Pith. sign in

REVIEW 3 major objections 5 minor 102 references

Asymptotic Giant Branch Stars in the Nearby Dwarf Galaxy Leo P

T0 review · 3 major / 5 minor · reviewed 2026-08-14 · deepseek-v4-flash

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

Pith's one-line read This paper reports a highly sensitive HST and Spitzer census of evolved stars in the metal-poor dwarf galaxy Leo P and identifies four asymptotic giant branch candidates, two with evidence of dust.

desk verdict A careful, honestly hedged HST/Spitzer census of Leo P's evolved stars; the two new dusty AGB candidates are plausible but unconfirmed, and the paper says so. read the letter →

arxiv 1909.01454 v2 pith:GWQQDZWH submitted 2019-09-03 astro-ph.SR astro-ph.GA

Steven R. Goldman , Martha L. Boyer , Kristen B. McQuinn , Greg C. Sloan , Iain McDonald , Jacco Th. van Loon , Albert A. Zijlstra , Alec S. Hirschauer
show 2 more authors
Evan D. Skillman Sundar Srinivasan
This is my paper · ORCID
classification astro-ph.SRastro-ph.GA
keywords asymptoticgiantbranchstarsLeoPdwarfgalaxiesmetal-poorstellarpopulationscircumstellardustHSTmedium-bandphotometryevolutionhigh-redshift
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

Leo P is the most metal-poor gas-rich galaxy that can be resolved into stars, with a metallicity of about 2% of the solar value, and its isolated, simple history makes it a local stand-in for galaxies seen at high redshift. Using Hubble Space Telescope medium-band near-infrared photometry and Spitzer infrared imaging, the paper identifies four asymptotic giant branch (AGB) star candidates in the galaxy and separates them by surface chemistry: one oxygen-rich source and three carbon-rich sources. Two of the four candidates show evidence of circumstellar dust, which would make them among the most metal-poor dust-producing stars known if confirmed. The paper also recovers two carbon stars previously confirmed spectroscopically and shows that most earlier broad-band AGB candidates in Leo P are actually resolved background galaxies or foreground stars. A confirmed dusty population at this metallicity would give an empirical anchor for whether and how AGB stars can form dust in the early universe.

What carries the argument

The load-bearing tool is the HST WFC3/IR medium-band color-color diagram using the F127M, F139M, and F153M filters, which separates oxygen-rich AGB stars (water absorption) from carbon-rich stars (CN and C2 absorption), a calibration established by Boyer et al. (2013, 2017). The paper applies this diagram to sources above the tip of the red giant branch or reddened beyond the RGB, combines it with Spitzer [3.6]−[4.5] colors to flag dust, and uses point-source sharpness and crowding cuts plus visual inspection to remove background galaxies. That combination is what turns the photometry into a claim about chemical type and dust production.

What would settle it

Take medium-resolution near-infrared spectra (e.g., with JWST NIRSpec) of the oxygen-rich candidate (Source 1) and the dusty carbon-rich candidate (Source 4) and measure their radial velocities against Leo P's systemic velocity (~262 km s−1, as measured for Source 7 by Evans et al. 2019) and look for molecular bands (CO, C2, H2O). If the velocities disagree with Leo P membership or the spectra show galaxy absorption features, the AGB interpretation fails; if the dusty sources show neither dust features nor stellar photospheric bands, the claim that they are dusty AGB stars collapses.

Watch

Extended reading notes

Core claim

The central claim is that Leo P hosts four genuine evolved-star candidates above the tip of the red giant branch: one oxygen-rich candidate with dust in both HST and Spitzer bands, one carbon-rich candidate with heavy optical obscuration, and two carbon-rich candidates with little or no dust. The oxygen-rich source is fainter than typical O-rich AGB stars and may be a planetary nebula or post-AGB object, while the dusty carbon-rich candidate shows a blue [3.6]−[4.5] color consistent with CO absorption rather than warm dust emission. On the authors' interpretation, the medium-band HST color-color method successfully classifies carbon-rich AGB stars at ~2% solar metallicity, and the detected population matches the roughly three massive AGB stars expected from synthetic color-magnitude fitting. If these identifications hold, Leo P provides the most metal-poor resolved examples of dust-producing AGB stars, directly relevant to dust enrichment in high-redshift galaxies.

