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"info": {
"author": "Geoffrey Ryan",
"author_email": "gsryan@umd.edu",
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"classifiers": [
"Development Status :: 4 - Beta",
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"License :: OSI Approved :: MIT License",
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"Programming Language :: C",
"Programming Language :: Python :: 3",
"Topic :: Scientific/Engineering :: Astronomy"
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"description": "# Numeric GRB Afterglow models\n\nA Python 3 module to calculate GRB afterglow light curves and spectra. Details of the methods can be found in [Ryan et al 2019](https://arxiv.org/abs/1909.11691). Builds on [van Eerten & MacFadyen 2010](https://arxiv.org/abs/1006.5125) and [van Eerten 2018](https://arxiv.org/abs/1801.01848). This code is under active development.\n\nDocumentation available at \n\n## Attribution\n\nIf you use this code in a publication, please refer to the package by name and cite \"Ryan, G., van Eerten, H., Piro, L. and Troja, E., 2019, arXiv:1910.11691\" [arXiv link](https://arxiv.org/abs/1909.11691).\n\n## Features\n\n_afterglowpy_ computes synchrotron emission from the forward shock of a relativistic blast wave. It includes:\n- Fully trans-relativistic shock evolution through a constant density medium.\n- On-the-fly integration over the equal-observer-time slices of the shock surface.\n- Approximate prescription for jet spreading.\n- Arbitrary viewing angles.\n- Angularly structured jets, ie. E(θ)\n- Spherical velocity-stratified outflows, ie. E(u)\n- Counter-jet emission.\n\nIt has limited support (these should be considered experimental) for:\n- Initial energy injection\n- Inverse comption spectra\n- Spatially-resolved intensity maps\n- Early coasting phase\n\nIt does not include (yet):\n- External wind medium, ie. n ∝ r-2\n- Synchrotron self-absorbtion\n- Reverse shock emission\n\n_afterglowpy_ has been calibrated to the BoxFit code ([van Eerten, van der Horst, & Macfadyen 2011](https://arxiv.org/abs/1110.5089), available at the [Afterglow Library](https://cosmo.nyu.edu/afterglowlibrary/boxfit2011.html)) and produces similar light curves for top hat jets (within 50% when same parameters are used) both on- and off-axis. Its jet models by default do not include an initial coasting phase, which may effect predictions for early observations.\n\n## Installation/Building\n\n\n_afterglowpy_ is available via `pip`:\n```bash\n$ pip install afterglowpy\n```\n\nIf you are working on a local copy of this repo and would like to install from source, you can the run the following from the top level directory of the project.\n```bash\n$ pip install -e .\n```\n\n## Using\n\n**This interface will be updated to be more sensible in the VERY near future**\n\nIn your python code, import the library with `import afterglowpy as grb`. \n\nThe main function of interest is`grb.fluxDensity(t, nu, jetType, specType, *pars, **kwargs)`. See `tests/plotLC.py` for a simple example.\n\n`jetType` can be -1 (top hat), 0 (Gaussian), 1 (Power Law w/ core), 2 (Gaussian w/ core), 3 (Cocoon), or 4 (Smooth Power Law). \n\n`specType` can be 0 (global cooling time, no inverse compton) or 1 (global cooling time, inverse compton).\n\nFor jet-like afterglows (`jetTypes` -2, -1, 0, 1, 2, and 4) `pars` has 14 positional arguments:\n- `0 thetaV` viewing angle in radians\n- `1 E0` on-axis isotropic equivalent energy in erg\n- `2 thetaC` half-width of the jet core in radians (jetType specific)\n- `3 thetaW` \"wing\" truncation angle of the jet, in radians\n- `4 b` power for power-law structure, θ-b\n- `5 L0` Fiducial luminosity for energy injection, in erg/s, typically 0.\n- `6 q` Temporal power-law index for energy injection, typically 0.\n- `7 ts` Fiducial time-scale for energy injection, in seconds, typically 0.\n- `8 n0` Number density of ISM, in cm-3\n- `9 p` Electron distribution power-law index (p>2)\n- `10 epsilon_e` Thermal energy fraction in electrons\n- `11 epsilon_B` Thermal energy fraction in magnetic field\n- `12 xi_N` Fraction of electrons that get accelerated\n- `13 d_L` Luminosity distance in cm\n\nFor cocoon-like afterglows (`jetType` 3) `pars` has 14 positional arguments:\n- `0 umax` Initial maximum outflow 4-velocity\n- `1 umin` Minium outflow 4-velocity\n- `2 Ei` Fiducial energy in velocity distribution, E(>u) = Ei u-k.\n- `3 k` Power-law index of energy velocity distribution \n- `4 Mej` Mass of material at `umax' in solar masses\n- `5 L0` Fiducial luminosity for energy injection, in erg/s, typically 0.\n- `6 q` Temporal power-law index for energy injection, typically 0.\n- `7 ts` Fiducial time-scale for energy injection, in seconds, typically 0.\n- `8 n0` Number density of ISM, in cm-3\n- `9 p` Electron distribution power-law index (p>2)\n- `10 epsilon_e` Thermal energy fraction in electrons\n- `11 epsilon_B` Thermal energy fraction in magnetic field\n- `12 xi_N` Fraction of electrons that get accelerated\n- `13 d_L` Luminosity distance in cm\n\nKeyword arguments are:\n- `z` redshift (defaults to 0)\n- `tRes` time resolution of shock-evolution scheme, number of sample points per decade in time\n- `latRes` latitudinal resolution for structured jets, number of shells per `thetaC`\n- `rtol` target relative tolerance of flux integration\n- `spread` boolean (defaults to True), whether to allow the jet to spread.\n\n\n\n\n\n",
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