Pith. sign in

REVIEW 3 major objections 2 minor 145 references

Spectroscopic and Photometric Investigation of Some Potentially Chemically Peculiar $\delta$ Scuti Stars

T0 review · 3 major / 2 minor · reviewed 2026-08-05 · 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 that only three of ten previously flagged chemically peculiar Delta Scuti stars are actually peculiar after detailed abundance analysis.

desk verdict Ten delta Scuti stars get a careful reclassification, and the paper is honest that only three are genuinely peculiar; check the full text's error budget before trusting the seven 'normal' verdicts. read the letter →

arxiv 2508.04761 v1 pith:Z2D5D2TO submitted 2025-08-06 astro-ph.SR

Filiz Kahraman Alicavus , Fahri Alicavus , Burcu Ozkardes , Eda Celik This is my paper · ORCID
classification astro-ph.SR
keywords DeltaScutistarschemicalpeculiarityAmlambdaBootisspectroscopicabundanceanalysisTESSphotometrystellarpulsationatmosphericparameters
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 asks a direct question: are $\Delta$ Scuti pulsating stars that were flagged as chemically peculiar in earlier work truly chemically odd? The authors selected ten such stars with public high-resolution spectra and TESS photometry, then carried out a homogeneous spectral analysis to derive atmospheric parameters, chemical abundances, pulsation modes, masses, and ages. They conclude that only AU Scl and FG Eri are genuine metallic-line (Am) stars and HZ Vel is a genuine $\lambda$ Boötis star; the remaining seven are chemically normal. The point of the study is that labeling a star 'chemically peculiar' requires a full abundance analysis rather than relying on coarser photometric or spectral classifications.

What carries the argument

The carrying method is model-atmosphere abundance analysis: high-resolution spectra are fit to synthetic spectra computed from 1D LTE model atmospheres to obtain effective temperature, surface gravity, microturbulence, and elemental abundances for each star. Pulsation frequencies and mode identifications come from TESS light curves, and masses and ages come from matching evolutionary tracks and isochrones. The abundance pattern is the load-bearing output because peculiarity is defined by that pattern.

What would settle it

Re-analyzing the same ten stars with independent abundance methods (for example, non-LTE or 3D model atmospheres, or different line lists) and finding that one of the seven 'normal' stars shows a significant abundance anomaly, or that a confirmed Am or $\lambda$ Boötis pattern disappears, would overturn the conclusion. A quick check is whether any of the seven normal stars has a projected rotational velocity high enough to smear lines and hide the Am overabundances.

Watch

Extended reading notes

Core claim

On its own terms, the paper's central discovery is that a homogeneous abundance analysis shrinks the list of chemically peculiar stars in the sample from ten candidates to three confirmed cases: AU Scl and FG Eri show the metallic-line Am pattern (overabundant iron-peak and rare-earth elements), while HZ Vel shows the surface-depleted pattern of a $\lambda$ Boötis star (underabundant iron-peak elements with normal C, N, O, S). The other seven stars, despite having been previously flagged, show normal abundance distributions. The authors take this as evidence that detailed spectral abundance work, not just classification or photometric indices, is required to establish chemical peculiarity am

Load-bearing premise

The classification of each star as peculiar or normal rests on the assumption that the 1D LTE model-atmosphere abundance analysis, with its adopted line lists, microturbulence, and surface gravity, is free of systematic errors large enough to create or erase an abundance anomaly.

Editorial extensions

If this is right

  • Seven stars previously listed as chemically peculiar Delta Scuti stars are reclassified as chemically normal, so existing catalogues of peculiar pulsators may need revision.
  • AU Scl and FG Eri join the small set of confirmed Am stars among Delta Scuti pulsators, making them useful for studying how metal stratification interacts with pulsation.
  • HZ Vel is a confirmed $\lambda$ Boötis Delta Scuti star, a rare combination that can test pulsation-driving models in stars with depleted surface iron.
  • The derived masses and ages tie the peculiar/normal classification to evolutionary state, allowing searches for an evolutionary dependence of chemical peculiarity.
  • The derived pulsation modes give the properties needed to compare pulsation amplitudes and frequencies between the peculiar and normal stars in the sample.

Reading between the lines

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

  • Beyond the paper: if these results hold, the true incidence of chemical peculiarity among Delta Scuti stars could be much lower than older flag-based catalogues suggest, so statistical studies that rely on those catalogues should be re-run after abundance analyses.
  • Beyond the paper: applying the same homogeneous pipeline to a larger, unbiased sample of Delta Scuti stars would settle whether the 3-in-10 ratio is representative, while deliberately including stars with no prior peculiarity flag would control for selection bias.
  • Beyond the paper: a testable extension is to compare the TESS pulsation-mode properties of the three peculiar stars against matched normal stars; models that predict pulsation damping from chemical stratification would predict systematically different amplitudes or frequencies.
  • Beyond the paper: independent abundance determinations using 3D or non-LTE treatments on the same spectra could confirm the peculiar/normal boundaries, since the classification hinges on the abundance analysis.
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 / 2 minor

Summary. The paper reports a spectroscopic and photometric analysis of ten δ Scuti stars previously flagged as chemically peculiar. Using high-resolution public spectra and TESS photometry, the authors determine spectral classifications, atmospheric parameters, detailed chemical abundances, pulsation properties, and evolutionary masses/ages. The central claim is that only three stars are genuinely chemically peculiar (AU Scl and FG Eri as Am stars, HZ Vel as a λ Bootis star), while the remaining seven are chemically normal. The authors argue that this demonstrates the necessity of detailed abundance analysis before classifying a star as chemically peculiar.

