def test_exponential_flux_scaling():
"""Test flux scaling for Exponential.
"""
# decimal point to go to for parameter value comparisons
param_decimal = 12
test_flux = 17.9
test_scale = 1.8
# init with scale and flux only (should be ok given last tests)
obj = galsim.Exponential(scale_radius=test_scale, flux=test_flux)
obj *= 2.
np.testing.assert_almost_equal(
obj.flux,
test_flux * 2.,
decimal=param_decimal,
err_msg="Flux param inconsistent after __imul__.")
obj = galsim.Exponential(scale_radius=test_scale, flux=test_flux)
obj /= 2.
np.testing.assert_almost_equal(
obj.flux,
test_flux / 2.,
decimal=param_decimal,
err_msg="Flux param inconsistent after __idiv__.")
obj = galsim.Exponential(scale_radius=test_scale, flux=test_flux)
obj2 = obj * 2.
# First test that original obj is unharmed...
np.testing.assert_almost_equal(
obj.flux,
test_flux,
decimal=param_decimal,
err_msg="Flux param inconsistent after __rmul__ (original).")
# Then test new obj2 flux
np.testing.assert_almost_equal(
obj2.flux,
test_flux * 2.,
decimal=param_decimal,
err_msg="Flux param inconsistent after __rmul__ (result).")
obj = galsim.Exponential(scale_radius=test_scale, flux=test_flux)
obj2 = 2. * obj
# First test that original obj is unharmed...
np.testing.assert_almost_equal(
obj.flux,
test_flux,
decimal=param_decimal,
err_msg="Flux param inconsistent after __mul__ (original).")
# Then test new obj2 flux
np.testing.assert_almost_equal(
obj2.flux,
test_flux * 2.,
decimal=param_decimal,
err_msg="Flux param inconsistent after __mul__ (result).")
obj = galsim.Exponential(scale_radius=test_scale, flux=test_flux)
obj2 = obj / 2.
# First test that original obj is unharmed...
np.testing.assert_almost_equal(
obj.flux,
test_flux,
decimal=param_decimal,
err_msg="Flux param inconsistent after __div__ (original).")
# Then test new obj2 flux
np.testing.assert_almost_equal(
obj2.flux,
test_flux / 2.,
decimal=param_decimal,
err_msg="Flux param inconsistent after __div__ (result).")
def test_fwhm():
"""Test the calculateFWHM method.
"""
# Compare the calculation for a simple Gaussian.
g1 = galsim.Gaussian(sigma=5, flux=1.7)
print('g1 native fwhm = ', g1.fwhm)
print('g1.calculateFWHM = ', g1.calculateFWHM())
# These should be exactly equal.
np.testing.assert_equal(
g1.fwhm,
g1.calculateFWHM(),
err_msg="Gaussian.calculateFWHM() returned wrong value.")
# Check for a convolution of two Gaussians. Should be equivalent, but now will need to
# do the calculation.
g2 = galsim.Convolve(galsim.Gaussian(sigma=3, flux=1.3),
galsim.Gaussian(sigma=4, flux=23))
test_fwhm = g2.calculateFWHM()
print('g2.calculateFWHM = ', test_fwhm)
print('ratio - 1 = ', test_fwhm / g1.fwhm - 1)
np.testing.assert_almost_equal(
test_fwhm / g1.fwhm,
1.0,
decimal=3,
err_msg="Gaussian.calculateFWHM() is not accurate.")
# The default scale already accurate to around 3 dp. Using scale = 0.1 is accurate to 8 dp.
test_fwhm = g2.calculateFWHM(scale=0.1)
print('g2.calculateFWHM(scale=0.1) = ', test_fwhm)
print('ratio - 1 = ', test_fwhm / g1.fwhm - 1)
np.testing.assert_almost_equal(
test_fwhm / g1.fwhm,
1.0,
decimal=8,
err_msg="Gaussian.calculateFWHM(scale=0.1) is not accurate.")
# Finally, we don't expect this to be accurate, but make sure the code can handle having
# only the central pixel higher than half-maximum.
test_fwhm = g2.calculateFWHM(scale=20)
print('g2.calculateFWHM(scale=20) = ', test_fwhm)
print('ratio - 1 = ', test_fwhm / g1.fwhm - 1)
np.testing.assert_almost_equal(
test_fwhm / g1.fwhm / 10,
0.1,
decimal=1,
err_msg="Gaussian.calculateFWHM(scale=20) is not accurate.")
# Next, use an Exponential profile
e1 = galsim.Exponential(scale_radius=5, flux=1.7)
# The true fwhm for this is analytic, but not an attribute.
e1_fwhm = 2. * np.log(2.0) * e1.scale_radius
print('true e1 fwhm = ', e1_fwhm)
# Test with the default scale and size.
test_fwhm = e1.calculateFWHM()
print('e1.calculateFWHM = ', test_fwhm)
print('ratio - 1 = ', test_fwhm / e1_fwhm - 1)
np.testing.assert_almost_equal(
test_fwhm / e1_fwhm,
1.0,
decimal=3,
err_msg="Exponential.calculateFWHM() is not accurate.")
# The default scale already accurate to around 3 dp. Using scale = 0.1 is accurate to 7 dp.
# We can also decrease the size, which should still be accurate, but maybe a little faster.
# Go a bit more that fwhm in units of the pixels.
size = int(1.2 * e1_fwhm / 0.1)
test_fwhm = e1.calculateFWHM(scale=0.1, size=size)
print('e1.calculateFWHM(scale=0.1) = ', test_fwhm)
print('ratio - 1 = ', test_fwhm / e1_fwhm - 1)
np.testing.assert_almost_equal(
test_fwhm / e1_fwhm,
1.0,
decimal=7,
err_msg="Exponential.calculateFWHM(scale=0.1) is not accurate.")
# Check that it works if the centroid is not at the origin
e3 = e1.shift(2, 3)
test_fwhm = e3.calculateFWHM(scale=0.1)
print('e3.calculateFWHM(scale=0.1) = ', test_fwhm)
print('ratio - 1 = ', test_fwhm / e1_fwhm - 1)
np.testing.assert_almost_equal(
test_fwhm / e1_fwhm,
1.0,
decimal=6,
err_msg="shifted Exponential FWHM is not accurate.")
# Can set a centroid manually. This should be equivalent to the default.
print('e3.centroid = ', e3.centroid())
test_fwhm = e3.calculateFWHM(scale=0.1, centroid=e3.centroid())
np.testing.assert_almost_equal(
test_fwhm / e1_fwhm,
1.0,
decimal=6,
err_msg="shifted FWHM with explicit centroid is not accurate.")
# Check the image version.
im = e1.drawImage(scale=0.1, method='sb')
test_fwhm = im.calculateFWHM(Imax=e1.xValue(0, 0))
print('im.calculateFWHM() = ', test_fwhm)
print('ratio - 1 = ', test_fwhm / e1_fwhm - 1)
np.testing.assert_almost_equal(
test_fwhm / e1_fwhm,
1.0,
decimal=6,
err_msg="image.calculateFWHM is not accurate.")
# Check that a non-square image works correctly. Also, not centered anywhere in particular.
bounds = galsim.BoundsI(-1234, -1234 + size * 2, 8234, 8234 + size)
offset = galsim.PositionD(29, 1)
im = e1.drawImage(scale=0.1, bounds=bounds, offset=offset, method='sb')
test_fwhm = im.calculateFWHM(Imax=e1.xValue(0, 0),
center=im.trueCenter() + offset)
print('im.calculateFWHM() = ', test_fwhm)
print('ratio - 1 = ', test_fwhm / e1_fwhm - 1)
np.testing.assert_almost_equal(
test_fwhm / e1_fwhm,
1.0,
decimal=6,
err_msg="non-square image.calculateFWHM is not accurate.")
def test_sigma():
"""Test the calculateMomentRadius method.
"""
import time
t1 = time.time()
# Compare the calculation for a simple Gaussian.
g1 = galsim.Gaussian(sigma=5, flux=1.7)
print 'g1 native sigma = ',g1.sigma
print 'g1.calculateMomentRadius = ',g1.calculateMomentRadius()
# These should be exactly equal.
np.testing.assert_equal(
g1.sigma, g1.calculateMomentRadius(),
err_msg="Gaussian.calculateMomentRadius() returned wrong value.")
np.testing.assert_equal(
g1.sigma, g1.calculateMomentRadius(rtype='trace'),
err_msg="Gaussian.calculateMomentRadius(trace) returned wrong value.")
np.testing.assert_equal(
g1.sigma, g1.calculateMomentRadius(rtype='det'),
err_msg="Gaussian.calculateMomentRadius(det) returned wrong value.")
np.testing.assert_equal(
(g1.sigma, g1.sigma), g1.calculateMomentRadius(rtype='both'),
err_msg="Gaussian.calculateMomentRadius(both) returned wrong value.")
# Check for a convolution of two Gaussians. Should be equivalent, but now will need to
# do the calculation.
g2 = galsim.Convolve(galsim.Gaussian(sigma=3, flux=1.3), galsim.Gaussian(sigma=4, flux=23))
test_sigma = g2.calculateMomentRadius()
print 'g2.calculateMomentRadius = ',test_sigma
print 'ratio - 1 = ',test_sigma/g1.sigma-1
np.testing.assert_almost_equal(
test_sigma/g1.sigma, 1.0, decimal=1,
err_msg="Gaussian.calculateMomentRadius() is not accurate.")
# The default scale and size is only accurate to around 1 dp. Using scale = 0.1 is accurate
# to 4 dp.
test_sigma = g2.calculateMomentRadius(scale=0.1)
print 'g2.calculateMomentRadius(scale=0.1) = ',test_sigma
print 'ratio - 1 = ',test_sigma/g1.sigma-1
np.testing.assert_almost_equal(
test_sigma/g1.sigma, 1.0, decimal=4,
err_msg="Gaussian.calculateMomentRadius(scale=0.1) is not accurate.")
# In this case, the different calculations are eqivalent:
np.testing.assert_almost_equal(
test_sigma, g2.calculateMomentRadius(scale=0.1, rtype='trace'),
err_msg="Gaussian.calculateMomentRadius(trace) is not accurate.")
np.testing.assert_almost_equal(
test_sigma, g2.calculateMomentRadius(scale=0.1, rtype='det'),
err_msg="Gaussian.calculateMomentRadius(trace) is not accurate.")
np.testing.assert_almost_equal(
(test_sigma, test_sigma), g2.calculateMomentRadius(scale=0.1, rtype='both'),
err_msg="Gaussian.calculateMomentRadius(trace) is not accurate.")
# However, when we shear it, the default (det) measure stays equal to the original sigma, but
# the trace measure increases by a factor of (1-e^2)^0.25
g3 = g2.shear(e1=0.4, e2=0.3)
esq = 0.4**2 + 0.3**2
sheared_sigma = g3.calculateMomentRadius(scale=0.1)
print 'g3.calculateMomentRadius(scale=0.1) = ',sheared_sigma
print 'ratio - 1 = ',sheared_sigma/g1.sigma-1
sheared_sigma2 = g3.calculateMomentRadius(scale=0.1, rtype='trace')
print 'g3.calculateMomentRadius(scale=0.1,trace) = ',sheared_sigma2
print 'ratio = ',sheared_sigma2 / g1.sigma
print '(1-e^2)^-0.25 = ',(1-esq)**-0.25
print 'ratio - 1 = ',sheared_sigma2/(g1.sigma*(1.-esq)**-0.25)-1
np.testing.assert_almost_equal(
sheared_sigma/g1.sigma, 1.0, decimal=4,
err_msg="sheared Gaussian.calculateMomentRadius(scale=0.1) is not accurate.")
np.testing.assert_almost_equal(
sheared_sigma2/(g1.sigma*(1.-esq)**-0.25), 1.0, decimal=4,
err_msg="sheared Gaussian.calculateMomentRadius(scale=0.1,trace) is not accurate.")
# Next, use an Exponential profile
e1 = galsim.Exponential(scale_radius=5, flux=1.7)
# The true "sigma" for this is analytic, but not an attribute.
e1_sigma = np.sqrt(3.0) * e1.scale_radius
print 'true e1 sigma = sqrt(3) * e1.scale_radius = ',e1_sigma
# Test with the default scale and size.
test_sigma = e1.calculateMomentRadius()
print 'e1.calculateMomentRadius = ',test_sigma
print 'ratio - 1 = ',test_sigma/e1_sigma-1
np.testing.assert_almost_equal(
test_sigma/e1_sigma, 1.0, decimal=1,
err_msg="Exponential.calculateMomentRadius() is not accurate.")
# The default scale and size is only accurate to around 1 dp. This time we have to both
# decrease the scale and also increase the size to get 4 dp of precision.
test_sigma = e1.calculateMomentRadius(scale=0.1, size=2000)
print 'e1.calculateMomentRadius(scale=0.1) = ',test_sigma
print 'ratio - 1 = ',test_sigma/e1_sigma-1
np.testing.assert_almost_equal(
test_sigma/e1_sigma, 1.0, decimal=4,
err_msg="Exponential.calculateMomentRadius(scale=0.1) is not accurate.")
# Check that it works if the centroid is not at the origin
e3 = e1.shift(2,3)
test_sigma = e3.calculateMomentRadius(scale=0.1, size=2000)
print 'e1.calculateMomentRadius(scale=0.1) = ',test_sigma
print 'ratio - 1 = ',test_sigma/e1_sigma-1
np.testing.assert_almost_equal(
test_sigma/e1_sigma, 1.0, decimal=4,
err_msg="shifted Exponential MomentRadius is not accurate.")
# Can set a centroid manually. This should be equivalent to the default.
print 'e3.centroid = ',e3.centroid()
test_sigma = e3.calculateMomentRadius(scale=0.1, size=2000, centroid=e3.centroid())
np.testing.assert_almost_equal(
test_sigma/e1_sigma, 1.0, decimal=4,
err_msg="shifted MomentRadius with explicit centroid is not accurate.")
# Check the image version.
size = 2000
im = e1.drawImage(scale=0.1, nx=size, ny=size)
test_sigma = im.calculateMomentRadius(flux=e1.flux)
print 'im.calculateMomentRadius() = ',test_sigma
print 'ratio - 1 = ',test_sigma/e1_sigma-1
np.testing.assert_almost_equal(
test_sigma/e1_sigma, 1.0, decimal=4,
err_msg="image.calculateMomentRadius is not accurate.")
# Check that a non-square image works correctly. Also, not centered anywhere in particular.
bounds = galsim.BoundsI(-1234, -1234+size*2, 8234, 8234+size)
offset = galsim.PositionD(29,1)
im = e1.drawImage(scale=0.1, bounds=bounds, offset=offset)
test_hlr = im.calculateMomentRadius(flux=e1.flux, center=im.trueCenter()+offset)
print 'im.calculateMomentRadius() = ',test_sigma
print 'ratio - 1 = ',test_sigma/e1_sigma-1
np.testing.assert_almost_equal(
test_sigma/e1_sigma, 1.0, decimal=4,
err_msg="non-square image.calculateMomentRadius is not accurate.")
t2 = time.time()
print 'time for %s = %.2f'%(funcname(),t2-t1)
def galSimFakeSersic(flux,
gal,
psfImage=None,
scaleRad=False,
returnObj=True,
expAll=False,
devAll=False,
plotFake=False,
trunc=0,
drawMethod="auto",
addPoisson=False,
scale=1.0,
transform=None,
addShear=False):
"""
Make a fake single Sersic galaxy using the galSim.Sersic function
Inputs: total flux of the galaxy, and a record array that stores the
necessary parameters [reffPix, nSersic, axisRatio, posAng]
Output: a 2-D image array of the galaxy model OR
a GalSim object of the model
Options:
psfImage: PSF image for convolution
trunc: Flux of Sersic models will truncate at trunc * reffPix
radius; trunc=0 means no truncation
drawMethod: The method for drawImage: ['auto', 'fft', 'real_space']
addPoisson: Add Poisson noise
plotFake: Generate a PNG figure of the model
expAll: Input model will be seen as nSersic=1
devAll: Input model will be seen as nSersic=4
returnObj: If TRUE, will return the GSObj, instead of the image array
"""
# Convert the numpy.float32 into normal float format
nSersic = float(gal["sersic_n"])
reff = float(gal["reff"])
axisRatio = float(gal["b_a"])
posAng = float(gal["theta"])
# Truncate the flux at trunc x reff
if trunc > 0:
trunc = trunc * reff
# Make sure Sersic index is not too large
if nSersic > 6.0:
raise ValueError("Sersic index is too large! Should be <= 6.0")
# Check the axisRatio value
if axisRatio <= 0.24:
raise ValueError("Axis Ratio is too small! Should be >= 0.24")
# Make the Sersic model based on flux, re, and Sersic index
if nSersic == 1.0 or expAll:
if scaleRad:
serObj = galsim.Exponential(scale_radius=reff)
else:
serObj = galsim.Exponential(half_light_radius=reff)
if expAll:
print " * This model is treated as a n=1 Exponential disk : %d" % (
gal["ID"])
elif nSersic == 4.0 or devAll:
serObj = galsim.DeVaucouleurs(half_light_radius=reff, trunc=trunc)
if devAll:
print " * This model is treated as a n=4 De Vaucouleurs model: %d" % (
gal["ID"])
elif nSersic <= 0.9:
serObj = galsim.Sersic(nSersic, half_light_radius=reff)
else:
serObj = galsim.Sersic(nSersic, half_light_radius=reff, trunc=trunc)
# If necessary, apply the Axis Ratio (q=b/a) using the Shear method
if axisRatio < 1.0:
serObj = serObj.shear(q=axisRatio, beta=0.0 * galsim.degrees)
# If necessary, apply the Position Angle (theta) using the Rotate method
#if posAng != 0.0 or posAng != 180.0:
serObj = serObj.rotate((90.0 - posAng) * galsim.degrees)
# If necessary, apply addtion shear (e.g. for weak lensing test)
if addShear:
try:
g1 = float(gal['g1'])
g2 = float(gal['g2'])
serObj = serObj.shear(g1=g1, g2=g2)
except ValueError:
# TODO: Should check other options
warnings.warn(
"Can not find g1 or g2 in the input! No shear has been added!")
