Commit 96a2932f authored by Stefano Covino's avatar Stefano Covino
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.gitignore

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.DS_Store

.DS_Store?

._*

.Spotlight-V100

.Trashes

ehthumbs.db

Thumbs.db

dist/*

Docs/*

Misc/*

LICENSE.txt

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Copyright (c) 2016 The Python Packaging Authority (PyPA)



Permission is hereby granted, free of charge, to any person obtaining a copy of

this software and associated documentation files (the "Software"), to deal in

the Software without restriction, including without limitation the rights to

use, copy, modify, merge, publish, distribute, sublicense, and/or sell copies

of the Software, and to permit persons to whom the Software is furnished to do

so, subject to the following conditions:



The above copyright notice and this permission notice shall be included in all

copies or substantial portions of the Software.



THE SOFTWARE IS PROVIDED "AS IS", WITHOUT WARRANTY OF ANY KIND, EXPRESS OR

IMPLIED, INCLUDING BUT NOT LIMITED TO THE WARRANTIES OF MERCHANTABILITY,

FITNESS FOR A PARTICULAR PURPOSE AND NONINFRINGEMENT. IN NO EVENT SHALL THE

AUTHORS OR COPYRIGHT HOLDERS BE LIABLE FOR ANY CLAIM, DAMAGES OR OTHER

LIABILITY, WHETHER IN AN ACTION OF CONTRACT, TORT OR OTHERWISE, ARISING FROM,

OUT OF OR IN CONNECTION WITH THE SOFTWARE OR THE USE OR OTHER DEALINGS IN THE

SOFTWARE.

MANIFEST.in

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# Include the README

include ./README.md



# Include the license file

include ./LICENSE.txt



# Include the data files

recursive-include SRP/SRPData/ *

include SRP/SRPCalFlux.data



# Include all python files

recursive-include . *.py



# Exclude MacOS files

recursive-exclude . .DS_Store



# Exclude working files

recursive-exclude build

recursive-exclude Misc

README.md

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# Swift Reduction Package





The Swift Reduction Package (hereafter SRP) is a packet of command line tools to solve problems (e.g. basic reduction and analysis tasks of optical/NIR astronomical data, quick cosmological computations, units conversions, etc.) often met in astronomical research activities.



SRP was originally developed in the context of the Swift follow-up activities of the Milan GRB team at the INAF/Brera Astronomical Observatory. The package is designed to be an aid to any researcher to drive further observation of a followed-up GRB counterpart and “swift” can therefore be read simply as “rapid”, “agile”, etc.

 

 Some technical comment

 This package, written in Python (v. 3.x), has been widely tested only on PC-Linux and on Mac OS X workstations.

SRP/SRPAfterglow.py

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""" Utility functions and classes for SRP



Context : SRP

Module  : SRPAfterglow.py

Version : 1.0.0

Status  : approved

Author  : Stefano Covino

Date    : 27/02/2007

E-mail  : stefano.covino@brera.inaf.it

URL     : http://www.merate.mi.astro.it/covino

Purpose : Collection of utility functions and classes for SRP.



Usage   : to be imported



Remarks : Data from Zhang & Meszaros, IJMPA A19, 2385 (2004) and

        : Hurley, Sari and Djorgovski, in "Compact Stellar X-ray Sources".



History : (27/02/2007) First version.

"""





#import SRPFiles, SRPConstants

#import os, string, math, copy

#import TimeAstro_algs

#import stats









def TypSynchrFreqConst (epse=0.1, epsb=0.01, energy=1e52, time=1, z=1):

 csie=1

 return 6*1e15 * (1+z)**0.5 * (energy/1e52)**0.5 * (epse/csie)**2 * (epsb)**0.5 * (time)**-1.5



def CoolSynchrFreqConst (epsb=0.01, energy=1e52, time=1, z=1, density=1):

 return 9*1e12 * (1+z)**-0.5 * (energy/1e52)**-0.5 * (density)**-1 * (epsb)**-1.5 * (time)**-0.5



def SelfAbsSynchrFreqConst (epse=0.1, epsb=0.01, energy=1e52, density=1, z=1):

 csie=1

 return 2*1e9 * (1+z)**-1 * (energy/1e52)**0.2 * (epse/csie)**-1 * (epsb)**0.2 * density**0.4



def TypSynchrFluxConst (epsb=0.01, energy=1e52, ldist=1e28, density=1, z=1):

