ‘b’ and ‘c’ show [S ii]/H𝛼 and [O iii]/H𝛽 ratios, respectively. H𝛽* is obtained as H𝛼/3.1 (which is consistent with median H𝛼/H𝛽, obtained from spectra). Mrk 71 and its outflow region (shown by magenta lines on pane… view at source ↗
Figure 3
Figure 3. Classification map (a) and 𝐼 − 𝜎 diagram (b) coloured according to classification described in the text (see Section 3.2). C1 refers to DIG, C2 – H ii regions, C3 – intermediate class with elevated velocity dispersion, C4 – regions of perturbed ionised gas (such as expanding bubbles and turbulent ISM), C5 – candidates to individual high mechanical energy sources. H𝛼 image (c) and velocity dispersion map (d) are give… view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: Profiles of regions exhibiting large velocity dispersion identified from FPI data. Central panel shows the intensity distribution in the H𝛼 line with superimposed slit positions (black lines). Locations of regions with turbulent motions revealed in the present work are…
Figure 5
Figure 5. Figure 5: Same as in Fig.4, but for The Mrk 71 region and its surroundings. (1999) reddening curve. The 𝐸(𝐵 − 𝑉) value is estimated from the Balmer decrement H𝛼/H𝛽 consistent with the electron temperature measured for the particular H ii region. We did not subtract the underlyin…
Figure 6
Figure 6. Figure 6: Slit locations are superimposed on the false-colour image (B + V + H𝛼) of NGC 2366 (a,b,c) and on the velocity dispersion map (d,e,f). Distribution of emission line intensity ratios along the slits for H𝛼, [S ii], [O iii] and [N ii] lines can be found on panels g,h,i f…
Figure 7
Figure 7. Figure 7: Diagnostic BPT diagram, based on relations from Kewley et al. (2001) (black line) and Kauffmann et al. (2003) (grey line), showing boundary between photoionised regions (to the left of the lines) and regions with high contributions of shock excitation. The models from …
Figure 8
Figure 8. Figure 8: We highlight two regions of spectrum 65 (central part of Mrk 71) around the H𝛼 and [O iii] spectral lines, demonstrating broad components. To obtain the reliable model, all the lines in each spectral window were fitted simultaniousely. The top two panels show the spect…

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

81 extracted references · 33 canonical work pages

  1. [1]

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

    ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all := #1 ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....

  3. [3]

    Optical observations of the nearby galaxy NGC 2366 through narrowband H$\alpha$ and SII filters. Supernova remnants status

    van Dyk S. D., Puche D., Wong T., 1998, AJ, 116, 2341. doi:10.1086/300584 @ARTICLE Vucetic2019, author = Vu c eti \'c , M. M. and Oni \'c , D. and Petrov , N. and \'C iprijanovi \'c , A. and Pavlovi \'c , M. Z. , title = " Optical Observations of the Nearby Galaxy NGC 2366 Through Narrowband H\_alpha and [SII] Filters. Supernova Remnants Status ", journal...

    work page Pith review arXiv 1998

  4. [4]

    L., Moiseev A

    Afanasiev V. L., Moiseev A. V., 2011, Baltic Astronomy, http://adsabs.harvard.edu/abs/2011BaltA..20..363A 20, 363

    work page 2011

  5. [5]

    Aparicio A., et al., 1995, @doi [ ] 10.1086/117509 , https://ui.adsabs.harvard.edu/abs/1995AJ....110..212A 110, 212

    work page doi:10.1086/117509 1995

  6. [6]

    Astropy Collaboration et al., 2013, @doi [ ] 10.1051/0004-6361/201322068 , http://adsabs.harvard.edu/abs/2013A

    doi:10.1051/0004-6361/201322068 2013

  7. [7]

    Astropy Collaboration et al., 2018, @doi [ ] 10.3847/1538-3881/aabc4f , https://ui.adsabs.harvard.edu/abs/2018AJ....156..123A 156, 123

    doi:10.3847/1538-3881/aabc4f 2018

  8. [8]