#do the transformation from sky to pixel coordinates, if given
if transform is not None:
serObj = serObj.transform(*tuple(transform.ravel()))
# Convolve the Sersic model using the provided PSF image
if psfImage is not None:
# Convert the PSF Image Array into a GalSim Object
# Norm=True by default
psfObj = arrayToGSObj(psfImage, norm=True)
serFinal = galsim.Convolve([serObj, psfObj])
else:
serFinal = serObj
# Pass the flux to the object
serFinal = serFinal.withFlux(float(flux))
# Make a PNG figure of the fake galaxy to check if everything is Ok
# TODO: For test, should be removed later
if plotFake:
plotFakeGalaxy(serFinal, galID=gal['ID'])
# Now, by default, the function will just return the GSObj
if returnObj:
return serFinal
else:
return galSimDrawImage(serFinal,
method=drawMethod,
scale=scale,
addPoisson=addPoisson)
def main(argv):
"""
Make a fits image cube where each frame has two images of the same galaxy drawn
with regular FFT convolution and with photon shooting.
We do this for 5 different PSFs and 5 different galaxies, each with 4 different (random)
fluxes, sizes, and shapes.
"""
logging.basicConfig(format="%(message)s",
level=logging.INFO,
stream=sys.stdout)
logger = logging.getLogger("demo7")
# To turn off logging:
#logger.propagate = False
# To turn on the debugging messages:
#logger.setLevel(logging.DEBUG)
# Define some parameters we'll use below.
# Make output directory if not already present.
if not os.path.isdir('output'):
os.mkdir('output')
file_name = os.path.join('output', 'cube_phot.fits.gz')
random_seed = 553728
sky_level = 1.e4 # ADU / arcsec^2
pixel_scale = 0.28 # arcsec
nx = 64
ny = 64
gal_flux_min = 1.e4 # Range for galaxy flux
gal_flux_max = 1.e5
gal_hlr_min = 0.3 # arcsec
gal_hlr_max = 1.3 # arcsec
gal_e_min = 0. # Range for ellipticity
gal_e_max = 0.8
psf_fwhm = 0.65 # arcsec
# This script is set up as a comparison between using FFTs for doing the convolutions and
# shooting photons. The two methods have trade-offs in speed and accuracy which vary
# with the kind of profile being drawn and the S/N of the object, among other factors.
# In addition, for each method, there are a number of parameters GalSim uses that control
# aspects of the calculation that further affect the speed and accuracy.
#
# We encapsulate these parameters with an object called GSParams. The default values
# are intended to be accurate enough for normal precision shear tests, without sacrificing
# too much speed.
#
# Any PSF or galaxy object can be given a gsparams argument on construction that can
# have different values to make the calculation more or less accurate (typically trading
# off for speed or memory).
#
# In this script, we adjust some of the values slightly, just to show you how it works.
# You could play around with these values and see what effect they have on the drawn images.
# Usually, it requires a pretty drastic change in these parameters for you to be able to
# notice the difference by eye. But subtle effects that may impact the shapes of galaxies
# can happen well before then.
# Type help(galsim.GSParams) for the complete list of parameters and more detailed
# documentation, including the default values for each parameter.
gsparams = galsim.GSParams(
folding_threshold=
1.e-2, # maximum fractional flux that may be folded around edge of FFT
maxk_threshold=
2.e-3, # k-values less than this may be excluded off edge of FFT
xvalue_accuracy=
1.e-4, # approximations in real space aim to be this accurate
kvalue_accuracy=
1.e-4, # approximations in fourier space aim to be this accurate
shoot_accuracy=
1.e-4, # approximations in photon shooting aim to be this accurate
minimum_fft_size=64) # minimum size of ffts
logger.info('Starting demo script 7')
# Make the PSF profiles:
psf1 = galsim.Gaussian(fwhm=psf_fwhm, gsparams=gsparams)
psf2 = galsim.Moffat(fwhm=psf_fwhm, beta=2.4, gsparams=gsparams)
psf3_inner = galsim.Gaussian(fwhm=psf_fwhm, flux=0.8, gsparams=gsparams)
psf3_outer = galsim.Gaussian(fwhm=2 * psf_fwhm,
flux=0.2,
gsparams=gsparams)
psf3 = psf3_inner + psf3_outer
atmos = galsim.Gaussian(fwhm=psf_fwhm, gsparams=gsparams)
# The OpticalPSF and set of Zernike values chosen below correspond to a reasonably well aligned,
# smallish ~0.3m / 12 inch diameter telescope with a central obscuration of ~0.12m or 5 inches
# diameter, being used in optical wavebands.
# In the Noll convention, the value of the Zernike coefficient also gives the RMS optical path
# difference across a circular pupil. An RMS difference of ~0.5 or larger indicates that parts
# of the wavefront are in fully destructive interference, and so we might expect aberrations to
# become strong when Zernike aberrations summed in quadrature approach 0.5 wave.
# The aberrations chosen in this case correspond to operating close to a 0.25 wave RMS optical
# path difference. Unlike in demo3, we specify the aberrations by making a list that we pass
# in using the 'aberrations' kwarg. The order of aberrations starting from index 4 is defocus,
# astig1, astig2, coma1, coma2, trefoil1, trefoil2, spher as in the Noll convention.
# We ignore the first 4 values so that the index number corresponds to the Zernike index
# in the Noll convention. This will be particularly convenient once we start allowing
# coefficients beyond spherical (index 11). c.f. The Wikipedia page about the Noll indices:
#
# http://en.wikipedia.org/wiki/Zernike_polynomials#Zernike_polynomials
aberrations = [0.0] * 12 # Set the initial size.
aberrations[4] = 0.06 # Noll index 4 = Defocus
aberrations[5:7] = [0.12, -0.08] # Noll index 5,6 = Astigmatism
aberrations[7:9] = [0.07, 0.04] # Noll index 7,8 = Coma
aberrations[11] = -0.13 # Noll index 11 = Spherical
# You could also define these all at once if that is more convenient:
#aberrations = [0.0, 0.0, 0.0, 0.0, 0.06, 0.12, -0.08, 0.07, 0.04, 0.0, 0.0, -0.13]
optics = galsim.OpticalPSF(lam_over_diam=0.6 * psf_fwhm,
obscuration=0.4,
aberrations=aberrations,
gsparams=gsparams)
psf4 = galsim.Convolve([atmos, optics
]) # Convolve inherits the gsparams from the first
# item in the list. (Or you can supply a gsparams
# argument explicitly if you want to override this.)
atmos = galsim.Kolmogorov(fwhm=psf_fwhm, gsparams=gsparams)
optics = galsim.Airy(lam_over_diam=0.3 * psf_fwhm, gsparams=gsparams)
psf5 = galsim.Convolve([atmos, optics])
psfs = [psf1, psf2, psf3, psf4, psf5]
psf_names = [
"Gaussian", "Moffat", "Double Gaussian", "OpticalPSF",
"Kolmogorov * Airy"
]
psf_times = [0, 0, 0, 0, 0]
psf_fft_times = [0, 0, 0, 0, 0]
psf_phot_times = [0, 0, 0, 0, 0]
# Make the galaxy profiles:
gal1 = galsim.Gaussian(half_light_radius=1, gsparams=gsparams)
gal2 = galsim.Exponential(half_light_radius=1, gsparams=gsparams)
gal3 = galsim.DeVaucouleurs(half_light_radius=1, gsparams=gsparams)
gal4 = galsim.Sersic(half_light_radius=1, n=2.5, gsparams=gsparams)
# A Sersic profile may be truncated if desired.
# The units for this are expected to be arcsec (or specifically -- whatever units
# you are using for all the size values as defined by the pixel_scale).
bulge = galsim.Sersic(half_light_radius=0.7,
n=3.2,
trunc=8.5,
gsparams=gsparams)
disk = galsim.Sersic(half_light_radius=1.2, n=1.5, gsparams=gsparams)
gal5 = 0.4 * bulge + 0.6 * disk # Net half-light radius is only approximate for this one.
gals = [gal1, gal2, gal3, gal4, gal5]
gal_names = [
"Gaussian", "Exponential", "Devaucouleurs", "n=2.5 Sersic",
"Bulge + Disk"
]
gal_times = [0, 0, 0, 0, 0]
gal_fft_times = [0, 0, 0, 0, 0]
gal_phot_times = [0, 0, 0, 0, 0]
# Other times to keep track of:
setup_times = 0
fft_times = 0
phot_times = 0
noise_times = 0
# Loop over combinations of psf, gal, and make 4 random choices for flux, size, shape.
all_images = []
k = 0
for ipsf in range(len(psfs)):
psf = psfs[ipsf]
psf_name = psf_names[ipsf]
logger.info('psf %d: %s', ipsf + 1, psf)
# Note that this implicitly calls str(psf). We've made an effort to give all GalSim
# objects an informative but relatively succinct str representation. Some details may
# be missing, but it should look essentially like how you would create the object.
logger.debug('repr = %r', psf)
# The repr() version are a bit more pedantic in form and should be completely informative,
# to the point where two objects that are not identical should never have equal repr
# strings. As such the repr strings may in some cases be somewhat unwieldy. For instance,
# since we set non-default gsparams in these, the repr includes that information, but
# it is omitted from the str for brevity.
for igal in range(len(gals)):
gal = gals[igal]
gal_name = gal_names[igal]
logger.info(' galaxy %d: %s', igal + 1, gal)
logger.debug(' repr = %r', gal)
for i in range(4):
logger.debug(' Start work on image %d', i)
t1 = time.time()
# Initialize the random number generator we will be using.
rng = galsim.UniformDeviate(random_seed + k + 1)
# Generate random variates:
flux = rng() * (gal_flux_max - gal_flux_min) + gal_flux_min
# Use a new variable name, since we'll want to keep the original unmodified.
this_gal = gal.withFlux(flux)
hlr = rng() * (gal_hlr_max - gal_hlr_min) + gal_hlr_min
this_gal = this_gal.dilate(hlr)
beta_ellip = rng() * 2 * math.pi * galsim.radians
ellip = rng() * (gal_e_max - gal_e_min) + gal_e_min
gal_shape = galsim.Shear(e=ellip, beta=beta_ellip)
this_gal = this_gal.shear(gal_shape)
# Build the final object by convolving the galaxy and PSF.
final = galsim.Convolve([this_gal, psf])
# Create the large, double width output image
# Rather than provide a scale= argument to the drawImage commands, we can also
# set the pixel scale in the image constructor.
# Note: You can also change it after the construction with im.scale=pixel_scale
image = galsim.ImageF(2 * nx + 2, ny, scale=pixel_scale)
# Assign the following two Image "views", fft_image and phot_image.
# Using the syntax below, these are views into the larger image.
# Changes/additions to the sub-images referenced by the views are automatically
# reflected in the original image.
fft_image = image[galsim.BoundsI(1, nx, 1, ny)]
phot_image = image[galsim.BoundsI(nx + 3, 2 * nx + 2, 1, ny)]
logger.debug(
' Read in training sample galaxy and PSF from file')
t2 = time.time()
# Draw the profile
# This default rendering method (method='auto') usually defaults to FFT, since
# that is normally the most efficient method. However, we can also set method
# to 'fft' explicitly to force it to always use FFTs for the convolution
# by the pixel response. (In this case, it doesn't have any effect, since
# the 'auto' method would have always chosen 'fft' anyway, so this is just
# for illustrative purposes.)
final.drawImage(fft_image, method='fft')
logger.debug(
' Drew fft image. Total drawn flux = %f. .flux = %f',
fft_image.array.sum(), final.getFlux())
t3 = time.time()
# Add Poisson noise
sky_level_pixel = sky_level * pixel_scale**2
fft_image.addNoise(
galsim.PoissonNoise(rng, sky_level=sky_level_pixel))
t4 = time.time()
# The next two lines are just to get the output from this demo script
# to match the output from the parsing of demo7.yaml.
rng = galsim.UniformDeviate(random_seed + k + 1)
rng()
rng()
rng()
rng()
# Repeat for photon shooting image.
# The max_extra_noise parameter indicates how much extra noise per pixel we are
# willing to tolerate. The sky noise will be adding a variance of sky_level_pixel,
# so we allow up to 1% of that extra.
final.drawImage(phot_image,
method='phot',
max_extra_noise=sky_level_pixel / 100,
rng=rng)
t5 = time.time()
# For photon shooting, galaxy already has Poisson noise, so we want to make
# sure not to add that noise again! Thus, we just add sky noise, which
# is Poisson with the mean = sky_level_pixel
pd = galsim.PoissonDeviate(rng, mean=sky_level_pixel)
# DeviateNoise just adds the action of the given deviate to every pixel.
phot_image.addNoise(galsim.DeviateNoise(pd))
# For PoissonDeviate, the mean is not zero, so for a background-subtracted
# image, we need to subtract the mean back off when we are done.
phot_image -= sky_level_pixel
logger.debug(
' Added Poisson noise. Image fluxes are now %f and %f',
fft_image.array.sum(), phot_image.array.sum())
t6 = time.time()
# Store that into the list of all images
all_images += [image]
k = k + 1
logger.info(
' %d: flux = %.2e, hlr = %.2f, ellip = (%.2f,%.2f)',
k, flux, hlr, gal_shape.getE1(), gal_shape.getE2())
logger.debug(' Times: %f, %f, %f, %f, %f', t2 - t1,
t3 - t2, t4 - t3, t5 - t4, t6 - t5)
psf_times[ipsf] += t6 - t1
psf_fft_times[ipsf] += t3 - t2
psf_phot_times[ipsf] += t5 - t4
gal_times[igal] += t6 - t1
gal_fft_times[igal] += t3 - t2
gal_phot_times[igal] += t5 - t4
setup_times += t2 - t1
fft_times += t3 - t2
phot_times += t5 - t4
noise_times += t4 - t3 + t6 - t5
logger.info('Done making images of galaxies')
logger.info('')
logger.info('Some timing statistics:')
logger.info(' Total time for setup steps = %f', setup_times)
logger.info(' Total time for regular fft drawing = %f', fft_times)
logger.info(' Total time for photon shooting = %f', phot_times)
logger.info(' Total time for adding noise = %f', noise_times)
logger.info('')
logger.info('Breakdown by PSF type:')
for ipsf in range(len(psfs)):
logger.info(' %s: Total time = %f (fft: %f, phot: %f)',
psf_names[ipsf], psf_times[ipsf], psf_fft_times[ipsf],
psf_phot_times[ipsf])
logger.info('')
logger.info('Breakdown by Galaxy type:')
for igal in range(len(gals)):
logger.info(' %s: Total time = %f (fft: %f, phot: %f)',
gal_names[igal], gal_times[igal], gal_fft_times[igal],
gal_phot_times[igal])
logger.info('')
# Now write the image to disk.
# With any write command, you can optionally compress the file using several compression
# schemes:
# 'gzip' uses gzip on the full output file.
# 'bzip2' uses bzip2 on the full output file.
# 'rice' uses rice compression on the image, leaving the fits headers readable.
# 'gzip_tile' uses gzip in tiles on the output image, leaving the fits headers readable.
# 'hcompress' uses hcompress on the image, but it is only valid for 2-d data, so it
# doesn't work for writeCube.
# 'plio' uses plio on the image, but it is only valid for positive integer data.
# Furthermore, the first three have standard filename extensions associated with them,
# so if you don't specify a compression, but the filename ends with '.gz', '.bz2' or '.fz',
# the corresponding compression will be selected automatically.
# In other words, the `compression='gzip'` specification is actually optional here:
galsim.fits.writeCube(all_images, file_name, compression='gzip')
logger.info('Wrote fft image to fits data cube %r', file_name)
def _run_ml(*, n_sims, rng, dudx, dudy, dvdx, dvdy):
"""Run metacal on an image composed of stamps w/ constant noise.
Parameters
----------
n_sims : int
The number of objects to run.
rng : np.random.RandomState
An RNG to use.
dudx : float
The du/dx Jacobian component.
dudy : float
The du/dy Jacobian component.
dydx : float
The dv/dx Jacobian component.
dvdy : float
The dv/dy Jacobian component.
Returns
-------
result : dict
A dictionary with each of the metacal catalogs.
