The grids of the NLTE abundance corrections for lines of Ca I are given in the following files.

The files have similar structure and include equivalent widths EW_LTE (mA) and NLTE abundance corrections: NLTE - LTE (dex). The NLTE corrections are provided for lines with EW(LTE) < 3 mA.
Everywhere, we use MARCS model atmospheres.

1. Ca1_NLTE_corrections_5000-6500_g2.5-4.5.dat
for 28 lines of Ca I, wavelength (in nm).
Teff = 5000 to 6500~K, with a 250 K step, log g = 2.5 to 4.5, with a 0.5 step, [Fe/H] = 0, -0.5, -1.0, -1.5, -2.0, -2.5, -3.0, -4.0. 
Collisions with H I atoms are treated following Mitrushchenkov et al. (2017, J. Chem. Phys.,
146, 014304).

When using the data from Ca1_NLTE_corrections_5000-6500_g2.5-4.5.dat in your research, cite please
Mashonkina, Sitnova, Belyaev, 2017, A&A, 605, A53.

2. Ca1_NLTE_corrections_4000-5000_g0.5-2.5.dat
for 28 lines of Ca I, wavelength (in nm).
Teff = 4000 K to 5000~K, with a 250 K step, log g = 0.5 to 2.5, with a 0.5 step, [Fe/H] = 0, -1.0, -2.0, -2.5, -3.0, -3.5, -4.0. 
For [Fe/H] = -3.5, we use the model atmospheres obtained by an interpolation with the FORTRAN-based routine written by Thomas Masseron (http://marcs.astro.uu.se).
Collisions with H I atoms are treated following Mitrushchenkov et al. (2017, J. Chem. Phys.,
146, 014304).

When using the data from Ca1_NLTE_corrections_4000-5000_g0.5-2.5.dat in your research, cite please
Mashonkina, Sitnova, Pakhomov, 2016, Astronomy Letters, 42, 606.