Load-bearing premise

The classification of the two new dusty candidates as AGB stars of specific chemistry rests on the assumption that the HST medium-band color-color separation, calibrated on higher-metallicity AGB populations, still holds at Leo P's ~2% solar metallicity; this has not been checked spectroscopically for these sources.

Editorial extensions

If this is right

  • If the four candidates are real, Leo P's evolved-star population matches the roughly three massive AGB stars expected from synthetic color-magnitude fitting, so a census of this depth can recover essentially the entire AGB population of the galaxy.
  • The medium-band HST method would be validated for carbon-rich AGB identification at ~2% solar metallicity, extending a tool previously tested on higher-metallicity Magellanic Cloud and dwarf galaxy samples.
  • If the two dusty candidates are confirmed, Leo P would provide concrete examples of dust production at [Fe/H] ≈ −1.8, placing empirical constraints on whether and how AGB stars can form dust with very few metals.
  • Since most previously reported Leo P AGB candidates are reclassified as extended galaxies or foreground stars, earlier broad-band surveys of metal-poor dwarfs may require high-resolution follow-up before their evolved-star counts can be trusted.

Reading between the lines

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

  • If the oxygen-rich candidate is confirmed as a planetary nebula or post-AGB star, the relevant question shifts from AGB dust production to whether short-lived post-AGB phases can contribute meaningful dust at 2% solar metallicity; the paper notes the possibility but does not quantify this contribution.
  • Because the dusty carbon-rich candidate lies outside the half-light radius, a confirmed AGB membership would support recent or spatially extended star formation in Leo P, consistent with inside-out assembly; other extremely metal-poor dwarfs could be checked for the same pattern.
  • A systematic extension of this HST medium-band census to other resolved low-metallicity dwarfs could test whether the number of dusty AGB stars per unit stellar mass rises or falls with metallicity, a comparison the paper calls for but does not run.
  • If the medium-band color-color method proves robust at this metallicity, it can be used to build clean AGB samples in other resolved dwarf galaxies without spectroscopy, allowing dust-production rates to be mapped across a wider metallicity range.
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 / 5 minor

Summary. This paper reports a census of evolved stars in the extremely metal-poor dwarf galaxy Leo P using HST WFC3/IR medium-band (F127M, F139M, F153M) and Spitzer IRAC ([3.6], [4.5]) imaging. The authors identify four candidate asymptotic giant branch (AGB) stars and classify them by chemical type using the Boyer et al. color-color method: one oxygen-rich candidate (Source 1) that appears dusty in both HST and Spitzer data, and three carbon-rich candidates (Sources 2, 3, and 4), one of which (Source 4) may be dusty. They independently recover the two previously spectroscopically confirmed carbon stars (Sources 2 and 3), reclassify many earlier Lee (2016) and Evans et al. (2019) candidates as foreground stars or background galaxies, and compare the observed number of AGB candidates with the MATCH-predicted value of about three. The paper explicitly states that spectroscopic follow-up is needed to confirm the nature of the two new dusty candidates and that they could be post-AGB stars, planetary nebulae, or other phases.

Significance. If confirmed, the two dusty candidates would be among the most metal-poor dust-producing AGB stars known, with direct relevance to dust formation at high redshift. The paper's main strengths are its careful photometric processing with established pipelines (DUSTiNGS, DOLPHOT), the use of previously calibrated medium-band color-color classification, and the explicitly hedged language that correctly labels the sources as candidates requiring follow-up. The recovery of the two spectroscopically confirmed carbon stars provides a useful validation of the classification method at low metallicity. The paper also makes testable predictions by identifying specific sources for JWST spectroscopy, and its DESK fitting tools are publicly available. The novelty rests almost entirely on Source 1 and Source 4, both of which lack spectroscopic confirmation, so the census claim is only as strong as the photometric classification and the derived photometry for those sources.

