Pith. sign in

REVIEW 3 major objections 4 minor 52 references

Heavy-metal enrichment in the intermediate He-sdOB pulsator Feige 46

T0 review · 3 major / 4 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 Pulsating hot subdwarf Feige 46 carries more than 10,000 times solar strontium, yttrium, and zirconium.

desk verdict First abundance analysis of Feige 46: solidly places it among heavy-metal subdwarfs, though the exact Sr/Y/Zr enrichment carries a plausible ~1 dex unquantified LTE systematic. read the letter →

arxiv 1908.04587 v1 pith:7B4LGPNN submitted 2019-08-13 astro-ph.SR

Marilyn Latour , Matti Dorsch , Ulrich Heber This is my paper · ORCID
classification astro-ph.SR
keywords hotsubdwarfstarsFeige46heavy-metalsubdwarfsV366Aqrpulsatorsstellarabundancestrans-ironelementsspectroscopicanalysisdiffusionandradiativelevitation
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 tries to show that Feige 46, a star already known as the second member of the rare V366 Aqr pulsating class, shares the chemical peculiarity of the class prototype LS IV-14 116. Using archived optical and ultraviolet spectra, the authors derive abundances for 16 metals and find yttrium and zirconium enriched by more than 10,000 times the solar values in optical absorption lines, with strontium equally enriched in the ultraviolet. If correct, this makes Feige 46 only the second star with such extreme strontium–yttrium–zirconium overabundances, and it ties the heavy-metal phenomenon to the pulsating iHe-sdOB stars rather than to a random quirk of one object. The result matters because it gives a rare sample for studying how diffusion, radiative levitation, and possibly pulsations build up trans-iron elements in hot subdwarf atmospheres.

What carries the argument

The argument is carried by absorption-line abundance analysis: archived optical and ultraviolet spectra are matched with synthetic spectra computed from model atmospheres at an effective temperature of 36,100 K and a surface gravity of log g = 5.93. The key diagnostics are lines of the minority ions Zr iv (three optical lines plus two ultraviolet lines), Y iii (two optical lines), and Sr iv (ultraviolet lines, principally the 1331 Å line), because these are the species through which the trans-iron enrichment is seen. The synthesis includes a large set of new atomic levels and partition functions for elements heavier than zinc, and a rotational broadening of about 10 km/s is applied to reproduce the observed line shapes. A spectral-energy-distribution fit then anchors the stellar mass, radius, and luminosity that place Feige 46 in the hot-subdwarf context.

What would settle it

Compute full non-LTE synthetic spectra for the observed Y iii, Zr iv, and Sr iv lines in Feige 46 at 36,100 K; if the best-fit abundances move downward by about 1 dex or more for yttrium or zirconium, the claimed 10,000-fold enrichments would not hold at face value. A simpler check would be a new high-signal-to-noise optical spectrum of the Y iii 4040 Å doublet and additional Y iv or Zr v lines, whose measured strengths would either confirm or contradict the two-line yttrium fit.

Watch

Extended reading notes

Core claim

On the paper's own terms, the central discovery is that Feige 46 belongs to the 'heavy-metal' group of intermediate-helium hot subdwarfs and has an abundance pattern closely matching LS IV-14 116, the only other star of the V366 Aqr pulsating class. The measured photospheric abundances are about 20,000 times solar for zirconium, roughly 50,000 times solar for yttrium, and about 40,000 times solar for strontium, with gallium, germanium, and tin also enriched. The paper reads this as confirming that the similarity between the two pulsators extends from pulsational, atmospheric, and kinematic properties to chemical composition, and it notes that no other heavy-metal subdwarf shows this trio of elements at such high abundances. It also derives a mass of 0.54 solar masses, a radius of 0.132 solar radii, and a luminosity of about 27 solar luminosities from the spectral energy distribution, parallax, and gravity.

