Pith. sign in

REVIEW 3 major objections 5 minor 89 references

The chemical compositions of the 2 new HgMn stars HD 30085 and HD 30963. Comparison to $\chi$ Lupi A, $\nu$ Cap and HD 174567

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 The paper argues that two stars previously classified as normal, HD 30085 and HD 30963, are actually mercury-manganese (HgMn) stars, and that HD 174567 is a mildly chemically peculiar star.

desk verdict Two new HgMn stars have solid Mn/Sr/Y/Zr support, but the quoted mercury abundance is not independently measured because the Hg II gf values were tuned to fit the line. read the letter →

arxiv 1908.05023 v1 pith:QUNWQII4 submitted 2019-08-14 astro-ph.SR

R. Monier , E. Griffin , M. Gebran , T. Kilicoglu , T. Merle , F. Royer This is my paper · ORCID
classification astro-ph.SR
keywords chemicallypeculiarstarsHgMnabundanceanalysismercury-manganeseradiativediffusionspectralsynthesisHD3008530963
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 argues that two stars previously classified as normal late-B/early-A stars, HD 30085 and HD 30963, are actually mercury-manganese (HgMn) stars, a class of chemically peculiar stars whose surface abundances are shaped by radiative diffusion. Using high-resolution spectra and synthetic-spectrum fits to about forty elements, it finds large overabundances of manganese, strontium, yttrium, zirconium, platinum, and mercury, and underabundances of helium, magnesium, scandium, and nickel, matching the HgMn pattern. It also finds that HD 174567, previously used as a normal comparison star, is mildly chemically peculiar. If the classification holds, the census of HgMn stars gains two members, and the two stars become additional laboratories for studying how atomic diffusion produces abundance anomalies in slow rotators.

What carries the argument

The analysis rests on LTE spectrum synthesis with model atmospheres (computed with ATLAS9 and ATLAS12) and the SYNSPEC49 code, fitting carefully selected unblended lines of forty elements. The load-bearing objects are the Hg II line at 3983.93 Å, modeled with nine hyperfine components from isotopes Hg 196 through Hg 204, and the Mn II lines with published hyperfine structure; the mercury oscillator strengths were iteratively adjusted to reproduce the observed flat-bottomed profile, yielding an isotope mix dominated by the heaviest isotopes. The abundance patterns are compared element by element with $\chi$ Lupi A and the normal star $\nu$ Cap, and the global pattern is interpreted as the result of radiative diffusion in a slow rotator.

What would settle it

A laboratory measurement of the nine Hg II hyperfine component oscillator strengths at 3983.93 Å would settle the mercury claim: if independent gf values, used in the same synthesis, cannot reproduce the observed flat-bottomed profile with an overabundance near $10^5$ solar, the mercury abundance and isotope fractions as quoted would be wrong.

Watch

Extended reading notes

Core claim

HD 30085 and HD 30963 are two new HgMn stars. The evidence is their effective temperatures ($\sim11300$ K and $\sim11480$ K), low projected rotational velocities (26 and 37 km s$^{-1}$), and abundance patterns that reproduce the characteristic HgMn signature: light elements depleted, iron-peak and heavy elements overabundant, with mercury overabundant by factors near $10^5$ relative to solar. Their patterns align with that of the well-known HgMn star $\chi$ Lupi A and fall within the compiled abundance range of confirmed HgMn stars. HD 174567 shows milder anomalies and is classified as a new mild chemically peculiar star, possibly a cool and mild HgMn star.

Load-bearing premise

The mercury result depends on the strengths assigned to the nine components of the mercury line, which the authors adjusted until the computed line matched the observed one; if those strengths are not physically real, the mercury overabundance and isotope mix are not independently measured, though the other element anomalies still point to HgMn.