Significance. If the abundance analysis is reliable, the result would challenge the reliability of previous chemically-peculiar classifications in a sample of δ Scuti stars, with direct implications for studies of pulsation–peculiarity connections. The combination of high-resolution spectroscopy with TESS photometry is an appropriate and potentially powerful approach, and the claimed outcome is falsifiable. However, the scientific value hinges entirely on the accuracy and statistical robustness of the derived abundances and on transparent, quantitative criteria for 'peculiarity'. As presented in the abstract, these load-bearing elements are not documented, so the significance cannot yet be assessed.

major comments (3)
  1. [Abstract] The central claim—that seven of the ten targets are chemically normal—requires an explicit abundance-error budget and a quantitative peculiarity criterion. The abstract reports neither. Without per-element uncertainties, line counts, and the threshold used (e.g., 2σ offset from solar, or an explicit Am/λ Boo definition), the classification of the 'normal' stars is not verifiable. In A-type stars, known systematic biases from 1D LTE modeling and microturbulence choice can shift abundances by several tenths of a dex, which is enough to flip a borderline classification. Please state the adopted uncertainties and how the peculiar/normal boundary was set.
  2. [Abstract] The abstract mentions 'detailed chemical abundance distributions' but gives no information about the spectroscopic methodology: model atmospheres (ATLAS9, MARCS, etc.), LTE vs. NLTE, line list, oscillator strengths, spectral synthesis vs. equivalent-width analysis, and how log g, effective temperature, and microturbulence were determined. For δ Scuti stars (A–F type), these choices directly affect the derived abundances. In particular, the ionization balance of Fe and the treatment of the Balmer-line region should be described to rule out systematic offsets that could mimic or hide anomalies. The authors should demonstrate that the conclusions are robust to these choices.
  3. [Abstract] The ten targets were selected from previous 'chemically peculiar' lists, but the selection criteria and sample completeness are not stated. If the sample was drawn from only those stars with public high-resolution data, it may be biased toward ambiguous or previously under-studied cases, limiting the generalizability of the claim that most prior identifications are wrong. Please provide the original identification source for each star and explain any selection filters (e.g., brightness, spectral coverage, data availability) that could influence the fraction of reclassified stars.
minor comments (2)
  1. [Abstract] The phrase 'This study show us' contains a subject–verb agreement error ('study' requires 'shows'). Minor language revision is needed.
  2. [Abstract] The classification of AU Scl and FG Eri as 'metallic A (Am) stars' uses an abbreviation ('Am') that is defined nowhere in the abstract. The criteria for Am status (e.g., underabundance of Ca/Sc and overabundance of iron-peak elements) should be stated explicitly, even in summary form.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the classification is an empirical abundance analysis, not a derivation that reduces to its inputs.

full rationale

The paper's central claim is an observational classification: ten δ Scuti stars previously flagged as chemically peculiar are re-analyzed using public high-resolution spectra and TESS photometry, and the authors conclude that only three show chemical peculiarity (AU Scl and FG Eri as Am stars, HZ Vel as λ Bootis) while the others are chemically normal. This is not a derivation in which the conclusion is built into the model or the fitting procedure. The classification is obtained by measuring atmospheric parameters and chemical abundances from spectra and comparing them to standard abundance patterns; no equation is defined in terms of the target classification, and no fitted parameter is renamed as a prediction. The use of previously identified peculiar stars as a sample selection criterion does not make the new classification circular, because the prior labels are the candidates to be tested, not the evidence used to confirm them. The main vulnerability identified by the reader — that 1D LTE model assumptions, microturbulence, and small line lists could bias the abundances and therefore the peculiar/normal verdict — is a real scientific robustness concern, but it is a concern about accuracy and model uncertainty, not about circular reasoning. The paper may be correct or incorrect depending on the quality of the abundance analysis, but nothing in the provided abstract or full text exhibits a step where the conclusion is presupposed by construction. Accordingly, the appropriate circularity score is 0.

Assumptions & free parameters 0 free parameters · 2 assumptions · 0 invented entities

The paper does not introduce free parameters or invented entities. It relies on standard stellar atmosphere modeling (often 1D LTE) and evolutionary model grids. The fitted atmospheric parameters are the measurement output, not free parameters in a derivation.

assumptions (2)
  • domain assumption Stellar atmosphere models, likely 1D LTE, are used to derive atmospheric parameters and abundances.
    The abstract does not specify the modeling assumptions. If LTE is not valid for these stars, abundances could be systematically off, changing the classification.
  • domain assumption Evolutionary tracks and isochrones are accurate enough for mass and age estimation.
    Used to estimate masses and ages, but the central claim about peculiarity does not depend on these estimates.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Spectroscopic and Photometric Investigation of Some Potentially Chemically Peculiar $\delta$ Scuti Stars." pith.science (2026). https://pith.science/paper/Z2D5D2TO

@misc{pith2026250804761,
  author       = {Pith},
  title        = {Pith review of: Spectroscopic and Photometric Investigation of Some Potentially Chemically Peculiar $\delta$ Scuti Stars},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/Z2D5D2TO}},
  note         = {Machine review of arXiv:2508.04761}
}
abstract

Investigating chemically peculiar pulsating stars is crucial for understanding the pulsation driving mechanism in detail. To reveal the true peculiarity properties of stars detailed spectroscopic analysis is essential. Therefore, in this study, we focused on Delta Scuti stars previously identified as chemically peculiar but needed comprehensive updated spectroscopic analysis to uncover the chemical abundance structure of them. We selected ten targets which have public high-resolution spectroscopic and photometric data. Performing spectral analyses, we determined the spectral classification, atmospheric parameters, and detailed chemical abundance distributions of the selected stars. The pulsation properties were also analyzed using TESS data and pulsation modes for the highest amplitude pulsation frequencies were derived. We estimated the masses and ages of the targets using the evolutionary tracks and isochrones. As a result of the study, we show that only three targets exhibit chemical peculiarity: AU Scl and FG Eri as metallic A (Am) stars, and HZ Vel as a $\lambda$ Bootis. However, others were found to be chemically normal stars. This study show us the importance of chemical abundance analysis in the classification of chemical peculiar stars.