    A., Phillips M

    Baldwin J. A., Phillips M. M., Terlevich R., 1981, @doi [ ] 10.1086/130766 , http://adsabs.harvard.edu/abs/1981PASP...93....5B 93, 5

    doi:10.1086/130766 1981

Show all 81 references
  1. [9]

    C., Robert C., Krongold Y., 2009, @doi [ ] 10.1051/0004-6361/200811132 , https://ui.adsabs.harvard.edu/abs/2009A&A...500..817B 500, 817

    Binette L., Drissen L., Ubeda L., Raga A. C., Robert C., Krongold Y., 2009, @doi [ ] 10.1051/0004-6361/200811132 , https://ui.adsabs.harvard.edu/abs/2009A&A...500..817B 500, 817

    2009 doi

  2. [10]

    Chen Y., et al., 2023, @doi [Nature Astronomy] 10.1038/s41550-023-01953-7 , https://ui.adsabs.harvard.edu/abs/2023NatAs...7..771C 7, 771

    2023 doi

  3. [11]

    M., 2009, @doi [ ] 10.1088/0004-6256/137/4/3869 , https://ui.adsabs.harvard.edu/abs/2009AJ....137.3869C 137, 3869

    Chomiuk L., Wilcots E. M., 2009, @doi [ ] 10.1088/0004-6256/137/4/3869 , https://ui.adsabs.harvard.edu/abs/2009AJ....137.3869C 137, 3869

    2009 doi

  4. [12]

    J., 2022, @doi [ ] 10.3847/1538-3881/ac4498 , https://ui.adsabs.harvard.edu/abs/2022AJ....163...97D 163, 97

    Davidge T. J., 2022, @doi [ ] 10.3847/1538-3881/ac4498 , https://ui.adsabs.harvard.edu/abs/2022AJ....163...97D 163, 97

    2022 doi

  5. [13]

    Dey A., et al., 2019, @doi [ ] 10.3847/1538-3881/ab089d , https://ui.adsabs.harvard.edu/abs/2019AJ....157..168D 157, 168

    2019 doi

  6. [14]

    Drissen L., Roy J.-R., Robert C., 1997, @doi [ ] 10.1086/310417 , https://ui.adsabs.harvard.edu/abs/1997ApJ...474L..35D 474, L35

    1997 doi

  7. [15]

    Drissen L., Roy J.-R., Robert C., Devost D., Doyon R., 2000, @doi [ ] 10.1086/301204 , https://ui.adsabs.harvard.edu/abs/2000AJ....119..688D 119, 688

    2000 doi

  8. [16]

    A., Smith L

    Drissen L., Crowther P. A., Smith L. J., Robert C., Roy J.-R., Hillier D. J., 2001, @doi [ ] 10.1086/318264 , https://ui.adsabs.harvard.edu/abs/2001ApJ...546..484D 546, 484

    2001 doi

  9. [17]

    V., Lozinskaya T

    Egorov O. V., Lozinskaya T. A., Moiseev A. V., Smirnov-Pinchukov G. V., 2018, @doi [ ] 10.1093/mnras/sty1158 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.478.3386E 478, 3386

    2018 doi

  10. [18]

    V., Lozinskaya T

    Egorov O. V., Lozinskaya T. A., Vasiliev K. I., Yarovova A. D., Gerasimov I. S., Kreckel K., Moiseev A. V., 2021, @doi [ ] 10.1093/mnras/stab2710 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.508.2650E 508, 2650

    2021 doi

  11. [19]

    V., et al., 2023, @doi [ ] 10.1051/0004-6361/202346919 , https://ui.adsabs.harvard.edu/abs/2023A&A...678A.153E 678, A153

    Egorov O. V., et al., 2023, @doi [ ] 10.1051/0004-6361/202346919 , https://ui.adsabs.harvard.edu/abs/2023A&A...678A.153E 678, A153

    2023 doi

  12. [20]

    N., Aktekin E., 2021, @doi [ ] 10.1016/j.newast.2020.101492 , https://ui.adsabs.harvard.edu/abs/2021NewA...8301492E 83, 101492

    Ercan E. N., Aktekin E., 2021, @doi [ ] 10.1016/j.newast.2020.101492 , https://ui.adsabs.harvard.edu/abs/2021NewA...8301492E 83, 101492

