species provides a coherent framework for spectral and photometric analysis of directly imaged planets and brown dwarfs. This page contains a short overview of the various data that are supported and some of the tools and features that are provided.

Supported data

The toolkit benefits from publicly available data resources such as photometric and spectral libraries, atmospheric model spectra, evolutionary tracks, and photometry of directly imaged, low-mass objects. The relevant data are automatically downloaded and added to the HDF5 database, which acts as the central data storage for a workflow. All data are stored in a fixed format such that the analysis and plotting tools can easily access and process the data.

The following data and models are currently supported:

Atmospheric model spectra

Spectral libraries

Photometric libraries

Evolutionary tracks


Dust extinction

Please give credit to the relevant references when using any of the external data in a publication. More information is available on the respective websites. Support for other datasets can be requested by creating an issue on the Github page.

Analysis tools

After adding the relevant data to the database, the user can take advantage of the suite of tools that have been implemented for spectral and photometric analysis. Here is an incomplete list of available features and tools:

  • Converting between fluxes and magnitudes (see SyntheticPhotometry).

  • Calculating synthetic photometry spectra (see SyntheticPhotometry).

  • Interpolating and plotting model spectra (see ReadModel and plot_spectrum()).

  • Grid retrievals with Bayesian inference (see FitModel and plot_mcmc).

  • Comparing a spectrum with a full grid of model spectra (see compare_model()).

  • Free retrievals with a frontend for petitRADTRANS (see AtmosphericRetrieval).

  • Creating color-magnitude diagrams (see ReadColorMagnitude and plot_color_magnitude).

  • Creating color-color diagrams (see ReadColorColor and plot_color_color).

  • Computing synthetic fluxes from isochrones and model spectra (see ReadIsochrone)

  • Flux calibration of photometric and spectroscopic data (see ReadCalibration, FitModel, and FitSpectrum).

  • Empirical comparison of spectra to infer the spectral type (see spectral_type()).

  • Analyzing emission lines from accreting planets (see EmissionLine).