Data on Stark Broadening of Sn II Spectral Lines
, Magdalena D. Christova 3, Cristina Yubero 4 and Sylvie Sahal-Bréchot 2
Round 1
Reviewer 1 Report
Comments and Suggestions for AuthorsThe Stark broadening data presented in this article are interesting because they are particularly significant for hot and dense stars like white dwarfs. However, a general background introduction is required for readers with different backgrounds to follow.
The manuscript is too focused on the topic of Stark broadening data, and the explanation of the scientific issues in the manuscript are not very clear, which affects the reading and reception by more readers later on. Therefore, I suggest a major revision of the manuscript with addressing the following comments:
1. Clearly describe the scientific issues and relevant research background in the introduction.
2. Please add explanations and applications of the equations, preferably with charts and graphs, so that ordinary readers can also understand the scientific paper.
3. It is difficult to verify that the author's findings are meaningful and accurate, although it might be useful.
4. The conclusion section is also very broad and lacks specificity.
Author Response
1. Clearly describe the scientific issues and relevant research background in the introduction.
This manuscript is Data descriptor and this is in detail described in the article (Ref [29] in the manuscript). So, we repeted parts of the Ref. [29] from original version, paraphrasing, trying to diminish self plagiarism. Now the first sentence in the first paragraph of introduction:
Data for Stark broadening of spectral lines are needed for analysis, investigation
and diagnostics of various plasmas in astrophysics, laboratory, physics and technology.
is now similarly as in the Ref. [29]:
Data for Stark broadening of spectral lines are needed for a number of
different scientific issues as e.g. for stellar [1,2], laboratory [3,4],
fusion [5,6], and laser produced plasma research, modelling and di-
agnostics [7–9], for development of lasers [2,10,11] and for investigation and optimization of various plasmas in technology [12], as e.g. for welding, melting and piercing of metals by lasers and, for plasma light sources [2,13].
and 13 new references have been added:
[1] Beauchamp A, Wesemael F F, Bergeron P. Spectroscopic studies of db white
dwarfs: improved stark profiles for optical transitions of neutral helium.
Astrophys J Suppl Ser 1997;108:559–73.
[2] Dimitrijević MS, Sahal-Bréchot S. On the application of stark broadening data
determined with a semiclassical perturbation approach. Atoms 2014;2:357–77.
[3] Konjević N. Plasma broadening and shifting of non-hydrogenic spectral lines:
present status and applications. Phys Rep 1999;316:339–401.
[4] Torres J, van de Sande MJ, van der Mullen JJAM, Gamero A, Sola A. Stark
broadening for simultaneous diagnostics of the electron density and temperature
in atmospheric microwave discharges. Spectrochim Acta B 2006;61:58–68.
[5] Griem HR. Plasma spectroscopy in inertial confinement fusion and soft x-ray
laser research. Phys Fluids 1992;4:2346–61.
[6] Iglesas E, Griem HR, Welch B, Weaver J. UV line profiles of B V from a 10-Ps
KrF-laser-produced plasma. Astrophys Space Sci 1997;256:327–31.
[7] Gornushkin IB, King LA, Smith BW, Omenetto N, Winefordner JD. Line broad-
ening mechanisms in the low pressure laser-induced plasma. Spectrochim Acta
1999;54:1207–17.
[8] Nicolosi P, Garifo L, Jannitti E, Malvezzi AM, Tondello G. Broadening and self-
absorption of the resonance lines of H-like light ions in laser-produced plasmas.
Nuovo Cimento B 1978;48:133–51, Nuovo Cimento B, 48 133.
[9] Sorge S, Wierling A, Röpke G, Theobald W, Sauerbrey R, Wilhein T. Diagnostics
of a laser-induced dense plasma by hydrogen-like carbon spectra. J Phys B
2000;33:2983–3000.
[10] Wang JS, Griem HR, Huang YW, F. Böttcher F. Measurements of line broadening
of B V Hα and Lδ in a laser-produced plasma. Phys Rev A 1992;45:4010–4.
[11] Csillag L, Dimitrijević MS. On the Stark broadening of the 537.8 nm and
441.6 nm Cd + lines excited in a hollow cathode laser discharge. Appl Phys B
2004;78:221–3.