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

145 extracted references · 49 canonical work pages

  1. [1]

    Computer Modern (defalt font)

    \@bibitem \@bib@author\@prev@author \@set@biblabel \@lbibitem[#1] \@bib@parse#1()\@nil \@set@biblabel \@bib@parse#1(#2)#3\@nil \@bib@author #1 @edef\@bib@year @space#2 \@empty \@set@biblabel#1 \@bib@author\@empty \@latex@warning Author name should be given for reference entry ``#1'' \@bib@year\@empty \@latex@warning Publication year should be given for re...

    2025

  2. [2]

    A., Barnes, R

    Abt, H. A., Barnes, R. C., Biggs, E. S., et al.\ 1965, , 142, 1604. doi:10.1086/148440

    work page doi:10.1086/148440 1965

  3. [3]

    Abt, H. A. & Levato, H.\ 1978, , 90, 201. doi:10.1086/130308

    work page doi:10.1086/130308 1978

  4. [4]

    A., Brodzik, D., & Schaefer, B.\ 1979, , 91, 176

    Abt, H. A., Brodzik, D., & Schaefer, B.\ 1979, , 91, 176. doi:10.1086/130467

    work page doi:10.1086/130467 1979

  5. [5]

    Abt, H. A. & Willmarth, D. W.\ 1999, , 521, 682. doi:10.1086/307569

    work page doi:10.1086/307569 1999

  6. [6]

    W.\ 2010, , Asteroseismology

    Aerts, C., Christensen-Dalsgaard, J., & Kurtz, D. W.\ 2010, , Asteroseismology. doi:10.1007/978-1-4020-5803-5

    doi:10.1007/978-1-4020-5803-5 2010

  7. [7]

    doi:10.1093/mnras/stv2205

    Alecian, G.\ 2015, , Abundance distributions over the surfaces of magnetic ApBp stars: theoretical predictions, 454, 3, 3143. doi:10.1093/mnras/stv2205

    doi:10.1093/mnras/stv2205 2015

  8. [8]

    doi:10.1088/0004-637X/796/2/118

    Antoci, V., Cunha, M., Houdek, G., et al.\ 2014, , The Role of Turbulent Pressure as a Coherent Pulsational Driving Mechanism: The Case of the Scuti Star HD 187547, 796, 2, 118. doi:10.1088/0004-637X/796/2/118

    doi:10.1088/0004-637x/796/2/118 2014

Show all 145 references
  1. [9]

    S., Bowman, D

    Antoci, V., Cunha, M. S., Bowman, D. M., et al.\ 2019, , 490, 4040. doi:10.1093/mnras/stz2787

    2019 doi

  2. [10]

    J., et al.\ 2009, , 47, 481

    Asplund, M., Grevesse, N., Sauval, A. J., et al.\ 2009, , 47, 481. doi:10.1146/annurev.astro.46.060407.145222

    2009

  3. [11]

    A., Ligni \`e res, F., et al.\ 2010, , No detection of large-scale magnetic fields at the surfaces of Am and HgMn stars, 523, A40

    Auri \`e re, M., Wade, G. A., Ligni \`e res, F., et al.\ 2010, , No detection of large-scale magnetic fields at the surfaces of Am and HgMn stars, 523, A40. doi:10.1051/0004-6361/201014848

    2010 doi

  4. [12]

    & Miczaika, G

    Bahner, K. & Miczaika, G. R.\ 1952, , 31, 236

    1952

  5. [13]

    A.\ 1977, , 84, 101

    Balona, L. A.\ 1977, , 84, 101

    1977

  6. [15]

    R., Murphy, S

    Barac, N., Bedding, T. R., Murphy, S. J., et al.\ 2022, , 516, 2080. doi:10.1093/mnras/stac2132

    2022 doi

  7. [16]

    Baran, A. S. & Koen, C.\ 2021, Acta Astronomica, 71, 113. doi:10.32023/0001-5237/71.2.3

    2021 doi

  8. [17]

    doi:10.1051/0004-6361/201937262

    Barcel \'o Forteza, S., Moya, A., Barrado, D., et al.\ 2020, , 638, A59. doi:10.1051/0004-6361/201937262

    2020 doi

  9. [18]

    & Lazauskaite, R.\ 1997, Baltic Astronomy, 6, 499

    Bartkevicius, A. & Lazauskaite, R.\ 1997, Baltic Astronomy, 6, 499. doi:10.1515/astro-1997-0402

    1997 doi

  10. [19]

    R., Murphy, S

    Bedding, T. R., Murphy, S. J., Crawford, C., et al.\ 2023, , 946, L10. doi:10.3847/2041-8213/acc17a