 return 20 * (1+z) * (epsb)**0.5 * density**0.5 * (energy/1e52) * (ldist/1e28)**-2



def SynchrSpectrConst (nu, epse=0.1, epsb=0.01, energy=1e52, time=1, z=1, density=1, ldist=1e28, p=2.2):

 ntyp = TypSynchrFreqConst (epse, epsb, energy, time, z)

 nsabs = SelfAbsSynchrFreqConst (epse, epsb, energy, density, z)

 ncool = CoolSynchrFreqConst (epsb, energy, time, z, density)

 normfl = TypSynchrFluxConst (epsb, energy, ldist, density, z)

 if ntyp < ncool:

  if nu < nsabs:

   return normfl * (nsabs/ntyp)**(1.0/3.0) * (nu/nsabs)**2

  elif nsabs <= nu < ntyp:

   return normfl * (nu/ntyp)**(1.0/3.0)

  elif ntyp <= nu < ncool:

   return normfl * (nu/ntyp)**((1-p)/2.0)

  else:

   return normfl * (ncool/ntyp)**((1-p)/2.0) * (nu/ncool)**(-p/2.0)

 else:

  if nu < nsabs:

   return normfl * (nsabs/ncool)**(1.0/3.0) * (nu/nsabs)**2

  elif nsabs <= nu < ncool:

   return normfl * (nu/ncool)**(1.0/3.0)

  elif ncool <= nu < ntyp:

   return normfl * (nu/ncool)**-0.5

  else:

   return normfl * (ntyp/ncool)**-0.5 * (nu/ntyp)**(-p/2.0)









# \rho R^2 = Astar * 5 x 10^11  gr/cm

def TypSynchrFreqWind (epse=0.1, epsb=0.01, energy=1e52, time=1, z=1):

 csie=1

 return 1.7*1e14 * (1+z)**0.5 * (energy/1e52)**0.5 * (epse/csie)**2 * (epsb)**0.5 * (time)**-1.5



def CoolSynchrFreqWind (epsb=0.01, energy=1e52, time=1, z=1, Astar=1):

 return 7*1e11 * (1+z)**-1.5 * (energy/1e52)**0.5 * (Astar)**-2 * (epsb)**-1.5 * (time)**0.5



def SelfAbsSynchrFreqWind (epse=0.1, epsb=0.01, energy=1e52, Astar=1, z=1, time=1):

 csie=1

 return 1.5*1e10 * (1+z)**-0.4 * (energy/1e52)**-0.4 * (epse/csie)**-1 * (epsb)**0.2 * Astar**1.2 * (time)**-0.4



def TypSynchrFluxWind (epsb=0.01, energy=1e52, ldist=1e28, Astar=1, z=1, time=1):

 return 180 * (1+z)**1.5 * (epsb)**0.5 * Astar * (energy/1e52)**0.5 * (ldist/1e28)**-2 * (time)**-0.5



def SynchrSpectrWind (nu, epse=0.1, epsb=0.01, energy=1e52, time=1, z=1, Astar=1, ldist=1e28, p=2.2):

 ntyp = TypSynchrFreqWind (epse, epsb, energy, time, z)

 nsabs = SelfAbsSynchrFreqWind (epse, epsb, energy, Astar, z, time)

 ncool = CoolSynchrFreqWind (epsb, energy, time, z, Astar)

 normfl = TypSynchrFluxWind (epsb, energy, ldist, Astar, z, time)

 if ntyp < ncool:

  if nu < nsabs:

   return normfl * (nsabs/ntyp)**(1.0/3.0) * (nu/nsabs)**2

  elif nsabs <= nu < ntyp:

   return normfl * (nu/ntyp)**(1.0/3.0)

  elif ntyp <= nu < ncool:

   return normfl * (nu/ntyp)**((1-p)/2.0)

  else:

   return normfl * (ncool/ntyp)**((1-p)/2.0) * (nu/ncool)**(-p/2.0)

 else:

  if nu < nsabs:

   return normfl * (nsabs/ncool)**(1.0/3.0) * (nu/nsabs)**2

  elif nsabs <= nu < ncool:

   return normfl * (nu/ncool)**(1.0/3.0)

  elif ncool <= nu < ntyp:

   return normfl * (nu/ncool)**-0.5

  else:

   return normfl * (ntyp/ncool)**-0.5 * (nu/ntyp)**(-p/2.0)