def psf(array_shape=(256, 256), dx=1., lam_over_diam=2., defocus=0., astig1=0., astig2=0., coma1=0.,
coma2=0., trefoil1=0., trefoil2=0., spher=0., circular_pupil=True, obscuration=0.,
nstruts=0, strut_thick=0.05, strut_angle=0.*galsim.degrees, flux=1.):
"""Return NumPy array containing circular (default) or square pupil PSF with low-order
aberrations.
The PSF is centred on the array[array_shape[0] / 2, array_shape[1] / 2] pixel by default, and
uses surface brightness rather than flux units for pixel values, matching SBProfile.
To ensure properly Nyquist sampled output any user should set lam_over_diam >= 2. * dx.
Ouput NumPy array is C-contiguous.
@param array_shape the NumPy array shape desired for the output array.
@param dx grid spacing of PSF in real space units
@param lam_over_diam lambda / telescope diameter in the physical units adopted for dx
(user responsible for consistency).
@param defocus defocus in units of incident light wavelength.
@param astig1 astigmatism (like e2) in units of incident light wavelength.
@param astig2 astigmatism (like e1) in units of incident light wavelength.
@param coma1 coma along y in units of incident light wavelength.
@param coma2 coma along x in units of incident light wavelength.
@param trefoil1 trefoil (one of the arrows along y) in units of incident light
wavelength.
@param trefoil2 trefoil (one of the arrows along x) in units of incident light
wavelength.
@param spher spherical aberration in units of incident light wavelength.
@param circular_pupil adopt a circular pupil?
@param obscuration linear dimension of central obscuration as fraction of pupil linear
dimension, [0., 1.).
@param nstruts Number of radial support struts to add to the central obscuration
[default `nstruts = 0`].
@param strut_thick Thickness of support struts as a fraction of pupil diameter
[default `strut_thick = 0.05`].
@param strut_angle Angle made between the vertical and the strut starting closest to it,
defined to be positive in the counter-clockwise direction; must be a
galsim.Angle instance [default `strut_angle = 0. * galsim.degrees`].
@param flux total flux of the profile [default flux=1.].
"""
wf = wavefront(
array_shape=array_shape, dx=dx, lam_over_diam=lam_over_diam, defocus=defocus, astig1=astig1,
astig2=astig2, coma1=coma1, coma2=coma2, trefoil1=trefoil1, trefoil2=trefoil2, spher=spher,
circular_pupil=circular_pupil, obscuration=obscuration, nstruts=nstruts,
strut_thick=strut_thick, strut_angle=strut_angle)
ftwf = np.fft.fft2(wf) # I think this (and the below) is quicker than np.abs(ftwf)**2
# The roll operation below restores the c_contiguous flag, so no need for a direct action
im = utilities.roll2d((ftwf * ftwf.conj()).real, (array_shape[0] / 2, array_shape[1] / 2))
return im * (flux / (im.sum() * dx**2))
def psf(array_shape=(256, 256), dx=1., lam_over_diam=2., defocus=0., astig1=0., astig2=0., coma1=0.,
coma2=0., spher=0., circular_pupil=True, obscuration=0., flux=1.):
"""Return NumPy array containing circular (default) or square pupil PSF with low-order
aberrations.
The PSF is centred on the array[array_shape[0] / 2, array_shape[1] / 2] pixel by default, and
uses surface brightness rather than flux units for pixel values, matching SBProfile.
To ensure properly Nyquist sampled output any user should set lam_over_diam >= 2. * dx.
Ouput NumPy array is C-contiguous.
@param array_shape the NumPy array shape desired for the output array.
@param dx grid spacing of PSF in real space units
@param lam_over_diam lambda / telescope diameter in the physical units adopted for dx
(user responsible for consistency).
@param defocus defocus in units of incident light wavelength.
@param astig1 first component of astigmatism (like e1) in units of incident light
wavelength.
@param astig2 second component of astigmatism (like e2) in units of incident light
wavelength.
@param coma1 coma along x in units of incident light wavelength.
@param coma2 coma along y in units of incident light wavelength.
@param spher spherical aberration in units of incident light wavelength.
@param circular_pupil adopt a circular pupil?
@param obscuration linear dimension of central obscuration as fraction of pupil linear
dimension, [0., 1.)
@param flux total flux of the profile [default flux=1.]
"""
wf = wavefront(
array_shape=array_shape, dx=dx, lam_over_diam=lam_over_diam, defocus=defocus, astig1=astig1,
astig2=astig2, coma1=coma1, coma2=coma2, spher=spher, circular_pupil=circular_pupil,
obscuration=obscuration)
ftwf = np.fft.fft2(wf) # I think this (and the below) is quicker than np.abs(ftwf)**2
# The roll operation below restores the c_contiguous flag, so no need for a direct action
im = utilities.roll2d((ftwf * ftwf.conj()).real, (array_shape[0] / 2, array_shape[1] / 2))
return im * (flux / (im.sum() * dx**2))
def psf(array_shape=(256, 256),
dx=1.,
lam_over_diam=2.,
defocus=0.,
astig1=0.,
astig2=0.,
coma1=0.,
coma2=0.,
trefoil1=0.,
trefoil2=0.,
spher=0.,
circular_pupil=True,
obscuration=0.,
flux=1.):
"""Return NumPy array containing circular (default) or square pupil PSF with low-order
aberrations.
The PSF is centred on the array[array_shape[0] / 2, array_shape[1] / 2] pixel by default, and
uses surface brightness rather than flux units for pixel values, matching SBProfile.
To ensure properly Nyquist sampled output any user should set lam_over_diam >= 2. * dx.
Ouput NumPy array is C-contiguous.
@param array_shape the NumPy array shape desired for the output array.
@param dx grid spacing of PSF in real space units
@param lam_over_diam lambda / telescope diameter in the physical units adopted for dx
(user responsible for consistency).
@param defocus defocus in units of incident light wavelength.
@param astig1 astigmatism (like e2) in units of incident light wavelength.
@param astig2 astigmatism (like e1) in units of incident light wavelength.
@param coma1 coma along y in units of incident light wavelength.
@param coma2 coma along x in units of incident light wavelength.
@param trefoil1 trefoil (one of the arrows along y) in units of incident light
wavelength.
@param trefoil2 trefoil (one of the arrows along x) in units of incident light
wavelength.
@param spher spherical aberration in units of incident light wavelength.
@param circular_pupil adopt a circular pupil?
@param obscuration linear dimension of central obscuration as fraction of pupil linear
dimension, [0., 1.)
@param flux total flux of the profile [default flux=1.]
"""
wf = wavefront(array_shape=array_shape,
dx=dx,
lam_over_diam=lam_over_diam,
defocus=defocus,
astig1=astig1,
astig2=astig2,
coma1=coma1,
coma2=coma2,
trefoil1=trefoil1,
trefoil2=trefoil2,
spher=spher,
circular_pupil=circular_pupil,
obscuration=obscuration)
ftwf = np.fft.fft2(
wf) # I think this (and the below) is quicker than np.abs(ftwf)**2
# The roll operation below restores the c_contiguous flag, so no need for a direct action
im = utilities.roll2d((ftwf * ftwf.conj()).real,
(array_shape[0] / 2, array_shape[1] / 2))
return im * (flux / (im.sum() * dx**2))