This repository contains scripts to perform all of the analysis presented in Smith, Hallman, Shull, & O'Shea (2001, ApJ, 731, 6). Star Formation Rate: figures 1, 2. Directory: star_formation_rate star_formation_rate_quick.py - calculates global star formation history from a single dataset. Creates an ascii file with columns: redshift; lookback time; comoving star formation rate density in Msun/yr/Mpc^3; number of star particles; total stellar density in Msun/Mpc^3; ratio of stellar density to critical density; metal formation rate in Msun/yr/Mpc^3; total metal density contained in stars in Msun/Mpc^3; and ratio of stellar metal density to critical density. Usage: mpirun -np <procs> python star_formation_rate_quick.py <dataset> Halo Mass Function: figure 3. Directory: halo_mass_function run_halo_finder.py - runs Parallel HOP on a single dataset. Usage: mpirun -np <procs> python run_halo_finder.py <dataset> --parallel get_halo_mass_function.py - calculates halo mass function from halo catalogs. Also, calculates the Warren mass function. Baryon Phases: figures 4, 5, 8, 9. Directory: baryon_phases sim_phase.py - calculates total baryon mass in warm, WHIM, hot, and condensed phases for all datasets. Phases are defined as: Condensed: baryon overdensity (rho/<rho>) >= 1000. All others for baryon overdensity < 1000. Warm: T <= 1e5 K WHIM: 1e5 K < T <= 1e7 K Hot: T > 1e7 K Usage: mpirun -np <procs> python sim_phase.py <sim_par_file> --parallel Note 1: the total baryon density will decrease as stars are formed. The total mass in the condensed phase is Omega_b - (Omega_warm + Omega_WHIM + Omega_Hot). Note 2: this script requires the field_utils module, available at https://bitbucket.org/brittonsmith/field_utils. Phase Flux: figures 6, 7. Directory phase_flux phase_flux.py - calculates flux of material from one phase to another for all datasets. plot_phase_fluxes.py - generates plot of total input/output of material for all phases (figure 6). plot_phase_fluxes_detail.py - generates plot of inputs and outputs to and from various phases (figure 7). Synthetic OVI Absorbers: figures 11-17, 21 (right panel) Directory: synthetic_absorbers plan_datasets.py - takes in an enzo parameter file and calculates a set of redshift outputs required to span the desired redshift interval for creating a sample of synthetic absorbers. make_light_rays.py - creates a set of 500 light rays extending from z = 0 to z = 0.4. Usage: mpirun -np <procs> python make_light_rays.py <sim_par_file> Note 1: do NOT add --parallel to this script. Note 2: to get OVI and other metal column densites, the ion_balance module is required. Please contact Britton Smith <firstname.lastname@example.org> to obtain this module. To calculate dn/dz, Omega_OVI, and average physical quantities associated with absorbers, use the light_ray_tools module, available at https://bitbucket.org/brittonsmith/light_ray_tools. Projections: figure 18. Directory: projections sim_full_projections.py - makes projections for all datasets. Usage: mpirun -np <procs> python sim_full_projections.py <sim_par_file> --parallel Note 1: to get OVI and other metal column densites, the ion_balance module is required. Please contact Britton Smith <email@example.com> to obtain this module. Note 2: image for figure 18 was produced using the plot_modifications module, available at: https://bitbucket.org/samskillman/plot_modifications. phase_profiles: figures 19, 20, 21 (left panel) Directory: phase_profiles make_phase_profiles.py - makes 2D profiles for a set of fields. Edit the profiles_2D variable to control which fields are profiled. Note: to get OVI and other metal column densites, the ion_balance module is required. Please contact Britton Smith <firstname.lastname@example.org> to obtain this module.