{ "info": { "author": "D. C. Price", "author_email": "dancpr@berkeley.edu", "bugtrack_url": null, "classifiers": [], "description": "[![Python application](https://github.com/FRBs/pygedm/actions/workflows/python-app.yml/badge.svg)](https://github.com/FRBs/pygedm/actions/workflows/python-app.yml)\n[![License: LGPL v3](https://img.shields.io/badge/License-LGPL%20v3-blue.svg)](https://www.gnu.org/licenses/lgpl-3.0)\n[![Coverage](https://codecov.io/gh/FRBs/pygedm/branch/master/graph/badge.svg?token=TlBiPzD7DP)](https://codecov.io/gh/FRBs/pygedm)[![Documentation Status](https://readthedocs.org/projects/pygedm/badge/?version=latest)](https://pygedm.readthedocs.io/en/latest/?badge=latest)\n\n# PyGEDM\n_Python bindings for the YMW16, NE2001 and YT2020 electron density models_\n\nThis package is a Python interface to the YMW16 and NE2001 electron density models, and YT2020 halo model.\nThe Yao, Manchester and Wang (2017, [Astrophys. J., 835, 29](https://iopscience.iop.org/article/10.3847/1538-4357/835/1/29/meta);\n[arXiv:1610.09448](https://arxiv.org/abs/1610.09448)) YMW16 electron density model, is written in C++, and the Cordes and Lazio \n(2001, [arXiv:0207156](https://arxiv.org/abs/astro-ph/)) NE2001 model is written in FORTRAN. This package, PyGEDM, wraps these\ntwo codes using [pybind11](https://pybind11.readthedocs.io/en/stable/intro.html) to make them usable from Python. Here, we have converted NE2001 to C++ using `f2c`.\n\n### Web app\n\nWe provide a web app at https://apps.datacentral.org.au/pygedm/ \n\nThe pygedm web app is kindly hosted by [Data Central](https://datacentral.org.au/).\n\n### Usage\n\nSome usage examples can be found in the [examples directory](https://github.com/telegraphic/pygedm/tree/master/examples). \n\n```python\nimport pygedm\n\n# calculate DM at a given distance\nDM, tau_sc = pygedm.dist_to_dm(204.0, -6.5, 200, method='ne2001')\nDM, tau_sc = pygedm.dist_to_dm(204.0, -6.5, 200, method='ymw16')\n\n# calculate distance for a given sky position and DM\ndist, tau_sc = pygedm.dm_to_dist(123.4, 4.0, 200)\n\n# calculate N_e density at xyz galactocentric coordinates\nne = pygedm.calculate_electron_density_xyz(1.0, 2.0, 3.0)\n\n# calculate N_e density at Galactic lat/long/distance coords\nne = pygedm.calculate_electron_density_lbr(204.0, -6.5, 3000.0)\n\n# Calculate halo DM contribution\ndm_halo = pygedm.calculate_halo_dm(gl=0, gb=30)\n```\n\nThe methods return astropy [Quantities](http://docs.astropy.org/en/stable/units/quantity.html#quantity), which have units attached, and can accept astropy [Angles](http://docs.astropy.org/en/stable/coordinates/angles.html#working-with-angles) and Quantities as arguments:\n\n```python\nimport pygedm\nimport astropy.units as u\nimport astropy.coordinates as c\nDM = u.Quantity(10.0, unit='pc cm^-3')\nra, dec = c.Angle(23.0, unit='hourangle'), c.Angle('-43:00:02', unit='degree')\nsky_coords = c.SkyCoord(ra, dec, frame='icrs')\ndist, tau_sc = pygedm.dm_to_dist(sky_coords.galactic.l, sky_coords.galactic.b, DM)\n\nprint(dist.to('lyr'))\n>> 3362.16343117 lyr\nprint(tau_sc.to('ns'))\n>> 7.758686138 ns\n```\n\n\n### Installation\n\nRequires `pybind11`, `astropy`, `numpy`, `scipy`, a newish C compiler with C++11 support (Ubuntu 16.04+ default gcc will work), plus `f2c`. \n\nPre-compiled wheels are generated for linux, meaning you can skip the `f2c` install step. Alternatively you can install via `apt-get f2c` in Ubuntu, or via `conda install -c conda-forge f2c` if you use conda.\n\nFor MacOS, you are best off using `conda` and getting `f2c` via `conda install -c conda-forge f2c`. Windows is not currently supported.\n\nYou should be able to install with:\n\n```\npip install pygedm\n```\n\nor \n\n```\npip install git+https://github.com/telegraphic/pygedm\n```\n\nto install the latest version from github. Alternatively, download this repository and install via\n\n```\npip install .\n```\n\nTo run unit tests, run `python setup.py test`. Note that these tests only check the Python bindings, \nnot the underlying C/FORTRAN source code (which is not supplied with unit tests).