Added descriptions to all scripts, checked functioning

scripts/gratama_seeing_limited_dispersion_test.py

@@ -1,97 +1,18 @@
 import numpy as np
 import sys
-sys.path.insert(0, '/Users/joost/Dropbox/Werk/PhD/Analyses/Python/Analytical/Fourier Optics')
+sys.path.insert(0, '/Users/joost/Dropbox/Werk/PhD/Documents/Published/FourierOptics GitHub release/')
 from fourierOptics import *
 import scipy.special as spc
-from pdb import set_trace
+
+
 '''
-def find_pixel_scale(x):
-	""" Calculate the pixel size from the x, y plane """
-	_dpix = np.mean(np.diff(x.real))
-	if _dpix < 1e-99:
-		_dpix = np.mean(np.diff((x.T).real))
-	return _dpix
-
-def seeing(wvl, r0):
-	"""
-		Seeing value in arcsec at wavelength wvl
-		wvl in millimeter
-		r0 in meter
-	"""
-	wvl *= 1e-3 # convert wvl from mm to meter
-	return 3600*180/np.pi*0.976*wvl/r0
-
-def fried_r0(wvl, seeing):
-	"""
-		Returns Fried's parameter value in meters
-		wvl in millimeter
-	"""
-	wvl *= 1e-3 # convert wvl from mm to meter
-	return 0.976*wvl/seeing*206264.8
-
-def airmass(z):
-	"""
-		Converts zenith angle in degrees to airmass
-	"""
-	return 1/np.cos(np.deg2rad(z))
-
-def spectrum(k, r0, L0=25):        
-	"""SPECTRUM Phase power spectrum density computes the phase power
-		spectrum density from the spatial frequency f and an
-		atmosphere object
-		
-		Normal value for L0 = 25.
-	"""                        
-	cte = (24*spc.gamma(6/5)/5)**(5/6)*(spc.gamma(11/6)**2./(2*np.pi**(11/3)))
-	return r0**(-5/3)*cte*(k**2 + 1/L0**2)**(-11/6)
-
-def add_seeing(wvl, sng, field_tuple):
-	"""
-		Computes the seeing limited PSF for a supplied amplitude
-		distribution.
-		
-		Parameters:
-		wvl - wavelength in mm
-		sng - seeing in arcseconds
-		field_tuple - tuple containing (amplitude array, x array, y array)
-		
-		Returns:
-		psf_seeing
-
-	"""
-	r01   = fried_r0(wvl, seeing=sng) * 1e3
-	A_psf, x_psf, y_psf = field_tuple
-	n,m = np.shape(x_psf)
-	fx = x_psf / (3200*wvl)
-	fy = y_psf / (3200*wvl)
-	dk = find_pixel_scale(fx)
-
-	# von-Karman spectrum of the atmosphere for the given frequencies in k-space
-	psd   = spectrum(np.hypot(fx.real, fy.real), r0=r01, L0=25*1e3)
-	psd[int(n/2),int(m/2)] = 0
-
-	# Compute the atmospheric OTF
-	# According to Roddier 1981, the atmospheric OTF can be derived from the phase structure function
-	# assuming that the phase is stationary accross the pupil and behaves as a Gaussian variable
-	Bphi = np.fft.fft2(np.fft.ifftshift(psd))*dk**2
-	Dphi = np.fft.ifftshift((2 * (Bphi[0,0] - Bphi))) # ifftshift in Bphi en Dphi!
-	otf_atm = np.exp(-0.5*Dphi)
-	
-	# Compute the OTF of the supplied PSF
-	# We can derive the OTF from the inverse Fourier transform of the PSF
-	psf = np.abs(A_psf)**2
-	otf_psf = np.fft.fftshift(np.fft.ifft2(np.fft.fftshift(psf)))
-	otf_psf = otf_psf/otf_psf.max()
-
-	# Compute the seeing-limited PSF
-	# Multiplication of OTF and then Fourier transform
-	otf  = otf_psf * otf_atm
-	psf_seeing = np.fft.fftshift(np.fft.ifft2(np.fft.ifftshift(otf)))
-	return psf_seeing
+	Description:
+	This script simulates the dispersed PSF of the small (40 cm)
+	Gratama telescope at the University of Groningen under 1.5
+	arcsecond seeing.
 '''
 
 
-
 if __name__ == '__main__':
 	l  = 0.5e-3      # mm
 	D_GT = 400          # mm