    2021

  13. [21]

    Esteban C., Bresolin F., Peimbert M., Garc \' a-Rojas J., Peimbert A., Mesa-Delgado A., 2009, @doi [ ] 10.1088/0004-637X/700/1/654 , https://ui.adsabs.harvard.edu/abs/2009ApJ...700..654E 700, 654

    2009 doi

  14. [22]

    M., Rodr \' guez M

    Feinstein C., Baume G., Vergne M. M., Rodr \' guez M. J., 2024, @doi [ ] 10.1093/mnras/stae2028 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.533.4300F 533, 4300

    2024 doi

  15. [23]

    L., 1999, @doi [ ] 10.1086/316293 , https://ui.adsabs.harvard.edu/abs/1999PASP..111...63F 111, 63

    Fitzpatrick E. L., 1999, @doi [ ] 10.1086/316293 , https://ui.adsabs.harvard.edu/abs/1999PASP..111...63F 111, 63

    1999 doi

  16. [24]

    R., 1992, @doi [ ] 10.1086/116146 , https://ui.adsabs.harvard.edu/abs/1992AJ....103.1330G 103, 1330

    Garnett D. R., 1992, @doi [ ] 10.1086/116146 , https://ui.adsabs.harvard.edu/abs/1992AJ....103.1330G 103, 1330

    1992 doi

  17. [25]

    S., Egorov O

    Gerasimov I. S., Egorov O. V., Lozinskaya T. A., Moiseev A. V., Oparin D. V., 2022, @doi [ ] 10.1093/mnras/stac3002 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.517.4968G 517, 4968

    2022 doi

  18. [26]

    S., Egorov O

    Gerasimov I. S., Egorov O. V., Moiseev A. V., Kniazev A. Y., Lozinskaya T. A., Egorova E. S., 2024, @doi [ ] 10.1093/mnras/stae462 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.529.1138G 529, 1138

    2024 doi

  19. [27]

    M., et al., 1994, @doi [ ] 10.1086/174992 , https://ui.adsabs.harvard.edu/abs/1994ApJ...437..239G 437, 239

    Gonzalez-Delgado R. M., et al., 1994, @doi [ ] 10.1086/174992 , https://ui.adsabs.harvard.edu/abs/1994ApJ...437..239G 437, 239

    1994 doi

  20. [28]

    Gutkin J., Charlot S., Bruzual G., 2016, @doi [ ] 10.1093/mnras/stw1716 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.462.1757G 462, 1757

    2016 doi

  21. [29]

    A., Elmegreen B

    Hunter D. A., Elmegreen B. G., van Woerden H., 2001, @doi [ ] 10.1086/321611 , https://ui.adsabs.harvard.edu/abs/2001ApJ...556..773H 556, 773

    2001 doi

  22. [30]

    A., Elmegreen B

    Hunter D. A., Elmegreen B. G., Ludka B. C., 2010, @doi [ ] 10.1088/0004-6256/139/2/447 , https://ui.adsabs.harvard.edu/abs/2010AJ....139..447H 139, 447

    2010 doi

  23. [31]

    A., et al., 2012, @doi [ ] 10.1088/0004-6256/144/5/134 , https://ui.adsabs.harvard.edu/abs/2012AJ....144..134H 144, 134

    Hunter D. A., et al., 2012, @doi [ ] 10.1088/0004-6256/144/5/134 , https://ui.adsabs.harvard.edu/abs/2012AJ....144..134H 144, 134

    2012 doi

  24. [32]

    A., Elmegreen B

    Hunter D. A., Elmegreen B. G., Madden S. C., 2024, @doi [ ] 10.1146/annurev-astro-052722-104109 , https://ui.adsabs.harvard.edu/abs/2024ARA&A..62..113H 62, 113

    2024 doi

  25. [33]

    I., Thuan T

    Izotov Y. I., Thuan T. X., 2011, @doi [ ] 10.1088/0004-637X/734/2/82 , https://ui.adsabs.harvard.edu/abs/2011ApJ...734...82I 734, 82

