MARDIGRAS

Mass-Radius DIaGRAm with Sliders (MARDIGRAS) is a visualization tool that allows simple and intuitive manipulation of mass-radius relationships (also known as iso-composition curves) using interactive sliders.

While mardigras screen captures can be implemented in your scientific work (talks, posters, communications), if you are looking for paper-quality mass-radius diagrams we recommend the use of mr-plotter.

Run the tool

Download and run

To run the program, download the repository and execute it with Python: git clone https://github.com/an0wen/MARDIGRAS cd MARDIGRAS python3 mardigras.py

Available options

mardigras can be run with the following options: 1. Choose exoplanet catalog: "NEA" or "PlanetS". python3 mardigras.py --catalog [NEA/PlanetS] Default is "NEA" (NASA Exoplanet Archive). 2. Updating the NEA catalog: python3 mardigras.py --update-nea-catalog This will print the following statement in the terminal: Catalog updated successfully and saved to ./data/catalog_exoplanets.dat 3. Updating the PlanetS catalog: Work in Progress 4. Path to catalog of targets: python3 mardigras.py --catalog-targets ./data/catalog_targets_compass.dat

Contents of v2

Interior structure models

Three curves are controlled by sliders: 1. Blue lines: Steam World model from Aguichine et al. 2025 (https://ui.adsabs.harvard.edu/abs/2025ApJ...988..186A/abstract), represents an envelope of pure water in a supercritical state, with a pure steam atmosphere on top. 2. Red lines: Gas dwarf model from Tang et al. 2025 (https://ui.adsabs.harvard.edu/abs/2025ApJ...989...28T/abstract), represents an H-He gas envelope with metallicity ranging from 1xSolar to 50xSolar. 3. Brown lines: Rocky planets model from Zeng et al. 2016 (https://ui.adsabs.harvard.edu/abs/2016ApJ...819..127Z/abstract), for terrestrial planets with variable (iron) core mass fractions.

Additionally, five static profiles from Zeng et al. 2016 are shown, from low to high radius: pure iron core, Earth-like composition, pure mantle, 50% liquid water, and 100% liquid water.

Planets catalogs

Three populations of planets are shown: 1. Exoplanets catalog (NEA or PlanetS) in the background (grey dots). 2. A smaller sample of highlighted targets (orange stars). 3. Planets of the Solar System (red symbols).

Since mardigras is a tool to infer composition based on mass and radius (and other parameters), it is critical to use actual measurements of mass and radius and avoid values that are upper/lower limits, derived from empirical mass-radius relations, or otherwise controversial. That being said, users are free to manipulate the catalogs in any way they see fit. The header can be of any length, as long as each line begins with #. The file must contain at least 7 columns separated by tabs. Extra columns will be ignored. The program can handle empty entries for mass, radius, and their error bars.

The developpers of mardigras do not take any responsibility for the scientific inaccuracies that may result from using incorrect data, implausible interior models, or from trying to explore creative scenarios that are not published in the peer-reviewed literature.

NASA Exoplanet Archive (NAE)

The NASA Exoplanet Archive (NAE) is updated using NEA's Table Access Protocol (TAP). The TAP allows to query the content of the catalog in machine readable format using a single link. Custom filters can be included in the link. The full link used in mardigras is:

https://exoplanetarchive.ipac.caltech.edu/TAP/sync?query=select+plname,plrade,plradeerr1,plradeerr2,plmasse,plmasseerr1,plmasseerr2,pleqt+from+ps+where+defaultflag=1+and+plcontrovflag=0+and+plrade+is+not+null+and+plmasse+is+not+null+and+plbmassprov='Mass'&format=tsv

The following arguments have been added to the query: - Planetary Systems "ps" database - The default flag is 1 - The controversial flag is 0 - The planet radius is not null - The planet mass is not null - The planet mass represents the actual mass, i.e., not Msini or Msini/sini - hardcoded in the script: the error on the planet mass is lower than 50%

Please refer to the NEA website for the full list and description of all catalog options.

PlanetS catalog

The PlanetS catalog is a curated catalog with precise and reliable mass and radius measurements. mardigras uses the updated version of this catalog published in Parc et al. 2024 (https://ui.adsabs.harvard.edu/abs/2024A%26A...688A..59P/abstract). This catalog is based on the NASA Exoplanet Archive, but only includes transiting planets with relative measurement uncertainties smaller than 25% in mass and 8% in radius. Each newly discovered planet is studied individually before being added to the PlanetS catalog to ensure reliability, with a special treatment of TTVs (Transit Timing Variations).

To show the PlanetS catalog, launch mardigras with the following command line argument: python3 mardigras.py --catalog PlanetS

Catalog of targets

Highlighted targets are intended for dedicated studies, discoveries, or parameter updates of a few planets, a system, or a group of planets. These planets are shown as big orange stars.

