Package pysynphot

source code

Package:  Astrolib Pysynphot

Purpose:
========

Object-oriented replacement for STSDAS synphot package.

This __init__ file is used to expose the desired elements of the user
interface for interactive use.


Dependencies:
=============
- numpy 1.0 or greater
- pyfits 1.1 or greater
- spark (syntax parser) (included in package tho; really dependency?)

Environment:
============
The environment variable PYSYN_CDBS must be set.

Example:
========

>>> import pysynphot as S
>>> print S.__version__
0.4d1
>>> #Read a spectrum from a file
>>> vega=S.FileSpectrum('alpha_lyr_stis_003.fits')
>>> print vega
alpha_lyr_stis_003.fits
>>> vega.wave
array([  9.00452026e+02,   9.01354004e+02,   9.02257996e+02, ...,
         2.99353200e+06,   2.99653275e+06,   2.99953700e+06], dtype=float32)
>>> vega.flux
array([  1.23810534e-17,   1.67559564e-17,   1.78002369e-17, ...,
         1.40140738e-19,   1.38734357e-19,   1.26490663e-19])
>>> bb=S.BlackBody(40000)
>>> print bb.wave
[   500.            500.19760122    500.39528054 ...,  25969.1985582
  25979.46164894  25989.72879567]
>>> print bb.flux
[ 1.15230179  1.15375888  1.15521646 ...,  0.00141824  0.0014166
  0.00141496]
>>> print bb
BlackBody(T=40000)

>>> pl=S.PowerLaw(10000,-2)
>>> print pl
Power law: refwave 10000.000000, index -2.000000
>>> print pl.wave
[   500.            500.19760122    500.39528054 ...,  25969.1985582
  25979.46164894  25989.72879567]
>>> print pl.flux
[  4.00000000e+02   3.99684021e+02   3.99368286e+02 ...,   1.48280114e-01
   1.48162976e-01   1.48045942e-01]

>>> g1=S.GaussianSource(18.3,18000,2000,fluxunits='abmag')
>>> print g1
Gaussian: mu=18000.000000,fwhm=2000.000000,flux=18.300000 abmag

>>> unitflux=S.UnitSpectrum(18,fluxunits='abmag')
>>> print unitflux
Unit spectrum of 18.000000 abmag

>>> bp1=S.ObsBandpass('acs,hrc,f555w')
>>> print bp1
acs,hrc,f555w
>>> print bp1.wave
[   500.   1000.   1001. ...,  11999.  30000.  30010.]
>>> print bp1.throughput
[ 0.  0.  0. ...,  0.  0.  0.]
>>> bp1.showfiles()
/grp/hst/cdbs/comp/ota/hst_ota_007_syn.fits
/grp/hst/cdbs/comp/acs/acs_hrc_m12_005_syn.fits
/grp/hst/cdbs/comp/acs/acs_hrc_m3_005_syn.fits
/grp/hst/cdbs/comp/acs/acs_f555w_003_syn.fits
/grp/hst/cdbs/comp/acs/acs_hrc_win_005_syn.fits
/grp/hst/cdbs/comp/acs/acs_hrc_ccd_011_syn.fits
>>> len(bp1)
6

>>> sp1=S.FileSpectrum('/grp/hst/cdbs/calspec/feige66_002.fits')
>>> print bp1.waveunits
angstrom
>>> print sp1.waveunits
angstrom
>>> obs1=sp1*bp1
>>> print obs1
/grp/hst/cdbs/calspec/feige66_002.fits * acs,hrc,f555w
>>> print obs1.wave
[   500.   1000.   1001. ...,  11999.  30000.  30010.]
>>> print obs1.flux.max()
7.47814099194e-14
>>> print obs1.flux.argmax()
6924

>>> sp2=S.FileSpectrum('/grp/hst/cdbs/calspec/feige66_002.fits')*S.ObsBandpass('acs,hrc,f555w')
>>> print sp2
/grp/hst/cdbs/calspec/feige66_002.fits * acs,hrc,f555w
>>> print sp2.waveunits
angstrom
>>> print sp2.fluxunits
flam