Plotting scripts for the genetically modified merger history study of globular clusters

Last reviewed: v1.0.1

A set of scripts and a repository of reduced data to reproduce the figures in the study of globular cluster (GC) formation, evolution, and destruction using genetically modified initial conditions (O. Newton et al., 2025).

This README file is located in the root directory of the plotting scripts package. All plotting scripts should be executed from here.

1.0 Installation

1.1 Pre-installation dependencies

This package uses the cairo graphics library. In particular, as of this release it requires

bash cairo >= 1.15.10

For relevant information about the current cairo dependencies please review the Pycairo package documentation.

In most cases cairo can be installed using:

Ubuntu

bash (sudo) apt-get update (sudo) apt-get install libcairo2-dev pkg-config

macOS

bash brew install cairo pkg-config

1.2 Package installation

Once you have installed cairo, this plotting package can be installed by cloning it from the github repository:

bash git clone git@github.com:Musical-Neutron/gc-gmics.git

It is recommended to create a clean virtual environment prior to installation. Once that is done the github repository can be installed by running the following:

bash cd gc-gmics pip install .

1.3 Tests

If you plan to review the package test suite, run the following from the package root directory:

bash pip install .[test] pytest

2.0 Configuration (settings.yaml)

Key settings in the repository are configured using the settings.yaml file. Some relevant settings are discussed below.

2.1 Core configuration

• Data Management:

  • data_dir defines the base directory where relevant data are stored.
  • Relevant observational data sets, set under Observations, are also stored in data_dir.

• Analysis settings:

  • gc_mass sets the minimum globular cluster mass, in units of solar masses.
  • cluster_mass_limit sets the mass (in solar masses) below which clusters are not tracked. The default reflects the settings with which the simulations were run.

2.2 Output control

• Printing

  • print_property_list specifies which properties will appear in terminal outputs when called by printpaperresults.py. The full list of available properties is provided in Property dictionary.

• Plotting

  • individual_panels specifies whether figure panels will also be created and saved as independent figures alongside the main ones. Default: False.

2.3 Visualisation

In addition to providing a complete list of available galaxy properties, the Property dictionary controls plot formatting:

• ylim sets the y-axis lower and upper limits. ~ is parsed as None when the settings are read.
• yscale sets the scale of the y-axis (linear or log-scale).
• ylabel enables the customisation of the y-axis label. LaTeX can be provided if the appropriate packages are installed.
• printlabel specifies how this property will appear when printed to screen.

Changes to settings.yaml are read at script runtime.

3.0 Scripts

There are seven scripts that can be executed independently:

Script name | Figure | Description :--- | :---: | :--- fig02keygalaxyproperties.py | Fig. 2 | Plots the halo mass, M₂₀₀; stellar mass, M; and mass in GCs, *M_GC vs. lookback time, t_lb fig03gasbhproperties.py | Fig. 3 | Plots the star formation rate, SFR; mass of star-forming gas, M_SF; and the central black hole mass, M_SMBH vs. t_lb. fig04z0massfunction.py | Fig. 4 | Plots the z=0 and birth mass functions of all clusters that survive to z=0. Note that the latter is averaged over time and is not equivalent to the initial cluster mass function. fig05ratesofchange.py | Fig. 5 | Plots the GC formation rate, GCFR; GC destruction rate, GCDR; and the net change in GC mass, dM_GC/dt vs. t_lb. fig0607gcproperties.py | 6 & 7 | Plots the stellar and GC birth pressures; M_c,*; and the cluster formation efficiency, $\Gamma$ vs. t_lb. Also plots the specific frequency, T_N; and the specific mass, S_M vs. t_lb. fig08fhalo.py | Fig. 8 | Plots the fraction of mass in halo stars contributed by the destruction of star clusters. printpaperresults.py | | Prints information relevant to the paper to stdout.

There is also a master script, runallscripts.py, that will run all of the above scripts when executed. This produces .svg and .pdf versions of each figure in the paper.

3.1 Supplementary scripts

• common_functions.py: A set of functions common to more than one of the main scripts.
• process_data.py: Contains classes and functions to handle basic processing of data.
• settings.py: Contains classes and functions to read in settings from settings.yaml.

4.0 Data

The data directory contains all files necessary to reproduce the figures in the paper. There are nine files containing reduced data from the simulations produced for this work, and seven files containing relevant observational data:

4.1 Simulation data

The following files contain data from simulations produced in this work.

File name | Figures needed for :--- | :--- suppressedmgc100000_data.hdf5 | All except Figs 4 & 8 organicmgc100000_data.hdf5 | All except Figs 4 & 8 enhancedmgc100000_data.hdf5 | All except Figs 4 & 8 suppressednoBHmgc100000data.hdf5 | Fig. 3 organicnoBHmgc100000data.hdf5 | Fig. 3 enhancednoBHmgc100000data.hdf5 | Fig. 3 suppressedz0gc_properties.hdf5 | Figs 4 & 8 organicz0gc_properties.hdf5 | Figs 4 & 8 enhancedz0gc_properties.hdf5 | Figs 4 & 8

4.2 Observational data

File name | Figures needed for | Citation | Notes :--- | :---: | :--- | :--- caldwell2009old_clusters.csv | Fig. 4 | Caldwell et al. (2009) caldwell2009intermediate_clusters.csv | Fig. 4 | Caldwell et al. (2009) caldwell2009young_clusters.csv | Fig. 4 | Caldwell et al. (2009) caldwell2011logMstar_FeH.csv | Fig. 4 | Caldwell et al. (2011) baumgardt2019mw_gcs.csv | Fig. 4 | Baumgardt et al. (2019) | Data retrieved from https://people.smp.uq.edu.au/HolgerBaumgardt/globular/. hunt2024NMbins.csv | Fig. 4 | Hunt et al. (2024, fig. 17) horta2021fGC.csv | Fig. 8 | Horta et al. (2021)

5.0 Citations

This code and the accompanying data are freely available.

5.1 If you use this code or derivative work

• O. Newton et al. (2025)
• O. Newton (2025)

5.2 If you use these data, a derivative work, or results thereof

• O. Newton et al. (2025)

6.0 Contact

If you have any questions or would like help in using the scripts, please email:

onewton 'at' cft.edu.pl