Circumstellar density (top panel) and velocity (bottom panel) as a function of the distance from the outer boundary of our 12.6 M_⊙ single star RSG model 1 year prior to collapse. Its radius as derived by MESA is R = 897 R_⊙, and its wind mass outflow rate 3.3 × 10⁻⁶ M_⊙ yr⁻¹. The three dashed lines correspond to an isothermal subsonic atmosphere which includes various turbulent pressure contributions (see legend), which transition to a β-wind law with β = 5 and v_∞ = 25 km s⁻¹ when the local velocity reaches the sound speed (marked by a thick dot). The purple line corresponds to the fiducial turbulent pressure-driven RSG wind model of Kee et al. (2021), while the green line represents the semi-empirical outflowing atmosphere model of González-Torà et al. (2023) which fits the interferometric observations of the Galactic nearby RSG HD 95687. The blue area represents the constraints for the circumstellar density distribution derived by Yaron et al. (2017) based on the flash-spectroscopy of the ordinary Type IIP SN 2013fs. The vertical shading marks the typical orbital separation found in our binary models at core collapse.