    2011 doi

  26. [34]

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

    Izotov Y. I., Stasi \'n ska G., Meynet G., Guseva N. G., Thuan T. X., 2006, @doi [ ] 10.1051/0004-6361:20053763 , https://ui.adsabs.harvard.edu/abs/2006A&A...448..955I 448, 955

    2006 doi

  27. [35]

    L., Auger M., Aloisi A., Calzetti D., Kewley L., 2016, @doi [ ] 10.3847/0004-637X/816/1/40 , https://ui.adsabs.harvard.edu/abs/2016ApJ...816...40J 816, 40

    James B. L., Auger M., Aloisi A., Calzetti D., Kewley L., 2016, @doi [ ] 10.3847/0004-637X/816/1/40 , https://ui.adsabs.harvard.edu/abs/2016ApJ...816...40J 816, 40

    2016 doi

  28. [36]

    L., Kumari N., Emerick A., Koposov S

    James B. L., Kumari N., Emerick A., Koposov S. E., McQuinn K. B. W., Stark D. P., Belokurov V., Maiolino R., 2020, @doi [ ] 10.1093/mnras/staa1280 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.495.2564J 495, 2564

    2020 doi

  29. [37]

    Kaaret P., Prestwich A., 2024, @doi [ ] 10.3847/1538-4357/ad4ed0 , https://ui.adsabs.harvard.edu/abs/2024ApJ...968...36K 968, 36

    2024 doi

  30. [38]

    Y., Chilingarian I

    Katkov I. Y., Chilingarian I. V., 2011, in Evans I. N., Accomazzi A., Mink D. J., Rots A. H., eds, Astronomical Society of the Pacific Conference Series Vol. 442, Astronomical Data Analysis Software and Systems XX. p. 143 ( @eprint arXiv 1012.4125 ), @doi 10.48550/arXiv.1012.4125

    2011 doi arXiv

  31. [39]

    Kauffmann G., et al., 2003, @doi [ ] 10.1111/j.1365-2966.2003.07154.x , http://adsabs.harvard.edu/abs/2003MNRAS.346.1055K 346, 1055

    2003

  32. [40]

    J., Dopita M

    Kewley L. J., Dopita M. A., 2002, @doi [ ] 10.1086/341326 , https://ui.adsabs.harvard.edu/abs/2002ApJS..142...35K 142, 35

    2002 doi

  33. [41]

    J., Dopita M

    Kewley L. J., Dopita M. A., Sutherland R. S., Heisler C. A., Trevena J., 2001, @doi [ ] 10.1086/321545 , http://adsabs.harvard.edu/abs/2001ApJ...556..121K 556, 121

    2001 doi

  34. [42]

    J., Nicholls D

    Kewley L. J., Nicholls D. C., Sutherland R. S., 2019, @doi [ ] 10.1146/annurev-astro-081817-051832 , https://ui.adsabs.harvard.edu/abs/2019ARA&A..57..511K 57, 511

    2019 doi

  35. [43]

    S., Krumholz M

    Komarova L., Oey M. S., Krumholz M. R., Silich S., Kumari N., James B. L., 2021, @doi [ ] 10.3847/2041-8213/ac2c09 , https://ui.adsabs.harvard.edu/abs/2021ApJ...920L..46K 920, L46

    2021 doi

  36. [44]

    R., et al., 2014, in Beuther H., Klessen R

    Krumholz M. R., et al., 2014, in Beuther H., Klessen R. S., Dullemond C. P., Henning T., eds, Protostars and Planets VI. p. 243 ( @eprint arXiv 1401.2473 ), @doi 10.2458/azu\_uapress\_9780816531240-ch011

    2014 arXiv

  37. [45]

    A., 2015, @doi [ ] 10.1051/0004-6361/201323152 , https://ui.adsabs.harvard.edu/abs/2015A&A...573A..42L 573, A42

    Luridiana V., Morisset C., Shaw R. A., 2015, @doi [ ] 10.1051/0004-6361/201323152 , https://ui.adsabs.harvard.edu/abs/2015A&A...573A..42L 573, A42

    2015 doi

  38. [46]