"""
method = 'no_pixel'
stamp_size = 33
psf_stamp_size = 33
cen = (stamp_size - 1) / 2
psf_cen = (psf_stamp_size - 1) / 2
s2n = 1e16
flux = 1e6
galsim_jac = galsim.JacobianWCS(dudx=dudx, dudy=dudy, dvdx=dvdx, dvdy=dvdy)
gal = galsim.Exponential(half_light_radius=0.5).withFlux(flux)
psf = galsim.Gaussian(fwhm=0.9).withFlux(1)
obj = galsim.Convolve(gal, psf)
obj_im = obj.drawImage(nx=111, ny=111).array
noise = np.sqrt(np.sum(obj_im**2)) / s2n
data = []
for ind in tqdm.trange(n_sims):
################################
# make the obs
# psf
psf_im = psf.drawImage(nx=psf_stamp_size,
ny=psf_stamp_size,
wcs=galsim_jac,
method=method).array
psf_noise = np.sqrt(np.sum(psf_im**2)) / 10000
wgt = np.ones_like(psf_im) / psf_noise**2
psf_im += (rng.normal(size=psf_im.shape) * psf_noise)
psf_jac = ngmix.Jacobian(x=psf_cen,
y=psf_cen,
dudx=dudx,
dudy=dudy,
dvdx=dvdx,
dvdy=dvdy)
psf_obs = ngmix.Observation(image=psf_im, weight=wgt, jacobian=psf_jac)
# now render object
scale = psf_jac.scale
shift = rng.uniform(low=-scale / 2, high=scale / 2, size=2)
_obj = obj.shift(dx=shift[0], dy=shift[1])
xy = galsim_jac.toImage(galsim.PositionD(shift))
im = _obj.drawImage(nx=stamp_size,
ny=stamp_size,
wcs=galsim_jac,
method=method).array
jac = ngmix.Jacobian(x=cen + xy.x,
y=cen + xy.y,
dudx=dudx,
dudy=dudy,
dvdx=dvdx,
dvdy=dvdy)
wgt = np.ones_like(im) / noise**2
nse = rng.normal(size=im.shape) * noise
im += (rng.normal(size=im.shape) * noise)
obs = ngmix.Observation(image=im,
weight=wgt,
noise=nse,
bmask=np.zeros_like(im, dtype=np.int32),
ormask=np.zeros_like(im, dtype=np.int32),
jacobian=jac,
psf=psf_obs)
# build the mbobs
mbobs = ngmix.MultiBandObsList()
obslist = ngmix.ObsList()
obslist.append(obs)
mbobs.append(obslist)
mbobs.meta['id'] = ind + 1
# these settings do not matter that much I think
mbobs[0].meta['Tsky'] = 1
mbobs[0].meta['magzp_ref'] = 26.5
mbobs[0][0].meta['orig_col'] = ind + 1
mbobs[0][0].meta['orig_row'] = ind + 1
################################
# run the fitters
try:
res = _run_ml_fitter(mbobs, rng)
except Exception as e:
print('err:', e, type(e))
res = None
if res is not None:
data.append(res)
if len(data) > 0:
res = data
else:
res = None
return res
def test_operations_simple():
"""Simple test of operations on InterpolatedImage: shear, magnification, rotation, shifting."""
import time
t1 = time.time()
# Make some nontrivial image that can be described in terms of sums and convolutions of
# GSObjects. We want this to be somewhat hard to describe, but should be at least
# critically-sampled, so put in an Airy PSF.
gal_flux = 1000.
pix_scale = 0.03 # arcsec
bulge_frac = 0.3
bulge_hlr = 0.3 # arcsec
bulge_e = 0.15
bulge_pos_angle = 30. * galsim.degrees
disk_hlr = 0.6 # arcsec
disk_e = 0.5
disk_pos_angle = 60. * galsim.degrees
lam = 800 # nm NB: don't use lambda - that's a reserved word.
tel_diam = 2.4 # meters
lam_over_diam = lam * 1.e-9 / tel_diam # radians
lam_over_diam *= 206265 # arcsec
im_size = 512
bulge = galsim.Sersic(4, half_light_radius=bulge_hlr)
bulge.applyShear(e=bulge_e, beta=bulge_pos_angle)
disk = galsim.Exponential(half_light_radius=disk_hlr)
disk.applyShear(e=disk_e, beta=disk_pos_angle)
gal = bulge_frac * bulge + (1. - bulge_frac) * disk
gal.setFlux(gal_flux)
psf = galsim.Airy(lam_over_diam)
pix = galsim.Pixel(pix_scale)
obj = galsim.Convolve(gal, psf, pix)
im = obj.draw(dx=pix_scale)
# Turn it into an InterpolatedImage with default param settings
int_im = galsim.InterpolatedImage(im)
# Shear it, and compare with expectations from GSObjects directly
test_g1 = -0.07
test_g2 = 0.1
test_decimal = 2 # in % difference, i.e. 2 means 1% agreement
comp_region = 30 # compare the central region of this linear size
test_int_im = int_im.createSheared(g1=test_g1, g2=test_g2)
ref_obj = obj.createSheared(g1=test_g1, g2=test_g2)
# make large images
im = galsim.ImageD(im_size, im_size)
ref_im = galsim.ImageD(im_size, im_size)
test_int_im.draw(image=im, dx=pix_scale)
ref_obj.draw(image=ref_im, dx=pix_scale)
# define subregion for comparison
new_bounds = galsim.BoundsI(1, comp_region, 1, comp_region)
new_bounds.shift((im_size - comp_region) / 2, (im_size - comp_region) / 2)
im_sub = im.subImage(new_bounds)
ref_im_sub = ref_im.subImage(new_bounds)
diff_im = im_sub - ref_im_sub
rel = diff_im / im_sub
zeros_arr = np.zeros((comp_region, comp_region))
# require relative difference to be smaller than some amount
np.testing.assert_array_almost_equal(
rel.array,
zeros_arr,
test_decimal,
err_msg='Sheared InterpolatedImage disagrees with reference')
# Magnify it, and compare with expectations from GSObjects directly
test_mag = 1.08
test_decimal = 2 # in % difference, i.e. 2 means 1% agreement
comp_region = 30 # compare the central region of this linear size
test_int_im = int_im.createMagnified(test_mag)
ref_obj = obj.createMagnified(test_mag)
# make large images
im = galsim.ImageD(im_size, im_size)
ref_im = galsim.ImageD(im_size, im_size)
test_int_im.draw(image=im, dx=pix_scale)
ref_obj.draw(image=ref_im, dx=pix_scale)
# define subregion for comparison
new_bounds = galsim.BoundsI(1, comp_region, 1, comp_region)
new_bounds.shift((im_size - comp_region) / 2, (im_size - comp_region) / 2)
im_sub = im.subImage(new_bounds)
ref_im_sub = ref_im.subImage(new_bounds)
diff_im = im_sub - ref_im_sub
rel = diff_im / im_sub
zeros_arr = np.zeros((comp_region, comp_region))
# require relative difference to be smaller than some amount
np.testing.assert_array_almost_equal(
rel.array,
zeros_arr,
test_decimal,
err_msg='Magnified InterpolatedImage disagrees with reference')
# Lens it (shear and magnify), and compare with expectations from GSObjects directly
test_g1 = -0.03
test_g2 = -0.04
test_mag = 0.74
test_decimal = 2 # in % difference, i.e. 2 means 1% agreement
comp_region = 30 # compare the central region of this linear size
test_int_im = int_im.createLensed(test_g1, test_g2, test_mag)
ref_obj = obj.createLensed(test_g1, test_g2, test_mag)
# make large images
im = galsim.ImageD(im_size, im_size)
ref_im = galsim.ImageD(im_size, im_size)
test_int_im.draw(image=im, dx=pix_scale)
ref_obj.draw(image=ref_im, dx=pix_scale)
# define subregion for comparison
new_bounds = galsim.BoundsI(1, comp_region, 1, comp_region)
new_bounds.shift((im_size - comp_region) / 2, (im_size - comp_region) / 2)
im_sub = im.subImage(new_bounds)
ref_im_sub = ref_im.subImage(new_bounds)
diff_im = im_sub - ref_im_sub
rel = diff_im / im_sub
zeros_arr = np.zeros((comp_region, comp_region))
# require relative difference to be smaller than some amount
np.testing.assert_array_almost_equal(
rel.array,
zeros_arr,
test_decimal,
err_msg='Lensed InterpolatedImage disagrees with reference')
# Rotate it, and compare with expectations from GSObjects directly
test_rot_angle = 32. * galsim.degrees
test_decimal = 2 # in % difference, i.e. 2 means 1% agreement
comp_region = 30 # compare the central region of this linear size
test_int_im = int_im.createRotated(test_rot_angle)
ref_obj = obj.createRotated(test_rot_angle)
# make large images
im = galsim.ImageD(im_size, im_size)
ref_im = galsim.ImageD(im_size, im_size)
test_int_im.draw(image=im, dx=pix_scale)
ref_obj.draw(image=ref_im, dx=pix_scale)
# define subregion for comparison
new_bounds = galsim.BoundsI(1, comp_region, 1, comp_region)
new_bounds.shift((im_size - comp_region) / 2, (im_size - comp_region) / 2)
im_sub = im.subImage(new_bounds)
ref_im_sub = ref_im.subImage(new_bounds)
diff_im = im_sub - ref_im_sub
rel = diff_im / im_sub
zeros_arr = np.zeros((comp_region, comp_region))
# require relative difference to be smaller than some amount
np.testing.assert_array_almost_equal(
rel.array,
zeros_arr,
test_decimal,
err_msg='Rotated InterpolatedImage disagrees with reference')
# Shift it, and compare with expectations from GSObjects directly
x_shift = -0.31
y_shift = 0.87
test_decimal = 2 # in % difference, i.e. 2 means 1% agreement
comp_region = 30 # compare the central region of this linear size
test_int_im = int_im.createShifted(x_shift, y_shift)
ref_obj = obj.createShifted(x_shift, y_shift)
# make large images
im = galsim.ImageD(im_size, im_size)
ref_im = galsim.ImageD(im_size, im_size)
test_int_im.draw(image=im, dx=pix_scale)
ref_obj.draw(image=ref_im, dx=pix_scale)
# define subregion for comparison
new_bounds = galsim.BoundsI(1, comp_region, 1, comp_region)
new_bounds.shift((im_size - comp_region) / 2, (im_size - comp_region) / 2)
im_sub = im.subImage(new_bounds)
ref_im_sub = ref_im.subImage(new_bounds)
diff_im = im_sub - ref_im_sub
rel = diff_im / im_sub
zeros_arr = np.zeros((comp_region, comp_region))
# require relative difference to be smaller than some amount
np.testing.assert_array_almost_equal(
rel.array,
zeros_arr,
test_decimal,
err_msg='Shifted InterpolatedImage disagrees with reference')
t2 = time.time()
print 'time for %s = %.2f' % (funcname(), t2 - t1)
def test_drawK_Exponential_Moffat():
"""Test the drawK function using known symmetries of the Exponential Hankel transform (which is
a Moffat with beta=1.5).
See http://mathworld.wolfram.com/HankelTransform.html.
"""
import time
t1 = time.time()
test_flux = 4.1 # Choose a non-unity flux
test_scale_radius = 13. # ...likewise for scale_radius
test_imsize = 45 # Dimensions of comparison image, doesn't need to be large
# Define an Exponential GSObject
gal = galsim.Exponential(scale_radius=test_scale_radius, flux=test_flux)
# Then define a related object which is in fact the opposite number in the Hankel transform pair
# For the Exponential we need a Moffat, with scale_radius=1/scale_radius. The total flux under
# this Moffat with unit amplitude at r=0 is is pi * scale_radius**(-2) / (beta - 1)
# = 2. * pi * scale_radius**(-2) in this case, so it works analagously to the Gaussian above.
gal_hankel = galsim.Moffat(beta=1.5,
scale_radius=1. / test_scale_radius,
flux=test_flux * 2. * np.pi /
test_scale_radius**2)
# Do a basic flux test: the total flux of the gal should equal gal_Hankel(k=(0, 0))
np.testing.assert_almost_equal(
gal.getFlux(),
gal_hankel.xValue(galsim.PositionD(0., 0.)),
decimal=12,
err_msg=
"Test object flux does not equal k=(0, 0) mode of its Hankel transform conjugate."
)
image_test = galsim.ImageD(test_imsize, test_imsize)
rekimage_test = galsim.ImageD(test_imsize, test_imsize)
imkimage_test = galsim.ImageD(test_imsize, test_imsize)
# Then compare these two objects at a couple of different scale (reasonably matched for size)
for scale_test in (0.15 / test_scale_radius, 0.6 / test_scale_radius):
gal.drawK(re=rekimage_test, im=imkimage_test, scale=scale_test)
gal_hankel.draw(image_test,
scale=scale_test,
use_true_center=False,
normalization="sb")
np.testing.assert_array_almost_equal(
rekimage_test.array,
image_test.array,
decimal=12,
err_msg=
"Test object drawK() and draw() from Hankel conjugate do not match for grid "
+ "spacing scale = " + str(scale_test))
np.testing.assert_array_almost_equal(
imkimage_test.array,
np.zeros_like(imkimage_test.array),
decimal=12,
err_msg=
"Non-zero imaginary part for drawK from test object that is purely centred on "
+ "the origin.")
t2 = time.time()
print 'time for %s = %.2f' % (funcname(), t2 - t1)
def test_offset():
"""Test the offset parameter to the draw and drawShoot function.
"""
import time
t1 = time.time()
scale = 0.23
# Use some more exact GSParams. We'll be comparing FFT images to real-space convolved values,
# so we don't want to suffer from our overall accuracy being only about 10^-3.
# Update: It turns out the only one I needed to reduce to obtain the accuracy I wanted
# below is maxk_threshold. Perhaps this is a sign that we ought to lower it in general?
params = galsim.GSParams(maxk_threshold=1.e-4)
# We use a simple Exponential for our object:
gal = galsim.Exponential(flux=test_flux, scale_radius=0.5, gsparams=params)
pix = galsim.Pixel(scale, gsparams=params)
obj = galsim.Convolve([gal, pix], gsparams=params)
# The shapes of the images we will build
# Make sure all combinations of odd/even are represented.
shape_list = [(256, 256), (256, 243), (249, 260), (255, 241), (270, 260)]
# Some reasonable (x,y) values at which to test the xValues (near the center)
xy_list = [(128, 128), (123, 131), (126, 124)]
# The offsets to test
offset_list = [(1, -3), (0.3, -0.1), (-2.3, -1.2)]
# Make the images somewhat large so the moments are measured accurately.
for nx, ny in shape_list:
#print '\n\n\nnx,ny = ',nx,ny
# First check that the image agrees with our calculation of the center
cenx = (nx + 1.) / 2.
ceny = (ny + 1.) / 2.
#print 'cen = ',cenx,ceny
im = galsim.ImageD(nx, ny, scale=scale)
true_center = im.bounds.trueCenter()
np.testing.assert_almost_equal(
cenx, true_center.x, 6,
"im.bounds.trueCenter().x is wrong for (nx,ny) = %d,%d" % (nx, ny))
np.testing.assert_almost_equal(
ceny, true_center.y, 6,
"im.bounds.trueCenter().y is wrong for (nx,ny) = %d,%d" % (nx, ny))
# Check that the default draw command puts the centroid in the center of the image.
obj.draw(im, normalization='sb')
moments = getmoments(im)
#print 'moments = ',moments
np.testing.assert_almost_equal(
moments[0], cenx, 5,
"obj.draw(im) not centered correctly for (nx,ny) = %d,%d" %
(nx, ny))
np.testing.assert_almost_equal(
moments[1], ceny, 5,
"obj.draw(im) not centered correctly for (nx,ny) = %d,%d" %
(nx, ny))
# Test that a few pixel values match xValue.
# Note: we don't expect the FFT drawn image to match the xValues precisely, since the
# latter use real-space convolution, so they should just match to our overall accuracy
# requirement, which is something like 1.e-3 or so. But an image of just the galaxy
# should use real-space drawing, so should be pretty much exact.
im2 = galsim.ImageD(nx, ny, scale=scale)
gal.draw(im2, normalization='sb')
for x, y in xy_list:
#print 'x,y = ',x,y
#print 'im(x,y) = ',im(x,y)
u = (x - cenx) * scale
v = (y - ceny) * scale
#print 'xval(x-cenx,y-ceny) = ',obj.xValue(galsim.PositionD(u,v))
np.testing.assert_almost_equal(
im(x, y), obj.xValue(galsim.PositionD(u, v)), 2,
"im(%d,%d) does not match xValue(%f,%f)" % (x, y, u, v))
np.testing.assert_almost_equal(
im2(x, y), gal.xValue(galsim.PositionD(u, v)), 6,
"im2(%d,%d) does not match xValue(%f,%f)" % (x, y, u, v))
# Check that offset moves the centroid by the right amount.
for offx, offy in offset_list:
# For integer offsets, we expect the centroids to come out pretty much exact.
# (Only edge effects of the image should produce any error, and those are very small.)
# However, for non-integer effects, we don't actually expect the centroids to be
# right, even with perfect image rendering. To see why, imagine using a delta function
# for the galaxy. The centroid changes discretely, not continuously as the offset
# varies. The effect isn't as severe of course for our Exponential, but the effect
# is still there in part. Hence, only use 2 decimal places for non-integer offsets.
if offx == int(offx) and offy == int(offy):
decimal = 4
else:
decimal = 2
#print 'offx,offy = ',offx,offy
offset = galsim.PositionD(offx, offy)
obj.draw(im, normalization='sb', offset=offset)
moments = getmoments(im)
#print 'moments = ',moments
np.testing.assert_almost_equal(
moments[0], cenx + offx, decimal,
"obj.draw(im,offset) not centered correctly for (nx,ny) = %d,%d"
% (nx, ny))
np.testing.assert_almost_equal(
moments[1], ceny + offy, decimal,
"obj.draw(im,offset) not centered correctly for (nx,ny) = %d,%d"
% (nx, ny))
# Test that a few pixel values match xValue
gal.draw(im2, normalization='sb', offset=offset)
for x, y in xy_list:
#print 'x,y = ',x,y
#print 'im(x,y) = ',im(x,y)
u = (x - cenx - offx) * scale
v = (y - ceny - offy) * scale
#print 'xval(x-cenx-offx,y-ceny-offy) = ',obj.xValue(galsim.PositionD(u,v))
np.testing.assert_almost_equal(
im(x, y), obj.xValue(galsim.PositionD(u, v)), 2,
"im(%d,%d) does not match xValue(%f,%f)" % (x, y, u, v))
np.testing.assert_almost_equal(
im2(x, y), gal.xValue(galsim.PositionD(u, v)), 6,
"im2(%d,%d) does not match xValue(%f,%f)" % (x, y, u, v))
# Check that applyShift also moves the centroid by the right amount.
shifted_obj = obj.createShifted(offset * scale)
shifted_obj.draw(im, normalization='sb')
moments = getmoments(im)
#print 'moments = ',moments
np.testing.assert_almost_equal(
moments[0], cenx + offx, decimal,
"shifted_obj.draw(im) not centered correctly for (nx,ny) = %d,%d"
% (nx, ny))
np.testing.assert_almost_equal(
moments[1], ceny + offy, decimal,
"shifted_obj.draw(im) not centered correctly for (nx,ny) = %d,%d"
% (nx, ny))
# Test that a few pixel values match xValue
shifted_gal = gal.createShifted(offset * scale)
shifted_gal.draw(im2, normalization='sb')
for x, y in xy_list:
#print 'x,y = ',x,y
#print 'im(x,y) = ',im(x,y)
u = (x - cenx) * scale
v = (y - ceny) * scale
#print 'shifted xval(x-cenx,y-ceny) = ',shifted_obj.xValue(galsim.PositionD(u,v))
np.testing.assert_almost_equal(
im(x, y), shifted_obj.xValue(galsim.PositionD(u, v)), 2,
"im(%d,%d) does not match shifted xValue(%f,%f)" %
(x, y, x - cenx, y - ceny))
np.testing.assert_almost_equal(
im2(x, y), shifted_gal.xValue(galsim.PositionD(u, v)), 6,
"im2(%d,%d) does not match shifted xValue(%f,%f)" %
(x, y, x - cenx, y - ceny))
u = (x - cenx - offx) * scale
v = (y - ceny - offy) * scale
#print 'xval(x-cenx-offx,y-ceny-offy) = ',obj.xValue(galsim.PositionD(u,v))
np.testing.assert_almost_equal(
im(x, y), obj.xValue(galsim.PositionD(u, v)), 2,
"im(%d,%d) does not match xValue(%f,%f)" % (x, y, u, v))
np.testing.assert_almost_equal(
im2(x, y), gal.xValue(galsim.PositionD(u, v)), 6,
"im2(%d,%d) does not match xValue(%f,%f)" % (x, y, u, v))
# Chcek the image's definition of the nominal center
nom_cenx = (nx + 2) / 2
nom_ceny = (ny + 2) / 2
nominal_center = im.bounds.center()
np.testing.assert_almost_equal(
nom_cenx, nominal_center.x, 6,
"im.bounds.center().x is wrong for (nx,ny) = %d,%d" % (nx, ny))
np.testing.assert_almost_equal(
nom_ceny, nominal_center.y, 6,
"im.bounds.center().y is wrong for (nx,ny) = %d,%d" % (nx, ny))
# Check that use_true_center = false is consistent with an offset by 0 or 0.5 pixels.
obj.draw(im, normalization='sb', use_true_center=False)
moments = getmoments(im)
#print 'moments = ',moments
np.testing.assert_almost_equal(
moments[0], nom_cenx, 4,
"obj.draw(im, use_true_center=False) not centered correctly for (nx,ny) = %d,%d"
% (nx, ny))
np.testing.assert_almost_equal(
moments[1], nom_ceny, 4,
"obj.draw(im, use_true_center=False) not centered correctly for (nx,ny) = %d,%d"
% (nx, ny))
cen_offset = galsim.PositionD(nom_cenx - cenx, nom_ceny - ceny)
#print 'cen_offset = ',cen_offset
obj.draw(im2, normalization='sb', offset=cen_offset)
np.testing.assert_array_almost_equal(
im.array, im2.array, 6,
"obj.draw(im, offset=%f,%f) different from use_true_center=False")
t2 = time.time()
print 'time for %s = %.2f' % (funcname(), t2 - t1)
def test_draw_methods():
"""Test the the different method options do the right thing.
"""
import time
t1 = time.time()
# We use a simple Exponential for our object:
obj = galsim.Exponential(flux=test_flux, scale_radius=1.09)
test_scale = 0.28
pix = galsim.Pixel(scale=test_scale)
obj_pix = galsim.Convolve(obj, pix)
N = 64
im1 = galsim.ImageD(N, N, scale=test_scale)
# auto and fft should be equivalent to drawing obj_pix with no_pixel
im1 = obj.drawImage(image=im1)
im2 = obj_pix.drawImage(image=im1.copy(), method='no_pixel')
print 'im1 flux diff = ', abs(im1.array.sum() - test_flux)
np.testing.assert_almost_equal(
im1.array.sum(), test_flux, 2,
"obj.drawImage() produced image with wrong flux")
print 'im2 flux diff = ', abs(im2.array.sum() - test_flux)
np.testing.assert_almost_equal(
im2.array.sum(), test_flux, 2,
"obj_pix.drawImage(no_pixel) produced image with wrong flux")
print 'im1, im2 max diff = ', abs(im1.array - im2.array).max()
np.testing.assert_array_almost_equal(
im1.array, im2.array, 6,
"obj.drawImage() differs from obj_pix.drawImage(no_pixel)")
im3 = obj.drawImage(image=im1.copy(), method='fft')
print 'im1, im3 max diff = ', abs(im1.array - im3.array).max()
np.testing.assert_array_almost_equal(
im1.array, im3.array, 6,
"obj.drawImage(fft) differs from obj.drawImage")
# real_space should be similar, but not precisely equal.
im4 = obj.drawImage(image=im1.copy(), method='real_space')
print 'im1, im4 max diff = ', abs(im1.array - im4.array).max()
np.testing.assert_array_almost_equal(
im1.array, im4.array, 4,
"obj.drawImage(real_space) differs from obj.drawImage")
# sb should match xValue for pixel centers. And be scale**2 factor different from no_pixel.
im5 = obj.drawImage(image=im1.copy(), method='sb', use_true_center=False)
im5.setCenter(0, 0)
print 'im5(0,0) = ', im5(0, 0)
print 'obj.xValue(0,0) = ', obj.xValue(0., 0.)
np.testing.assert_almost_equal(
im5(0, 0), obj.xValue(0., 0.), 6,
"obj.drawImage(sb) values do not match surface brightness given by xValue"
)
np.testing.assert_almost_equal(
im5(3, 2), obj.xValue(3 * test_scale, 2 * test_scale), 6,
"obj.drawImage(sb) values do not match surface brightness given by xValue"
)
im5 = obj.drawImage(image=im5, method='sb')
print 'im5(0,0) = ', im5(0, 0)
print 'obj.xValue(dx/2,dx/2) = ', obj.xValue(test_scale / 2.,
test_scale / 2.)
np.testing.assert_almost_equal(
im5(0, 0), obj.xValue(0.5 * test_scale, 0.5 * test_scale), 6,
"obj.drawImage(sb) values do not match surface brightness given by xValue"
)
np.testing.assert_almost_equal(
im5(3, 2), obj.xValue(3.5 * test_scale, 2.5 * test_scale), 6,
"obj.drawImage(sb) values do not match surface brightness given by xValue"
)
im6 = obj.drawImage(image=im1.copy(), method='no_pixel')
print 'im6, im5*scale**2 max diff = ', abs(im6.array - im5.array *
test_scale**2).max()
np.testing.assert_array_almost_equal(
im5.array * test_scale**2, im6.array, 6,
"obj.drawImage(sb) * scale**2 differs from obj.drawImage(no_pixel)")
# Drawing a truncated object, auto should be identical to real_space
obj = galsim.Sersic(flux=test_flux, n=3.7, half_light_radius=2, trunc=4)
obj_pix = galsim.Convolve(obj, pix)
# auto and real_space should be equivalent to drawing obj_pix with no_pixel
im1 = obj.drawImage(image=im1)
im2 = obj_pix.drawImage(image=im1.copy(), method='no_pixel')
print 'im1 flux diff = ', abs(im1.array.sum() - test_flux)
np.testing.assert_almost_equal(
im1.array.sum(), test_flux, 2,
"obj.drawImage() produced image with wrong flux")
print 'im2 flux diff = ', abs(im2.array.sum() - test_flux)
np.testing.assert_almost_equal(
im2.array.sum(), test_flux, 2,
"obj_pix.drawImage(no_pixel) produced image with wrong flux")
print 'im1, im2 max diff = ', abs(im1.array - im2.array).max()
np.testing.assert_array_almost_equal(
im1.array, im2.array, 6,
"obj.drawImage() differs from obj_pix.drawImage(no_pixel)")
im4 = obj.drawImage(image=im1.copy(), method='real_space')
print 'im1, im4 max diff = ', abs(im1.array - im4.array).max()
np.testing.assert_array_almost_equal(
im1.array, im4.array, 6,
"obj.drawImage(real_space) differs from obj.drawImage")
# fft should be similar, but not precisely equal.
import warnings
with warnings.catch_warnings():
warnings.simplefilter("ignore")
# This emits a warning about convolving two things with hard edges.
im3 = obj.drawImage(image=im1.copy(), method='fft')
print 'im1, im3 max diff = ', abs(im1.array - im3.array).max()
np.testing.assert_array_almost_equal(
im1.array,
im3.array,
3, # Should be close, but not exact.
"obj.drawImage(fft) differs from obj.drawImage")
# sb should match xValue for pixel centers. And be scale**2 factor different from no_pixel.
im5 = obj.drawImage(image=im1.copy(), method='sb')
im5.setCenter(0, 0)
print 'im5(0,0) = ', im5(0, 0)
print 'obj.xValue(dx/2,dx/2) = ', obj.xValue(test_scale / 2.,
test_scale / 2.)
np.testing.assert_almost_equal(
im5(0, 0), obj.xValue(0.5 * test_scale, 0.5 * test_scale), 6,
"obj.drawImage(sb) values do not match surface brightness given by xValue"
)
np.testing.assert_almost_equal(
im5(3, 2), obj.xValue(3.5 * test_scale, 2.5 * test_scale), 6,
"obj.drawImage(sb) values do not match surface brightness given by xValue"
)
im6 = obj.drawImage(image=im1.copy(), method='no_pixel')
print 'im6, im5*scale**2 max diff = ', abs(im6.array - im5.array *
test_scale**2).max()
np.testing.assert_array_almost_equal(
im5.array * test_scale**2, im6.array, 6,
"obj.drawImage(sb) * scale**2 differs from obj.drawImage(no_pixel)")
t2 = time.time()
print 'time for %s = %.2f' % (funcname(), t2 - t1)
def test_draw():
"""Test the various optional parameters to the draw function.
In particular test the parameters image, dx, and wmult in various combinations.
"""
import time
t1 = time.time()
# We use a simple Exponential for our object:
obj = galsim.Exponential(flux=test_flux, scale_radius=2)
# First test draw() with no kwargs. It should:
# - create a new image
# - return the new image
# - set the scale to obj.nyquistDx()
# - set the size large enough to contain 99.5% of the flux
im1 = obj.draw()
dx_nyq = obj.nyquistDx()
np.testing.assert_almost_equal(
im1.scale, dx_nyq, 9, "obj.draw() produced image with wrong scale")
#print 'im1.bounds = ',im1.bounds
assert im1.bounds == galsim.BoundsI(
1, 56, 1, 56), ("obj.draw() produced image with wrong bounds")
np.testing.assert_almost_equal(CalculateScale(im1), 2, 1,
"Measured wrong scale after obj.draw()")
# The flux is only really expected to come out right if the object has been
# convoled with a pixel:
obj2 = galsim.Convolve([obj, galsim.Pixel(im1.scale)])
im2 = obj2.draw()
dx_nyq = obj2.nyquistDx()
np.testing.assert_almost_equal(
im2.scale, dx_nyq, 9, "obj2.draw() produced image with wrong scale")
np.testing.assert_almost_equal(
im2.array.astype(float).sum(), test_flux, 2,
"obj2.draw() produced image with wrong flux")
assert im2.bounds == galsim.BoundsI(
1, 56, 1, 56), ("obj2.draw() produced image with wrong bounds")
np.testing.assert_almost_equal(CalculateScale(im2), 2, 1,
"Measured wrong scale after obj2.draw()")
# Test if we provide an image argument. It should:
# - write to the existing image
# - also return that image
# - set the scale to obj2.nyquistDx()
# - zero out any existing data
im3 = galsim.ImageD(56, 56)
im4 = obj2.draw(im3)
np.testing.assert_almost_equal(
im3.scale, dx_nyq, 9, "obj2.draw(im3) produced image with wrong scale")
np.testing.assert_almost_equal(
im3.array.sum(), test_flux, 2,
"obj2.draw(im3) produced image with wrong flux")
np.testing.assert_almost_equal(
im3.array.sum(),
im2.array.astype(float).sum(), 6,
"obj2.draw(im3) produced image with different flux than im2")
np.testing.assert_almost_equal(
CalculateScale(im3), 2, 1, "Measured wrong scale after obj2.draw(im3)")
np.testing.assert_array_equal(im3.array, im4.array,
"im4 = obj2.draw(im3) produced im4 != im3")
im3.fill(9.8)
np.testing.assert_array_equal(
im3.array, im4.array, "im4 = obj2.draw(im3) produced im4 is not im3")
im4 = obj2.draw(im3)
np.testing.assert_almost_equal(
im3.array.sum(),
im2.array.astype(float).sum(), 6,
"obj2.draw(im3) doesn't zero out existing data")
# Test if we provide an image with undefined bounds. It should:
# - resize the provided image
# - also return that image
# - set the scale to obj2.nyquistDx()
im5 = galsim.ImageD()
obj2.draw(im5)
np.testing.assert_almost_equal(
im5.scale, dx_nyq, 9, "obj2.draw(im5) produced image with wrong scale")
np.testing.assert_almost_equal(
im5.array.sum(), test_flux, 2,
"obj2.draw(im5) produced image with wrong flux")
np.testing.assert_almost_equal(
CalculateScale(im5), 2, 1, "Measured wrong scale after obj2.draw(im5)")
np.testing.assert_almost_equal(
im5.array.sum(),
im2.array.astype(float).sum(), 6,
"obj2.draw(im5) produced image with different flux than im2")
assert im5.bounds == galsim.BoundsI(
1, 56, 1, 56), ("obj2.draw(im5) produced image with wrong bounds")
# Test if we provide wmult. It should:
# - create a new image that is wmult times larger in each direction.
# - return the new image
# - set the scale to obj2.nyquistDx()
im6 = obj2.draw(wmult=4.)
np.testing.assert_almost_equal(
im6.scale, dx_nyq, 9,
"obj2.draw(wmult) produced image with wrong scale")
# Can assert accuracy to 4 decimal places now, since we're capturing much more
# of the flux on the image.
np.testing.assert_almost_equal(
im6.array.astype(float).sum(), test_flux, 4,
"obj2.draw(wmult) produced image with wrong flux")
np.testing.assert_almost_equal(
CalculateScale(im6), 2, 2,
"Measured wrong scale after obj2.draw(wmult)")
#print 'im6.bounds = ',im6.bounds
assert im6.bounds == galsim.BoundsI(
1, 220, 1, 220), ("obj2.draw(wmult) produced image with wrong bounds")
# Test if we provide an image argument and wmult. It should:
# - write to the existing image
# - also return that image
# - set the scale to obj2.nyquistDx()
# - zero out any existing data
# - the calculation of the convolution should be slightly more accurate than for im3
im3.setZero()
im5.setZero()
obj2.draw(im3, wmult=4.)
obj2.draw(im5)
np.testing.assert_almost_equal(
im3.scale, dx_nyq, 9, "obj2.draw(im3) produced image with wrong scale")
np.testing.assert_almost_equal(
im3.array.sum(), test_flux, 2,
"obj2.draw(im3,wmult) produced image with wrong flux")
np.testing.assert_almost_equal(
CalculateScale(im3), 2, 1,
"Measured wrong scale after obj2.draw(im3,wmult)")
assert ((im3.array - im5.array)**2).sum() > 0, (
"obj2.draw(im3,wmult) produced the same image as without wmult")
# Test if we provide a dx to use. It should:
# - create a new image using that dx for the scale
# - return the new image
# - set the size large enough to contain 99.5% of the flux
im7 = obj2.draw(scale=0.51)
np.testing.assert_almost_equal(
im7.scale, 0.51, 9, "obj2.draw(dx) produced image with wrong scale")
np.testing.assert_almost_equal(
im7.array.astype(float).sum(), test_flux, 2,
"obj2.draw(dx) produced image with wrong flux")
np.testing.assert_almost_equal(CalculateScale(im7), 2, 1,
"Measured wrong scale after obj2.draw(dx)")
#print 'im7.bounds = ',im7.bounds
assert im7.bounds == galsim.BoundsI(
1, 68, 1, 68), ("obj2.draw(dx) produced image with wrong bounds")
# Test with dx and wmult. It should:
# - create a new image using that dx for the scale
# - set the size a factor of wmult times larger in each direction.
# - return the new image
im8 = obj2.draw(scale=0.51, wmult=4.)