Editorial extensions

If this is right

  • The census of known HgMn stars grows by at least two, both relatively bright and observable from the northern hemisphere.
  • The two stars can be added to samples used to test radiative-diffusion models of HgMn abundance anomalies, especially the correlation between effective temperature and mercury isotope fraction.
  • HD 174567 should no longer be treated as a normal comparison star in abundance studies; its mild anomalies need to be accounted for.
  • The heavy-isotope dominance suggested for mercury in both stars, if confirmed, links them to the cool HgMn stars rather than the hotter ones.
  • The line identifications and abundances for HD 30085 provide an empirical linelist for future analyses of similar stars.

Reading between the lines

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

  • A direct check of the mercury result would be new laboratory oscillator strengths for the nine Hg II components; without that, the extreme mercury overabundance and the heavy-isotope mix remain dependent on the model.
  • The same line-by-line synthesis could be run on other slow rotators from the sample used here; the paper implies the bright-end census of HgMn stars may still be incomplete.
  • The intermediate pattern of HD 174567 leaves open whether mild HgMn stars form a continuum with normal stars or a separate regime; the paper does not settle that.
  • A higher-resolution, higher-signal-to-noise observation of the Hg II profile in both stars, ideally over several epochs, could test whether the flat core and isotope fractions are stable or variable.
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. The paper presents a detailed LTE abundance analysis of 40 elements in four late-B/early-A stars: HD 30085, HD 30963, HD 174567 and the known HgMn star χ Lupi A, using SOPHIE, DAO and FEROS spectra. Effective temperatures and surface gravities are derived from Strömgren photometry, microturbulent velocities from Fe II line dispersion, and abundances from SYNSPEC spectrum synthesis with ATLAS9/ATLAS12 model atmospheres, with NLTE corrections for Na, Mg and Ca. The central claim is that HD 30085 and HD 30963 are two new HgMn stars, based on the strong Hg II 3983.93 Å line and on large overabundances of Mn, Sr, Y, Zr, Pt and Hg together with light-element deficiencies, while HD 174567 is a mild chemically peculiar star. A reanalysis of χ Lupi A on the same temperature scale and with the same line list is used as a comparison anchor.

Significance. If the classification claim holds, the paper adds two new members to the small class of cool, sharp-lined HgMn stars and identifies a new mild CP star, which is valuable for studies of radiative diffusion in late-B/early-A stars. The paper has clear strengths: the HgMn classification is supported by several independent abundance anomalies (Mn II, Sr II, Y II, Zr II) that do not depend on the Hg line modeling; the comparison of all stars on a common effective-temperature scale and with the same atomic data is methodologically sound; and the list of line identifications for HD 30085 (Table 10) is a useful resource. The quantitative mercury abundance and especially the isotope fractions are, however, compromised by the iterative adjustment of the Hg II hyperfine oscillator strengths described in Section 5.7.4, so those specific numbers should not be presented as independent measurements until that issue is resolved.