    A., et al., 2013, @doi [ ] 10.1051/0004-6361/201321956 , https://ui.adsabs.harvard.edu/abs/2013A&A...559A.114M 559, A114

    Marino R. A., et al., 2013, @doi [ ] 10.1051/0004-6361/201321956 , https://ui.adsabs.harvard.edu/abs/2013A&A...559A.114M 559, A114

    2013 doi

  39. [47]

    L., Peng Z., Li Y., 2024, @doi [ ] 10.3847/1538-4357/ad34ac , https://ui.adsabs.harvard.edu/abs/2024ApJ...966..190M 966, 190

    Martin C. L., Peng Z., Li Y., 2024, @doi [ ] 10.3847/1538-4357/ad34ac , https://ui.adsabs.harvard.edu/abs/2024ApJ...966..190M 966, 190

    2024 doi

  40. [48]

    McQuinn K. B. W., et al., 2010, @doi [ ] 10.1088/0004-637X/721/1/297 , https://ui.adsabs.harvard.edu/abs/2010ApJ...721..297M 721, 297

    2010 doi

  41. [49]

    E., Esteban C., Garc \' a-Rojas J., Kreckel K., Peimbert M., 2024, @doi [Nature Astronomy] 10.1038/s41550-024-02198-8 , https://ui.adsabs.harvard.edu/abs/2024NatAs...8..275M 8, 275

    M \'e ndez-Delgado J. E., Esteban C., Garc \' a-Rojas J., Kreckel K., Peimbert M., 2024, @doi [Nature Astronomy] 10.1038/s41550-024-02198-8 , https://ui.adsabs.harvard.edu/abs/2024NatAs...8..275M 8, 275

    2024 doi

  42. [50]

    S., Jaskot A

    Micheva G., Oey M. S., Jaskot A. E., James B. L., 2017, @doi [ ] 10.3847/1538-4357/aa830b , https://ui.adsabs.harvard.edu/abs/2017ApJ...845..165M 845, 165

    2017 doi

  43. [51]

    M., \"O stlin G., Girichidis P., 2019, @doi [ ] 10.1051/0004-6361/201834838 , https://ui.adsabs.harvard.edu/abs/2019A&A...623A.145M 623, A145

    Micheva G., Christian Herenz E., Roth M. M., \"O stlin G., Girichidis P., 2019, @doi [ ] 10.1051/0004-6361/201834838 , https://ui.adsabs.harvard.edu/abs/2019A&A...623A.145M 623, A145

    2019 doi

  44. [52]

    V., 2002, Bulletin of the Special Astrophysics Observatory, http://adsabs.harvard.edu/abs/2002BSAO...54...74M 54, 74

    Moiseev A. V., 2002, Bulletin of the Special Astrophysics Observatory, http://adsabs.harvard.edu/abs/2002BSAO...54...74M 54, 74

    2002

  45. [53]

    V., 2021, @doi [Astrophysical Bulletin] 10.1134/S1990341321030081 , https://ui.adsabs.harvard.edu/abs/2021AstBu..76..316M 76, 316

    Moiseev A. V., 2021, @doi [Astrophysical Bulletin] 10.1134/S1990341321030081 , https://ui.adsabs.harvard.edu/abs/2021AstBu..76..316M 76, 316

    2021 doi

  46. [54]

    V., Egorov O

    Moiseev A. V., Egorov O. V., 2008, @doi [Astrophysical Bulletin] 10.1134/S1990341308020089 , http://adsabs.harvard.edu/abs/2008AstBu..63..181M 63, 181

    2008 doi

  47. [55]

    V., Lozinskaya T

    Moiseev A. V., Lozinskaya T. A., 2012, , 423, 1831

    2012

  48. [56]

    O., Terlevich R., 1996, @doi [ ] 10.1086/118129 , https://ui.adsabs.harvard.edu/abs/1996AJ....112.1636M 112, 1636

    Munoz-Tunon C., Tenorio-Tagle G., Castaneda H. O., Terlevich R., 1996, @doi [ ] 10.1086/118129 , https://ui.adsabs.harvard.edu/abs/1996AJ....112.1636M 112, 1636