np.testing.assert_almost_equal(
im8.scale, 0.51, 9,
"obj2.draw(dx,wmult) produced image with wrong scale")
np.testing.assert_almost_equal(
im8.array.astype(float).sum(), test_flux, 4,
"obj2.draw(dx,wmult) produced image with wrong flux")
np.testing.assert_almost_equal(
CalculateScale(im8), 2, 2,
"Measured wrong scale after obj2.draw(dx,wmult)")
#print 'im8.bounds = ',im8.bounds
assert im8.bounds == galsim.BoundsI(
1, 270, 1,
270), ("obj2.draw(dx,wmult) produced image with wrong bounds")
# Test if we provide an image with a defined scale. It should:
# - write to the existing image
# - use the image's scale
im9 = galsim.ImageD(200, 200, scale=0.51)
obj2.draw(im9)
np.testing.assert_almost_equal(
im9.scale, 0.51, 9, "obj2.draw(im9) produced image with wrong scale")
np.testing.assert_almost_equal(
im9.array.sum(), test_flux, 4,
"obj2.draw(im9) produced image with wrong flux")
np.testing.assert_almost_equal(
CalculateScale(im9), 2, 2, "Measured wrong scale after obj2.draw(im9)")
# Test if we provide an image with a defined scale <= 0. It should:
# - write to the existing image
# - set the scale to obj2.nyquistDx()
im9.scale = -0.51
im9.setZero()
obj2.draw(im9)
np.testing.assert_almost_equal(
im9.scale, dx_nyq, 9, "obj2.draw(im9) produced image with wrong scale")
np.testing.assert_almost_equal(
im9.array.sum(), test_flux, 4,
"obj2.draw(im9) produced image with wrong flux")
np.testing.assert_almost_equal(
CalculateScale(im9), 2, 2, "Measured wrong scale after obj2.draw(im9)")
im9.scale = 0
im9.setZero()
obj2.draw(im9)
np.testing.assert_almost_equal(
im9.scale, dx_nyq, 9, "obj2.draw(im9) produced image with wrong scale")
np.testing.assert_almost_equal(
im9.array.sum(), test_flux, 4,
"obj2.draw(im9) produced image with wrong flux")
np.testing.assert_almost_equal(
CalculateScale(im9), 2, 2, "Measured wrong scale after obj2.draw(im9)")
# Test if we provide an image and dx. It should:
# - write to the existing image
# - use the provided dx
# - write the new dx value to the image's scale
im9.scale = 0.73
im9.setZero()
obj2.draw(im9, scale=0.51)
np.testing.assert_almost_equal(
im9.scale, 0.51, 9,
"obj2.draw(im9,dx) produced image with wrong scale")
np.testing.assert_almost_equal(
im9.array.sum(), test_flux, 4,
"obj2.draw(im9,dx) produced image with wrong flux")
np.testing.assert_almost_equal(
CalculateScale(im9), 2, 2,
"Measured wrong scale after obj2.draw(im9,dx)")
# Test if we provide an image and dx <= 0. It should:
# - write to the existing image
# - set the scale to obj2.nyquistDx()
im9.scale = 0.73
im9.setZero()
obj2.draw(im9, scale=-0.51)
np.testing.assert_almost_equal(
im9.scale, dx_nyq, 9,
"obj2.draw(im9,dx<0) produced image with wrong scale")
np.testing.assert_almost_equal(
im9.array.sum(), test_flux, 4,
"obj2.draw(im9,dx<0) produced image with wrong flux")
np.testing.assert_almost_equal(
CalculateScale(im9), 2, 2,
"Measured wrong scale after obj2.draw(im9,dx<0)")
im9.scale = 0.73
im9.setZero()
obj2.draw(im9, scale=0)
np.testing.assert_almost_equal(
im9.scale, dx_nyq, 9,
"obj2.draw(im9,scale=0) produced image with wrong scale")
np.testing.assert_almost_equal(
im9.array.sum(), test_flux, 4,
"obj2.draw(im9,scale=0) produced image with wrong flux")
np.testing.assert_almost_equal(
CalculateScale(im9), 2, 2,
"Measured wrong scale after obj2.draw(im9,scale=0)")
# Test if we provide nx, ny, and scale. It should:
# - create a new image with the right size
# - set the scale
im10 = obj2.draw(nx=200, ny=100, scale=dx_nyq)
np.testing.assert_almost_equal(
im10.array.shape, (100, 200), 9,
"obj2.draw(nx=200, ny=100) produced image with wrong size")
np.testing.assert_almost_equal(
im10.scale, dx_nyq, 9,
"obj2.draw(nx=200, ny=100) produced image with wrong scale")
np.testing.assert_almost_equal(
im10.array.sum(), test_flux, 4,
"obj2.draw(nx=200, ny=100) produced image with wrong flux")
try:
# Test if we provide nx, ny, and no scale. It should:
# - raise a ValueError
im10 = galsim.ImageF()
kwargs = {'nx': 200, 'ny': 100}
np.testing.assert_raises(ValueError, obj2.draw, kwargs)
# Test if we provide nx, ny, scale, and an existing image. It should:
# - raise a ValueError
im10 = galsim.ImageF()
kwargs = {'nx': 200, 'ny': 100, 'scale': dx_nyq, 'image': im10}
np.testing.assert_raises(ValueError, obj2.draw, kwargs)
except ImportError:
print 'The assert_raises tests require nose'
# Test if we provide bounds and scale. It should:
# - create a new image with the right size
# - set the scale
bounds = galsim.BoundsI(1, 200, 1, 100)
im10 = obj2.draw(bounds=bounds, scale=dx_nyq)
np.testing.assert_almost_equal(
im10.array.shape, (100, 200), 9,
"obj2.draw(bounds=galsim.Bounds(1,200,1,100)) produced image with wrong size"
)
np.testing.assert_almost_equal(
im10.scale, dx_nyq, 9,
"obj2.draw(bounds=galsim.Bounds(1,200,1,100)) produced image with wrong scale"
)
np.testing.assert_almost_equal(
im10.array.sum(), test_flux, 4,
"obj2.draw(bounds=galsim.Bounds(1,200,1,100)) produced image with wrong flux"
)
try:
# Test if we provide bounds and no scale. It should:
# - raise a ValueError
bounds = galsim.BoundsI(1, 200, 1, 100)
kwargs = {'bounds': bounds}
np.testing.assert_raises(ValueError, obj2.draw, kwargs)
# Test if we provide bounds, scale, and an existing image. It should:
# - raise a ValueError
bounds = galsim.BoundsI(1, 200, 1, 100)
kwargs = {'bounds': bounds, 'scale': dx_nyq, 'image': im10}
np.testing.assert_raises(ValueError, obj2.draw, kwargs)
except ImportError:
print 'The assert_raises tests require nose'
t2 = time.time()
print 'time for %s = %.2f' % (funcname(), t2 - t1)
def main(argv):
"""
A little bit more sophisticated, but still pretty basic:
- Use a sheared, exponential profile for the galaxy.
- Convolve it by a circular Moffat PSF.
- Add Poisson noise to the image.
"""
# In non-script code, use getLogger(__name__) at module scope instead.
logging.basicConfig(format="%(message)s",
level=logging.INFO,
stream=sys.stdout)
logger = logging.getLogger("demo2")
gal_flux = 1.e5 # counts
gal_r0 = 0.7 # arcsec radius
g1 = 0.8 # shear
g2 = 0.1 # shear
psf_beta = 5 #
psf_re = 1.0 # arcsec
# Fixed parameters
nx = 33
ny = 33
pixel_scale = 0.2 # arcsec / pixel
sky_level = 0 # counts / arcsec^2
# This time use a particular seed, so the image is deterministic.
# This is the same seed that is used in demo2.yaml, which means the images produced
# by the two methods will be precisely identical.
random_seed = 1534225
logger.info('Starting demo script 2 using:')
logger.info(
' - sheared (%.2f,%.2f) exponential galaxy (flux = %.1e, scale radius = %.2f),',
g1, g2, gal_flux, gal_r0)
logger.info(' - circular Moffat PSF (beta = %.1f, re = %.2f),',
psf_beta, psf_re)
logger.info(' - pixel scale = %.2f,', pixel_scale)
logger.info(' - Poisson noise (sky level = %.1e).', sky_level)
# Initialize the (pseudo-)random number generator that we will be using below.
# For a technical reason that will be explained later (demo9.py), we add 1 to the
# given random seed here.
rng = galsim.BaseDeviate(random_seed + 1)
# Define the galaxy profile.
gal = galsim.Exponential(flux=gal_flux, scale_radius=gal_r0)
# Shear the galaxy by some value.
# There are quite a few ways you can use to specify a shape.
# q, beta Axis ratio and position angle: q = b/a, 0 < q < 1
# e, beta Ellipticity and position angle: |e| = (1-q^2)/(1+q^2)
# g, beta ("Reduced") Shear and position angle: |g| = (1-q)/(1+q)
# eta, beta Conformal shear and position angle: eta = ln(1/q)
# e1,e2 Ellipticity components: e1 = e cos(2 beta), e2 = e sin(2 beta)
# g1,g2 ("Reduced") shear components: g1 = g cos(2 beta), g2 = g sin(2 beta)
# eta1,eta2 Conformal shear components: eta1 = eta cos(2 beta), eta2 = eta sin(2 beta)
gal = gal.shear(g1=g1, g2=g2)
logger.debug('Made galaxy profile')
# Define the PSF profile.
psf = galsim.Moffat(beta=psf_beta, flux=1., half_light_radius=psf_re)
logger.debug('Made PSF profile')
# Final profile is the convolution of these.
final = galsim.Convolve([gal, psf])
logger.debug('Convolved components into final profile')
# Draw the image with a particular pixel scale.
image = final.drawImage(scale=pixel_scale)
# The "effective PSF" is the PSF as drawn on an image, which includes the convolution
# by the pixel response. We label it epsf here.
image_epsf = psf.drawImage(scale=pixel_scale)
logger.debug('Made image of the profile')
# To get Poisson noise on the image, we will use a class called PoissonNoise.
# However, we want the noise to correspond to what you would get with a significant
# flux from tke sky. This is done by telling PoissonNoise to add noise from a
# sky level in addition to the counts currently in the image.
#
# One wrinkle here is that the PoissonNoise class needs the sky level in each pixel,
# while we have a sky_level in counts per arcsec^2. So we need to convert:
sky_level_pixel = sky_level * pixel_scale**2
noise = galsim.PoissonNoise(rng, sky_level=sky_level_pixel)
image.addNoise(noise)
logger.debug('Added Poisson noise')
# Write the image to a file.
if not os.path.isdir('output'):
os.mkdir('output')
file_name = os.path.join('output', 'demo2.fits')
file_name_epsf = os.path.join('output', 'demo2_epsf.fits')
image.write(file_name)
image_epsf.write(file_name_epsf)
logger.info('Wrote image to %r', file_name)
logger.info('Wrote effective PSF image to %r', file_name_epsf)
results = galsim.hsm.EstimateShear(image, image_epsf)
logger.info('HSM reports that the image has observed shape and size:')
logger.info(' e1 = %.3f, e2 = %.3f, sigma = %.3f (pixels)',
results.observed_shape.e1, results.observed_shape.e2,
results.moments_sigma)
logger.info(
'When carrying out Regaussianization PSF correction, HSM reports distortions'
)
logger.info(' e1, e2 = %.3f, %.3f', results.corrected_e1,
results.corrected_e2)
logger.info(
'Expected values in the limit that noise and non-Gaussianity are negligible:'
)
exp_shear = galsim.Shear(g1=g1, g2=g2)
logger.info(' g1, g2 = %.3f, %.3f', exp_shear.e1, exp_shear.e2)
## NR added
plt.imshow(image.array)
plt.show()
return image
def main(argv):
# Where to find and output data
path, filename = os.path.split(__file__)
datapath = os.path.abspath(os.path.join(path, "data/"))
outpath = os.path.abspath(os.path.join(path, "output/"))
# In non-script code, use getLogger(__name__) at module scope instead.
logging.basicConfig(format="%(message)s",
level=logging.INFO,
stream=sys.stdout)
logger = logging.getLogger("demo12")
# initialize (pseudo-)random number generator
random_seed = 1234567
rng = galsim.BaseDeviate(random_seed)
# read in SEDs
SED_names = ['CWW_E_ext', 'CWW_Sbc_ext', 'CWW_Scd_ext', 'CWW_Im_ext']
SEDs = {}
for SED_name in SED_names:
SED_filename = os.path.join(datapath, '{0}.sed'.format(SED_name))
# Here we create some galsim.SED objects to hold star or galaxy spectra. The most
# convenient way to create realistic spectra is to read them in from a two-column ASCII
# file, where the first column is wavelength and the second column is flux. Wavelengths in
# the example SED files are in Angstroms, flux in flambda. The default wavelength type for
# galsim.SED is nanometers, however, so we need to override by specifying
# `wave_type = 'Ang'`.
SED = galsim.SED(SED_filename, wave_type='Ang')
# The normalization of SEDs affects how many photons are eventually drawn into an image.
# One way to control this normalization is to specify the flux density in photons per nm
# at a particular wavelength. For example, here we normalize such that the photon density
# is 1 photon per nm at 500 nm.
SEDs[SED_name] = SED.withFluxDensity(target_flux_density=1.0,
wavelength=500)
logger.debug('Successfully read in SEDs')
# read in the LSST filters
filter_names = 'ugrizy'
filters = {}
for filter_name in filter_names:
filter_filename = os.path.join(datapath,
'LSST_{0}.dat'.format(filter_name))
# Here we create some galsim.Bandpass objects to represent the filters we're observing
# through. These include the entire imaging system throughput including the atmosphere,
# reflective and refractive optics, filters, and the CCD quantum efficiency. These are
# also conveniently read in from two-column ASCII files where the first column is
# wavelength and the second column is dimensionless flux. The example filter files have
# units of nanometers and dimensionless throughput, which is exactly what galsim.Bandpass
# expects, so we just specify the filename.
filters[filter_name] = galsim.Bandpass(filter_filename)
# For speed, we can thin out the wavelength sampling of the filter a bit.
# In the following line, `rel_err` specifies the relative error when integrating over just
# the filter (however, this is not necessarily the relative error when integrating over the
# filter times an SED)
filters[filter_name] = filters[filter_name].thin(rel_err=1e-4)
logger.debug('Read in filters')
pixel_scale = 0.2 # arcseconds
#-----------------------------------------------------------------------------------------------
# Part A: chromatic de Vaucouleurs galaxy
# Here we create a chromatic version of a de Vaucouleurs profile using the Chromatic class.
# This class lets one create chromatic versions of any galsim GSObject class. The first
# argument is the GSObject instance to be chromaticized, and the second argument is the
# profile's SED.
logger.info('')
logger.info('Starting part A: chromatic De Vaucouleurs galaxy')
redshift = 0.8
mono_gal = galsim.DeVaucouleurs(half_light_radius=0.5)
SED = SEDs['CWW_E_ext'].atRedshift(redshift)
gal = galsim.Chromatic(mono_gal, SED)
# You can still shear, shift, and dilate the resulting chromatic object.
gal = gal.shear(g1=0.5, g2=0.3).dilate(1.05).shift((0.0, 0.1))
logger.debug('Created Chromatic')
# convolve with PSF to make final profile
PSF = galsim.Moffat(fwhm=0.6, beta=2.5)
final = galsim.Convolve([gal, PSF])
logger.debug('Created final profile')
# draw profile through LSST filters
gaussian_noise = galsim.GaussianNoise(rng, sigma=0.1)
for filter_name, filter_ in filters.iteritems():
img = galsim.ImageF(64, 64, scale=pixel_scale)
final.drawImage(filter_, image=img)
img.addNoise(gaussian_noise)
logger.debug('Created {0}-band image'.format(filter_name))
out_filename = os.path.join(outpath,
'demo12a_{0}.fits'.format(filter_name))
galsim.fits.write(img, out_filename)
logger.debug('Wrote {0}-band image to disk'.format(filter_name))
logger.info('Added flux for {0}-band image: {1}'.format(
filter_name, img.added_flux))
logger.info(
'You can display the output in ds9 with a command line that looks something like:'
)
logger.info(
'ds9 output/demo12a_*.fits -match scale -zoom 2 -match frame image &')
#-----------------------------------------------------------------------------------------------
# Part B: chromatic bulge+disk galaxy
logger.info('')
logger.info('Starting part B: chromatic bulge+disk galaxy')
redshift = 0.8
# make a bulge ...
mono_bulge = galsim.DeVaucouleurs(half_light_radius=0.5)
bulge_SED = SEDs['CWW_E_ext'].atRedshift(redshift)
# The `*` operator can be used as a shortcut for creating a chromatic version of a GSObject:
bulge = mono_bulge * bulge_SED
bulge = bulge.shear(g1=0.12, g2=0.07)
logger.debug('Created bulge component')
# ... and a disk ...
mono_disk = galsim.Exponential(half_light_radius=2.0)
disk_SED = SEDs['CWW_Im_ext'].atRedshift(redshift)
disk = mono_disk * disk_SED
disk = disk.shear(g1=0.4, g2=0.2)
logger.debug('Created disk component')
# ... and then combine them.
bdgal = 1.1 * (
0.8 * bulge + 4 * disk
) # you can add and multiply ChromaticObjects just like GSObjects
bdfinal = galsim.Convolve([bdgal, PSF])
# Note that at this stage, our galaxy is chromatic but our PSF is still achromatic. Part C)
# below will dive into chromatic PSFs.
logger.debug('Created bulge+disk galaxy final profile')
# draw profile through LSST filters
gaussian_noise = galsim.GaussianNoise(rng, sigma=0.02)
for filter_name, filter_ in filters.iteritems():
img = galsim.ImageF(64, 64, scale=pixel_scale)
bdfinal.drawImage(filter_, image=img)
img.addNoise(gaussian_noise)
logger.debug('Created {0}-band image'.format(filter_name))
out_filename = os.path.join(outpath,
'demo12b_{0}.fits'.format(filter_name))
galsim.fits.write(img, out_filename)
logger.debug('Wrote {0}-band image to disk'.format(filter_name))
logger.info('Added flux for {0}-band image: {1}'.format(
filter_name, img.added_flux))
logger.info(
'You can display the output in ds9 with a command line that looks something like:'
)
logger.info(
'ds9 -rgb -blue -scale limits -0.2 0.8 output/demo12b_r.fits -green -scale limits'
+
' -0.25 1.0 output/demo12b_i.fits -red -scale limits -0.25 1.0 output/demo12b_z.fits'
+ ' -zoom 2 &')
#-----------------------------------------------------------------------------------------------
# Part C: chromatic PSF
logger.info('')
logger.info('Starting part C: chromatic PSF')
redshift = 0.0
mono_gal = galsim.Exponential(half_light_radius=0.5)
SED = SEDs['CWW_Im_ext'].atRedshift(redshift)
# Here's another way to set the normalization of the SED. If we want 50 counts to be drawn
# when observing an object with this SED through the LSST g-band filter, for instance, then we
# can do:
SED = SED.withFlux(50.0, filters['g'])
# The flux drawn through other bands, which sample different parts of the SED and have different
# throughputs, will, of course, be different.
gal = mono_gal * SED
gal = gal.shear(g1=0.5, g2=0.3)
logger.debug('Created `Chromatic` galaxy')
