HI cloud identification method
- Version: 1.0.1
- Author: Gina Panopoulou
cloudcount uses a Gaussian decomposition of HI line emission data to identify kinematicaly distinct peaks in the spectra (clouds).
Please cite our paper if you use cloudcount for your projects.
@ARTICLE{2020arXiv200400647P, author = {{Panopoulou}, G.~V. and {Lenz}, D.}, title = "{Maps of the number of HI clouds along the line of sight at high galactic latitude}", journal = {arXiv e-prints}, keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics}, year = 2020, month = apr, eid = {arXiv:2004.00647}, pages = {arXiv:2004.00647}, archivePrefix = {arXiv}, eprint = {2004.00647}, primaryClass = {astro-ph.GA}, adsurl = {https://ui.adsabs.harvard.edu/abs/2020arXiv200400647P}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }
The program has been tested to work with the following package versions:
- python 2.7
- healpy 1.12.9
- astropy 2.0.9
- pytables 3.4.4
- numpy
If you want to run the notebooks yourself, you will also need the Jupyter server and matplotlib.
- If you wish to run the method on a selected patch of sky, follow the notebook `Running_the_method' (or it's .py version)
- If you wish to use the data products presented in the paper, follow the notebook `PublicData/DataUsageTutorial' (or it's .py version)