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.