# For a ground-based PSF, two chromatic effects are introduced by the atmosphere:
# (i) differential chromatic refraction (DCR), and (ii) wavelength-dependent seeing.
#
# DCR shifts the position of the PSF as a function of wavelength. Blue light is shifted
# toward the zenith slightly more than red light.
#
# Kolmogorov turbulence in the atmosphere leads to a seeing size (e.g., FWHM) that scales with
# wavelength to the (-0.2) power.
#
# The ChromaticAtmosphere function will attach both of these effects to a fiducial PSF at
# some fiducial wavelength.
# First we define a monochromatic PSF to be the fiducial PSF.
PSF_500 = galsim.Moffat(beta=2.5, fwhm=0.5)
# Then we use ChromaticAtmosphere to manipulate this fiducial PSF as a function of wavelength.
# ChromaticAtmosphere also needs to know the wavelength of the fiducial PSF, and the location
# and orientation of the object with respect to the zenith. This final piece of information
# can be specified in several ways (see the ChromaticAtmosphere docstring for all of them).
# Here are a couple ways: let's pretend our object is located near M101 on the sky, we observe
# it 1 hour before it transits and we're observing from Mauna Kea.
ra = galsim.HMS_Angle("14:03:13") # hours : minutes : seconds
dec = galsim.DMS_Angle("54:20:57") # degrees : minutes : seconds
m101 = galsim.CelestialCoord(ra, dec)
latitude = 19.8207 * galsim.degrees # latitude of Mauna Kea
HA = -1.0 * galsim.hours # Hour angle = one hour before transit
# Then we can compute the zenith angle and parallactic angle (which is is the position angle
# of the zenith measured from North through East) of this object:
za, pa = galsim.dcr.zenith_parallactic_angles(m101,
HA=HA,
latitude=latitude)
# And then finally, create the chromatic PSF
PSF = galsim.ChromaticAtmosphere(PSF_500,
500.0,
zenith_angle=za,
parallactic_angle=pa)
# We could have also just passed `m101`, `latitude` and `HA` to ChromaticAtmosphere directly:
PSF = galsim.ChromaticAtmosphere(PSF_500,
500.0,
obj_coord=m101,
latitude=latitude,
HA=HA)
# and proceed like normal.
# convolve with galaxy to create final profile
final = galsim.Convolve([gal, PSF])
logger.debug('Created chromatic PSF finale profile')
# Draw profile through LSST filters
gaussian_noise = galsim.GaussianNoise(rng, sigma=0.03)
for filter_name, filter_ in filters.iteritems():
img = galsim.ImageF(64, 64, scale=pixel_scale)
final.drawImage(filter_, image=img)
img.addNoise(gaussian_noise)
logger.debug('Created {0}-band image'.format(filter_name))
out_filename = os.path.join(outpath,
'demo12c_{0}.fits'.format(filter_name))
galsim.fits.write(img, out_filename)
logger.debug('Wrote {0}-band image to disk'.format(filter_name))
logger.info('Added flux for {0}-band image: {1}'.format(
filter_name, img.added_flux))
logger.info(
'You can display the output in ds9 with a command line that looks something like:'
)
logger.info(
'ds9 output/demo12c_*.fits -match scale -zoom 2 -match frame image -blink &'
)
def test_exponential():
"""Test the generation of a specific exp profile against a known result.
"""
re = 1.0
# Note the factor below should really be 1.6783469900166605, but the value of 1.67839 is
# retained here as it was used by SBParse to generate the original known result (this changed
# in commit b77eb05ab42ecd31bc8ca03f1c0ae4ee0bc0a78b.
# The value of this test for regression purposes is not harmed by retaining the old scaling, it
# just means that the half light radius chosen for the test is not really 1, but 0.999974...
r0 = re / 1.67839
savedImg = galsim.fits.read(os.path.join(imgdir, "exp_1.fits"))
dx = 0.2
myImg = galsim.ImageF(savedImg.bounds, scale=dx)
myImg.setCenter(0, 0)
expon = galsim.Exponential(flux=1., scale_radius=r0)
expon.drawImage(myImg, scale=dx, method="sb", use_true_center=False)
np.testing.assert_array_almost_equal(
myImg.array,
savedImg.array,
5,
err_msg="Using GSObject Exponential disagrees with expected result")
# Check with default_params
expon = galsim.Exponential(flux=1.,
scale_radius=r0,
gsparams=default_params)
expon.drawImage(myImg, scale=dx, method="sb", use_true_center=False)
np.testing.assert_array_almost_equal(
myImg.array,
savedImg.array,
5,
err_msg=
"Using GSObject Exponential with default_params disagrees with expected result"
)
expon = galsim.Exponential(flux=1.,
scale_radius=r0,
gsparams=galsim.GSParams())
expon.drawImage(myImg, scale=dx, method="sb", use_true_center=False)
np.testing.assert_array_almost_equal(
myImg.array,
savedImg.array,
5,
err_msg=
"Using GSObject Exponential with GSParams() disagrees with expected result"
)
# Use non-unity values.
expon = galsim.Exponential(flux=1.7, scale_radius=0.91)
gsp = galsim.GSParams(xvalue_accuracy=1.e-8, kvalue_accuracy=1.e-8)
expon2 = galsim.Exponential(flux=1.7, scale_radius=0.91, gsparams=gsp)
assert expon2 != expon
assert expon2 == expon.withGSParams(gsp)
check_basic(expon, "Exponential")
# Test photon shooting.
do_shoot(expon, myImg, "Exponential")
# Test kvalues
do_kvalue(expon, myImg, "Exponential")
# Check picklability
do_pickle(expon, lambda x: x.drawImage(method='no_pixel'))
do_pickle(expon)
# Should raise an exception if both scale_radius and half_light_radius are provided.
assert_raises(TypeError,
galsim.Exponential,
scale_radius=3,
half_light_radius=1)
# Or neither.
assert_raises(TypeError, galsim.Exponential)
def get_catsim_galaxy(entry,
filt,
survey,
no_disk=False,
no_bulge=False,
no_agn=False):
"""Returns a bulge/disk/agn Galsim galaxy profile based on entry.
This function returns a composite galsim galaxy profile with bulge, disk and AGN based on the
parameters in entry, and using observing conditions defined by the survey
and the filter.
Credit: WeakLensingDeblending (https://github.com/LSSTDESC/WeakLensingDeblending)
Args:
entry (astropy.table.Table): single astropy line containing information on the galaxy
survey (btk.survey.Survey): BTK Survey object
filt (btk.survey.Filter): BTK Filter object
no_disk (bool): Sets the flux for the disk to zero
no_bulge (bool): Sets the flux for the bulge to zero
no_agn (bool): Sets the flux for the AGN to zero
Returns:
Galsim galaxy profile
"""
components = []
total_flux = get_flux(entry[filt.name + "_ab"], filt, survey)
# Calculate the flux of each component in detected electrons.
total_fluxnorm = entry["fluxnorm_disk"] + entry["fluxnorm_bulge"] + entry[
"fluxnorm_agn"]
disk_flux = 0.0 if no_disk else entry[
"fluxnorm_disk"] / total_fluxnorm * total_flux
bulge_flux = 0.0 if no_bulge else entry[
"fluxnorm_bulge"] / total_fluxnorm * total_flux
agn_flux = 0.0 if no_agn else entry[
"fluxnorm_agn"] / total_fluxnorm * total_flux
if disk_flux + bulge_flux + agn_flux == 0:
raise SourceNotVisible
if disk_flux > 0:
beta_radians = np.radians(entry["pa_disk"])
if bulge_flux > 0:
assert entry["pa_disk"] == entry[
"pa_bulge"], "Sersic components have different beta."
a_d, b_d = entry["a_d"], entry["b_d"]
disk_hlr_arcsecs = np.sqrt(a_d * b_d)
disk_q = b_d / a_d
disk = galsim.Exponential(flux=disk_flux,
half_light_radius=disk_hlr_arcsecs).shear(
q=disk_q,
beta=beta_radians * galsim.radians)
components.append(disk)
if bulge_flux > 0:
beta_radians = np.radians(entry["pa_bulge"])
a_b, b_b = entry["a_b"], entry["b_b"]
bulge_hlr_arcsecs = np.sqrt(a_b * b_b)
bulge_q = b_b / a_b
bulge = galsim.DeVaucouleurs(
flux=bulge_flux, half_light_radius=bulge_hlr_arcsecs).shear(
q=bulge_q, beta=beta_radians * galsim.radians)
components.append(bulge)
if agn_flux > 0:
agn = galsim.Gaussian(flux=agn_flux, sigma=1e-8)
components.append(agn)
profile = galsim.Add(components)
return profile
def _buildParametric(record,
gsparams=None,
chromatic=False,
bandpass=None,
sed=None):
# Get fit parameters. For 'sersicfit', the result is an array of 8 numbers for each
# galaxy:
# SERSICFIT[0]: intensity of light profile at the half-light radius.
# SERSICFIT[1]: half-light radius measured along the major axis, in units of pixels
# in the COSMOS lensing data reductions (0.03 arcsec).
# SERSICFIT[2]: Sersic n.
# SERSICFIT[3]: q, the ratio of minor axis to major axis length.
# SERSICFIT[4]: boxiness, currently fixed to 0, meaning isophotes are all
# elliptical.
# SERSICFIT[5]: x0, the central x position in pixels.
# SERSICFIT[6]: y0, the central y position in pixels.
# SERSICFIT[7]: phi, the position angle in radians. If phi=0, the major axis is
# lined up with the x axis of the image.
# For 'bulgefit', the result is an array of 16 parameters that comes from doing a
# 2-component sersic fit. The first 8 are the parameters for the disk, with n=1, and
# the last 8 are for the bulge, with n=4.
bparams = record['bulgefit']
sparams = record['sersicfit']
# Get the status flag for the fits. Entries 0 and 4 in 'fit_status' are relevant for
# bulgefit and sersicfit, respectively.
bstat = record['fit_status'][0]
sstat = record['fit_status'][4]
# Get the precomputed bulge-to-total flux ratio for the 2-component fits.
dvc_btt = record['fit_dvc_btt']
# Get the precomputed median absolute deviation for the 1- and 2-component fits.
# These quantities are used to ascertain whether the 2-component fit is really
# justified, or if the 1-component Sersic fit is sufficient to describe the galaxy
# light profile.
bmad = record['fit_mad_b']
smad = record['fit_mad_s']
# First decide if we can / should use bulgefit, otherwise sersicfit. This decision
# process depends on: the status flags for the fits, the bulge-to-total ratios (if near
# 0 or 1, just use single component fits), the sizes for the bulge and disk (if <=0 then
# use single component fits), the axis ratios for the bulge and disk (if <0.051 then use
# single component fits), and a comparison of the median absolute deviations to see
# which is better. The reason for the 0.051 cutoff is that the fits were bound at 0.05
# as a minimum, so anything below 0.051 generally means that the fitter hit the boundary
# for the 2-component fits, typically meaning that we don't have enough information to
# make reliable 2-component fits.
use_bulgefit = True
if (bstat < 1 or bstat > 4 or dvc_btt < 0.1 or dvc_btt > 0.9
or np.isnan(dvc_btt) or bparams[9] <= 0 or bparams[1] <= 0
or bparams[11] < 0.051 or bparams[3] < 0.051 or smad < bmad):
use_bulgefit = False
# Then check if sersicfit is viable; if not, this galaxy is a total failure.
# Note that we can avoid including these in the catalog in the first place by using
# `exclude_fail=True` when making the catalog.
if sstat < 1 or sstat > 4 or sparams[1] <= 0 or sparams[0] <= 0:
raise RuntimeError("Cannot make parametric model for this galaxy!")
# If we're supposed to use the 2-component fits, get all the parameters.
if use_bulgefit:
# Bulge parameters:
# Minor-to-major axis ratio:
bulge_q = bparams[11]
# Position angle, now represented as a galsim.Angle:
bulge_beta = bparams[15] * galsim.radians
# We have to convert from the stored half-light radius along the major axis, to an
# azimuthally averaged one (multiplying by sqrt(bulge_q)). We also have to convert
# to our native units of arcsec, from units of COSMOS pixels.
bulge_hlr = cosmos_pix_scale * np.sqrt(bulge_q) * bparams[9]
# The stored quantity is the surface brightness at the half-light radius. We have
# to convert to total flux within an n=4 surface brightness profile.
bulge_flux = 2.0 * np.pi * 3.607 * (
bulge_hlr**2) * bparams[8] / cosmos_pix_scale**2
# Disk parameters, defined analogously:
disk_q = bparams[3]
disk_beta = bparams[7] * galsim.radians
disk_hlr = cosmos_pix_scale * np.sqrt(disk_q) * bparams[1]
disk_flux = 2.0 * np.pi * 1.901 * (
disk_hlr**2) * bparams[0] / cosmos_pix_scale**2
bfrac = bulge_flux / (bulge_flux + disk_flux)
# Make sure the bulge-to-total flux ratio is not nonsense.
if bfrac < 0 or bfrac > 1 or np.isnan(bfrac):
raise RuntimeError(
"Cannot make parametric model for this galaxy")
# Then make the two components of the galaxy.
if chromatic:
# We define the GSObjects with flux=1, then multiply by an SED defined to have
# the appropriate (observed) magnitude at the redshift in the COSMOS passband.
z = record['zphot']
target_bulge_mag = record['mag_auto'] - 2.5 * math.log10(bfrac)
bulge_sed = sed[0].atRedshift(z).withMagnitude(
target_bulge_mag, bandpass)
bulge = galsim.DeVaucouleurs(half_light_radius=bulge_hlr,
gsparams=gsparams)
bulge *= bulge_sed
target_disk_mag = record['mag_auto'] - 2.5 * math.log10(
(1. - bfrac))
disk_sed = sed[1].atRedshift(z).withMagnitude(
target_disk_mag, bandpass)
disk = galsim.Exponential(half_light_radius=disk_hlr,
gsparams=gsparams)
disk *= disk_sed
else:
bulge = galsim.DeVaucouleurs(flux=bulge_flux,
half_light_radius=bulge_hlr,
gsparams=gsparams)
disk = galsim.Exponential(flux=disk_flux,
half_light_radius=disk_hlr,
gsparams=gsparams)
# Apply shears for intrinsic shape.
if bulge_q < 1.:
bulge = bulge.shear(q=bulge_q, beta=bulge_beta)
if disk_q < 1.:
disk = disk.shear(q=disk_q, beta=disk_beta)
gal = bulge + disk
else:
# Do a similar manipulation to the stored quantities for the single Sersic profiles.
gal_n = sparams[2]
# Fudge this if it is at the edge of the allowed n values. Since GalSim (as of
# #325 and #449) allow Sersic n in the range 0.3<=n<=6, the only problem is that
# the fits occasionally go as low as n=0.2. The fits in this file only go to n=6,
# so there is no issue with too-high values, but we also put a guard on that side
# in case other samples are swapped in that go to higher value of sersic n.
if gal_n < 0.3: gal_n = 0.3
if gal_n > 6.0: gal_n = 6.0
gal_q = sparams[3]
gal_beta = sparams[7] * galsim.radians
gal_hlr = cosmos_pix_scale * np.sqrt(gal_q) * sparams[1]
