Morisset created pyCloudy. This allows you to
- Define and write input file(s) for Cloudy code. As you can have it in a code, you may generate automatically sets of input files, changing parameters from one to the other.
- Read the Cloudy output files and play with the data: you will be able to plot line emissivity ratio vs. the radius of the nebula, the electron temperature, or any Cloudy output.
- Build pseudo-3D models, a la Cloudy_3D. This means: run a set of models, changing parameters (e.g. inner radius, density) following angular laws, read the outputs of the set of models and interpolate the results (Te, ne, line emissivities) in a 3D cube.
They have a discussion forum to answer questions.
Morisset and Stasinska created Cloudy 3D.
This uses IDL scripts to drive Cloudy as a subprogram and create simulations of complex geometries.
Nebular emission is included in the Flexible Stellar Population Synthesis (FSPS; Conroy+2009) code using Cloudy (v13.03). The nebular model is described in Byler+2017 which predicts nebular line and continuum emission for complex stellar populations. The model was generated using the code cloudyFSPS, which is available at http://nell-byler.github.io/cloudyfsps/. Users can (a) download the pre-computed FSPS SSP ascii tables and (b) find usage examples for how to use FSPS to generate SEDs for complex stellar populations that include nebular line and continuum emission. More generally, users can also (c) use cloudyFSPS to generate their own ascii tables for use within Cloudy, and format the output for use within FSPS.
Wang Ye's helper scripts for extracting information related to the gas cooling are given here.
Kyujin Kwak's grids of radiation fields from turbulent mixing layer simulations, suitable for use in the
Return to main page