major comments (3)
  1. [§2.1 and Table 2] The [3.6] magnitude of Source 1 is not measured directly but is derived by applying an aperture-photometry color (≈0.5 mag) to the PSF-based [4.5] magnitude. This derived value directly underlies the claim that Source 1 is dusty in the Spitzer bands. The paper should quantify the uncertainty in this color and magnitude, and demonstrate explicitly that the conclusion of a red [3.6]−[4.5] color is robust to the choice of aperture radius and to possible contamination from nearby sources or foreground stars. Without such a demonstration, the 'dusty in Spitzer' classification for Source 1 is not on the same footing as a direct measurement.
  2. [§3.2 and Figure 6] The oxygen-rich classification and dustiness of Source 1 are weakened by the facts that (a) the DESK/DUSTY SED fit does not reproduce all of the HST filters, (b) the source is about two magnitudes fainter at 4.5 µm than LMC oxygen-rich AGB stars, and (c) the authors concede it could be a planetary nebula or post-AGB star. Since this source is one of only two new objects that carry the paper's novel claim of dust production at 2% solar, the manuscript should either present a quantitative membership or phase assessment (e.g., PN/post-AGB discriminator using the IRAC colors and SED shape) or explicitly rephrase the abstract and conclusion so that 'oxygen-rich' and 'dusty' are presented as tentative classifications subject to spectroscopy, rather than as detections.
  3. [§3.3 and Table 2] Source 4's classification as a dusty carbon star rests on very red HST colors (F127M−F139M = 1.12, F127M−F153M = 1.55) for which no photometric uncertainties are quoted, plus a blue [3.6]−[4.5] = −0.42 interpreted as CO absorption. The source lies outside the half-light radius, and no variability or membership information is presented. The paper should provide the photometric uncertainties (including the error on the [3.6]−[4.5] color) and discuss the probability of a background galaxy, YSO, or other evolved phase. As it stands, the claim that Leo P hosts three carbon-rich candidates, one of which is dusty, is not robustly quantified and could be overturned by a single misclassification.
minor comments (5)
  1. [Table 2] The table lists photometry without uncertainties; for a paper whose main conclusions rest on color measurements, at least the HST colors for the four AGB candidates should include error bars or limits.
  2. [Figure 3] The color-color diagram does not show error bars for the candidate sources; adding them would help the reader judge whether the separation into oxygen- and carbon-rich groups is statistically significant.
  3. [§3.2] The phrase 'full eidth at half maximum' appears to be a typo for 'full width at half maximum.'
  4. [§2.3] The description of the Evans et al. (2019) membership status is slightly confusing: the text says Source 22 has a confirmed membership via Ca ii absorption, while the caption of Figure 1 appears to reverse this. Please check the consistency.
  5. [§3.4] The statement that the two new dusty candidates 'may have been too faint to be detected in the broad-band near-IR imaging with NIRI' is plausible but could be supported by a quantitative comparison of the NIRI detection limits with the F127M/F153M magnitudes of Sources 1 and 4.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: the AGB census uses externally calibrated HST color classification and an independent MATCH prediction.

full rationale

The paper's derivation chain is observational: Spitzer and HST photometry, point-spread-function fitting, cuts in sharpness/crowding/TRGB, then classification by F127M-F139M vs F139M-F153M color-color position using the method of Boyer et al. (2013, 2017). Those prior papers calibrated the medium-band filters on spectroscopically characterized AGB populations, so the classification boundary is external evidence rather than something fitted to Leo P. The two spectroscopically confirmed carbon stars (Sources 2 and 3) are independently recovered, which validates the method in this field. The MATCH prediction of roughly three AGB stars is compared with the four detected candidates without adjusting any model parameter to force agreement. The derived [3.6] magnitude for Source 1 is a photometric construction from an aperture color plus PSF [4.5] magnitude, but it is not used to define the AGB candidate itself, and the paper explicitly cautions that Source 1 may be a PN or post-AGB object. Self-citations to the DUSTiNGS pipeline and DESK are software/tool citations, not load-bearing theoretical premises. The paper's own admission that the dusty-candidate classification 'remains to be confirmed' is a stated observational limitation, not evidence that the result is equivalent to its inputs. No equation or fitted parameter reduces to a predicted quantity, so no circular step can be exhibited.