[12] Yilbas BS, Patel F, Karatas C. Laser controlled melting of H12 hot-work tool steel
with B 4 C particles at the surface opt. Laser Technol 2015;74:36–42.
[13] Hoffman J, Szymański Z, Azharonok V. Plasma plume induced during laser
welding of magnesium alloys PLASMA. In: Sadowski J, et al., editors. Int. Conf.
on Research and Applications of Plasmas; 3rd German-Polish Conf.on Plasma
Diagnostics for Fusion and Applications; 5th French-Polish Seminar on Thermal
Plasma in Space and Laboratory (AIP Cof. Proc.) 812(Opole - Turawa (Poland),
6–9). 2005, p. 469–72.
Concerning the "relevant research background" we gave this in detail in Ref. [29]. Here, we enlarged the corresponding paragraph, so that instead of:
About great interest for the Stark broadening parameters for Sn II witness and a relatively large number of experiments \cite{Mi79, La83b, Pu85, Dj90, Dj92, Ma99, Dj06, Al08, Sc20}. Critical comments of some of them may be found in Refs. \citep{Ko02, Le09}. We note that several calculations also exist \cite{Bl17, He80, Ko00, Co06, La83}.
We put:
About great interest for the Stark broadening parameters for Sn II witness and a relatively large number of experiments \cite{Mi79, La83b, Pu85, Dj90, Dj92, Ma99, Dj06, Al08, Sc20}. Critical comments of some of them may be found in Refs. \citep{Ko02, Le09}. We note that several calculations also exist. In Ref. \cite{Bl17}
the semiclassical method has been employed, in Refs. \cite{He80, Ko00, Co06}
different variants of semiempirical method were used, and in Ref. \cite{La83}, in order to estimate
Stark broadening parameters, regularities and systematic trends were considered.
2. Please add explanations and applications of the equations, preferably with charts and graphs,
so that ordinary readers can also understand the scientific paper.
In the references cited in the article the used theory is described in detail:
Sahal--Br\'echot, S. Impact Theory of the Broadening and Shift of Spectral Lines due to Electrons and Ions in a Plasma. {\it Astron. Astrophys.} {\bf 1969}, {\it 1}, 91--123.
Sahal--Br\'echot, S. Impact Theory of the Broadening and Shift of Spectral Lines due to Electrons and Ions in a Plasma (Continued). {\it Astron. Astrophys.} {\bf 1969}, {\it 2}, 322--354.
Sahal-Br\'echot, S.; Dimitrijevi\'c, M.S.; Ben Nessib, N. Widths and Shifts of Isolated Lines of Neutral and Ionized Atoms Perturbed by Collisions with Electrons and Ions: An
Outline of the Semiclassical Perturbation (SCP) Method and of the Approximations Used for the Calculations. {\it Atoms} {\bf 2014}, {\it 2}, 225--252.
In more than hunderd papers are given basic formulae, more or less in detail. Nowhere there are charts and grafs. If Reviewer describe precisely what charts and grafs he want we will do them.
3. It is difficult to verify that the author's findings are meaningful and accurate, although it might be useful.
We added the following text at the end of Sect. 3:
In the ref. [29] of original version, the accuracy of obtained results is checked by comparison with existing experimental and theoretical data. Theoretical error of the semiclassical perturbation method is estimated to be arround 20\% in the case of simple spectra. For a more complex spectrum as Sn II, we assume that it is arround 30\%.
4. The conclusion section is also very broad and lacks specificity.
At the end we added:
We also underline that excellent
targets for optimal laser-induced plasma formation are the metal elements from
the fifth period of the periodic table where tin belongs.
Also, according to the suggestion of Reviewer 3, we mentioned and the importance of obtained results for hot subdwarfs.
Reviewer 2 Report
Comments and Suggestions for Authors
This manuscript reports the emission line broadening characteristics of Sn(II) ions due to their interactions with electrons, protons and ionized helium. This work provides useful results to the realms of photonics, materials science and physics for the insights of spectral line broadening. As such, I am in favor of its publication in Data, however there are numerous issues that need to be properly addressed before it can be formally accepted for publication.