Load-bearing premise

The heavy-element abundances come from synthetic spectra that treat Sr, Y, Zr, and the other trans-iron elements under the assumption of local thermodynamic equilibrium in a 36,100 K atmosphere, and the yttrium value rests on only two lines in a low-quality spectral region; if that assumption shifts the fitted abundances by more than about a factor of ten, the specific 10,000-fold enrichment numbers would be overestimated, while the broader heavy-metal classification would probably survive.

Editorial extensions

If this is right

  • Feige 46 becomes the second object, after LS IV-14 116, in which Sr, Y, and Zr are all enriched by roughly 4 to 4.5 dex, making the coincidence specific to the V366 Aqr pulsating class.
  • The two pulsators also agree in the lighter elements C, N, O, Mg, and Si, so the chemical similarity is broader than just the heavy trio.
  • At an effective temperature near 36,000 K, the paper suggests that atmospheric conditions may be optimal for radiative levitation to support Sr, Y, and Zr; if true, other stars in this temperature range should be checked for the same pattern.
  • No other heavy-metal subdwarf studied so far reaches the Sr/Y/Zr levels seen in the two pulsators, so Feige 46 helps define a distinct subgroup of heavy-metal iHe-sdOB stars.

Reading between the lines

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

  • If the LTE treatment of heavy elements overestimates the fitted abundances, the quantitative 10,000-fold enrichments could shrink by a factor of ten or more; the qualitative conclusion that Feige 46 and LS IV-14 116 share a heavy-metal pattern would likely survive because both are analyzed with the same assumptions.
  • A decisive next step the paper does not take would be to compute NLTE model atoms for Y iii, Zr iv, and Sr iv; a comparison of those fits against the LTE fits would settle the size of the systematic error.
  • The paper leaves open whether pulsations cause, sustain, or merely coexist with the heavy-metal abundance; the similarity of the two pulsators makes it plausible that the high opacity of trans-iron elements participates in the pulsation-driving mechanism, which could be tested with time-resolved spectroscopy.
  • Under the paper's diffusion picture, Feige 46's enrichment pattern offers a boundary condition for radiative-levitation models: any successful model must reproduce roughly 4 to 4.5 dex overabundances of Sr, Y, and Zr at 36,000 K while leaving iron near solar and lead below about 700 times solar.
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 an abundance analysis of the hot subdwarf Feige 46 using archival CASPEC optical, GHRS UV, and IUE UV spectroscopy, modeled with TLUSTY/SYNSPEC NLTE model atmospheres. The authors derive abundances for 16 metallic elements and upper limits for 4 more, finding that Sr, Y, and Zr are enriched by more than 10,000 times solar, making Feige 46 a heavy-metal iHe-sdOB with an abundance pattern strikingly similar to the pulsating prototype LS IV−14°116. They also fit the spectral energy distribution and parallax to obtain radius, mass, and luminosity, and they discuss the possible role of rotation versus pulsation in the additional line broadening. The central claim is the quantitative similarity of the heavy-element enrichment pattern between Feige 46 and LS IV−14°116.

Significance. If the abundance result holds, Feige 46 becomes the second known member of the V366 Aqr pulsating class with extreme Sr/Y/Zr overabundances, substantially strengthening the empirical connection between this pulsation class and heavy-metal enrichment. The paper is careful in several respects: it uses standard NLTE model atmospheres, cross-checks the adopted atmospheric parameters with the independent TMAP code, compares optical and UV Zr lines as a consistency check, and provides explicit line-by-line fits and uncertainties. The SED fit gives physically consistent stellar parameters and independently validates the adopted Teff and log g. The main weakness is that the key heavy-element abundances are derived with LTE spectral synthesis for minority ionization stages, and the formal uncertainties do not include systematic NLTE or atomic-data errors; this makes the quantitative 10,000× solar figure somewhat fragile, though the qualitative classification as a heavy-metal subdwarf is robust.