    1996 doi

  49. [57]

    G., Guseva N

    Noeske K. G., Guseva N. G., Fricke K. J., Izotov Y. I., Papaderos P., Thuan T. X., 2000, @doi [ ] 10.48550/arXiv.astro-ph/0007130 , https://ui.adsabs.harvard.edu/abs/2000A&A...361...33N 361, 33

    2000 doi arXiv

  50. [58]

    S., Herrera C

    Oey M. S., Herrera C. N., Silich S., Reiter M., James B. L., Jaskot A. E., Micheva G., 2017, @doi [ ] 10.3847/2041-8213/aa9215 , https://ui.adsabs.harvard.edu/abs/2017ApJ...849L...1O 849, L1

    2017 doi

  51. [59]

    S., et al., 2023, @doi [ ] 10.3847/2041-8213/ad07dd , https://ui.adsabs.harvard.edu/abs/2023ApJ...958L..10O 958, L10

    Oey M. S., et al., 2023, @doi [ ] 10.3847/2041-8213/ad07dd , https://ui.adsabs.harvard.edu/abs/2023ApJ...958L..10O 958, L10

    2023 doi

  52. [60]

    Ouchi M., et al., 2009, @doi [ ] 10.1088/0004-637X/706/2/1136 , https://ui.adsabs.harvard.edu/abs/2009ApJ...706.1136O 706, 1136

    2009 doi

  53. [61]

    L., Thibodeaux P., Zhang J., Hu W., Li Y., 2023, @doi [ ] 10.3847/1538-4357/ace9c0 , https://ui.adsabs.harvard.edu/abs/2023ApJ...954..214P 954, 214

    Peng Z., Martin C. L., Thibodeaux P., Zhang J., Hu W., Li Y., 2023, @doi [ ] 10.3847/1538-4357/ace9c0 , https://ui.adsabs.harvard.edu/abs/2023ApJ...954..214P 954, 214

    2023 doi

  54. [62]

    S., Grebel E

    Pilyugin L. S., Grebel E. K., 2016, @doi [ ] 10.1093/mnras/stw238 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.457.3678P 457, 3678

    2016 doi

  55. [63]

    Roy J.-R., Boulesteix J., Joncas G., Grundseth B., 1991, @doi [ ] 10.1086/169609 , https://ui.adsabs.harvard.edu/abs/1991ApJ...367..141R 367, 141

    1991 doi

  56. [64]

    L., Dufour R

    Roy J.-R., Aube M., McCall M. L., Dufour R. J., 1992, @doi [ ] 10.1086/171035 , https://ui.adsabs.harvard.edu/abs/1992ApJ...386..498R 386, 498

    1992 doi

  57. [65]

    Roy J.-R., Belley J., Dutil Y., Martin P., 1996, @doi [ ] 10.1086/176968 , https://ui.adsabs.harvard.edu/abs/1996ApJ...460..284R 460, 284

    1996 doi

  58. [66]

    K., 2024, @doi [ ] 10.1146/annurev-astro-071221-052651 , https://ui.adsabs.harvard.edu/abs/2024ARA&A..62..369S 62, 369

    Schinnerer E., Leroy A. K., 2024, @doi [ ] 10.1146/annurev-astro-071221-052651 , https://ui.adsabs.harvard.edu/abs/2024ARA&A..62..369S 62, 369

    2024 doi

  59. [67]

    I., Yakunin I

    Shatsky N., et al., 2020, in Romanyuk I. I., Yakunin I. A., Valeev A. F., Kudryavtsev D. O., eds, Ground-Based Astronomy in Russia. 21st Century. pp 127--132 ( @eprint arXiv 2010.10850 ), @doi 10.26119/978-5-6045062-0-2_2020_127

    2020 arXiv

  60. [68]

    J., et al., 2023, @doi [ ] 10.3847/1538-4357/ad00b4 , https://ui.adsabs.harvard.edu/abs/2023ApJ...958..194S 958, 194

    Smith L. J., et al., 2023, @doi [ ] 10.3847/1538-4357/ad00b4 , https://ui.adsabs.harvard.edu/abs/2023ApJ...958..194S 958, 194

