The grids of the NLTE abundance corrections for lines of Ba II are given in the following files.
Everywhere, we use MARCS model atmospheres.

1. Ba2_NLTE_corrections_4500-6500_g3.0-4.5.dat
Teff = 4500 to 6500 K, log g = 3.0 to 4.5, [Fe/H] = 0 to -3. The computations were performed with [Ba/Fe] = 0 and xi_t = 1.5 km/s. Collisions with H I atoms are treated following Belyaev, Yakovleva (2018, Mon. Not. Roy. Astron. Soc. 478, 3952).

When using the data from Ba2_NLTE_corrections_4500-6500_g3.0-4.5.dat in your research, cite please
Mashonkina, Belyaev (2019, Astron. Letters, 45, in press)

2. Ba2_NLTE_corrections_4500-4750_g0.5-2.5.dat
Teff = 4500 to 4750 K, log g = 0.5 to 2.5, [Fe/H] = 0 to -3. The computations were performed with [Ba/Fe] = 0 and xi_t = 2 km/s. Collisions with H I atoms are treated following Belyaev, Yakovleva (2018, Mon. Not. Roy. Astron. Soc. 478, 3952).

When using the data from Ba2_NLTE_corrections_4500-4750_g0.5-2.5.dat in your research, cite please
Mashonkina, Belyaev (2019, Astron. Letters, 45, 341)

The two above 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.

3. Ba2_NLTE_corrections_4500-5000_g1.0-2.5.dat
includes equivalent widths EW_LTE (mA) and NLTE abundance corrections (dex) for lines of Ba II in the metal-poor model atmospheres. All the computations were performed with xi_t = 1.8 km/s except for the log g = 4.8 model, where xi_t = 0 was adopted. Collisions with H I atoms are treated with the Drawinian rates scaled by S_H = 0.01. The NLTE corrections are provided for lines with EW(LTE) < 5 mA.

When using the data from Ba2_NLTE_corrections_4500-5000_g1.0-2.5.dat in your research, cite please
Mashonkina, Christlieb, 2014, A&A, 565, A123.