major comments (3)
  1. [5.7.4 and Table 5] The mercury abundance and isotope fractions are not independently measured. The text states that the oscillator strengths of the nine Hg II hyperfine components were 'iteratively altered' until the synthetic profile matched the observed line; these modified gf values are then used to derive log Hg/H and the isotope fractions. This is circular at the line-formation level, because any mismatch between model and observation can be absorbed into the gf rescaling. The Appendix A uncertainty budget (Eq. A1 and Table 7) treats sigma_log gf as an independent input, but for Hg II the gf values were tuned to the same data used to measure the abundance, so the quoted ±0.12–0.23 dex does not include the dominant systematic error. The authors should either use the published Dolk et al. (2003) gf values and report the resulting abundance with an explicit un-modeled systematic uncertainty, or validate any gf modification against independent data, e.g., the Hg II 6149.47 Å line that is resolved in χ Lupi A. The HgMn classification itself is not endangered, since the Mn II, Sr II, Y II and Zr II overabundances are independent of this issue.
  2. [Abstract and Section 5.2.10 / Table 8] The abstract's abundance-pattern summary is incorrect for scandium. The abstract lists scandium among the underabundant elements, but Section 5.2.10 states that scandium is overabundant in HD 30085, HD 30963 and HD 174567, and Table 8 gives [Sc/H] = +0.30, +0.70 and +0.11 for these three stars; only χ Lupi A is scandium-underabundant ([Sc/H] = -1.30). This is a load-bearing inconsistency in the summary of the paper's main result and must be corrected.
  3. [5.7.4 and Table 8] There is an internal inconsistency in the final mercury abundance for HD 30085. Section 5.7.4 reports log Hg/H ≈ -5.83 for HD 30085, while Table 8 lists log Hg/H = -5.12 for the same star and the same line. This 0.71 dex discrepancy in the defining element of the HgMn classification needs to be reconciled. In addition, the isotope fractions quoted in Section 5.7.4 are derived from equivalent-width ratios of hyperfine components whose gf values were changed by hand; given that arbitrariness, the isotope fractions should either be removed or presented only as a rough line-profile decomposition with no quantitative claim.
minor comments (5)
  1. [5.2.8] The sulfur paragraph is self-contradictory: it reads 'Sulfur is solar in HD 30085, overabundant in HD 30963 and χ Lupi A and underabundant in HD 30963'. The last occurrence should presumably refer to HD 174567.
  2. [Table 5] The header of Table 5 is malformed: 'The Hg II 3983.93 Å linelist' is merged with the column names. The table should be reformatted, and the caption should state that the listed log gf values are the authors' modified values, not the original Dolk et al. (2003) values.
  3. [Table 8] Several entries contain placeholder references such as 'V ALD??' and '?', and some lines are labelled 'no data' or 'nd'. These should be resolved or explicitly marked as upper limits with a consistent notation.
  4. [Figures 4, 5, 7, 8] The captions and axis labels should be checked: Figure 7 is captioned as synthesizing 'Hg II 3983.87 Å' while the text and Table 5 refer to 3983.93 Å, and Figure 4/5 captions should identify the plotted wavelength ranges more clearly.
  5. [4.1.2] The evolutionary tracks are said to include microscopic diffusion while the isochrones are 'retrieved for the current solar composition'; the text should clarify whether the adopted diffusion treatment matters for the quoted masses and ages.

Circularity Check

1 steps flagged · score 6.0 of 10

The Hg abundance and isotope mix are derived after hand-tuning the Hg II gf values to the same observed profile, making that specific quantitative result circular; the HgMn classification itself rests on independent Mn and heavy-element lines.

  1. fitted input called prediction [Section 5.7.4 (Mercury), Table 5 and Fig. 7]
    "In order to shift redwards the synthetic line core and give it a flat shape comparable to the observed one, we have iteratively altered the oscillator strengths of the individual hyperfine components until the overall observed line profile could be reproduced. The final combination of oscillator strengths is recorded in Table 5."

    The Hg II 3983.93 Å oscillator strengths are atomic-data inputs to the synthesis. The paper adjusts them until the synthetic profile matches the same observed line that is then used to derive the Hg abundance and isotope fractions. Because line opacity scales with gf × abundance, the reported log Hg/H values and isotope contributions are not independent measurements: after this tuning the model reproduces the observation by construction. The Appendix A error budget treats σ_log gf as a known quantity and does not propagate the freedom used to alter the gf values, so the quoted ±0.12 dex underestimates this systematic effect.

full rationale

This is an abundance-analysis paper rather than a first-principles derivation. The fundamental parameters come from standard uvbyβ photometry calibrations, microturbulence is set by the conventional Fe II scatter-minimization procedure, and the abundance patterns are derived by spectrum synthesis with externally referenced atomic data (NIST, VALD, Dolk et al. 2003, etc.). The comparison to χ Lupi A uses the same temperature scale and line list but is a consistency check, not an input to the classifications. The prior self-citations (Royer et al. 2014, Monier et al. 2015, Monier et al. 2018) are not load-bearing: the present paper rederives the abundances directly. The one genuine circular step is Sec. 5.7.4: the Hg II hyperfine gf values are iteratively altered until the observed 3983.93 Å profile is matched, and the Hg abundance and isotope mix are then read off from that same tuned model. That makes the quantitative mercury result fitted rather than measured. It does not, however, make the HgMn classification circular, because the strong Hg feature itself plus the independent Mn II, Sr II, Y II and Zr II overabundances would still support the classification, and even the unmodified Dolk gf values produce a large Hg overabundance. Score 6 reflects a partial circularity limited to the mercury abundance and isotope ratios.