Assumptions & free parameters 1 free parameters · 4 assumptions · 0 invented entities

The central claim rests on externally calibrated photometric methods and published distances and metallicities; the paper introduces no new physical entities. The only hand-picked value is the assumed [3.6]-[4.5] color for Source 1, an approximation that does not affect the main detection claim.

free parameters (1)
  • Assumed [3.6]-[4.5] color for Source 1 = ~0.5 mag
    Used to derive the 3.6 micron magnitude for Source 1 via aperture photometry because the pipeline did not detect the counterpart. This is an ad hoc approximation but does not drive the census result.
assumptions (4)
  • domain assumption The F127M-F139M vs F139M-F153M color-color classification boundaries from Boyer et al. (2013, 2017), calibrated on higher-metallicity samples, separate carbon-rich and oxygen-rich AGB stars at [Fe/H] ~ -1.8.
    Invoked in Section 2.4 and Figure 3. The paper itself notes this 'remains to be confirmed in our dusty AGB candidates' (Section 3).
  • domain assumption Leo P is at a distance of 1.62 +/- 0.15 Mpc (McQuinn et al. 2013, 2015a), used to place sources relative to the TRGB and to compare luminosities.
    Used in Section 2.4 to define the TRGB cut and in the discussion of absolute magnitudes.
  • domain assumption Galactic extinction toward Leo P is E(B-V) = 0.0227 mag (Schlafly & Finkbeiner 2011) with R_V = 3.1.
    Used in Section 2.2 to correct the HST photometry.
  • domain assumption The stellar models of Aringer et al. (2009, 2016) and Nanni et al. (2013-2018) are adequate for interpreting the colors and SEDs of AGB stars at low metallicity.
    Used in Figures 3 and 7 to classify sources and fit SEDs; these models are external to the paper.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Asymptotic Giant Branch Stars in the Nearby Dwarf Galaxy Leo P." pith.science (2026). https://pith.science/paper/GWQQDZWH

@misc{pith2026190901454,
  author       = {Pith},
  title        = {Pith review of: Asymptotic Giant Branch Stars in the Nearby Dwarf Galaxy Leo P},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/GWQQDZWH}},
  note         = {Machine review of arXiv:1909.01454}
}
read the original abstract

We have conducted a highly sensitive census of the evolved-star population in the metal-poor dwarf galaxy Leo P and detected four asymptotic giant branch (AGB) star candidates. Leo P is one of the best examples of a nearby analog of high-redshift galaxies because of its primitive metal content (2% of the solar value), proximity, and isolated nature, ensuring a less complicated history. Using medium-band optical photometry from the Hubble Space Telescope (HST), we have classified the AGB candidates by their chemical type. We have identified one oxygen-rich source which appears to be dusty in both the HST and Spitzer observations. Its brightness, however, suggests it may be a planetary nebula or post-AGB object. We have also identified three carbon-rich candidates, one of which may be dusty. Follow-up observations are needed to confirm the nature of these sources and to study the composition of any dust that they produce. If dust is confirmed, these stars would likely be among the most metal-poor examples of dust-producing stars known and will provide valuable insight into our understanding of dust formation at high redshift.

Figures

Figures reproduced from arXiv: 1909.01454 by the authors.