major comments (3)
  1. [Sect. 2 / Appendix A / Sects. 3.1–3.2] The central quantitative claims—Sr, Y, and Zr overabundances of roughly 4.3–4.7 dex—rest on LTE spectral synthesis of the minority ions Sr iv, Y iii, and Zr iv, whereas at Teff = 36,100 K these are not the dominant ionization stages. The paper states in Sect. 2 that all elements heavier than zinc are treated in LTE, and Appendix A shows that only a Boltzmann partition function is used for these ions. No NLTE test is presented for Sr, Y, or Zr. A systematic offset of even 0.5–1 dex would not change the qualitative membership in the heavy-metal group, but it would change the quantitative 'more than 10,000× solar' figure in the abstract and the strength of the similarity claim to LS IV−14°116. I ask the authors to either perform a limited NLTE calculation for at least one line of each of these elements, or explicitly quantify this systematic uncertainty and carry it into Table 1 and the abstract.
  2. [Sect. 3.1 / Sect. 3.2] The Y abundance is based entirely on two Y iii lines (λλ4039.602, 4040.112) in a low-S/N region of the CASPEC spectrum, and the authors themselves note that these are the only yttrium features identified in hot subdwarfs. The Sr abundance is estimated by eye from blended GHRS lines with a 0.4 dex uncertainty. Under these conditions, unrecognized blends, continuum-placement errors, and gf-value uncertainties are likely to dominate over the quoted line-to-line scatter. I recommend that the authors (i) test the sensitivity of the Y abundance to plausible changes in the neighboring C/N/O line opacities and continuum normalization, and (ii) state in the abstract and conclusion that the Y and Sr abundances carry an additional systematic uncertainty of several tenths of a dex beyond the formal values.
  3. [Table A.1 / Sect. 2] For the trans-iron elements, the line list is assembled from the Kurucz database and literature sources, but no quantitative estimate of the gf-value accuracy is provided. The formal uncertainties in Table 1 (e.g., 0.10 dex for Zr) are internal line-to-line scatters, not total error budgets. Because the paper's main conclusion is a quantitative comparison of the abundance pattern of Feige 46 to LS IV−14°116, the authors should include a short discussion of the accuracy of the oscillator strengths for the critical ions (Zr iv, Sr iv, Y iii) and, where possible, check abundances against independent gf sources or different ionization stages. Without this, the claimed agreement with LS IV−14°116 is stronger than the atomic data warrant.
minor comments (4)
  1. [Sect. 2] The name of the Tübingen NLTE Model-Atmosphere Package is misspelled as 'Tübigen' in the text; it should be 'Tübingen'.
  2. [Table C.1] The Gaia GRP magnitude is listed as '13,5488' with a comma; it should be '13.5488'.
  3. [References] Dorsch, Latour & Heber 2019 is cited as 'submitted' in several places (Sections 3.1, 3.2, and 5); since the manuscript is dated 2021, the citation should be updated to the published or arXiv version and the 'submitted' qualifier removed.
  4. [Fig. C.1] The caption notes that broad-line mismatches are due to normalization deficiencies; since the Y iii lines at 4039–4040 Å lie in a region where such deficiencies are visible in Fig. C.1, a brief statement on how continuum placement affects the Y abundance would help the reader judge the robustness of that measurement.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the heavy-element abundances are measured by fitting synthetic spectra to observed optical and UV lines, with atmospheric parameters independently cross-checked, and the similarity to LS IV-14 116 is a post-measurement comparison rather than an input.