Assumptions & free parameters 3 free parameters · 6 assumptions · 0 invented entities

The paper's contribution is mostly observational: it applies standard model-atmosphere synthesis to four stars. The non-standard elements are the tuned Hg II gf values and the fitted microturbulence, and the domain assumptions are the usual LTE and photometric calibration assumptions of this field. No invented entities are introduced.

free parameters (3)
  • Microturbulent velocities = HD 30085: 0.0 km/s; HD 30963: 0.1; HD 174567: 0.95; values in Table 2
    Chosen to minimize the standard deviation of iron abundances derived from fifty Fe II lines (Section 4.1.1); a standard but fitted model parameter.
  • Hg II hyperfine oscillator strengths = Nine modified log gf values listed in Table 5
    Oscillator strengths of the Hg II 3983.93 A hyperfine components were altered iteratively to reproduce the observed line profile (Section 5.7.4); no independent laboratory measurement is provided for the modified values.
  • NLTE abundance corrections = Na: -0.52 and -0.60 dex; Mg: -0.33 dex; Ca: +0.37 dex (Section 5)
    Corrections computed from model atoms and adopted collision rates; the choice of atomic model and Drawin/Seaton recipes affects the final abundances.
assumptions (6)
  • domain assumption LTE is valid for the majority of the synthesized lines; NLTE is applied only to Na I, Mg I and Ca II.
    Sections 4 and 5. The paper notes weaker Cr I, Mn I and Fe I lines yield lower abundances than the corresponding ion lines, indicating possible NLTE departures for neutrals.
  • domain assumption ATLAS9 and ATLAS12 plane-parallel hydrostatic LTE model atmospheres adequately represent the stellar photospheres.
    Section 4.2; standard assumption, but no 3D or non-LTE structure tests are presented.
  • domain assumption The adopted Teff and log g from uvby-beta photometry are accurate to about 125 K and 0.20 dex.
    Section 4.1, errors quoted from Napiwotzki et al. 1993; the derived abundances depend on these values.
  • domain assumption The selected unblended lines and their NIST or VALD atomic data are reliable; for elements with one line the abundance is provisional.
    Sections 4.4 and 5; several elements, including Pt, Hg and rare earths, rely on one line or on modified data.
  • ad hoc to paper The modified Hg II hyperfine gf values in Table 5 are valid for abundance and isotope-ratio measurement.
    Section 5.7.4; these values were tuned to the observed profile and are not from an independent source.
  • domain assumption The observed spectra are single-star slow rotators with no significant veiling or unrecognized binarity.
    Section 3; the authors checked for radial velocity variations, but unrecognized continuum dilution or a faint companion would bias the abundance pattern.

how reviews work

0 comments
Cite this review

Pith. "Pith review of The chemical compositions of the 2 new HgMn stars HD 30085 and HD 30963. Comparison to $\chi$ Lupi A, $\nu$ Cap and HD 174567." pith.science (2026). https://pith.science/paper/QUNWQII4

@misc{pith2026190805023,
  author       = {Pith},
  title        = {Pith review of: The chemical compositions of the 2 new HgMn stars HD 30085 and HD 30963. Comparison to $\chi$ Lupi A, $\nu$ Cap and HD 174567},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/QUNWQII4}},
  note         = {Machine review of arXiv:1908.05023}
}
read the original abstract

