Simulating high-resolution cross-correlation spectroscopy for exoplanet atmospheres. Currently supports simulating IGRINS (on Gemini-S), IGRINS-2 (on Gemini-N), and CRIRES+ (on the VLT) observations of transmission and emission spectra.
You can install scope using pip:
pip install scope-astr
To install from source, run
python3 -m pip install -U pip
python3 -m pip install -U setuptools setuptools_scm pep517
git clone https://github.com/arjunsavel/scope
cd scope
python3 -m pip install -e .
You'll also need to download some data files. Currently, these data files are about 141 MB large. You can download them (to the correct directory, even!) with the following:
cd src/scope
chmod +x download_data.bash
./download_data.bash
This will create a data directory and plop the relevant files into it. You're also welcome to run the tests to
make sure everything's been installed correctly:
pytest .
For more details, see the documentation.
Ideally, most user interaction with scope will simply occur through the input file (scope/input.txt).
Any data field in a row marked with the [DB] flag can be pulled from a local database by inputting DATABASE. In our case, a database simply refers
to a CSV containing contents from the Exoplanet Archive,
with planet parameters resolved with the planet name. You can also specify most arguments from the command line, overwriting the input file.
Simply edit the input file to the desired parameters, then run:
python run_simulation.py
Running the script requires exoplanet, stellar, and telluric spectra. Default spectra and parameters currently correspond to the exoplanet WASP-77Ab.
Once completed, the code will create a directory for the data in output/ (based on the input modelname)
with the following types of files:
simdata_: the simulated flux cube with PCA performed. That is, the principal components with the largest variance have been removed.nopca_simdata_: the simulated flux cube, including all spectral components (exoplanet, star, blaze function, tellurics).A_noplanet_: the simulated flux cube with the lowest-variance principal component(s) removed.lls_: the log-likelihood surface for the simulated flux cube, as a Kp--Vsys map.ccfs_: the cross-correlation function for the simulated flux cube, as a Kp--Vsys map.
If you use scope in your work, please cite our paper: https://arxiv.org/abs/2411.07303