    2023 doi

  61. [69]

    X., Bauer F

    Thuan T. X., Bauer F. E., Izotov Y. I., 2014, @doi [ ] 10.1093/mnras/stu716 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.441.1841T 441, 1841

    2014 doi

  62. [70]

    G., McQuade K., 1995, @doi [ ] 10.1086/117637 , https://ui.adsabs.harvard.edu/abs/1995AJ....110.1640T 110, 1640

    Tolstoy E., Saha A., Hoessel J. G., McQuade K., 1995, @doi [ ] 10.1086/117637 , https://ui.adsabs.harvard.edu/abs/1995AJ....110.1640T 110, 1640

    1995 doi

  63. [71]

    G., Smith L., Leitherer C., 2024, in American Astronomical Society Meeting Abstracts

    Troshynski S., Oey M., Castro N., Bruzual-A. G., Smith L., Leitherer C., 2024, in American Astronomical Society Meeting Abstracts. p. 406.04

    2024

  64. [72]

    B., et al., 2013, @doi [ ] 10.1088/0004-6256/146/4/86 , https://ui.adsabs.harvard.edu/abs/2013AJ....146...86T 146, 86

    Tully R. B., et al., 2013, @doi [ ] 10.1088/0004-6256/146/4/86 , https://ui.adsabs.harvard.edu/abs/2013AJ....146...86T 146, 86

    2013 doi

  65. [73]

    Vale Asari N., Stasi \'n ska G., Morisset C., Cid Fernandes R., 2016, @doi [ ] 10.1093/mnras/stw971 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.460.1739V 460, 1739

    2016 doi

  66. [74]

    E., 1987, @doi [ ] 10.1086/191166 , https://ui.adsabs.harvard.edu/abs/1987ApJS...63..295V 63, 295

    Veilleux S., Osterbrock D. E., 1987, @doi [ ] 10.1086/191166 , https://ui.adsabs.harvard.edu/abs/1987ApJS...63..295V 63, 295

    1987 doi

  67. [75]

    M., Oni \'c D., Petrov N., \'C iprijanovi \'c A., Pavlovi \'c M

    Vu c eti \'c M. M., Oni \'c D., Petrov N., \'C iprijanovi \'c A., Pavlovi \'c M. Z., 2019, @doi [Serbian Astronomical Journal] 10.2298/SAJ190131003V , https://ui.adsabs.harvard.edu/abs/2019SerAJ.198...13V 198, 13

    2019 doi

  68. [76]

    R., Skillman E

    Weisz D. R., Skillman E. D., Cannon J. M., Dolphin A. E., Kennicutt Robert C. J., Lee J., Walter F., 2008, @doi [ ] 10.1086/592323 , https://ui.adsabs.harvard.edu/abs/2008ApJ...689..160W 689, 160

    2008 doi

  69. [77]

    D., Sramek R

    Yang H., Skillman E. D., Sramek R. A., 1994, @doi [ ] 10.1086/116885 , https://ui.adsabs.harvard.edu/abs/1994AJ....107..651Y 107, 651

    1994 doi

  70. [78]

    D., Egorov O

    Yarovova A. D., Egorov O. V., Moiseev A. V., Maryeva O. V., 2023, @doi [ ] 10.1093/mnras/stac2949 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.518.2256Y 518, 2256

    2023 doi

  71. [79]

    J., Weis K., Dettmar R

    van Eymeren J., Bomans D. J., Weis K., Dettmar R. J., 2007, @doi [ ] 10.1051/0004-6361:20077335 , https://ui.adsabs.harvard.edu/abs/2007A&A...474...67V 474, 67

    2007 doi

  72. [80]

    J., Bomans D

    van Eymeren J., Marcelin M., Koribalski B., Dettmar R. J., Bomans D. J., Gach J. L., Balard P., 2009, @doi [ ] 10.1051/0004-6361:200809585 , https://ui.adsabs.harvard.edu/abs/2009A&A...493..511V 493, 511

    2009 doi

  73. [81]

    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.stat...

Pith tools

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