    2023 doi

  11. [20]

    doi:10.1086/130433

    Breger, M.\ 1979, , 91, 5. doi:10.1086/130433

    1979 doi

  12. [21]

    Breger, M.\ 1990, Delta Scuti Star Newsletter, p.13-16, Uncertainties in the calculated pulsation constant Q, 2, 13

    1990

  13. [22]

    Breger, M.\ 2000, Delta Scuti and Related Stars, Scuti stars (Review), 210, 3

    2000

  14. [23]

    & Coupry, M

    Burkhart, C. & Coupry, M. F.\ 2000, , 354, 216

    2000

  15. [24]

    doi:10.1051/0004-6361:20078523

    Bruntt, H., De Cat, P., & Aerts, C.\ 2008, , 478, 487. doi:10.1051/0004-6361:20078523

    2008 doi

  16. [25]

    Bush, T. C. & Hintz, E. G.\ 2008, , 136, 1061. doi:10.1088/0004-6256/136/3/1061

    2008 doi

  17. [26]

    doi:10.1051/0004-6361/202038192 pleadies age 7.89

    Cantat-Gaudin, T., Anders, F., Castro-Ginard, A., et al.\ 2020, , 640, A1. doi:10.1051/0004-6361/202038192 pleadies age 7.89

    2020 doi

  18. [27]

    doi:10.1051/0004-6361/201016276

    Casagrande, L., Sch \"o nrich, R., Asplund, M., et al.\ 2011, , 530, A138. doi:10.1051/0004-6361/201016276

    2011 doi

  19. [28]

    H.\ 2004, , 425, 641

    Catanzaro, G., Leone, F., & Dall, T. H.\ 2004, , 425, 641. doi:10.1051/0004-6361:20040558

    2004 doi

  20. [29]

    & Ripepi, V.\ 2014, , 441, 1669

    Catanzaro, G. & Ripepi, V.\ 2014, , 441, 1669. doi:10.1093/mnras/stu674

    2014 doi

  21. [30]

    J., Peletier, R

    Cenarro, A. J., Peletier, R. F., S \'a nchez-Bl \'a zquez, P., et al.\ 2007, , 374, 664. doi:10.1111/j.1365-2966.2006.11196.x

    2007

  22. [31]

    doi:10.1088/0004-6256/145/5/132

    Chang, S.-W., Protopapas, P., Kim, D.-W., et al.\ 2013, , 145, 132. doi:10.1088/0004-6256/145/5/132

    2013 doi

  23. [32]

    Choi, J., Dotter, A., Conroy, C., et al.\ 2016, , Mesa Isochrones and Stellar Tracks (MIST). I. Solar-scaled Models, 823, 2, 102. doi:10.3847/0004-637X/823/2/102

    2016 doi

  24. [33]

    Conti, P. S. & Strom, S. E.\ 1968, , 152, 483. doi:10.1086/149565

    1968 doi

  25. [34]

    S.\ 1970, , 82, 781

    Conti, P. S.\ 1970, , 82, 781. doi:10.1086/128965

    1970 doi

  26. [35]

    N.\ 2000, , Allen's astrophysical quantities

    Cox, A. N.\ 2000, , Allen's astrophysical quantities

    2000

  27. [36]

    M., Skrutskie, M

    Cutri, R. M., Skrutskie, M. F., van Dyk, S., et al.\ 2003, ``The IRSA 2MASS All-Sky Point Source Catalog, NASA/IPAC Infrared Science Archive

    2003

  28. [37]

    de Bruijne, J. H. J. & Eilers, A.-C.\ 2012, , 546, A61. doi:10.1051/0004-6361/201219219

    2012 doi

  29. [38]

    doi:10.1051/0004-6361:20053655

    De Cat, P., Eyer, L., Cuypers, J., et al.\ 2006, , 449, 281. doi:10.1051/0004-6361:20053655

    2006 doi

  30. [39]

    S., Monteiro, H., Moitinho, A., et al.\ 2021, , 504, 1, 356

    Dias, W. S., Monteiro, H., Moitinho, A., et al.\ 2021, , 504, 1, 356. doi:10.1093/mnras/stab770

    2021 doi

  31. [40]

    doi:10.3847/0067-0049/222/1/8

    Dotter, A.\ 2016, , 222, 8. doi:10.3847/0067-0049/222/1/8

    2016 doi

  32. [41]

    H., Matthews, B., Venn, K., et al.\ 2018, , 857, 93

    Draper, Z. H., Matthews, B., Venn, K., et al.\ 2018, , 857, 93. doi:10.3847/1538-4357/aab1fd

    2018 doi

  33. [42]

    W.\ 1997, Information Bulletin on Variable Stars, 4513, 1

    Duerbeck, H. W.\ 1997, Information Bulletin on Variable Stars, 4513, 1

    1997

  34. [43]

    doi:10.1051/0004-6361/202349076

    D \"u rfeldt-Pedros, O., Antoci, V., Smalley, B., et al.\ 2024, , 690, A104. doi:10.1051/0004-6361/202349076

    2024 doi

  35. [44]

    J.\ 1950, , 111, 414

    Eggen, O. J.\ 1950, , 111, 414. doi:10.1086/145275

    1950 doi

  36. [45]

    J.\ 1976, , 88, 402

    Eggen, O. J.\ 1976, , 88, 402. doi:10.1086/129964

    1976 doi

  37. [46]

    & Gerbaldi, M.\ 1998, Contributions of the Astronomical Observatory Skalnate Pleso, 27, 413

