HI column density map (units: cm^-2) for an MHD turbulent box irradiated by isotropic/beamed UV field (two files).

Description:
The UVradiation (in the LW-band) photo dissociates H2 and produces an HI layer at the cloud boundary. 
The HI column density of this layer depends on the UV intensity, gas density and dust absorption cross section.
Turbulence produces density fluctuations in the gas resulting in fluctuations in the HI column density for different lines of sight.
See Bialy, Burkhart & Sternberg (2017, ApJ 843 92) for details.

Assumed Parameters in the files
Ms=4.5 (sonic Mach number)
Ma=0.7 (Alfvenic Mach number)
I_UV=1.3 (UV intensity in Draine Units)
sigma_g=1.9e-21 cm^2 (dust absorption cross section in the Lyman-Werner band [typical for Galactic dust-to-gas ratio])
<n>=30 cm^-3 (n fluctuates such that s.t.d(n/<n>)~Ms/3 )
L_dec/LHI=0.1 (equivalent to tau_dec=~0.1, or ~10 density fluctuations along an HI column)


Cite: Bialy, Burkhart & Sternberg (2017, ApJ 843 92)