We report on a detailed abundance study of the fairly bright slow rotators HD 30085 (A0 IV), HD 30963 (B9 III) and HD 174567 (A0 V), hitherto reported as normal stars and the sharp-lined chi Lupi A (B9 IV HgMn). In the spectra of HD 30085, HD 30963, the Hg II line at 3984 A line is conspicuous and numerous lines of silicon, manganese, chromium, titanium, iron, strontium, yttrium and zirconium appear to be strong absorbers. A comparison of the mean spectra of HD 30085 and HD 30963 with a grid of synthetic spectra for selected unblended lines having reliable updated atomic data reveals large overabundances of phosphorus, titanium, chromium, manganese, strontium, yttrium, and zirconium, barium, platinum and mercury and underabundances of helium, magnesium, scandium, nickel. The surface abundances of chi Lupi A have been rederived on the same effective temperature scale and using the same atomic data for consistency and comparison for HD 30085 and HD 30963. For HD 174567, milder deficiencies and excesses are found. The abundances of sodium, magnesium and calcium have been corrected for NLTE effects. The effective temperatures, surface gravities, low projected rotational velocities and the peculiar abundance patterns of HD 30085 and HD 30963 show that these stars are 2 new HgMn stars and should be reclassified as such. HD 174567 is most likely a new marginally Chemically Peculiar star. A list of the identifications of lines absorbing more than 2% in the spectrum of HD 30085 is also provided.

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

89 extracted references · 70 canonical work pages

  1. [1]

    Adelman , S. J. 1991, , 252, 116

    1991

  2. [2]

    2011, , 414, 3350

    Bi \'e mont , \'E ., Blagoev , K., Engstr \"o m , L., et al. 2011, , 414, 3350

    2011

  3. [3]

    M., Marsden , G., & Lawler , J

    Biemont , E., Grevesse , N., Faires , L. M., Marsden , G., & Lawler , J. E. 1989, , 209, 391, (BGF)

    1989

  4. [4]

    2012, , 427, 127

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

    2012

  5. [5]

    & Zeippen, C

    Butler, K. & Zeippen, C. J. 1991, J. Phys. IV France, 01, C1

    1991

  6. [6]

    1986, Uppsala Astronomical Observatory Reports, 33

    Carlsson , M. 1986, Uppsala Astronomical Observatory Reports, 33

    1986

  7. [7]

    1992, in Astronomical Society of the Pacific Conference Series, Vol

    Carlsson , M. 1992, in Astronomical Society of the Pacific Conference Series, Vol. 26, Cool Stars, Stellar Systems, and the Sun, ed. M. S. Giampapa & J. A. Bookbinder , 499

    1992

  8. [8]

    & Hubrig , S

    Castelli , F. & Hubrig , S. 2004, , 425, 263

    2004

Show all 89 references
  1. [9]

    & Kurucz , R

    Castelli , F. & Kurucz , R. L. 2003, in IAU Symposium, Vol. 210, Modelling of Stellar Atmospheres, ed. N. Piskunov , W. W. Weiss , & D. F. Gray , A20

    2003

  2. [10]

    1969, , 74, 375

    Cowley , A., Cowley , C., Jaschek , M., & Jaschek , C. 1969, , 74, 375

    1969

  3. [11]

    & Mendoza , C

    Cunto , W. & Mendoza , C. 1992, , 23

    1992

  4. [12]

    D., Snoek , L

    Davidson , M. D., Snoek , L. C., Volten , H., & Doenszelmann , A. 1992, , 255, 457

    1992

  5. [13]

    A., Lawler , J

    Den Hartog , E. A., Lawler , J. E., Sneden , C., & Cowan , J. J. 2003, , 148, 543

    2003

  6. [14]

    A., Lawler , J

    Den Hartog , E. A., Lawler , J. E., Sneden , C., & Cowan , J. J. 2006, , 167, 292

    2006

  7. [15]

    Dimitrijevic , M. S. & Sahal-Brechot , S. 1984, , 136, 289

    1984

  8. [16]

    M., & Hubrig , S

    Dolk , L., Wahlgren , G. M., & Hubrig , S. 2003, , 402, 299

    2003

  9. [17]

    2006, Springer Handbook of Atomic, Molecular, and Optical Physics, ed

    Drake, G. 2006, Springer Handbook of Atomic, Molecular, and Optical Physics, ed. G. Drake (New York, NY: Springer New York), 199--219