1. Authors have already published a nearly the same paper elsewhere as: Milan S. Dimitrijević et al. Stark broadening of Sn II spectral lines. Journal of Quantitative Spectroscopy and Radiative Transfer 2025, 330, 109241. What is the relationship and difference between this paper and the currently submitted work? Authors should exemplify. Authors also didn’t cite this paper as a source.
2. Shouldn’t authors plot out all the width and shift results of Sn(II) spectral lines and place the figures in the main text? Or at least authors should plot out the most representative ones and include the rest as supplementary data.
3. Out of the optical and physical features of Sn(II) ions, Sn(II) are very unstable especially in environments with oxygen and water.[1-3] Authors are expected to discuss the relevant perspectives of these ions in such chemical environments, and how will these environmental stresses affect the spectral line features.
References
1. Gong, J. et al. Suppressed Oxidation and Photodarkening of Hybrid Tin Iodide Perovskite Achieved with Reductive Organic Small Molecule. ACS Appl. Energy Mater. 2021, 4(5), 4704-4710.
2. Hu, M. et al. Antioxidative solution processing yields exceptional Sn(II) stability for sub-1.4 eV bandgap inorganic perovskite solar cells. J. Energy Chem. 2022, 72, 487-494.
3. Kong, L. et al. Revealing the Universal Pressure-Driven Behavior of Hybrid Halide Perovskites and Unique Optical Modifiability in Extremely Soft 2D Tin-Based System. Adv. Funct. Mater. 2024, 34(46), 2414437.
Author Response
We are grateful to reviewer for his efforts to improve our manuscript.
1. Authors have already published a nearly the same paper elsewhere as: Milan S. Dimitrijević et al.
Stark broadening of Sn II spectral lines. Journal of Quantitative Spectroscopy and Radiative Transfer, 2025, 330, 109241. What is the relationship and difference between this paper and the currently submitted work? Authors should exemplify. Authors also didn’t cite this paper as a source.
All this is explained in the paper in the last paragraph of Introduction and the mentioned paper is cited as the article (see Ref. 29 in previous version). The last paragraph of the Introduction is:
With the help of the semiclassical perturbation theory [26–28], we calculated Stark
widths and shifts for 44 Sn II spectral lines [29], broadened by collisions with electrons, pro-
tons and He II ions, for a grid of temperatures and electron densities. Detailed explanation
f calculations, analysis of obtained results, their comparison with existing experimental
and theoretical data and investigation of the influence of Stark broadening in stellar atmo-
spheres are given in Ref. [29]. In [29] are also data for perturber density of 10 15 cm − 3 and
temperature values: 5 000, 10 000, 20 000, 30 000, 50 000 and 100 000 K, in tabular form.
Here, in Supplement material, data for perturber densities from 10 14 cm − 3 , up to 10 20 cm − 3 ,
are given on line, in computer readable form.
The Reference [29] of previous version is the reference mentioned in the Reviewer's sentence:
"Authors also didn’t cite this paper as a source."
The Reference 29 is just this source:
Dimitrijevi ́c, M.S.; Christova, M.D.; Yubero, C.; Sahal-Bréchot, S. Stark broadening of Sn II spectral lines. J. Quant. Spectrosc. Radiative Transfer 2024, 330, 109241.
2. Shouldn’t authors plot out all the width and shift results of Sn(II) spectral lines and place the figures in the main text? Or at least authors should plot out the most representative ones and include the rest as supplementary data.
The data are already included as Supplementary data as Tables from S1-14 up to S7-20. All analyzes and figures are in Ref. [29 of previous version]. This manuscript is Data Descriptor and provides on-line data, their explanation and how to use it.
3. Out of the optical and physical features of Sn(II) ions, Sn(II) are very unstable especially in environments with oxygen and water.[1-3] Authors are expected to discuss the relevant perspectives of these ions in such chemical environments, and how will these environmental stresses affect the spectral line features.
References
1. Gong, J. et al. Suppressed Oxidation and Photodarkening of Hybrid Tin Iodide Perovskite Achieved with Reductive Organic Small Molecule. ACS Appl. Energy Mater. 2021, 4(5), 4704-4710.
