Toolkit used to analyze data and create plots of Illustris TNG-50 halos post-processed with the radiation transfer code CRASH to obtain the state of radiational equilibrium.
The findings are summarized in this paper.
To use the notebooks the dataframes containing the halo properties are needed. To get the dataframes please contact me under ivkos@mpa-garching.mpg.de.
These files interact directly with either the CRASH post-processing runs or TNG50 snapshot data
- build_df.py: Goes through the folder of simulation runs and creates a pandas dataframe containing the properties of the examined halos
- update_df.py: Adds several additional columns to the halo dataframe namely the ages of stellar particles in the halo as well as the gas clumping, surface stellar density and surface gas density of the central galaxy, defined to be enclosed by 0.2Rvir.
- add_metallicities.py: Adds an additional column to the dataframe containing stellar metallicities. Should be moved into update_df.py in the future
- prepare_new_runs.py: Tools for preparing a new CRASH post-processing run.
- synchronize_folders.py: Tools for moving halos from the RT simulations performed with a reduced number of stellar particles to the escape fraction calculation performed with the full set of stellar particles.
- build_radius_df.py: Deprecated code originally used to analyze the escape fraction at different distances from the halo center. Should this become necessary in the future I would recommend to change build_df.py with elements from this file.
- fix_stellar_ages.py: Deprecated code which was only used when update_df.py used the wrong stellar particles in a data frame update.
Most of these notebooks interact with the dataframe summarizing the results of the simulation and can be used idependently from the simulation runs. The exceptions arer uv_emissivity.ipynb which interacts with the TNG-50 database as well as esc_fraction.ipynb and halo_image.ipynb which require the simulation runs of the halos that need to be plotted.
- counts_histogram.ipynb: Used to create plots summarizing the halo population as seen in fig. 1 of the paper.
- esc_fraction.ipynb: A python implementation of the code used to obtain escape fractions along lines of sight and create maps of densities and escape fractions of the halo as seen in fig. 5. Note that this code requires the full density and ionization maps and therefore needs the full simulation data of a halo. To be more readable, in the future this code needs to be refactored and most of it moved to a python file.
- fesc_vs_quant.ipynb: Used for analyzing the average escape fraction as a function of different properties.
- halo_image.ipynb: Used to create projected images of halos as seen in fig. 4. This notebook needs the full halo maps and therefore also the full simulation results.
- large_radii.ipynb: Used to analyze the escape fraction as a function of distance from the halo center. Not used in the final project.
- loc_esc.ipynb: Used to analyze the effect of using different local escape fractions as seen in fig. 7 of the paper.
- median_fesc.ipynb: Used to analyze the dependence of the escape fraction as a function of stellar and halo mass, as well as to compare the escape fraction with and without dust and compare our results to literature. Figs. 2, 3 and 13 were created using this notebook.
- numerical_convergence_tests.ipynb: A number of tests to investigate the numerical convergence obtained with the source number reduction. Fig. A1 was created using this notebook.
- r_fesc.ipynb: Used to analyze the properties including the escape fraction of individual stellar particles. Used to create fig. 10.
- histograms.ipynb: Used to create 2D histograms to investigate the effect halo properties have on the escape fraction. This was used to create fig. 6. In addition, there are some tools developed to separate the two modes of escape fractions at lower stellar masses which were not utilised in the paper.
- spectra.ipynb: Used to analyze the spectral dependence of the escape fraction as seen in figs. 11 and 12.
- uv_emissivity.ipynb: Used to analyze the escaped ionizing photon density in TNG-50 given the ionizing photon escape as predicted with the CRASH radiation transfer and compare the results to literature. This was used to create figs.8 and 9 of the paper.
These notebooks contain tools to prepare and handle simulation runs and were not used for the final data analysis.
- clean_up.ipynb: Collection of short scripts to delete unnecessary files in the simulation runs in order to reduce memory usage.
- merge_sources.ipynb: Used in the preprocessing of the halo runs in particular to reduce the number of sources. Also contains a number of tests run on the results. Requires the full simulation data to work with.