full rationale

The paper's central claim is an abundance measurement, not a prediction. Sr, Y, and Zr abundances are obtained by fitting observed absorption lines in the CASPEC optical spectrum and GHRS UV spectra using TLUSTY/SYNSPEC model atmospheres and synthetic spectra. The adopted atmospheric parameters (Teff = 36,100 K, log g = 5.93) come from Latour et al. (2019), but the authors explicitly re-derive them with TMAP H/He-only models, obtaining Teff = 36,200 ± 1,500 K, log g = 6.1 ± 0.3 and a helium abundance in excellent agreement with the earlier value. Thus the atmospheric parameters are not imported as an unverified self-citation. Initial abundances from Bauer & Husfeld (1995) and Naslim et al. (2011) are used only as starting guesses for the iterative spectral synthesis; the final abundances are determined by the line fits themselves, so the target result is not an input. The LTE approximation for trans-iron elements is an acknowledged modeling limitation (Sect. 2) that affects the accuracy and possible systematic offset of the abundance scale, but it is not a circular step: the abundances are not defined in terms of the conclusion, and no fitted parameter is renamed as a prediction. The claimed similarity to LS IV-14 116 is drawn after the abundances are measured, by comparing Figs. 5 and Table 1, rather than being imposed as a constraint. Self-citations (Dorsch et al. 2019 for method and atomic data; Latour et al. 2019 for parameters) are methodological or independently checked, and none is load-bearing in the sense of forcing the conclusion. No derivation chain in the paper reduces to its own inputs by construction.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

The central claim is an observational abundance measurement; it rests on standard stellar atmosphere modeling. The free parameters are the fitted/assumed model inputs (broadening, atmospheric parameters). No new physical entities are introduced.

free parameters (4)
  • Projected rotational velocity v sin i = 10 km/s
    Fitted to reproduce line shapes in the GHRS UV spectra (Sect. 3); adopted in the synthetic spectra for all abundance determinations. It affects line depth and hence the fitted abundances.
  • Microturbulent velocity vt = 2 km/s
    Assumed, following the method in Dorsch et al. (2019); not fitted. The paper tests vt = 5 km/s and finds it cannot reproduce the UV lines, so vt = 2 km/s is retained.
  • Adopted effective temperature Teff = 36,100 K
    Taken from Latour et al. (2019), re-derived consistently with a TMAP fit (36,200 +/- 1,500 K). Temperature shifts would alter derived abundances.
  • Adopted surface gravity log g = 5.93
    Taken from Latour et al. (2019); cross-checked with TMAP (6.1 +/- 0.3). Affects the atmospheric structure and abundance results.
assumptions (5)
  • domain assumption LTE approximation for heavy elements (Sr, Y, Zr, Ga, Ge, Sn, Pb) in the spectral synthesis
    Sect. 2 states that only H, He, C, N, O, Mg, Si, Fe, Ni are treated in NLTE; all other elements use LTE. At Teff = 36,100 K, NLTE effects can be significant for minority species, which may bias the derived abundances. The paper does not test this for the key elements.
  • domain assumption Reliability of atomic data (oscillator strengths, energy levels) for trans-iron ions
    The analysis relies on the Kurucz line list supplemented with literature data. The paper notes missing or discrepant lines (e.g., Ga iii 1507.96, Sn iii 1251.4) indicating that atomic data for these elements are incomplete. For Y, only two Y iii lines are available, with no independent gf values.
  • domain assumption Adopted atmospheric parameters from Latour et al. (2019) are accurate
    The final model atmospheres use Teff and log g from Latour et al. (2019); an independent TMAP fit gives consistent values but with larger uncertainties. If the true parameters differ substantially, the derived abundances would shift.
  • domain assumption Continuum normalization deficiencies in the CASPEC spectrum do not bias the sharp metal line measurements
    The authors state in Fig. C.1 caption that mismatches of broad lines are due to normalization shortcomings but do not compromise sharp metal lines. This is asserted, not quantitatively tested.
  • standard math Boltzmann partition functions without level dissolution are adequate for the added heavy ions
    Appendix A computes partition functions with the Boltzmann equation, ignoring level dissolution and electron shielding. This is a standard approximation but may be inaccurate for highly excited states.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Heavy-metal enrichment in the intermediate He-sdOB pulsator Feige 46." pith.science (2026). https://pith.science/paper/7B4LGPNN

@misc{pith2026190804587,
  author       = {Pith},
  title        = {Pith review of: Heavy-metal enrichment in the intermediate He-sdOB pulsator Feige 46},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/7B4LGPNN}},
  note         = {Machine review of arXiv:1908.04587}
}
abstract