2. Hu, M. et al. Antioxidative solution processing yields exceptional Sn(II) stability for sub-1.4 eV bandgap inorganic perovskite solar cells. J. Energy Chem. 2022, 72, 487-494.
3. Kong, L. et al. Revealing the Universal Pressure-Driven Behavior of Hybrid Halide Perovskites and Unique Optical Modifiability in Extremely Soft 2D Tin-Based System. Adv. Funct. Mater. 2024, 34(46), 2414437.
The present data are for stellar spectra and atmospheres modelling where environment is hydrogen and helium and not oxygen and water. Other field of interest is diagnostics of laser-induced plasmas for high-order harmonics generation in ablated materials of the fourth group metals. Oxygen and water here are not of interest as well as the mentioned references.
Reviewer 3 Report
Comments and Suggestions for AuthorsThis is an interesting work introducing and providing open-access data on Stark broadening of Sn II spectral lines for interest in astrophysics and laser-induced plasma. It follows a harder paper from the same authors but the originality of this article is that it provides computer-readable data tables as supplementary materials for a larger grid of conditions. I recommend this paper for publication, almost as it is. I only propose to add another potential interest for these lines in the abstract/introduction/conclusion (please see below).
Lines 22-26 :
In your introduction, you could also mention a potential application for hot subdwarfs in addition to white dwarfs. Actually, through a recent collaboration, I am aware that such heavy elements have also recently been observed in hot subdwrafs, in particular Sn. I don't think Sn II has been observed so far in such objects, but since you also mention the observation of Sn I lines, I think it could be useful to mention the observation of Sn in hot subdwarfs as well and the potential interest in this regards (which would even more strengthen the interest for such Sn lines, thus the interest of this work). Here are some recent references (from the same group) you could mention: Dorsch et al., A&A 630, A130 (2019)
Dorsch et al., A&A 643, A22 (2020)
Dorsch et al., A&A 653, A120 (2021)
The potential interest of Sn lines for hot subdwarfs could thus also be mentioned in the abstract (line 6) and conclusion (line 93).
Author Response
We are grateful to Reviewer for the improvement of our article.
1. In your introduction, you could also mention a potential application for hot subdwarfs in addition to white dwarfs.
...Here are some recent references (from the same group) you could mention:
Dorsch et al., A&A 630, A130 (2019)
Dorsch et al., A&A 643, A22 (2020)
Dorsch et al., A&A 653, A120 (2021)
At the end of second paragraph in Introduction we added:
We note as well that the abundance of tin in HZ 44 and HD 127493, hot subdwarfs of sdO type, has been determined using Sn III and Sn IV spectral lines \cite{Do19}. Sn IV lines have been observed and in spectra of He-sdOB stars Feige 46 and LS IV-14$^o$116 \cite{Do20}
Also, we added references:
Dorsch, M.; Latour, M.; Heber, U. Heavy metals in intermediate He-rich hot subdwarfs: the chemical composition of HZ 44 and HD 127493. {\it Astron. Astrophys.} {\bf 2019}, {\it 630}, A130.
Dorsch, M.; Latour, M.; Heber, U.; Irrgang, A.; Charpinet, S.; Jeffery, C. S. Heavy-metal enrichment of intermediate He-sdOB stars: the pulsators Feige 46 and LS IV-14$^o$116 revisited. {\it Astron. Astrophys.} {\bf 2020}, {\it 643}, A22.
In the third reference, Dorsch et al., A&A 653, A120 (2021), there is no mention of lines or ionization stage of tin but only tin is mentioned so that we did not included it
2. The potential interest of Sn lines for hot subdwarfs could thus also be mentioned in the abstract (line 6)
We added this so that: for example for white dwarfs, and for modelling of their atmospheres.
is now: for example for white dwarfs, hot subdwarfs, and for modelling of their atmospheres.
3. and conclusion (line 93).
We added this so that: ...dense stars like white dwarfs, but also...
is now:
...dense stars like white dwarfs and hot subdwarfs, but also
Round 2
Reviewer 1 Report
Comments and Suggestions for AuthorsIt can be accepted in the present form.
Reviewer 2 Report
Comments and Suggestions for AuthorsThis manuscript was previously reviewed, and authors have properly addressed all of my comments and concerns. It can now be accepted for publication.