    2006

  10. [18]

    Drawin , H. W. 1969, Zeitschrift fur Physik, 225, 483

    1969

  11. [19]

    M., Jomaron , C

    Dworetsky , M. M., Jomaron , C. M., & Smith , C. A. 1998, , 333, 665

    1998

  12. [20]

    R., Martin , G

    Fuhr , J. R., Martin , G. A., & Wiese , W. L. 1988, Journal of Physical and Chemical Reference Data, 17

    1988

  13. [21]

    & Alecian , G

    Ghazaryan , S. & Alecian , G. 2016, , 460, 1912

    2016

  14. [22]

    & Sauval , A

    Grevesse , N. & Sauval , A. J. 1998, , 85, 161

    1998

  15. [23]

    2015, Chemical Physics, 462, 94 , inelastic Processes in Atomic, Molecular and Chemical Physics

    Guitou, M., Spielfiedel, A., Rodionov, D., et al. 2015, Chemical Physics, 462, 94 , inelastic Processes in Atomic, Molecular and Chemical Physics

    2015

  16. [24]

    & Mermilliod , M

    Hauck , B. & Mermilliod , M. 1998, , 129, 431

    1998

  17. [25]

    A., Scholl , T

    Holt , R. A., Scholl , T. J., & Rosner , S. D. 1999, , 306, 107

    1999

  18. [26]

    R., & McSwain , M

    Huang , W., Gies , D. R., & McSwain , M. V. 2010, , 722, 605

    2010

  19. [27]

    & Lanz , T

    Hubeny , I. & Lanz , T. 1992, , 262, 501

    1992

  20. [28]

    1976, Ultraviolet bright-star spectrophotometric catalogue

    Jamar , C., Macau-Hercot , D., Monfils , A., et al. 1976, Ultraviolet bright-star spectrophotometric catalogue. A compilation of absolute spectrophotometric data obtained with the Sky Survey Telescope (S2/68) on the European Astronomical Satellite TD-1

    1976

  21. [29]

    2001, The Astrophysical Journal Supplement Series, 134, 173

    Kling, R., Schnabel, R., & Griesmann, U. 2001, The Astrophysical Journal Supplement Series, 134, 173

    2001

  22. [30]

    2017, http://physics.nist.gov/asd, 5

    Kramida , A., Ralchenko , Y., Reader , J., & NIST ASD Team . 2017, http://physics.nist.gov/asd, 5

    2017

  23. [31]

    2018, http://physics.nist.gov/asd, 5

    Kramida , A., Ralchenko , Y., Reader , J., & NIST ASD Team . 2018, http://physics.nist.gov/asd, 5

    2018

  24. [32]

    Kurucz , R. L. 1992, , 23

    1992

  25. [33]

    Kurucz , R. L. 1993, (GUES)

    1993

  26. [34]

    Kurucz , R. L. 2003, Robert L. Kurucz on-line database of observed and predicted atomic transitions

    2003

  27. [35]

    Kurucz , R. L. 2005, Memorie della Societa Astronomica Italiana Supplementi, 8, 14

    2005

  28. [36]

    Kurucz , R. L. 2010, Robert L. Kurucz on-line database of observed and predicted atomic transitions

    2010

  29. [37]

    Kurucz , R. L. 2013, ATLAS12: Opacity sampling model atmosphere program , Astrophysics Source Code Library

    2013

  30. [38]

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

    1981

  31. [39]

    Kurucz , R. L. & Peytremann , E. 1975, SAO Special Report, 362, 1, (KP)

    1975

  32. [40]

    C., Didelon , P., & Mathys , G

    Lanz , T., Artru , M. C., Didelon , P., & Mathys , G. 1993, , 272, 465

    1993

  33. [41]

    S., & Artru , M.-C

    Lanz , T., Dimitrijevic , M. S., & Artru , M.-C. 1988, , 192, 249

    1988

  34. [42]