\n\n### References\n\nIf using PyGEDM in a journal article, please remember to cite the underlying electron density models:\n\n[Cordes, J. M., & Lazio, T. J. W. (2002)](https://ui.adsabs.harvard.edu/abs/2002astro.ph..7156C/abstract), \n_NE2001.I. A New Model for the Galactic Distribution of Free Electrons and its Fluctuations_, \narXiv e-prints, astro-ph/0207156.\n\n[Cordes, J. M., & Lazio, T. J. W. (2003)](https://ui.adsabs.harvard.edu/abs/2003astro.ph..1598C/abstract), \n_NE2001. II. Using Radio Propagation Data to Construct a Model for the Galactic Distribution of Free Electrons_, \narXiv e-prints, astro-ph/0301598.\n\n[Yao, J. M., Manchester, R. N., & Wang, N. (2017)](https://ui.adsabs.harvard.edu/abs/2017ApJ...835...29Y/abstract), \n_A New Electron-density Model for Estimation of Pulsar and FRB Distances_, \nThe Astrophysical Journal, Volume 888, Issue 2, id.105, Colume 835, id.29\n\n[Yamasaki, S., & Totani, T. (2020)](https://ui.adsabs.harvard.edu/abs/2019arXiv190900849Y/abstract), \n_The Galactic Halo Contribution to the Dispersion Measure of Extragalactic Fast Radio Bursts_, \nThe Astrophysical Journal, Volume 888, Issue 2, id.105\n\nThese are available in bibtex format in [references.bib](https://github.com/telegraphic/pygedm/references.bib),\nand also as an [ADS library](https://ui.adsabs.harvard.edu/public-libraries/Ci6_0-TlSySPMLrHxTvhhw). \n\n## YMW16 C README\n\nYMW16 is a model for the distribution of free electrons in the Galaxy,\nthe Magellanic Clouds and the inter-galactic medium, that can be used\nto estimate distances for real or simulated pulsars and fast radio\nbursts (FRBs) based on their position and dispersion measure.\n\nThe Galactic model is based on 189 pulsars that have independently\ndetermined distances as well as dispersion measures, whereas simpler\nmodels are used for the electron density in the MC and the IGM. It is\nestimated that the 95% of predicted Galactic pulsar distances will\nhave a relative error of less than a factor of 0.9. Pulse broadening\ndue to scattering in the Galactic interstellar medium, the Magellanic\nClouds, the intergalactic medium and FRB host galaxies is estimated.\n\nAs well as the ymw16 dm-distance program, we also provide a program,\nymw16_ne, which gives the electron density at any point in the Galaxy\nor Magellanic Clouds.\n\nA paper (Yao, Manchester and Wang, 2017,\n[Astrophys. J., 835, 29](https://iopscience.iop.org/article/10.3847/1538-4357/835/1/29/meta);\n[arXiv:1610.09448](https://arxiv.org/abs/1610.09448)) describes the model and compares its predictions\nwith those of earlier Galactic electron density models. YMW16 is the\nfirst electron-density model to estimate extragalactic pulsar\ndistances and FRB distances.\n\nTo make a command-line executable version of the program, download and\nunpack the latest version of the program. Then run \"make_ymw16\" to\ncreate the executable. The environment variable YMW16_DIR may be set\nup to point at a directory containing ymw16par.txt and\nspiral.txt. Access to these files is needed at runtime.\n\nWebsites allowing interactive access to the YMW16 distance model and\ndownload of the latest program version are available at:\n* [http://www.xao.ac.cn/ymw16/](http://www.xao.ac.cn/ymw16/),\n* [http://www.atnf.csiro.au/research/pulsar/ymw16/](http://www.atnf.csiro.au/research/pulsar/ymw16/]) and\n* [https://bitbucket.org/psrsoft/ymw16/](https://bitbucket.org/psrsoft/ymw16/).\n\nPlease report any issues or bugs at\nhttps://bitbucket.org/psrsoft/ymw16/issues/new/ or directly to the\nauthors. Please provide an example illustrating the problem.\n\n### YMW16 C LICENSE\n\n```\nCopyright (C) 2016, 2017 J. M. Yao, R. N. Manchester, N. Wang.\n\nYMW16 is free software: you can redistribute it and/or modify\u3000it\nunder the terms of the GNU General Public License as published by the\nFree Software Foundation, either version 3 of the License, or (at your\noption) any later version.\n\nYMW16 is distributed in the hope that it will be useful,\u3000but WITHOUT\nANY WARRANTY; without even the implied warranty of\u3000MERCHANTABILITY or\nFITNESS FOR A PARTICULAR PURPOSE. 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