# Below is the calculation of the full Sersic n-dependent quantity that goes into
# the conversion from surface brightness to flux, which here we're calling
# 'prefactor'. In the n=4 and n=1 cases above, this was precomputed, but here we
# have to calculate for each value of n.
tmp_ser = galsim.Sersic(gal_n,
half_light_radius=gal_hlr,
gsparams=gsparams)
gal_flux = sparams[0] / tmp_ser.xValue(
0, gal_hlr) / cosmos_pix_scale**2
if chromatic:
gal = galsim.Sersic(gal_n,
flux=1.,
half_light_radius=gal_hlr,
gsparams=gsparams)
if gal_n < 1.5:
use_sed = sed[1] # disk
elif gal_n >= 1.5 and gal_n < 3.0:
use_sed = sed[2] # intermediate
else:
use_sed = sed[0] # bulge
target_mag = record['mag_auto']
z = record['zphot']
gal *= use_sed.atRedshift(z).withMagnitude(
target_mag, bandpass)
else:
gal = galsim.Sersic(gal_n,
flux=gal_flux,
half_light_radius=gal_hlr,
gsparams=gsparams)
# Apply shears for intrinsic shape.
if gal_q < 1.:
gal = gal.shear(q=gal_q, beta=gal_beta)
return gal
print "Sky noise: {}".format(etc.sigma_sky)
try:
os.mkdir(args.outdir)
except:
pass
psfimg = psf.drawImage(nx=args.nx, ny=args.nx, scale=0.2)
psfimg.write(os.path.join(args.outdir, 'psf.fits'))
infile = h5py.File(args.h5read)
for i, datum in enumerate(infile['data']):
ra, dec, z, r, mag, e1, e2, g1, g2 = datum
flux = etc.flux(mag)
print i, mag, flux, e1, e2
gal = (galsim.Exponential(half_light_radius=0.3).shear(e1=e1, e2=e2).shear(
e1=g1, e2=g2).withFlux(flux))
obj = galsim.Convolve(gal, psf)
img = obj.drawImage(nx=args.nx, ny=args.nx, scale=0.2)
img.addNoise(noise)
h1 = galsim.FitsHeader()
h1['RA'] = ra
h1['DEC'] = dec
h1['z'] = z
h1['r'] = r
h1['mag'] = mag
h1['e1'] = e1
h1['e2'] = e2
h1['g1'] = g1
h1['g2'] = g2
img.header = h1
def test_photon_array():
"""Test the basic methods of PhotonArray class
"""
nphotons = 1000
# First create from scratch
photon_array = galsim.PhotonArray(nphotons)
assert len(photon_array.x) == nphotons
assert len(photon_array.y) == nphotons
assert len(photon_array.flux) == nphotons
assert not photon_array.hasAllocatedWavelengths()
assert not photon_array.hasAllocatedAngles()
# Initial values should all be 0
np.testing.assert_array_equal(photon_array.x, 0.)
np.testing.assert_array_equal(photon_array.y, 0.)
np.testing.assert_array_equal(photon_array.flux, 0.)
# Check picklability
do_pickle(photon_array)
# Check assignment via numpy [:]
photon_array.x[:] = 5
photon_array.y[:] = 17
photon_array.flux[:] = 23
np.testing.assert_array_equal(photon_array.x, 5.)
np.testing.assert_array_equal(photon_array.y, 17.)
np.testing.assert_array_equal(photon_array.flux, 23.)
# Check assignment directly to the attributes
photon_array.x = 25
photon_array.y = 37
photon_array.flux = 53
np.testing.assert_array_equal(photon_array.x, 25.)
np.testing.assert_array_equal(photon_array.y, 37.)
np.testing.assert_array_equal(photon_array.flux, 53.)
# Now create from shooting a profile
obj = galsim.Exponential(flux=1.7, scale_radius=2.3)
rng = galsim.UniformDeviate(1234)
photon_array = obj.shoot(nphotons, rng)
orig_x = photon_array.x.copy()
orig_y = photon_array.y.copy()
orig_flux = photon_array.flux.copy()
assert len(photon_array.x) == nphotons
assert len(photon_array.y) == nphotons
assert len(photon_array.flux) == nphotons
assert not photon_array.hasAllocatedWavelengths()
assert not photon_array.hasAllocatedAngles()
# Check arithmetic ops
photon_array.x *= 5
photon_array.y += 17
photon_array.flux /= 23
np.testing.assert_almost_equal(photon_array.x, orig_x * 5.)
np.testing.assert_almost_equal(photon_array.y, orig_y + 17.)
np.testing.assert_almost_equal(photon_array.flux, orig_flux / 23.)
# Check picklability again with non-zero values
do_pickle(photon_array)
# Now assign to the optional arrays
photon_array.dxdz = 0.17
assert photon_array.hasAllocatedAngles()
assert not photon_array.hasAllocatedWavelengths()
np.testing.assert_array_equal(photon_array.dxdz, 0.17)
np.testing.assert_array_equal(photon_array.dydz, 0.)
photon_array.dydz = 0.59
np.testing.assert_array_equal(photon_array.dxdz, 0.17)
np.testing.assert_array_equal(photon_array.dydz, 0.59)
# Start over to check that assigning to wavelength leaves dxdz, dydz alone.
photon_array = obj.shoot(nphotons, rng)
photon_array.wavelength = 500.
assert photon_array.hasAllocatedWavelengths()
assert not photon_array.hasAllocatedAngles()
np.testing.assert_array_equal(photon_array.wavelength, 500)
photon_array.dxdz = 0.23
photon_array.dydz = 0.88
photon_array.wavelength = 912.
assert photon_array.hasAllocatedWavelengths()
assert photon_array.hasAllocatedAngles()
np.testing.assert_array_equal(photon_array.dxdz, 0.23)
np.testing.assert_array_equal(photon_array.dydz, 0.88)
np.testing.assert_array_equal(photon_array.wavelength, 912)
# Check picklability again with non-zero values for everything
do_pickle(photon_array)
def __generateGAL(self, re):
self.gal = galsim.Exponential(flux=1.0, half_light_radius=re * self.galData.resolution)
e20[i] = 0
if ((e10[i]**2) + (e20[i]**2) > 0.64):
e10[i] = 0.0
e20[i] = 0.0
gsparams=galsim.GSParams(folding_threshold=1.e-2,maxk_threshold=2.e-3,\
xvalue_accuracy=1.e-4,kvalue_accuracy=1.e-4,\
shoot_accuracy=1.e-4,minimum_fft_size=64)
#psf1=galsim.Moffat(fwhm=psf_fwhm[0],beta=2.5,gsparams=gsparams) #to be continue
#psf1=psf1.shear(e1=e1_psf,e2=e2_psf)
psf1 = galsim.Gaussian(fwhm=psf_fwhm[0], gsparams=gsparams)
#psf1=galsim.Kolmogorov(fwhm=psf_fwhm[0],gsparams=gsparams)
gal1 = galsim.Gaussian(half_light_radius=2, gsparams=gsparams)
gal2 = galsim.Exponential(half_light_radius=1, gsparams=gsparams)
gal3 = galsim.DeVaucouleurs(half_light_radius=1, gsparams=gsparams)
gal4 = galsim.Sersic(half_light_radius=1, n=2.5,
gsparams=gsparams) #to be continue
psf = psf1
final_epsf_image = psf1.drawImage(scale=pixel_scale)
gal = [gal1, gal2, gal3, gal4]
BJe1 = [[], [], [], []]
BJe2 = [[], [], [], []]
RGe1 = [[], [], [], []]
RGe2 = [[], [], [], []]
Me1 = [[], [], [], []]
Me2 = [[], [], [], []]
Wucha = [[], [], [], []]
def _inject_fake_objects(self, mbobs):
"""
inject a simple model for quick tests
"""
import galsim
iconf = self.config['inject']
model_name = iconf['model']
hlr = iconf['hlr']
flux = iconf['flux']
if model_name == 'exp':
model = galsim.Exponential(
half_light_radius=hlr,
flux=flux,
)
elif model_name == 'bdf':
fracdev = iconf['fracdev']
model = galsim.Add(
galsim.Exponential(
half_light_radius=hlr,
flux=(1 - fracdev),
), galsim.DeVaucouleurs(
half_light_radius=hlr,
flux=fracdev,
)).withFlux(flux)
else:
raise ValueError('bad model: "%s"' % model_name)
if 'psf' in iconf:
psf_model = galsim.Gaussian(fwhm=iconf['psf']['fwhm'], )
method = 'fft'
else:
psf_model = None
method = 'no_pixel'
Tfake = ngmix.moments.fwhm_to_T(hlr / 0.5)
for obslist in mbobs:
obslist.meta['Tsky'] = Tfake
for obs in obslist:
gsimage = galsim.Image(
obs.image.copy(),
wcs=obs.jacobian.get_galsim_wcs(),
)
if psf_model is None:
psf_gsimage = galsim.Image(
obs.psf.image / obs.psf.image.sum(),
wcs=obs.psf.jacobian.get_galsim_wcs(),
)
psf_to_conv = galsim.InterpolatedImage(
psf_gsimage,
#x_interpolant='lanczos15',
)
obs.psf.image = psf_gsimage.array
else:
pshape = obs.psf.image.shape
psf_gsimage = psf_model.drawImage(
nx=pshape[1],
ny=pshape[0],
wcs=obs.psf.jacobian.get_galsim_wcs(),
)
psf_to_conv = galsim.InterpolatedImage(psf_gsimage, )
obs.psf.image = psf_gsimage.array
tmodel = galsim.Convolve(
model,
psf_to_conv,
)
tmodel.drawImage(
image=gsimage,
method=method,
)
image = gsimage.array
wtmax = obs.weight.max()
err = np.sqrt(1.0 / wtmax)
image += self.rng.normal(
scale=err,
size=image.shape,
)
obs.image = image
def test_gsparams():
"""Test withGSParams with some non-default gsparams
"""
obj1 = galsim.Exponential(half_light_radius=1.7)
obj2 = galsim.Pixel(scale=0.2)
gsp = galsim.GSParams(folding_threshold=1.e-4, maxk_threshold=1.e-4, maximum_fft_size=1.e4)
gsp2 = galsim.GSParams(folding_threshold=1.e-2, maxk_threshold=1.e-2)
# Convolve
conv = galsim.Convolve(obj1, obj2)
conv1 = conv.withGSParams(gsp)
assert conv.gsparams == galsim.GSParams()
assert conv1.gsparams == gsp
assert conv1.obj_list[0].gsparams == gsp
assert conv1.obj_list[1].gsparams == gsp
conv2 = galsim.Convolve(obj1.withGSParams(gsp), obj2.withGSParams(gsp))
conv3 = galsim.Convolve(galsim.Exponential(half_light_radius=1.7, gsparams=gsp),
galsim.Pixel(scale=0.2))
conv4 = galsim.Convolve(obj1, obj2, gsparams=gsp)
assert conv != conv1
assert conv1 == conv2
assert conv1 == conv3
assert conv1 == conv4
print('stepk = ',conv.stepk, conv1.stepk)
assert conv1.stepk < conv.stepk
print('maxk = ',conv.maxk, conv1.maxk)
assert conv1.maxk > conv.maxk
conv5 = galsim.Convolve(obj1, obj2, gsparams=gsp, propagate_gsparams=False)
assert conv5 != conv4
assert conv5.gsparams == gsp
assert conv5.obj_list[0].gsparams == galsim.GSParams()
assert conv5.obj_list[1].gsparams == galsim.GSParams()
conv6 = conv5.withGSParams(gsp2)
assert conv6 != conv5
assert conv6.gsparams == gsp2
assert conv6.obj_list[0].gsparams == galsim.GSParams()
assert conv6.obj_list[1].gsparams == galsim.GSParams()
# AutoConvolve
conv = galsim.AutoConvolve(obj1)
conv1 = conv.withGSParams(gsp)
assert conv.gsparams == galsim.GSParams()
assert conv1.gsparams == gsp
assert conv1.orig_obj.gsparams == gsp
conv2 = galsim.AutoConvolve(obj1.withGSParams(gsp))
conv3 = galsim.AutoConvolve(obj1, gsparams=gsp)
assert conv != conv1
assert conv1 == conv2
assert conv1 == conv3
print('stepk = ',conv.stepk, conv1.stepk)
assert conv1.stepk < conv.stepk
print('maxk = ',conv.maxk, conv1.maxk)
assert conv1.maxk > conv.maxk
conv4 = galsim.AutoConvolve(obj1, gsparams=gsp, propagate_gsparams=False)
assert conv4 != conv3
assert conv4.gsparams == gsp
assert conv4.orig_obj.gsparams == galsim.GSParams()
conv5 = conv4.withGSParams(gsp2)
assert conv5 != conv4
assert conv5.gsparams == gsp2
assert conv5.orig_obj.gsparams == galsim.GSParams()
# AutoCorrelate
conv = galsim.AutoCorrelate(obj1)
conv1 = conv.withGSParams(gsp)
assert conv.gsparams == galsim.GSParams()
assert conv1.gsparams == gsp
assert conv1.orig_obj.gsparams == gsp
conv2 = galsim.AutoCorrelate(obj1.withGSParams(gsp))
conv3 = galsim.AutoCorrelate(obj1, gsparams=gsp)
assert conv != conv1
assert conv1 == conv2
assert conv1 == conv3
print('stepk = ',conv.stepk, conv1.stepk)
assert conv1.stepk < conv.stepk
print('maxk = ',conv.maxk, conv1.maxk)
assert conv1.maxk > conv.maxk
conv4 = galsim.AutoCorrelate(obj1, gsparams=gsp, propagate_gsparams=False)
assert conv4 != conv3
assert conv4.gsparams == gsp
assert conv4.orig_obj.gsparams == galsim.GSParams()
conv5 = conv4.withGSParams(gsp2)
assert conv5 != conv4
assert conv5.gsparams == gsp2
assert conv5.orig_obj.gsparams == galsim.GSParams()
# Deconvolve
conv = galsim.Convolve(obj1, galsim.Deconvolve(obj2))
conv1 = conv.withGSParams(gsp)
assert conv.gsparams == galsim.GSParams()
assert conv1.gsparams == gsp
assert conv1.obj_list[0].gsparams == gsp
assert conv1.obj_list[1].gsparams == gsp
assert conv1.obj_list[1].orig_obj.gsparams == gsp
conv2 = galsim.Convolve(obj1, galsim.Deconvolve(obj2.withGSParams(gsp)))
conv3 = galsim.Convolve(obj1.withGSParams(gsp), galsim.Deconvolve(obj2))
conv4 = galsim.Convolve(obj1, galsim.Deconvolve(obj2, gsparams=gsp))
assert conv != conv1
assert conv1 == conv2
assert conv1 == conv3
assert conv1 == conv4
print('stepk = ',conv.stepk, conv1.stepk)
assert conv1.stepk < conv.stepk
print('maxk = ',conv.maxk, conv1.maxk)
assert conv1.maxk > conv.maxk
conv5 = galsim.Convolve(obj1, galsim.Deconvolve(obj2, gsparams=gsp, propagate_gsparams=False))
assert conv5 != conv4
assert conv5.gsparams == gsp
assert conv5.obj_list[0].gsparams == gsp
assert conv5.obj_list[1].gsparams == gsp
assert conv5.obj_list[1].orig_obj.gsparams == galsim.GSParams()
conv6 = conv5.withGSParams(gsp2)
assert conv6 != conv5
assert conv6.gsparams == gsp2
assert conv6.obj_list[0].gsparams == gsp2
assert conv6.obj_list[1].gsparams == gsp2
assert conv6.obj_list[1].orig_obj.gsparams == galsim.GSParams()
# FourierSqrt
conv = galsim.Convolve(obj1, galsim.FourierSqrt(obj2))
conv1 = conv.withGSParams(gsp)
assert conv.gsparams == galsim.GSParams()
assert conv1.gsparams == gsp
assert conv1.obj_list[0].gsparams == gsp
assert conv1.obj_list[1].gsparams == gsp
assert conv1.obj_list[1].orig_obj.gsparams == gsp
conv2 = galsim.Convolve(obj1, galsim.FourierSqrt(obj2.withGSParams(gsp)))
conv3 = galsim.Convolve(obj1.withGSParams(gsp), galsim.FourierSqrt(obj2))
conv4 = galsim.Convolve(obj1, galsim.FourierSqrt(obj2, gsparams=gsp))
assert conv != conv1
assert conv1 == conv2
assert conv1 == conv3
assert conv1 == conv4
print('stepk = ',conv.stepk, conv1.stepk)
assert conv1.stepk < conv.stepk
print('maxk = ',conv.maxk, conv1.maxk)
assert conv1.maxk > conv.maxk
conv5 = galsim.Convolve(obj1, galsim.FourierSqrt(obj2, gsparams=gsp, propagate_gsparams=False))
assert conv5 != conv4
assert conv5.gsparams == gsp
assert conv5.obj_list[0].gsparams == gsp
assert conv5.obj_list[1].gsparams == gsp
assert conv5.obj_list[1].orig_obj.gsparams == galsim.GSParams()
conv6 = conv5.withGSParams(gsp2)
assert conv6 != conv5
assert conv6.gsparams == gsp2
assert conv6.obj_list[0].gsparams == gsp2
assert conv6.obj_list[1].gsparams == gsp2
assert conv6.obj_list[1].orig_obj.gsparams == galsim.GSParams()
def test_hsmparams_nodefault():
"""Test that when non-default hsmparams are used, the results change."""