The intermediate He-enriched hot subdwarf star Feige 46 was recently reported as the second member of the V366 Aqr (or He-sdOBV) pulsating class. Feige 46 is very similar to the prototype of the class, LS IV$-$14116, not only in terms of pulsational properties, but also in terms of atmospheric parameters and kinematic properties. LS IV$-$14116 is additionally characterized by a very peculiar chemical composition, with extreme overabundances of the trans-iron elements Ge, Sr, Y, and Zr. In this paper, we investigate the possibility that the similitude between both pulsators extends to their chemical composition. We retrieved archived optical and UV spectroscopic observations of Feige 46 and perform an abundance analysis using model atmospheres and synthetic spectra computed with TLUSTY and SYNSPEC. In total, we derive abundances for 16 metallic elements and provide upper limits for four additional elements. From absorption lines in the optical spectrum of the star we measure an enrichment of more than 10 000$\times$ solar for yttrium and zirconium. As for strontium, the UV spectrum revealed it to be equally enriched. Our results confirm that Feige 46 is not only a member of the now growing group of "heavy-metal" subdwarfs, but also has an abundance pattern remarkably similar to that of LS IV$-$14116.

Figures

Figures reproduced from arXiv: 1908.04587 by the authors.

Figure 1
Figure 1. Best fit of the three Zr iv lines seen in the CASPEC spectrum with a resulting abundance of log Zr/H = −5.0. A synthetic spectrum com￾puted without the contribution of Zr is shown as comparison in red. shorter notation "log X/H" to refer to the abundance by num￾ber with respect to hydrogen "log N(X)/N(H)". Our final abun￾dances are presented in [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Some of the strongest Sr iv lines in the GHRS spectra compared with synthetic spectra including [Sr/H] = −4.0 (green), −4.4 (blue), −4.8 (red) and without the contribution of Sr (dashed red). 1228.0 1232.0 0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 GaIV ZnIV ZnIV GeIV CII CII CIV SrIV ZnIV CIII 1250.0 1252.0 1254.0 SII SII NiV ZnIV PbIII ZnIV SnIII MnIV NiIV ZnIII ZnIV FeIV 1312.0 1316.0 NiIV PbIV PbIV PbIV PbIV PbIV SnIV GaIV… view at source ↗
Figure 3
Figure 3. Comparison between the IUE and synthetic spectra in the ranges where Ge, Sn and Pb lines are seen. The model spectra shown in blue includes the estimated abundances of Ge and Sn (from [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figures from the paper (3 more)
Figure 4
Figure 4. Figure 4: Comparison of the synthetic spectrum (gray line) of Feige 46 with photometric data. The three black data points labeled “box” are binned fluxes from a low-dispersion IUE spectrum. Filter-averaged fluxes are shown as colored data points that were converted from observed…
Figure 5
Figure 5. Figure 5: Comparison between the abundance pattern of Feige 46, LS IV−14◦116 (Naslim et al. 2011) and HZ 44 (Dorsch et al. 2019). Light elements (23 ≤ Z) are marked by green symbols, iron-peak elements (24 ≤ Z ≤ 30) in purple, and heavier elements (Z ≥ 31) in red. The stellar ma…
Figure 6
Figure 6. Figure 6: Comparison between the observed spec￾tra and synthetic spectra having vt = 2 km s−1 , v sin i = 12 km s−1 (red) and vt = 5 km s−1 , v sin i = 0 km s−1 (blue). et al. (2015) showed that the atmospheric motion due to pulsa￾tions in LS IV−14◦116 produces radial velocity v…

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

52 extracted references · 43 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]

    Battich , T., Bertolami , M. M. M., C \'o rsico , A. H., & Althaus , L. G. 2018, , 614, A136

    work page 2018

  4. [4]

    & Husfeld , D

    Bauer , F. & Husfeld , D. 1995, , 300, 481

    work page 1995

  5. [5]

