This package includes plot and particle files from the 22 simulations described
in Table 2 of Hill, Mac Low, Gatto, & Ibanez-Mejia (resubmitted to AAS Journals
on June 12, 2018). All plot files are from the 200 Myr timestep. The files are
output by simulations conducted using Flash version 4.2 with the implementation
described in the paper. The files are in the HDF5 format. All values are in
Gaussian cgs units.

Contact the corresponding author Alex S Hill at ashill@astro.ubc.ca (as of 2018)

There is an example python script (example_plot_script.py) which reads the data
and generates a few simple plots. This script is a simplified version of the
code used to produce Figures 1-4 and 7 in the paper. The script uses the yt
visualization package (Turk et al 2011; http://yt-project.org).

The plot files all contain the following fields:

'dens': gas density in units of g/cm^3. The simulations were conducted assuming
    a mean gas phase mass per hydrogen atom mu=1.375; we divided by 1.375 times
    the mass of a proton to convert to 1/cm^3.
'temp': temperature in K
'velx', 'vely', 'velz': x, y, and z components of bulk velocity in cm/s

Magnetized (bx5) models also include:
'magx', 'magy', 'magz': x, y, and z components of magnetic field strength B in G

The particle files include the positions of superbubbles which were active at
200 Myr.

The file names identify the simulation and midplane resolution; see Tables 1 and
2 of Hill et al (2018). The fields in the file name have the following meanings:

sn: total supernova rate (Myr^-1 kpc^-2)
smd: surface mass density (0.1 msun pc^-2)
bx: initial x-component of the magnetic field (microGauss); zero unless
    specified
nigm: approximate log of IGM density (cm^-3); -7 unless specified
pe: photoelectric heating rate (1E-27 erg s^-1)
pc: midplane resolution (pc)