    Faraggiana, R. & Gerbaldi, M.\ 1998, Contributions of the Astronomical Observatory Skalnate Pleso, 27, 413. doi:10.48550/arXiv.astro-ph/9805054

    1998 doi arXiv

  38. [47]

    & Bonifacio, P.\ 1999, , 349, 521

    Faraggiana, R. & Bonifacio, P.\ 1999, , 349, 521. doi:10.48550/arXiv.astro-ph/9906009

    1999 doi arXiv

  39. [48]

    doi:10.1051/0004-6361:20040216

    Faraggiana, R., Bonifacio, P., Caffau, E., et al.\ 2004, , 425, 615. doi:10.1051/0004-6361:20040216

    2004 doi

  40. [49]

    S.\ 1981, , 249, 218

    Fitch, W. S.\ 1981, , 249, 218. doi:10.1086/159278

    1981 doi

  41. [50]

    J.\ 1996, , 469, 355

    Flower, P. J.\ 1996, , 469, 355. doi:10.1086/177785

    1996 doi

  42. [51]

    doi:10.1051/0004-6361:20011668

    Fox-Machado, L., \'A lvarez, M., Michel, E., et al.\ 2002, , 382, 556. doi:10.1051/0004-6361:20011668

    2002 doi

  43. [52]

    C., et al.\ 2006, , 77, 455

    Fox Machado, L., P \'e rez Hern \'a ndez, F., Su \'a rez, J. C., et al.\ 2006, , 77, 455

    2006

  44. [53]

    Gaia Collaboration, Vallenari, A., Brown, A. G. A., et al.\ 2023, , 674, A1. doi:10.1051/0004-6361/202243940

    2023 doi

  45. [54]

    doi:10.1051/0004-6361:20078807

    Gebran, M., Monier, R., & Richard, O.\ 2008, , 479, 189. doi:10.1051/0004-6361:20078807

    2008 doi

  46. [55]

    doi:10.1051/0004-6361:20031472

    Gerbaldi, M., Faraggiana, R., & Lai, O.\ 2003, , 412, 447. doi:10.1051/0004-6361:20031472

    2003 doi

  47. [56]

    A.\ 2018, , 480, 2953

    Ghazaryan, S., Alecian, G., & Hakobyan, A. A.\ 2018, , 480, 2953. doi:10.1093/mnras/sty1912

    2018 doi

  48. [57]

    Graham, J. A. & Slettebak, A.\ 1973, , 78, 295. doi:10.1086/111416

    1973 doi

  49. [58]

    Gray, R. O. & Corbally, C.\ 2009, Stellar Spectral Classification by Richard O. Gray and Christopher J. Corbally. Princeton University Press, 2009. ISBN: \^A 978-0-691-12511-4

    2009

  50. [59]

    M., Schlafly, E., Zucker, C., et al.\ 2019, , 887, 93

    Green, G. M., Schlafly, E., Zucker, C., et al.\ 2019, , 887, 93. doi:10.3847/1538-4357/ab5362

    2019 doi

  51. [60]

    doi:10.1051/aas:1999186

    Grenier, S., Burnage, R., Faraggiana, R., et al.\ 1999, , 135, 503. doi:10.1051/aas:1999186

    1999 doi

  52. [61]

    Gontcharov, G. A. & Mosenkov, A. V.\ 2019, , 483, 299. doi:10.1093/mnras/sty2978

    2019 doi

  53. [63]

    Hauck, B.\ 1986, , 155, 371

    1986

  54. [64]

    Heck, A., Albert, A., Delays, D., et al.\ 1977, , 61, 563

    1977

  55. [65]

    V., et al.\ 2000, , 355, L27

    H g, E., Fabricius, C., Makarov, V. V., et al.\ 2000, , 355, L27

    2000

  56. [66]

    & Cowley, A

    Houk, N. & Cowley, A. P.\ 1975, University of Michigan Catalogue of two-dimensional spectral types for the HD stars. Volume I. Declinations -90\_ to -53\_ 0., by Houk, N.; Cowley, A. P.. Ann Arbor, MI (USA): Department of Astronomy, University of Michigan, 19 + 452 p

    1975

  57. [67]

    Volume\_3

    Houk, N.\ 1982, Michigan Catalogue of Two-dimensional Spectral Types for the HD stars. Volume\_3. Declinations -40\_ 0 to -26\_ 0., by Houk, N.. Ann Arbor, MI(USA): Department of Astronomy, University of Michigan, 12 + 390 p

    1982

  58. [68]

    Hui-Bon-Hoa, A., Burkhart, C., & Alecian, G.\ 1997, , 323, 901

    1997

  59. [69]

    Johnson, H. L. & Knuckles, C. F.\ 1955, , 122, 209. doi:10.1086/146079

    1955 doi

  60. [70]

    doi:10.1093/mnras/stw393

    Kahraman Ali c avu s , F., Niemczura, E., De Cat, P., et al.\ 2016, , 458, 2307. doi:10.1093/mnras/stw393

    2016 doi

  61. [71]

    u m \"u s , D., K rm z ta s , \

    Kahraman Ali c avu s , F., G \"u m \"u s , D., K rm z ta s , \"O ., et al.\ 2022, Research in Astronomy and Astrophysics, 22, 085003. doi:10.1088/1674-4527/ac71a4

    2022 doi

  62. [73]

    B., Handler, G., Krisciunas, K., et al.\ 1999, , 111, 840

    Kaye, A. B., Handler, G., Krisciunas, K., et al.\ 1999, , 111, 840. doi:10.1086/316399

