Simplified framework for modeling the global 21-cm absorption signal, with a focus on studying the implications of non-standard 21-cm CMB temperature evolution. For details about the model, see 2009.xxxx.
Derived 21-cm absorption temperature (left) for various amounts of excess power-law photon temperature parameterization (right) from Fialkov and Barkana (2019).
The dependencies of the code are listed in environments.yml. In addition to the usual Python scientific stack, the astropy
, classy
, COLOSSUS
, and tqdm
packages are required.
- The notebook 01_basic_examples.ipynb contains basic high-level examples for running the code.
- The notebook 02_advanced_usage.ipynb describes components of the code that can be used for finer control over the X-ray and Ly-A emitting populations.
- Andrea Caputo; andrea dot caputo at uv dot es
- Hongwan Liu; hongwanl at princeton dot edu
- Siddharth Mishra-Sharma; sm8383 at nyu dot edu
- Maxim Pospelov; pospelov at umn dot edu
- Joshua T. Ruderman; ruderman at nyu dot edu
- Alfredo Urbano; alfredo dot urbano at sissa dot it
If you use this code, please cite:
@article{Caputo:2020xxx,
author = "Caputo, Andrea and Liu, Hongwan and Mishra-Sharma, Siddharth and Pospelov, Maxim and Ruderman, Joshua T. and Urbano, Alfredo",
archivePrefix = "arXiv",
eprint = "2009.xxxxx",
month = "9",
primaryClass = "astro-ph.CO",
title = "{Edges and Endpoints in 21-cm from Resonant Photon Production}",
year = "2020"
}
Various components of the code are based on astro-ph/0507102, 1804.02406, 0910.4410, 0802.2102, 1312.4948, and 1904.09296.