Review Reports

Round 1

Reviewer 1 Report

Comments for author File: Comments.pdf

Author Response

Reviewer 1
We are very grateful to reviewer for careful reading of our manuscript and valuable remarks which will improve our work.

Reviewers remarks and our answers:

1. Line 19, define “DO”, “DB” and “DA”.

Answer:
This part is now:
 The influence of Stark broadening has been considered in DO (D stands for Degenerate
- The atmosphere of these stars is abundant with helium, which is indicated by the presence of ionized helium (He II) in their spectral lines), DB (they have atmosphere of helium, which is indicated by the presence of neutral helium (He I) in their spectral lines)(see e. g. \citet{Di21b}), DA (with atmospheres of hydrogen) dwarfs (see e.g. \citet{Ma20a}) and in B subdwarfs (see e.g. \citet{Ha17}). 

2. Line 22, change “zinc” by “Zinc”.

Answer:
We do not understand this remark. Within a sentence "zinc" is not capitalized. In article,
"zinc" is mentioned many times as "zinc" and not "Zinc" as well as other elements like "hydrogen" and "helium". Why capitalize only in this particular place?  

3. Line 24 “which” by “whic”

Answer: Corrected, thanks

4. Remove an equal in Eq. 2.

Answer: Corrected, thanks

5 Line 132. Change, “is” by “are”

Answer: We do not understand this remark. There is no "is" on line 132. The sentence is:
"In Fig. 2  are presented their Stark and Doppler widths..." and "are...widths" is correct.

6. Line 44, a space is needed after the dot.

Answer: This is corrected on line 144. Thanks

7. Remove white spaces in Figures. For example, between 1e-5 and 5e-3 in Figure 1.

Answer: Corrected, thanks. Figures now look much better.

 

Reviewer 2 Report

Up to now  there is no experimentally obtained data for Zn III spectral lines although zinc is significant for examination of the star formation rate, the chemical evolution of the Universe at high redshifts.  Modified semiempirical method proposed earlier the  team led by Dr.Dimitrijevic ;has been applied. The results for Stark FWHM due to collisions with electrons for Zn III

 multiplets  and belonging to two s-p supermultiplet  and two transition arrays 4s-4p and 4p-4d for an electron density of 10^-17  cm^3  and plasma temperatures of 5 000–100 000K are presented  in the Tabel format. The publication of the paper will be useful for  analysis and synthesis of Zn III lines in stellar spectra,

 opacity calculations, investigation, modelling and diagnostics of laboratory plasmas.

 

 

Author Response

We are very grateful to reviewer for good opinion for this work.

Reviewer 3 Report

Comments are attached.

Comments for author File: Comments.pdf

Author Response

Reviewer 3
We are very grateful to the reviewer  for valuable comments.
Here are our answers to Reviewer's comments:

1. Please use some new journals for stark broadening study in laboratory
plasma. Some examples are listed below:
Effects of N2 and O2 plasma treatments of quartz surfaces exposed to H2 plasmas
Journal of Vacuum Science & Technology A 40, 053002 (2022); https://doi.org/10.1116/6.0001896
S. G. Belostotskiy, T. Ouk, V. M. Donnelly, D. J. Economou, and N. Sadeghi, J. Appl. Phys. 107,
053305 (2010). https://doi.org/10.1063/1.3318498

Answer: We added these two references in the Introduction and literature
 
2. There is no experimental data for Zn III spectral lines. How much error
will you get by using six Zn III multiplets. What are the assumptions?
Authors need to explain more about this.

Answer:
In Sect. 3, Results, we added:
We estimate that the errors are within the limit of 40 per cent.