    1999 doi

  63. [74]

    doi:10.1093/mnras/277.1.217

    Koen, C., Kilkenny, D., van Wyk, F., et al.\ 1995, , 277, 217. doi:10.1093/mnras/277.1.217

    1995 doi

  64. [75]

    doi:10.1046/j.1365-8711.1999.02928.x

    Koen, C., van Rooyen, R., van Wyk, F., et al.\ 1999, , 309, 1051. doi:10.1046/j.1365-8711.1999.02928.x

    1999

  65. [76]

    W.\ 1976, , Metallicism and pulsation: an analysis of the Delta Delphini stars., 32, 651

    Kurtz, D. W.\ 1976, , Metallicism and pulsation: an analysis of the Delta Delphini stars., 32, 651. doi:10.1086/190411

    1976 doi

  66. [77]

    W.\ 1978, , 221, 869

    Kurtz, D. W.\ 1978, , 221, 869. doi:10.1086/156090

    1978 doi

  67. [78]

    W.\ 1979, , 186, 575

    Kurtz, D. W.\ 1979, , 186, 575. doi:10.1093/mnras/186.3.575

    1979 doi

  68. [79]

    Kurucz, R. L. & Avrett, E. H.\ 1981, SAO Special Report, 391

    1981

  69. [80]

    Kurucz, R.\ 1993, Robert Kurucz CD-ROM, 13

    1993

  70. [81]

    W.\ 1989, , 238, 1077

    Kurtz, D. W.\ 1989, , 238, 1077. doi:10.1093/mnras/238.3.1077

    1989 doi

  71. [82]

    & Breger, M.\ 2005, Communications in Asteroseismology, 146, 53

    Lenz, P. & Breger, M.\ 2005, Communications in Asteroseismology, 146, 53. doi:10.1553/cia146s53

    2005 doi

  72. [83]

    V.\ 2003, , 126, 2408

    Makarov, V. V.\ 2003, , 126, 2408. doi:10.1086/378483

    2003 doi

  73. [84]

    doi:10.1051/0004-6361:20054021

    Masana, E., Jordi, C., & Ribas, I.\ 2006, , 450, 735. doi:10.1051/0004-6361:20054021

    2006 doi

  74. [85]

    Mayor, M., Pepe, F., Queloz, D., et al.\ 2003, The Messenger, 114, 20

    2003

  75. [86]

    N., Mamajek, E

    Mellon, S. N., Mamajek, E. E., Stuik, R., et al.\ 2019, , 244, 15. doi:10.3847/1538-4365/ab3662

    2019 doi

  76. [87]

    & Heck, A.\ 1980, , 85, 93

    Mersch, G. & Heck, A.\ 1980, , 85, 93

    1980

  77. [88]

    Milone, A. D. C., Sansom, A. E., & S \'a nchez-Bl \'a zquez, P.\ 2011, , 414, 1227. doi:10.1111/j.1365-2966.2011.18457.x

    2011

  78. [89]

    & Richard, O.\ 2004, The A-Star Puzzle, 224, 209

    Monier, R. & Richard, O.\ 2004, The A-Star Puzzle, 224, 209. doi:10.1017/S1743921304004570

    2004 doi

  79. [90]

    Moon, T. T. & Dworetsky, M. M.\ 1985, , 217, 305. doi:10.1093/mnras/217.2.305

    1985 doi

  80. [91]

    W.\ 1932, , 75, 46

    Morgan, W. W.\ 1932, , 75, 46. doi:10.1086/143354

    1932 doi

  81. [92]

    A., Mathieu, R

    Morse, J. A., Mathieu, R. D., & Levine, S. E.\ 1991, , 101, 1495. doi:10.1086/115782

    1991 doi

  82. [93]

    A., Prugniel, P., et al.\ 2004, , 116, 693

    Moultaka, J., Ilovaisky, S. A., Prugniel, P., et al.\ 2004, , 116, 693. doi:10.1086/422177

    2004 doi

  83. [94]

    Murphy, S. J. & Paunzen, E.\ 2017, , 466, 546. doi:10.1093/mnras/stw3141

    2017 doi

  84. [95]

    J., Hey, D., Van Reeth, T., et al.\ 2019, , 485, 2380

    Murphy, S. J., Hey, D., Van Reeth, T., et al.\ 2019, , 485, 2380. doi:10.1093/mnras/stz590

    2019 doi

  85. [96]

    J., Paunzen, E., Bedding, T

    Murphy, S. J., Paunzen, E., Bedding, T. R., et al.\ 2020, , 495, 1888. doi:10.1093/mnras/staa1271

    2020 doi

  86. [97]

    J., Saio, H., Takada-Hidai, M., et al.\ 2020, , 498, 3, 4272

    Murphy, S. J., Saio, H., Takada-Hidai, M., et al.\ 2020, , 498, 3, 4272. doi:10.1093/mnras/staa2667

    2020 doi

  87. [98]

    Niemczura et al

    Niemczura, E., Smalley, B., & Pych, W.\ 2014, Determination of Atmopsheric Parameters of B-, A-, F- and G-Type Stars Lectures from the School of Spectroscopic Data Analyses, edited by E. Niemczura et al. ISBN 978-3-319-06955-5. Berlin: Springer-Verlag, 2014

    2014

  88. [99]

    J., et al.\ 2017, , Spectroscopic survey of Kepler stars - II

    Niemczura, E., Poli \'n ska, M., Murphy, S. J., et al.\ 2017, , Spectroscopic survey of Kepler stars - II. FIES/NOT observations of A- and F-type stars, 470, 3, 2870. doi:10.1093/mnras/stx1256