    2008, , 678, 1329

    Blanchette , J.-P., Chayer , P., Wesemael , F., et al. 2008, , 678, 1329

    work page 2008

  6. [6]

    M., Sweigart , A

    Brown , T. M., Sweigart , A. V., Lanz , T., Landsman , W. B., & Hubeny , I. 2001, , 562, 368

    work page 2001

  7. [7]

    C., Magnier , E

    Chambers , K. C., Magnier , E. A., Metcalfe , N., et al. 2016, arXiv e-prints, arXiv:1612.05560

    arXiv 2016

  8. [8]

    2006, Baltic Astronomy, 15, 131

    Chayer , P., Fontaine , M., Fontaine , G., Wesemael , F., & Dupuis , J. 2006, Baltic Astronomy, 15, 131

    work page 2006

Show all 52 references
  1. [9]

    T., & O'Connell , R

    Dorman , B., Rood , R. T., & O'Connell , R. W. 1993, , 419, 596

    1993

  2. [10]

    2019, arXiv e-prints, arXiv:1907.07781

    Dorsch , M., Latour , M., & Heber , U. 2019, arXiv e-prints, arXiv:1907.07781

    2019 arXiv

  3. [11]

    Drilling , J. S. & Heber , U. 1987, in IAU Colloq. 95: Second Conference on Faint Blue Stars, ed. A. G. D. Philip , D. S. Hayes , & J. W. Liebert , 603--606

    1987

  4. [12]

    Fitzpatrick , E. L. 1999, , 111, 63

    1999

  5. [13]

    2018, VizieR Online Data Catalog, 1345

    Gaia Collaboration . 2018, VizieR Online Data Catalog, 1345

    2018

  6. [14]

    H., Nemeth , P., et al

    Geier , S., stensen , R. H., Nemeth , P., et al. 2017, Open Astronomy, 26, 164

    2017

  7. [15]

    Graham , J. A. 1970, , 82, 1305

    1970

  8. [16]

    2016, , 128, 082001

    Heber , U. 2016, , 128, 082001

    2016

  9. [17]

    2018, Open Astronomy, 27, 35

    Heber , U., Irrgang , A., & Schaffenroth , J. 2018, Open Astronomy, 27, 35

    2018

  10. [18]

    Hirsch , H. A. 2009, PhD thesis, Friedrich-Alexander University Erlangen-N \"u rnberg

    2009

  11. [19]

    A., Glebbeek , E., & Dupret , M.-A

    Hu , H., Tout , C. A., Glebbeek , E., & Dupret , M.-A. 2011, , 418, 195

    2011

  12. [20]

    1988, Computer Physics Communications, 52, 103

    Hubeny, I. 1988, Computer Physics Communications, 52, 103

    1988

  13. [21]

    & Lanz , T

    Hubeny , I. & Lanz , T. 2011, TLUSTY: Stellar Atmospheres, Accretion Disks, and Spectroscopic Diagnostics , Astrophysics Source Code Library

    2011

  14. [22]

    S., Ahmad , A., Naslim , N., & Kerzendorf , W

    Jeffery , C. S., Ahmad , A., Naslim , N., & Kerzendorf , W. 2015, , 446, 1889

    2015

  15. [23]

    S., Baran , A

    Jeffery , C. S., Baran , A. S., Behara , N. T., et al. 2017, , 465, 3101

    2017

  16. [24]

    2005, , 442, 1015

    Kuassivi , Bonanno , A., & Ferlet , R. 2005, , 442, 1015

    2005

  17. [25]

    & Hubeny , I

    Lanz , T. & Hubeny , I. 2003, , 146, 417

    2003

  18. [26]

    2013, , 773, 84

    Latour , M., Fontaine , G., Chayer , P., & Brassard , P. 2013, , 773, 84

    2013

  19. [27]

    M., & Fontaine , G

    Latour , M., Green , E. M., & Fontaine , G. 2019, , 623, L12

    2019

  20. [28]

    2016, , 585, A115

    Latour , M., Heber , U., Irrgang , A., et al. 2016, , 585, A115

    2016

  21. [29]