    E., Den Hartog , E

    Lawler , J. E., Den Hartog , E. A., Sneden , C., & Cowan , J. J. 2006, , 162, 227

    2006

  35. [43]

    E., Sneden , C., & Cowan , J

    Lawler , J. E., Sneden , C., & Cowan , J. J. 2004, , 604, 850

    2004

  36. [44]

    E., Sneden , C., Cowan , J

    Lawler , J. E., Sneden , C., Cowan , J. J., Ivans , I. I., & Den Hartog , E. A. 2009, Astrophys. J. Suppl. Ser., 182, 51, (LSCI)

    2009

  37. [45]

    E., Sneden , C., Cowan , J

    Lawler , J. E., Sneden , C., Cowan , J. J., et al. 2008, , 178, 71

    2008

  38. [46]

    E., Wickliffe , M

    Lawler , J. E., Wickliffe , M. E., Cowley , C. R., & Sneden , C. 2001 a , , 137, 341

    2001

  39. [47]

    E., Wickliffe , M

    Lawler , J. E., Wickliffe , M. E., den Hartog , E. A., & Sneden , C. 2001 b , Astrophys. J., 563, 1075, (LWHS)

    2001

  40. [48]

    2006, , 456, 1181

    Ljung , G., Nilsson , H., Asplund , M., & Johansson , S. 2006, , 456, 1181

    2006

  41. [49]

    A., Fuhr , J

    Martin , G. A., Fuhr , J. R., & Wiese , W. L. 1988, Atomic transition probabilities. Scandium through Manganese

    1988

  42. [50]

    Martin, W. C. 1960, J. Opt. Soc. Am., 50, 174

    1960

  43. [51]

    F., Corliss , C

    Meggers , W. F., Corliss , C. H., & Scribner , B. F. 1975, Tables of spectral-line intensities. Part I, II\_- arranged by elements

    1975

  44. [52]

    Miles , B. M. & Wiese , W. L. 1969, Atomic Data, 1, 1

    1969

  45. [53]

    H., Wilkerson , T

    Miller , M. H., Wilkerson , T. D., Roig , R. A., & Bengtson , R. D. 1974, , 9, 2312, (MWRB)

    1974

  46. [54]

    Molnar , M. R. 1972, , 175, 453

    1972

  47. [55]

    2015, , 577, A96

    Monier , R., Gebran , M., & Royer , F. 2015, , 577, A96

    2015

  48. [56]

    2018, , 854, 50

    Monier , R., Gebran , M., Royer , F., Kilicoglu , T., & Fr \'e mat , Y. 2018, , 854, 50

    2018

  49. [57]

    Moon , T. T. & Dworetsky , M. M. 1985, , 217, 305

    1985

  50. [58]

    1993, , 268, 653

    Napiwotzki , R., Schoenberner , D., & Wenske , V. 1993, , 268, 653

    1993

  51. [59]

    Nielsen , K., Karlsson , H., & Wahlgren , G. M. 2000 a , , 363, 815

    2000

  52. [60]

    Nielsen , K., Karlsson , H., & Wahlgren , G. M. 2000 b , , 363, 815

    2000

  53. [61]

    Nilsson , H., Ljung , G., Lundberg , H., & Nielsen , K. E. 2006, , 445, 1165

    2006

  54. [62]

    2010, , 516, A13

    Palacios , A., Gebran , M., Josselin , E., et al. 2010, , 516, A13

    2010

  55. [63]

    2000, Physica Scripta, 61, 323, (PQWB)

    Palmeri , P., Quinet , P., Wyart , J., & Bi \'e mont , E. 2000, Physica Scripta, 61, 323, (PQWB)

    2000

  56. [64]

    2008, in , Vol

    Perruchot , S., Kohler , D., Bouchy , F., et al. 2008, in , Vol. 7014, Ground-based and Airborne Instrumentation for Astronomy II, 70140J

    2008

  57. [65]

    H., Berends, R

    Pinnington, E. H., Berends, R. W., & Lumsden, M. 1995, Journal of Physics B: Atomic, Molecular and Optical Physics, 28, 2095

