NLTE abundance corrections (dex) for the selected lines in the stellar parameter range characteristic of very metal-poor stars

IonN linesWavelength, ATeff, Klog g[Fe/H][X/Fe]
Ba II = Ba2 54554.030 .. 6496.9004000 .. 65000.5 .. 5.0-5.0 .. -2.0-1.5 .. 0.5
Ca I = Ca1 284226.728 .. 6717.6814000 .. 65000.5 .. 5.0-5.0 .. -2.0 0.0 .. 0.4
Ca II = Ca2 43706.030 .. 8662.1404000 .. 65000.5 .. 5.0-5.0 .. -2.0 0.0 .. 0.4
Eu II = Eu2 113724.930 .. 6645.0604000 .. 57500.5 .. 3.0-3.0 .. -2.0-0.5 .. 1.5
Fe I = Fe12623392.305 .. 6653.8504000 .. 65000.5 .. 5.0-5.0 .. -2.0 0.0 .. 0.0
Mg I = Mg1 153829.355 .. 6319.4904000 .. 65000.5 .. 5.0-5.0 .. -2.0 0.4 .. 0.4
Na I = Na1 85682.640 .. 5895.9204000 .. 65000.5 .. 5.0-5.0 .. -2.0-0.6 .. 0.6
Sr II = Sr2 24077.710 .. 4215.5404000 .. 65000.5 .. 5.0-5.0 .. -2.0-1.5 .. 1.0
Ti II = Ti2 543380.279 .. 6680.1304000 .. 65000.5 .. 5.0-4.0 .. 0.0 0.3 .. 0.3
Zn I = Zn1 72138.573 .. 6362.3384000 .. 65000.5 .. 5.0-5.0 .. 0.5 0.0 .. 0.0
Zn II = Zn2 22025.484 .. 2062.0014000 .. 65000.5 .. 5.0-5.0 .. 0.5 0.0 .. 0.0

Notes:
  • NLTE calculations were performed with the grid of MARCS model atmospheres.
  • For Ti II, Fe I, and Eu II, collisions with H I atoms were treated with the Drawinian rates scaled by a factor of S_H = 1, 0.5, and 0.1, respectively.
  • NLTE abundance correction for given Teff, log g, [Fe/H], [X/Fe] is obtained by linear interpolation in the grids.

In case of using these data in your studies, cite please :
This database:Mashonkina, Pakhomov, Sitnova, et al., 2023, MNRAS, 524, 3526
Na I: Alexeeva, Pakhomov, Mashonkina, 2014, Astron. Lett., 40, 406
Mg I: Mashonkina, 2013, A&A, 550, A28
Ca I: Mashonkina, Sitnova, Belyaev, 2017, A&A, 605, A53
Ca II: Neretina, Mashonkina, Sitnova, et al., 2020, Astron. Lett., 46, 621
Ti II: Sitnova, Mashonkina, Ryabchikova, 2016, MNRAS, 461, 1000 (SH = 1.0)
Fe I: Mashonkina, Gehren, Shi, et al., 2011, A&A, 528, A87 (SH = 0.5)
Zn I-II: Sitnova, Yakovleva, Belyaev, Mashonkina, 2022, MNRAS, 515, 1510
Sr II: Mashonkina, Pakhomov, Sitnova, et al., 2022, MNRAS, 509, 3626
Ba II: Mashonkina, Belyaev, 2019, Astron. Lett., 45, 341
Eu II: Mashonkina, Gehren, 2000, A&A, 364, 249 (S_H = 0.1)

Bibliography of model atoms for non-LTE line-formation calculations is available on https://non-lte.com/bibliography.html

Select the chemical species, indicate the line, indicate Teff, log g, [Fe/H], [X/Fe].

Species Wavelength Teff log g [Fe/H] [X/Fe]
 

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List or upload stellar atmosphere parameters and [X/Fe].
One star per row, format: Teff log g [Fe/H] [X/Fe].





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Upload your list of lines. Wavelengths (in A) have to be indicated as given in the linelist for the corresponding chemical species (see the Table).
One line per row, format: Species Wavelength(A) [X/Fe] 

Fe1 5171.610 0  
Ca2 8498.0195 0.2
Ti2 4571.968 0.3

Choose linelist Teff log g [Fe/H]