    J., Almaini , O., et al

    Lawrence , A., Warren , S. J., Almaini , O., et al. 2013, VizieR Online Data Catalog, 2319

    2013

  22. [30]

    Mermilliod , J. C. 2006, VizieR Online Data Catalog, 2168

    2006

  23. [31]

    2011, , 529, A60

    Michaud , G., Richer , J., & Richard , O. 2011, , 529, A60

    2011

  24. [32]

    M., C \'o rsico , A

    Miller Bertolami , M. M., C \'o rsico , A. H., & Althaus , L. G. 2011, , 741, L3

    2011

  25. [33]

    Morton , D. C. 2000, , 130, 403

    2000

  26. [34]

    Morton , D. C. 2003, , 149, 205

    2003

  27. [35]

    S., Behara , N

    Naslim , N., Jeffery , C. S., Behara , N. T., & Hibbert , A. 2011, , 412, 363

    2011

  28. [36]

    S., Hibbert , A., & Behara , N

    Naslim , N., Jeffery , C. S., Hibbert , A., & Behara , N. T. 2013, , 434, 1920

    2013

  29. [37]

    O'Toole , S. J. 2004, , 423, L25

    2004

  30. [38]

    O'Toole , S. J. & Heber , U. 2006, , 452, 579

    2006

  31. [39]

    K., Bagnulo , S., Ziegerer , E., Geier , S., & Fontaine , G

    Randall , S. K., Bagnulo , S., Ziegerer , E., Geier , S., & Fontaine , G. 2015, , 576, A65

    2015

  32. [40]

    2015, Tuebingen Oscillator Strengths Service Form Interface, VO resource provided by the GAVO Data Center

    Rauch, T., Quinet, P., Hoyer, D., et al. 2015, Tuebingen Oscillator Strengths Service Form Interface, VO resource provided by the GAVO Data Center

    2015

  33. [41]

    R., Winn , J

    Ricker , G. R., Winn , J. N., Vanderspek , R., et al. 2014, in , Vol. 9143, Space Telescopes and Instrumentation 2014: Optical, Infrared, and Millimeter Wave, 914320

    2014

  34. [42]

    & Jeffery , C

    Saio , H. & Jeffery , C. S. 2019, , 482, 758

    2019

  35. [43]

    2007, , 462, 269

    Stroeer , A., Heber , U., Lisker , T., et al. 2007, , 462, 269

    2007

  36. [44]

    & Reader , J

    Tauheed , A. & Reader , J. 2005, , 72, 158

    2005

  37. [45]

    H., Geier , S., stensen , R

    Telting , J. H., Geier , S., stensen , R. H., et al. 2008, , 492, 815

    2008

  38. [46]

    2008, , 486, 923

    Unglaub , K. 2008, , 486, 923

    2008

  39. [47]

    K., Latour , M., et al

    Van Grootel , V., Randall , S. K., Latour , M., et al. 2019, arXiv e-prints [ [arXiv] 1905.00654 ]

    2019 arXiv

  40. [48]

    van Hoof , P. A. M. 2018, Galaxies, 6, 63

    2018

  41. [49]

    2000, Astrophysics and Space Science, 273, 155

    Wamsteker, W., Skillen, I., Ponz, J., et al. 2000, Astrophysics and Space Science, 273, 155

    2000

  42. [50]

    2012, TMAP: T \"u bingen NLTE Model-Atmosphere Package , Astrophysics Source Code Library

    Werner , K., Dreizler , S., & Rauch , T. 2012, TMAP: T \"u bingen NLTE Model-Atmosphere Package , Astrophysics Source Code Library

    2012

  43. [51]

    T., Mason , P

    Williams , T., McGraw , J. T., Mason , P. A., & Grashuis , R. 2001, , 113, 944

    2001

  44. [52]

    & Jeffery, C

    Zhang, X. & Jeffery, C. S. 2012, , 419, 452

    2012

Pith tools

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