    2017 doi

  89. [100]

    Olivares, J., Lodieu, N., B \'e jar, V. J. S., et al.\ 2023, , 675, A28. doi:10.1051/0004-6361/202244703

    2023 doi

  90. [101]

    M., Hogg, D

    Oh, S., Price-Whelan, A. M., Hogg, D. W., et al.\ 2017, , 153, 257. doi:10.3847/1538-3881/aa6ffd

    2017 doi

  91. [102]

    & Duffee, B.\ 1996, Information Bulletin on Variable Stars, 4297, 1

    Paunzen, E. & Duffee, B.\ 1996, Information Bulletin on Variable Stars, 4297, 1

    1996

  92. [103]

    W., Heiter, U., et al.\ 1997, , 123, 93

    Paunzen, E., Weiss, W. W., Heiter, U., et al.\ 1997, , 123, 93. doi:10.1051/aas:1997308

    1997 doi

  93. [104]

    & Maitzen, H

    Paunzen, E. & Maitzen, H. M.\ 1998, , 133, 1. doi:10.1051/aas:1998305

    1998 doi

  94. [105]

    W., Kuschnig, R., et al.\ 1998, , 335, 533

    Paunzen, E., Weiss, W. W., Kuschnig, R., et al.\ 1998, , 335, 533

    1998

  95. [106]

    K., et al.\ 1999, , 345, 597

    Paunzen, E., Kamp, I., Iliev, I. K., et al.\ 1999, , 345, 597

    1999

  96. [107]

    doi:10.1051/0004-6361:20010630

    Paunzen, E., Duffee, B., Heiter, U., et al.\ 2001, , 373, 625. doi:10.1051/0004-6361:20010630

    2001 doi

  97. [108]

    doi:10.1051/0004-6361:20010631

    Paunzen, E.\ 2001, , 373, 633. doi:10.1051/0004-6361:20010631

    2001 doi

  98. [109]

    K., Kamp, I., et al.\ 2002, , 336, 1030

    Paunzen, E., Iliev, I. K., Kamp, I., et al.\ 2002, , 336, 1030. doi:10.1046/j.1365-8711.2002.05865.x

    2002

  99. [110]

    doi:10.1051/0004-6361/201526413

    Paunzen, E.\ 2015, , 580, A23. doi:10.1051/0004-6361/201526413

    2015 doi

  100. [111]

    doi:10.1017/S1743921323003538

    Paunzen, E.\ 2024, IAU Symposium, 376, 91. doi:10.1017/S1743921323003538

    2024 doi

  101. [112]

    Pearce, J. A. & Hill, G.\ 1975, Publications of the Dominion Astrophysical Observatory Victoria, 14, 319

    1975

  102. [113]

    & Thomsen, B.\ 1977, , 30, 11

    Pedersen, H. & Thomsen, B.\ 1977, , 30, 11

    1977

  103. [114]

    doi:10.1117/12.787379

    Perruchot, S., Kohler, D., Bouchy, F., et al.\ 2008, , 7014, 70140J. doi:10.1117/12.787379

    2008 doi

  104. [115]

    L.\ 1991, , 103, 494

    Perry, C. L.\ 1991, , 103, 494. doi:10.1086/132849

    1991 doi

  105. [116]

    Perry, C. L. & Christodoulou, D. M.\ 1996, , 108, 772. doi:10.1086/133800

    1996 doi

  106. [117]

    W.\ 1974, , 12, 257

    Preston, G. W.\ 1974, , 12, 257. doi:10.1146/annurev.aa.12.090174.001353

    1974

  107. [118]

    doi:10.1051/0004-6361/201116769

    Prugniel, P., Vauglin, I., & Koleva, M.\ 2011, , 531, A165. doi:10.1051/0004-6361/201116769

    2011 doi

  108. [119]

    doi:10.1088/1538-3873/ac12dc

    Poro, A., Paki, E., Mazhari, G., et al.\ 2021, , 133, 084201. doi:10.1088/1538-3873/ac12dc

    2021 doi

  109. [120]

    J., Harzandjadidi, R., et al.\ 2024, Research in Astronomy and Astrophysics, Period Luminosity Relationship for Scuti Stars Revisited, 24, 2, 025011

    Poro, A., Jafarzadeh, S. J., Harzandjadidi, R., et al.\ 2024, Research in Astronomy and Astrophysics, Period Luminosity Relationship for Scuti Stars Revisited, 24, 2, 025011. doi:10.1088/1674-4527/ad1b0f

    2024 doi

  110. [121]

    L.\ 1998, , 505, 255

    Rachford, B. L.\ 1998, , 505, 255. doi:10.1086/306148

    1998 doi

  111. [122]

    doi:10.3847/0004-6256/152/6/207

    Rainer, M., Poretti, E., Mist \`o , A., et al.\ 2016, , 152, 207. doi:10.3847/0004-6256/152/6/207

    2016 doi

  112. [123]

    Randich, S., Schmitt, J. H. M. M., & Prosser, C.\ 1996, , 313, 815

    1996

  113. [124]

    & Manfroid, J.\ 2009, , 498, 961

    Renson, P. & Manfroid, J.\ 2009, , 498, 961. doi:10.1051/0004-6361/200810788

    2009 doi

  114. [125]

    R., Winn, J

    Ricker, G. R., Winn, J. N., Vanderspek, R., et al.\ 2015, Journal of Astronomical Telescopes, Instruments, and Systems, 1, 014003. doi:10.1117/1.JATIS.1.1.014003