Figure 1
Figure 1. An HST F127M medium-band drizzled mosaic of Leo P (half-light radius shown with the gray dashed oval) with sources categorized as oxygen- (blue) and carbon-rich (red). Our AGB classifications as well as those made by Lee (2016) and Evans et al. (2019) are shown with different shapes, where the label “Evans AGB” corresponds to the source with a confirmed membership to Leo P using Ca ii absorption (Source 22), and “Ev… view at source ↗
Figure 2
Figure 2. The luminosity function of the Spitzer [4.5] pho￾tometry. The histogram shows a drop in sensitivity below ∼ 18 mag. it is an excellent environment to study the effects of metallicity on stellar evolution and dust production. In this paper we present the results from a highly sen￾sitive census of the evolved star population in the metal￾poor dwarf galaxy Leo P. We have detected four AGB candidates, two of which show … view at source ↗
Figure 3
Figure 3. HST color-magnitude and color-color diagrams showing (Left) sources above the Tip of the Red Giant Branch (TRGB) or dusty enough to be considered AGB candidates and (Right) a utilization of the method successfully used by Boyer et al. (2013, 2017, 2019) to disentangle carbon- (C-type; red) and oxygen-rich (M-type; blue) evolved stars, and sources classified as either foreground stars or K-type giants (white squares)… view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: HST:ACS F814W mosaic cutouts of our four AGB candidates. All four sources are point-like and unlikely to be background galaxies. Source 1 (Left) and Source 4 (Right) are expected to be dusty. thus we expect contamination from these sources to be rare. Of the twenty-fiv…
Figure 5
Figure 5. Figure 5: An IRAC CMD showing our oxygen (blue circle) and carbon (red circles) AGB candidates in Leo P, along with the locations of other spectroscopically confirmed classes of LMC stars from SAGE-Spec (Jones et al. 2017). Shown are AGB stars (solid lines), PNe (dashed lines), …
Figure 6
Figure 6. Figure 6: The Spectral Energy Distribution of the oxygen-rich AGB candidate, shown with Spitzer and HST photometry, as well as a DUSTY radiative transfer model (Elitzur & Ivezi´c 2001) that uses a black body and grains from Ossenkopf, Henning & Mathis (1992), fitted using the Du…
Figure 8
Figure 8. Figure 8: HST /ACS F814W mosaic cutouts of sources above the TRGB or reddened, but that we have not classified as foreground sources or AGB candidates based on a visual inspection of the image. Source 494 is not likely to be a real source but rather the result of noise near the …
Figure 9
Figure 9. Figure 9: HST /ACS F814W mosaic cutouts of sources that were determined AGB candidates by Lee (2016) but that we have subsequently categorized as extended sources [PITH_FULL_IMAGE:figures/full_fig_p015_9.png]

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

102 extracted references · 78 canonical work pages

  1. [1]

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

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month note number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.co...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.doi doi empty "" "doi:" doi * if FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix ":" * if eprint field.or.null * if FUNCTION format.pid eprint empty format.doi format.eprint if FUNCTION n.dashify 't := "" t...

  3. [3]

    a v-^A_ p[N c, `c ^ ufKK& @*Uz / U, s 1m!ΤR) ٸ1rI'a x сիW㤓N¾뮻 ]t ͚i P, 4d<e <\/_6n [օ/^浰[ |lRZ M 3k WZ͛!Bbҳ ׯNJ +p

    thebibliography [1] 20pt to REFERENCES 6pt =0pt 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 Each re...

    2017

  4. [4]

    Aoki W., Tsuji T., Ohnaka K., 1999, , 350, 945

    1999

  5. [5]

    Aringer B. et al. , 2016, , 457, 3611

    2016

  6. [6]

    Aringer B. et al. , 2009, A&A, 503, 913

    2009

  7. [7]

    Bacon R. et al. , 2010, in , Vol. 7735, Ground-based and Airborne Instrumentation for Astronomy III, p. 773508

    2010

  8. [8]

    Battinelli P., Demers S., 2008, A&A, 493, 1075

    2008

Show all 102 references
  1. [9]

    Battinelli P., Demers S., Mannucci F., 2007, A&A, 474, 35

    2007

  2. [10]

    Beelen A. et al. , 2006, , 642, 694

    2006

  3. [11]

    Bellazzini M. et al. , 2014, , 566, A44

    2014

  4. [12]

    Berg D. A. et al. , 2012, , 754, 98

    2012

  5. [13]

    Bernstein-Cooper E. Z. et al. , 2014, , 148, 35

    2014

  6. [14]

    Bertoldi F. et al. , 2003, , 406, L55

    2003

  7. [15]

    Blum R. D. et al. , 2014, , 148, 86

    2014

  8. [16]

    I., Sackmann I

    Boothroyd A. I., Sackmann I. J., Ahern S. C., 1993, , 416, 762

    1993

  9. [17]

    Boyer M. L. et al. , 2013, , 774, 83

    2013

  10. [18]

    Boyer M. L. et al. , 2015 a , , 216, 10

    2015

  11. [19]

    Boyer M. L. et al. , 2015 b , , 800, 51

    2015

  12. [20]

    Boyer M. L. et al. , 2017, , 851, 152

    2017

  13. [21]

    Boyer M. L. et al. , 2011, , 142, 103

    2011

  14. [22]

    Boyer M. L. et al. , 2019, , 879, 109

    2019

  15. [23]