    1995

  58. [66]

    Raassen , A. J. J. & Uylings , P. H. M. 1998, Journal of Physics B Atomic Molecular Physics, 31, 3137

    1998

  59. [67]

    1989, , 209, 233

    Ramella , M., Boehm , C., Gerbaldi , M., & Faraggiana , R. 1989, , 209, 233

    1989

  60. [68]

    2014, , 562, A84

    Royer , F., Gebran , M., Monier , R., et al. 2014, , 562, A84

    2014

  61. [69]

    L., et al

    Ryabchikova , T., Piskunov , N., Kurucz , R. L., et al. 2015, , 90, 054005

    2015

  62. [70]

    2006, Astron

    Ryabchikova , T., Ryabtsev , A., Kochukhov , O., & Bagnulo , S. 2006, Astron. and Astrophys., 456, 329, (RRKB)

    2006

  63. [71]

    2007, , 473, 907

    Ryabchikova , T., Sachkov , M., Kochukhov , O., & Lyashko , D. 2007, , 473, 907

    2007

  64. [72]

    Ryabtsev , A. N. 2010, private communication, (ISAN)

    2010

  65. [73]

    Sakhibullin , N. A. 1987, , 31, 151

    1987

  66. [74]

    Sansonetti, C. J. & Nave, G. 2014, The Astrophysical Journal Supplement Series, 213, 28

    2014

  67. [75]

    Sansonetti, C. J. & Reader, J. 2001, Physica Scripta, 63, 219

    2001

  68. [76]

    Seaton , M. J. 1962, Proceedings of the Physical Society, 79, 1105

    1962

  69. [77]

    Shamey , L. J. 1969, PhD thesis, UNIVERSITY OF COLORADO AT BOULDER

    1969

  70. [78]

    Shenstone, A. G. 1961, Proceedings of the Royal Society of London A: Mathematical, Physical and Engineering Sciences, 261, 153

    1961

  71. [79]

    Smith , K. C. & Dworetsky , M. M. 1993, , 274, 335

    1993

  72. [80]

    Theodosiou , C. E. 1989, , 39, 4880

    1989

  73. [81]

    R., Cooper , J., & Smith , E

    Vidal , C. R., Cooper , J., & Smith , E. W. 1973, , 25, 37

    1973

  74. [82]

    M., Adelman , S

    Wahlgren , G. M., Adelman , S. J., & Robinson , R. D. 1994, , 434, 349

    1994

  75. [83]

    E., Vaughan , Jr., A

    White , R. E., Vaughan , Jr., A. H., Preston , G. W., & Swings , J. P. 1976, , 204, 131

    1976

  76. [84]

    E., Lawler , J

    Wickliffe , M. E., Lawler , J. E., & Nave , G. 2000, J. Quant. Spectrosc. Radiat. Transfer, 66, 363, (WLN)

    2000

  77. [85]

    L., Fuhr , J

    Wiese , W. L., Fuhr , J. R., & Deters , T. M. 1996, Atomic transition probabilities of carbon, nitrogen, and oxygen : a critical data compilation

    1996

  78. [86]

    P., Lawler , J

    Wood , M. P., Lawler , J. E., Den Hartog , E. A., Sneden , C., & Cowan , J. J. 2014, , 214, 18

    2014

  79. [87]

    Woolf , V. M. & Lambert , D. L. 1999, , 521, 414

    1999

  80. [88]

    S., Lundberg , H., et al

    Zhiguo , Z., Li , Z. S., Lundberg , H., et al. 2000, Journal of Physics B Atomic Molecular Physics, 33, 521, (ZLLZ)

    2000

  81. [89]

    1999, The European Physical Journal D - Atomic, Molecular, Optical and Plasma Physics, 7, 499

    Zhiguo, Z., Zhongshan, L., & Zhankui, J. 1999, The European Physical Journal D - Atomic, Molecular, Optical and Plasma Physics, 7, 499

    1999

Pith tools

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