    2015 doi

  115. [126]

    Rodriguez, E., Lopez de Coca, P., Rolland, A., et al.\ 1994, , 106, 21

    1994

  116. [127]

    J., & L \'o pez de Coca, P.\ 2000, , 144, 469

    Rodr \' guez, E., L \'o pez-Gonz \'a lez, M. J., & L \'o pez de Coca, P.\ 2000, , 144, 469. doi:10.1051/aas:2000221

    2000 doi

  117. [128]

    doi:10.1051/0004-6361:20020943

    Royer, F., Grenier, S., Baylac, M.-O., et al.\ 2002, , 393, 897. doi:10.1051/0004-6361:20020943

    2002 doi

  118. [129]

    doi:10.1051/0004-6361/202346847

    Royer, P., Merle, T., Dsilva, K., et al.\ 2024, , 681, A107. doi:10.1051/0004-6361/202346847

    2024 doi

  119. [130]

    doi:10.1051/0004-6361/202141480

    R \'o \.z a \'n ski, T., Niemczura, E., Lemiesz, J., et al.\ 2022, , 659, A199. doi:10.1051/0004-6361/202141480

    2022 doi

  120. [131]

    L.\ 1991, , 101, 2177

    Schutt, R. L.\ 1991, , 101, 2177. doi:10.1086/115840

    1991 doi

  121. [132]

    & Fukugita, M.\ 2000, , 120, 1072

    Sekiguchi, M. & Fukugita, M.\ 2000, , 120, 1072. doi:10.1086/301490

    2000 doi

  122. [133]

    & Landstreet, J

    Silaj, J. & Landstreet, J. D.\ 2014, , 566, A132. doi:10.1051/0004-6361/201321468

    2014 doi

  123. [134]

    & Stock, J.\ 1959, Astronomische Abhandlungen der Hamburger Sternwarte, 5, 105

    Slettebak, A. & Stock, J.\ 1959, Astronomische Abhandlungen der Hamburger Sternwarte, 5, 105

    1959

  124. [135]

    W., Smith, A

    Smalley, B., Kurtz, D. W., Smith, A. M. S., et al.\ 2011, , 535, A3. doi:10.1051/0004-6361/201117230

    2011 doi

  125. [136]

    L., et al.\ 2017, , Pulsation versus metallicism in Am stars as revealed by LAMOST and WASP, 465, 3, 2662

    Smalley, B., Antoci, V., Holdsworth, D. L., et al.\ 2017, , Pulsation versus metallicism in Am stars as revealed by LAMOST and WASP, 465, 3, 2662. doi:10.1093/mnras/stw2903

    2017 doi

  126. [137]

    R., Caillault, J.-P., Gagne, M., et al.\ 1994, , 91, 625

    Stauffer, J. R., Caillault, J.-P., Gagne, M., et al.\ 1994, , 91, 625. doi:10.1086/191951

    1994 doi

  127. [138]

    R.\ 1972, , 160, 155

    Stokes, N. R.\ 1972, , 160, 155. doi:10.1093/mnras/160.2.155

    1972 doi

  128. [139]

    R., Huber, D., et al.\ 2022, , 927, 1, 31

    Tayar, J., Claytor, Z. R., Huber, D., et al.\ 2022, , 927, 1, 31. doi:10.3847/1538-4357/ac4bbc

    2022 doi

  129. [140]

    S.\ 2005, , 443, 627

    Th \'e ado, S., Vauclair, S., & Cunha, M. S.\ 2005, , 443, 627. doi:10.1051/0004-6361:20052933

    2005 doi

  130. [141]

    doi:10.1117/12.968154

    Tody, D.\ 1986, , The IRAF Data Reduction and Analysis System, 627, 733. doi:10.1117/12.968154

    1986 doi

  131. [142]

    G.\ 1982, , 26, 666

    Tsvetkov, T. G.\ 1982, , 26, 666

    1982

  132. [143]

    doi:10.48550/arXiv.astro-ph/0006272

    Turcotte, S., Richer, J., Michaud, G., et al.\ 2000, , The effect of diffusion on pulsations of stars on the upper main sequence --- Scuti and metallic A stars, 360, 603. doi:10.48550/arXiv.astro-ph/0006272

    2000 doi arXiv

  133. [144]

    A.\ 1980, , 44, 1

    Twarog, B. A.\ 1980, , 44, 1. doi:10.1086/190683

    1980 doi

  134. [145]

    Uytterhoeven, K., Moya, A., Grigahc \`e ne, A., et al.\ 2011, , The Kepler characterization of the variability among A- and F-type stars. I. General overview, 534, A125. doi:10.1051/0004-6361/201117368

    2011 doi

  135. [146]

    Xu, Y., Li, Z.-P., Deng, L.-C., et al.\ 2002, Chinese J. Astron. Astrophys., 2, 441. doi:10.1088/1009-9271/2/5/441

    2002 doi

  136. [147]

    J., Smalley, B., et al.\ 1994, , 267, 1045

    Wonnacott, D., Kellett, B. J., Smalley, B., et al.\ 1994, , 267, 1045. doi:10.1093/mnras/267.4.1045

    1994 doi

  137. [148]

    & Ottaviani, D

    Worthey, G. & Ottaviani, D. L.\ 1997, , 111, 377. doi:10.1086/313021

    1997 doi

Pith tools

Reviewed August 5, 2026 · model on record in the stance chip above.