    Boyer M. L. et al. , 2006, , 132, 1415

    2006

  16. [24]

    A., Clayton G

    Cardelli J. A., Clayton G. C., Mathis J. S., 1989, , 345, 245

    1989

  17. [25]

    Cernicharo J. et al. , 1999, , 526, L41

    1999

  18. [26]

    Clement C. M. et al. , 2001, , 122, 2587

    2001

  19. [27]

    E., 2000, , 112, 1383

    Dolphin A. E., 2000, , 112, 1383

    2000

  20. [28]

    E., 2002, , 332, 91

    Dolphin A. E., 2002, , 332, 91

    2002

  21. [29]

    El-Badry K. et al. , 2016, , 820, 131

    2016

  22. [30]

    Elitzur M., Ivezi \'c Z ., 2001, , 327, 403

    2001

  23. [31]

    Evans C. J. et al. , 2019, A & A, 622, A129

    2019

  24. [32]

    Feast M., Whitelock P., Menzies J., 2002, , 329, L7

    2002

  25. [33]

    A., Hyland A

    Frogel J. A., Hyland A. R., 1972, in Les Spectres des Astres dans l'Infrarouge et les Microondes, pp. 111--120

    1972

  26. [34]

    Giovanelli R. et al. , 2005, , 130, 2598

    2005

  27. [35]

    Goldman S. R. et al. , 2019, , 877, 49

    2019

  28. [36]

    Goldman S. R. et al. , 2017, , 465, 403

    2017

  29. [37]

    S., 1988, Infrared observations of comets halley and wilson and properties of the grains

    Hanner M. S., 1988, Infrared observations of comets halley and wilson and properties of the grains. Tech. rep., Jet Propulsion Lab., California Institute of Technology, Pasadena

    1988

  30. [38]

    Herwig F., 2004, , 155, 651

    2004

  31. [39]

    Hirschauer A. S. et al. , 2016, , 822, 108

    2016

  32. [40]

    Hodapp K. W. et al. , 2003, , 115, 1388

    2003

  33. [41]

    H \"o fner S., Olofsson H., 2018, , 26

    2018

  34. [42]

    Jones O. C. et al. , 2018, , 854, 117

    2018

  35. [43]

    Jones O. C. et al. , 2017, , 470, 3250

    2017

  36. [44]

    Karambelkar V. R. et al. , 2019, , 877, 110

    2019

  37. [45]

    Kasliwal M. M. et al. , 2017, , 839, 88

    2017

  38. [46]

    Kraemer K. E. et al. , 2002, , 140, 389

    2002

  39. [47]

    A., 2008, , 390, L59

    Lagadec E., Zijlstra A. A., 2008, , 390, L59

    2008

  40. [48]

    Laki \'c evi \'c M. et al. , 2015, , 799, 50

    2015

  41. [49]

    R., 2005, , 441, 1117

    Lebzelter T., Wood P. R., 2005, , 441, 1117

    2005

  42. [50]

    Lee C.-H., 2016, , 461, L37

    2016

  43. [51]

    Lee H. et al. , 2006, , 647, 970

    2006

  44. [52]

    Levesque E. M. et al. , 2006, , 645, 1102

    2006

  45. [53]

    Lorenz D. et al. , 2011, , 532, 78

    2011

  46. [54]

    Marigo P. et al. , 2017, , 835, 77

    2017

  47. [55]

    Marshall J. R. et al. , 2004, , 355, 1348

    2004

  48. [56]

    Massey P. et al. , 2007, , 660, 301

    2007

  49. [57]

    Matsunaga N. et al. , 2007, in Astronomical Society of the Pacific Conference Series, Vol. 378, Why Galaxies Care About AGB Stars: Their Importance as Actors and Probes, Kerschbaum F., Charbonnel C., Wing R. F., eds., p. 86

    2007

  50. [58]

    W., 2012, , 144, 4

    McConnachie A. W., 2012, , 144, 4

    2012

  51. [59]

    McDonald I. et al. , 2011 a , , 730, 71

    2011

  52. [60]

    McDonald I. et al. , 2011 b , , 193, 23

    2011

  53. [61]

    McDonald I. et al. , 2009, , 394, 831

    2009

  54. [62]

