{
    "info": {
        "author": "Manuel Silva",
        "author_email": "madusilva@gmail.com",
        "bugtrack_url": null,
        "classifiers": [
            "Intended Audience :: Developers",
            "Intended Audience :: Science/Research",
            "License :: OSI Approved :: GNU General Public License (GPL)",
            "Operating System :: OS Independent",
            "Programming Language :: Python",
            "Topic :: Scientific/Engineering :: Astronomy"
        ],
        "description": "pysysp: Synthetic Stellar Photometry for Python\n\nThis is a set of tools to compute synthetic photometry in a simple way,\nideal to integrate in larger projects.\nThe inputs are photonic response functions for the desired phtometric bands and \nstellar spectra. The units used in this package are: erg cm^-2 s^-1 Ang^-1 for fluxes; \nAng^-1 for wavelength. Note that this implies units of cm Ang^-1 for the speed of light.\nThese units must be used in all inputs for the package to operate properly.\nIt is possible to compute magnitudes in Vega and AB systems, and interstellar \nextinction, for any given photometric passband, given an extinction law, which must \nbe a callable object function of wavelength only. The only extinction law provided \nis the one by Cardelli, Clayton & Mathis (1989), but others can be easily added if \nneeded.\nAt the moment only the bandpasses for Bessel's UBVRI and Gaia's G filters are provided.\n\nReferences: Casagrande & VandenBerg (2014); Bessel & Murphy (2012)\nAcknowledgments:  Vega CALSPEC spectrum alpha_lyr_stis_006\n                http://www.stsci.edu/hst/observatory/cdbs/calspec.html\n                  photonic response functions by Bessel & Murphy (2012)\n                  for the U, B, V, R, I filters\n\n\n\n\n-------------------------\nUsage example:\n\n>>> import pysysp\n\n#load a spectrum from a fits file\n>>> vega = pysysp.StarSpectrum('alpha_lyr_stis_006.fits')\n\n#print the flux\n>>> vega.flux\narray([  1.23810533e-17,   1.67559561e-17,   1.78002369e-17, ...,\n         1.40140733e-19,   1.38734358e-19,   1.26490663e-19], dtype=float32)\n\n#Check available filters\n>>> pysysp.showfilters\n{'Gaia': ['G'], 'Bessel': ['B', 'I', 'R', 'U', 'V']}\n         \n#load the photonic response for the bands B and V with linear smoothing\n>>> V=pysysp.BandPass('V',smt='linear')\n>>> B=pysysp.BandPass('B',smt='linear')\n\n#You can also load any ascii file with two columns (first wavelength, second filter response)\n>>> B2 = pysysp.BandPass('./filters/B.dat')\n\n#compute the V magnitude in Vega system\n#The magnitude of Vega in V band is not 0, so in order to\n#compute the correct value we should correct the zero point\n>>> vega.apmag(V,mag='Vega',mzero=0.03)\n0.029999999999999999\n\n#Same in AB system\n>>> vega.apmag(V,mag='AB')\n0.0062420242892642364\n\n\n#Compute E(B-V) for a (monochromatic) extinction Av=0.5\n>>> ab=vega.extinction(B,law='cardelli',A=0.5,Rv=3.1)\n>>> av=vega.extinction(V,law='cardelli',A=0.5,Rv=3.1)\n>>> ab-av\n0.15954421668471008\n\n\nChangelog\n---------\n\nchangelog:\n\n1.0.0 (09/04/2015)\n------------------\n\n- Initial release.\n\n1.0.1 (21/10/2015)\n------------------\n\n- added MANIFEST.in file",
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        "license": "GPLv2",
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        "name": "pysysp",
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        "summary": "A package for Synthetic Stellar Photometry",
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