To switch between different catalogs of targets, run mardigras by specifying the path to the desired target catalog: python3 mardigras.py --catalog-targets ./data/catalog_targets_compass.dat In the command above, the highlighted targets correspond to the targets of the COMPASS program (https://compass-jwst.github.io/).

Compatibility

mardigras is developed and tested on MacOS (Retina) with Python 3.12.4. It uses the following libraries: - numpy v2.0.1 - matplotlib v3.10.0 - scipy v1.15.2

In addition to this, mardigras uses Python built-in packages requests, os, datetime, argparse and pathlib.

We strive for using simple packages to minimize compatibility issues.

Additional information about interior structure models and sliders interpretation

Zeng et al. 2016: rocky planets

The Zeng et al. 2016 model is a 4-layer interior structure model (center to surface: solid iron core, liquid iron core, lower mantle, upper mantle). It was calibrated to reproduce the interior or Earth according to the Preliminary Earth Reference Model (PREM, Dziewonski and Anderson 1981, https://doi.org/10.1016/0031-9201(81)90046-7).

The slider controls the Core Mass Fraction (CMF), which is the mass occupied by the iron core (solid+liquid). When CMF=0, the planet is 100% mantle. When CMF=1, the planet is 100% iron core. The CMF needed to reproduce the radius of the Earth is 0.325, and for Mercury it is estimated to be ~0.6.

NB: The iron core is not made of pure iron. The model is calibrated on Earth, meaning that some volatile is added to the iron to lower the density, just as on Earth.

Aguichine et al. 2025: steam worlds

The Aguichine et al. 2025 model is a 5-layer interior structure model (center to surface: iron core, lower mantle, upper mantle, H₂O envelope, H₂O atmosphere). The three core+mantle layers are calibrated to reproduce the radius of the Earth, and is based on Brugger et al. 2017 (https://ui.adsabs.harvard.edu/abs/2017ApJ...850...93B/abstract). The envelope and atmosphere is made of pure H₂O. The model is adapted to planets in post-runaway greenhouse stage (> 350 K), planets that cannot maintain water in condensed phase, and where a steam atmosphere with a supercritical water envelop forms instead. Most sub-Neptunes (~97%) are in post-runaway greenhouse stage.

This model is controled with 5 sliders: - Stellar type: M or G. Affects the properties of the steam atmosphere. - Age of the planet: planets cool down and contract with age. - Teq: equilibrium temperature of the planet. - WMF: water mass fraction. - Atmosphere top pressure: 20 mbar or 1 µbar, pressure level at which the atmosphere is assumed to be opaque (measured radius). Most telescopes measure the planetary radius a wavelength of around 1 µm. For most atmospheric compositions, the atmosphere becomes optically thick at around 20 mbar. However, it is possible to form high-alitude aerosols that will make the atmosphere opaque at a pressure level of 1 µbar. It is thus important to know 1) the telescope filter, 2) the atmosphere composition, and 3) the atmosphere microphysics to understand what radius is being measured.

Tang et al. 2024: gas dwarf

The Tang et al. 2024 model is a 6-layer interior structure model (center to surface: solid iron core, liquid iron core, solid mantle, liquid mantle, H₂-He dominated envelope, H₂-He dominated atmosphere).

This model is controled with 5 sliders: - Metallicity: 1 to 50 times solar. Changes both the atmosphere and envelope properties. In the envelope, H₂O is used as a proxy for all volatiles, and a metallicity of 50 times solar corresponds to an envelope ~40% of H₂O by mass. - Age of the planet: planets cool down and contract with age. - Teq: equilibrium temperature of the planet. - f_env: envelope mass fraction. - Atmosphere top pressure: RCB, 20 mbar or 1 µbar, pressure level at which the atmosphere is assumed to be opaque (measured radius). See above.

Credits

If you use mardigras, please give credit to the initial release: @article{Aguichine_2024, doi = {10.3847/2515-5172/ad7506}, url = {https://dx.doi.org/10.3847/2515-5172/ad7506}, year = {2024}, month = {aug}, publisher = {The American Astronomical Society}, volume = {8}, number = {8}, pages = {216}, author = {Artyom Aguichine}, title = {mardigras: A Visualization Tool of Theoretical Mass–Radius Relations in the Context of Planetary Science}, journal = {Research Notes of the AAS}, abstract = {Over the past two decades, mass–radius relations have become a crucial tool for inferring the bulk composition of exoplanets using only their measured masses and radii. These relations, often referred to as isocomposition curves, are derived from interior structure models by calculating the theoretical radius as a function of mass for a given fixed planetary composition. Each mass–radius curve can be influenced by a variety of parameters, such as planetary composition, age, and equilibrium temperature. Navigating this parameter space can be cumbersome, particularly when models or their results are not open-source. To address this challenge, I have developed MAss–Radius DIaGRAm with Sliders, a visualization tool that enables simple, fast, and interactive exploration of the parameter space that governs mass–radius relations for any given model.} }