    McDonald I. et al. , 2011 c , , 417, 20

    2011

  55. [63]

    McDonald I. et al. , 2012, , 427, 2647

    2012

  56. [64]

    McQuinn K. B. W. et al. , 2017, , 834

    2017

  57. [65]

    McQuinn K. B. W. et al. , 2013, , 146, 145

    2013

  58. [66]

    McQuinn K. B. W. et al. , 2015 a , , 812, 158

    2015

  59. [67]

    McQuinn K. B. W. et al. , 2015 b , , 815, L17

    2015

  60. [68]

    Menzies J. et al. , 2008, , 385, 1045

    2008

  61. [69]

    Menzies J. W. et al. , 2011, , 414, 3492

    2011

  62. [70]

    W., Whitelock P

    Menzies J. W., Whitelock P. A., Feast M. W., 2015, , 452, 910

    2015

  63. [71]

    Menzies J. W. et al. , 2010, , 406, 86

    2010

  64. [72]

    Nanni A. et al. , 2013, , 434, 2390

    2013

  65. [73]

    Nanni A. et al. , 2014, , 438, 2328

    2014

  66. [74]

    Nanni A. et al. , 2018, , 473, 5492

    2018

  67. [75]

    Nanni A. et al. , 2016, , 462, 1215

    2016

  68. [76]

    Origlia L. et al. , 2002, , 571, 458

    2002

  69. [77]

    S., 1992, , 261, 567

    Ossenkopf V., Henning T., Mathis J. S., 1992, , 261, 567

    1992

  70. [78]

    Rafelski M. et al. , 2012, , 755, 89

    2012

  71. [79]

    Rhode K. L. et al. , 2013, , 145, 149

    2013

  72. [80]

    Robson I. et al. , 2004, , 351, L29

    2004

  73. [81]

    Saviane I. et al. , 2002, , 390, 59

    2002

  74. [82]

    F., Finkbeiner D

    Schlafly E. F., Finkbeiner D. P., 2011, , 737, 103

    2011

  75. [83]

    D., Kennicutt, Jr

    Skillman E. D., Kennicutt, Jr. R. C., 1993, , 411, 655

    1993

  76. [84]

    Skillman E. D. et al. , 2013, , 146

    2013

  77. [85]

    Sloan G. C. et al. , 2016, , 826, 44

    2016

  78. [86]

    Sloan G. C. et al. , 2008, , 686, 1056

    2008

  79. [87]

    Sloan G. C. et al. , 2010, , 719, 1274

    2010

  80. [88]

    Sloan G. C. et al. , 2012, , 752, 140

    2012

  81. [89]

    Sloan G. C. et al. , 2009, Science, 323, 353

    2009

  82. [90]

    Smith V. V. et al. , 2000, , 119, 1239

    2000

  83. [91]

    B., 1987, , 99, 191

    Stetson P. B., 1987, , 99, 191

    1987

  84. [92]

    Temim T. et al. , 2015, , 799, 158

    2015

  85. [93]

    T., 2006, in ASP Conference Series, Vol

    van Loon J. T., 2006, in ASP Conference Series, Vol. 353, Stellar Evolution at Low Metallicity: Mass Loss, Explosions, Cosmology, Lamers H. J. G. L. M., Langer N., Nugis T., Annuk K., eds., p. 211

    2006

  86. [94]

    van Loon J. T. et al. , 2008, A&A , 487, 1055

    2008

  87. [95]

    Ventura P., D'Antona F., Mazzitelli I., 2002, A & A, 393, 215

    2002

  88. [96]

    Volk K., Xiong G.-Z., Kwok S., 2000, , 530, 408

    2000

  89. [97]

    A., 1986, , 219, 525

    Whitelock P. A., 1986, , 219, 525

    1986

  90. [98]

    A., 2012, , 341, 123

    Whitelock P. A., 2012, , 341, 123

    2012

  91. [99]

    Whitelock P. A. et al. , 2018, , 473, 173

    2018

  92. [100]

    Whitelock P. A. et al. , 2009, , 394, 795

    2009

  93. [101]

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

    ENTRY address author booktitle chapter edition editor howpublished institution 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 a...

  94. [102]

    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 gl...

Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.