import time
t1 = time.time()
# First make some profile
bulge = galsim.DeVaucouleurs(half_light_radius = 0.3)
disk = galsim.Exponential(half_light_radius = 0.5)
disk.applyShear(e1=0.2, e2=-0.3)
psf = galsim.Kolmogorov(fwhm = 0.6)
pix = galsim.Pixel(0.18)
gal = bulge + disk # equal weighting, i.e., B/T=0.5
tot_gal = galsim.Convolve(gal, psf, pix)
tot_psf = galsim.Convolve(psf, pix)
tot_gal_image = tot_gal.draw(dx=0.18)
tot_psf_image = tot_psf.draw(dx=0.18)
# Check that recompute_flux changes give results that are as expected
test_t = time.time()
res = galsim.hsm.EstimateShear(tot_gal_image, tot_psf_image)
dt = time.time() - test_t
res2 = galsim.hsm.EstimateShear(tot_gal_image, tot_psf_image, recompute_flux = 'sum')
assert(res.moments_amp < res2.moments_amp),'Incorrect behavior with recompute_flux=sum'
res3 = galsim.hsm.EstimateShear(tot_gal_image, tot_psf_image, recompute_flux = 'none')
assert(res3.moments_amp == 0),'Incorrect behavior with recompute_flux=none'
# Check that results, timing change as expected with nsig_rg
# For this, use Gaussian as galaxy and for ePSF, i.e., no extra pixel response
p = galsim.Gaussian(fwhm=10.)
g = galsim.Gaussian(fwhm=20.)
g.applyShear(g1=0.5)
obj = galsim.Convolve(g, p)
im = obj.draw(dx=1.)
psf_im = p.draw(dx=1.)
test_t1 = time.time()
g_res = galsim.hsm.EstimateShear(im, psf_im)
test_t2 = time.time()
g_res2 = galsim.hsm.EstimateShear(im, psf_im, hsmparams=galsim.hsm.HSMParams(nsig_rg=0.))
dt2 = time.time()-test_t2
dt1 = test_t2-test_t1
if test_timing:
assert(dt2 > dt1),'Should take longer to estimate shear without truncation of galaxy'
assert(not equal_hsmshapedata(g_res, g_res2)),'Results should differ with diff nsig_rg'
# Check that results, timing change as expected with max_moment_nsig2
test_t2 = time.time()
res2 = galsim.hsm.EstimateShear(tot_gal_image, tot_psf_image,
hsmparams=galsim.hsm.HSMParams(max_moment_nsig2 = 9.))
dt2 = time.time() - test_t2
if test_timing:
assert(dt2 < dt),'Should be faster to estimate shear with lower max_moment_nsig2'
assert(not equal_hsmshapedata(res, res2)),'Outputs same despite change in max_moment_nsig2'
assert(res.moments_sigma > res2.moments_sigma),'Sizes do not change as expected'
assert(res.moments_amp > res2.moments_amp),'Amplitudes do not change as expected'
# Check that max_amoment, max_ashift work as expected
try:
np.testing.assert_raises(RuntimeError, galsim.hsm.EstimateShear, tot_gal_image,
tot_psf_image, hsmparams=galsim.hsm.HSMParams(max_amoment = 10.))
np.testing.assert_raises(RuntimeError, galsim.hsm.EstimateShear, tot_gal_image,
tot_psf_image, guess_x_centroid=47.,
hsmparams=galsim.hsm.HSMParams(max_ashift=0.1))
except ImportError:
print 'The assert_raises tests require nose'
t2 = time.time()
print 'time for %s = %.2f'%(funcname(),t2-t1)
def test_wavelength_sampler():
nphotons = 1000
obj = galsim.Exponential(flux=1.7, scale_radius=2.3)
rng = galsim.UniformDeviate(1234)
photon_array = obj.shoot(nphotons, rng)
sed = galsim.SED(os.path.join(sedpath, 'CWW_E_ext.sed'), 'A',
'flambda').thin()
bandpass = galsim.Bandpass(os.path.join(bppath, 'LSST_r.dat'), 'nm').thin()
sampler = galsim.WavelengthSampler(sed, bandpass, rng)
sampler.applyTo(photon_array)
# Note: the underlying functionality of the sampleWavelengths function is tested
# in test_sed.py. So here we are really just testing that the wrapper class is
# properly writing to the photon_array.wavelengths array.
assert photon_array.hasAllocatedWavelengths()
assert not photon_array.hasAllocatedAngles()
print('mean wavelength = ', np.mean(photon_array.wavelength))
print('min wavelength = ', np.min(photon_array.wavelength))
print('max wavelength = ', np.max(photon_array.wavelength))
assert np.min(photon_array.wavelength) > bandpass.blue_limit
assert np.max(photon_array.wavelength) < bandpass.red_limit
# This is a regression test based on the value at commit 134a119
np.testing.assert_allclose(np.mean(photon_array.wavelength),
622.755128,
rtol=1.e-4)
# If we use a flat SED (in photons/nm), then the mean sampled wavelength should very closely
# match the bandpass effective wavelength.
photon_array2 = galsim.PhotonArray(100000)
sed2 = galsim.SED('1', 'nm', 'fphotons')
sampler2 = galsim.WavelengthSampler(sed2, bandpass, rng)
sampler2.applyTo(photon_array2)
np.testing.assert_allclose(
np.mean(photon_array2.wavelength),
bandpass.effective_wavelength,
rtol=0,
atol=0.2, # 2 Angstrom accuracy is pretty good
err_msg="Mean sampled wavelength not close to effective_wavelength")
# Test that using this as a surface op works properly.
# First do the shooting and clipping manually.
im1 = galsim.Image(64, 64, scale=1)
im1.setCenter(0, 0)
photon_array.flux[photon_array.wavelength < 600] = 0.
photon_array.addTo(im1)
# Make a dummy surface op that clips any photons with lambda < 600
class Clip600(object):
def applyTo(self, photon_array, local_wcs=None):
photon_array.flux[photon_array.wavelength < 600] = 0.
# Use (a new) sampler and clip600 as surface_ops in drawImage
im2 = galsim.Image(64, 64, scale=1)
im2.setCenter(0, 0)
clip600 = Clip600()
rng2 = galsim.BaseDeviate(1234)
sampler2 = galsim.WavelengthSampler(sed, bandpass, rng2)
obj.drawImage(im2,
method='phot',
n_photons=nphotons,
use_true_center=False,
surface_ops=[sampler2, clip600],
rng=rng2)
print('sum = ', im1.array.sum(), im2.array.sum())
np.testing.assert_array_equal(im1.array, im2.array)
def main(argv):
"""
Make images similar to that done for the Great08 challenge:
- Each fits file is 10 x 10 postage stamps.
(The real Great08 images are 100x100, but in the interest of making the Demo
script a bit quicker, we only build 100 stars and 100 galaxies.)
- Each postage stamp is 40 x 40 pixels.
- One image is all stars.
- A second image is all galaxies.
- Applied shear is the same for each galaxy.
- Galaxies are oriented randomly, but in pairs to cancel shape noise.
- Noise is Poisson using a nominal sky value of 1.e6.
- Galaxies are Exponential profiles.
"""
logging.basicConfig(format="%(message)s",
level=logging.INFO,
stream=sys.stdout)
logger = logging.getLogger("demo5")
# Define some parameters we'll use below.
# Normally these would be read in from some parameter file.
nx_tiles = 10 #
ny_tiles = 10 #
stamp_xsize = 40 #
stamp_ysize = 40 #
random_seed = 6424512 #
pixel_scale = 1.0 # arcsec / pixel
sky_level = 1.e6 # ADU / arcsec^2
# Make output directory if not already present.
if not os.path.isdir('output'):
os.mkdir('output')
psf_file_name = os.path.join('output', 'g08_psf.fits')
psf_beta = 3 #
psf_fwhm = 2.85 # arcsec (=pixels)
psf_trunc = 2. * psf_fwhm # arcsec (=pixels)
psf_e1 = -0.019 #
psf_e2 = -0.007 #
gal_file_name = os.path.join('output', 'g08_gal.fits')
gal_signal_to_noise = 200 # Great08 "LowNoise" run
gal_resolution = 0.98 # r_gal / r_psf (use r = half_light_radius)
# Note: Great08 defined their resolution as r_obs / r_psf, using the convolved
# size rather than the pre-convolved size.
# Therefore, our r_gal/r_psf = 0.98 approximately corresponds to
# their r_obs / r_psf = 1.4.
gal_ellip_rms = 0.2 # using "distortion" definition of ellipticity:
# e = (a^2-b^2)/(a^2+b^2), where a and b are the
# semi-major and semi-minor axes, respectively.
gal_ellip_max = 0.6 # Maximum value of e, to avoid getting near e=1.
gal_g1 = 0.013 # Applied shear, using normal shear definition:
gal_g2 = -0.008 # g = (a-b)/(a+b)
shift_radius = 1.0 # arcsec (=pixels)
logger.info('Starting demo script 5 using:')
logger.info(' - image with %d x %d postage stamps', nx_tiles, ny_tiles)
logger.info(' - postage stamps of size %d x %d pixels', stamp_xsize,
stamp_ysize)
logger.info(' - Moffat PSF (beta = %.1f, FWHM = %.2f, trunc = %.2f),',
psf_beta, psf_fwhm, psf_trunc)
logger.info(' - PSF ellip = (%.3f,%.3f)', psf_e1, psf_e2)
logger.info(' - Exponential galaxies')
logger.info(' - Resolution (r_gal / r_psf) = %.2f', gal_resolution)
logger.info(' - Ellipticities have rms = %.1f, max = %.1f',
gal_ellip_rms, gal_ellip_max)
logger.info(' - Applied gravitational shear = (%.3f,%.3f)', gal_g1,
gal_g2)
logger.info(' - Poisson noise (sky level = %.1e).', sky_level)
logger.info(' - Centroid shifts up to = %.2f pixels', shift_radius)
# Define the PSF profile
psf = galsim.Moffat(beta=psf_beta, fwhm=psf_fwhm, trunc=psf_trunc)
# When something can be constructed from multiple sizes, e.g. Moffat, then
# you can get any size out even if it wasn't the way the object was constructed.
# In this case, we extract the half-light radius, even though we built it with fwhm.
# We'll use this later to set the galaxy's half-light radius in terms of a resolution.
psf_re = psf.getHalfLightRadius()
psf = psf.shear(e1=psf_e1, e2=psf_e2)
logger.debug('Made PSF profile')
# Define the galaxy profile
# First figure out the size we need from the resolution
gal_re = psf_re * gal_resolution
# Make the galaxy profile starting with flux = 1.
gal = galsim.Exponential(flux=1., half_light_radius=gal_re)
logger.debug('Made galaxy profile')
# This profile is placed with different orientations and noise realizations
# at each postage stamp in the gal image.
gal_image = galsim.ImageF(stamp_xsize * nx_tiles - 1,
stamp_ysize * ny_tiles - 1,
scale=pixel_scale)
psf_image = galsim.ImageF(stamp_xsize * nx_tiles - 1,
stamp_ysize * ny_tiles - 1,
scale=pixel_scale)
shift_radius_sq = shift_radius**2
first_in_pair = True # Make pairs that are rotated by 90 degrees
k = 0
for iy in range(ny_tiles):
for ix in range(nx_tiles):
# The normal procedure for setting random numbers in GalSim is to start a new
# random number generator for each object using sequential seed values.
# This sounds weird at first (especially if you were indoctrinated by Numerical
# Recipes), but for the boost random number generator we use, the "random"
# number sequences produced from sequential initial seeds are highly uncorrelated.
#
# The reason for this procedure is that when we use multiple processes to build
# our images, we want to make sure that the results are deterministic regardless
# of the way the objects get parcelled out to the different processes.
#
# Of course, this script isn't using multiple processes, so it isn't required here.
# However, we do it nonetheless in order to get the same results as the config
# version of this demo script (demo5.yaml).
ud = galsim.UniformDeviate(random_seed + k)
# Any kind of random number generator can take another RNG as its first
# argument rather than a seed value. This makes both objects use the same
# underlying generator for their pseudo-random values.
gd = galsim.GaussianDeviate(ud, sigma=gal_ellip_rms)
# The -1's in the next line are to provide a border of
# 1 pixel between postage stamps
b = galsim.BoundsI(ix * stamp_xsize + 1,
(ix + 1) * stamp_xsize - 1,
iy * stamp_ysize + 1,
(iy + 1) * stamp_ysize - 1)
sub_gal_image = gal_image[b]
sub_psf_image = psf_image[b]
# Great08 randomized the locations of the two galaxies in each pair,
# but for simplicity, we just do them in sequential postage stamps.
if first_in_pair:
# Use a random orientation:
beta = ud() * 2. * math.pi * galsim.radians
# Determine the ellipticity to use for this galaxy.
ellip = 1
while (ellip > gal_ellip_max):
# Don't do `ellip = math.fabs(gd())`
# Python basically implements this as a macro, so gd() is called twice!
val = gd()
ellip = math.fabs(val)
first_in_pair = False
else:
# Use the previous ellip and beta + 90 degrees
beta += 90 * galsim.degrees
first_in_pair = True
# Make a new copy of the galaxy with an applied e1/e2-type distortion
# by specifying the ellipticity and a real-space position angle
this_gal = gal.shear(e=ellip, beta=beta)
# Apply the gravitational reduced shear by specifying g1/g2
this_gal = this_gal.shear(g1=gal_g1, g2=gal_g2)
# Apply a random shift_radius:
rsq = 2 * shift_radius_sq
while (rsq > shift_radius_sq):
dx = (2 * ud() - 1) * shift_radius
dy = (2 * ud() - 1) * shift_radius
rsq = dx**2 + dy**2
this_gal = this_gal.shift(dx, dy)
# Note that the shifted psf that we create here is purely for the purpose of being able
# to draw a separate, shifted psf image. We do not use it when convolving the galaxy
# with the psf.
this_psf = psf.shift(dx, dy)
# Make the final image, convolving with the (unshifted) psf
final_gal = galsim.Convolve([psf, this_gal])
# Draw the image
final_gal.drawImage(sub_gal_image)
# Now add an appropriate amount of noise to get our desired S/N
# There are lots of definitions of S/N, but here is the one used by Great08
# We use a weighted integral of the flux:
# S = sum W(x,y) I(x,y) / sum W(x,y)
# N^2 = Var(S) = sum W(x,y)^2 Var(I(x,y)) / (sum W(x,y))^2
# Now we assume that Var(I(x,y)) is constant so
# Var(I(x,y)) = noise_var
# We also assume that we are using a matched filter for W, so W(x,y) = I(x,y).
# Then a few things cancel and we find that
# S/N = sqrt( sum I(x,y)^2 / noise_var )
#
# The above procedure is encapsulated in the function image.addNoiseSNR which
# sets the flux appropriately given the variance of the noise model.
# In our case, noise_var = sky_level_pixel
sky_level_pixel = sky_level * pixel_scale**2
noise = galsim.PoissonNoise(ud, sky_level=sky_level_pixel)
sub_gal_image.addNoiseSNR(noise, gal_signal_to_noise)
# Draw the PSF image
# No noise on PSF images. Just draw it as is.
this_psf.drawImage(sub_psf_image)
# For first instance, measure moments
if ix == 0 and iy == 0:
psf_shape = sub_psf_image.FindAdaptiveMom()
temp_e = psf_shape.observed_shape.e
if temp_e > 0.0:
g_to_e = psf_shape.observed_shape.g / temp_e
else:
g_to_e = 0.0
logger.info(
'Measured best-fit elliptical Gaussian for first PSF image: '
)
logger.info(' g1, g2, sigma = %7.4f, %7.4f, %7.4f (pixels)',
g_to_e * psf_shape.observed_shape.e1,
g_to_e * psf_shape.observed_shape.e2,
psf_shape.moments_sigma)
x = b.center().x
y = b.center().y
logger.info(
'Galaxy (%d,%d): center = (%.0f,%0.f) (e,beta) = (%.4f,%.3f)',
ix, iy, x, y, ellip, beta / galsim.radians)
k = k + 1
logger.info('Done making images of postage stamps')
# Now write the images to disk.
psf_image.write(psf_file_name)
logger.info('Wrote PSF file %s', psf_file_name)
gal_image.write(gal_file_name)
logger.info('Wrote image to %r',
gal_file_name) # using %r adds quotes around filename for us
def test_photon_array():
"""Test the basic methods of PhotonArray class
"""
nphotons = 1000
# First create from scratch
photon_array = galsim.PhotonArray(nphotons)
assert len(photon_array.x) == nphotons
assert len(photon_array.y) == nphotons
assert len(photon_array.flux) == nphotons
assert not photon_array.hasAllocatedWavelengths()
assert not photon_array.hasAllocatedAngles()
# Initial values should all be 0
np.testing.assert_array_equal(photon_array.x, 0.)
np.testing.assert_array_equal(photon_array.y, 0.)
np.testing.assert_array_equal(photon_array.flux, 0.)
# Check picklability
do_pickle(photon_array)
# Check assignment via numpy [:]
photon_array.x[:] = 5
photon_array.y[:] = 17
photon_array.flux[:] = 23
np.testing.assert_array_equal(photon_array.x, 5.)
np.testing.assert_array_equal(photon_array.y, 17.)
np.testing.assert_array_equal(photon_array.flux, 23.)
# Check assignment directly to the attributes
photon_array.x = 25
photon_array.y = 37
photon_array.flux = 53
np.testing.assert_array_equal(photon_array.x, 25.)
np.testing.assert_array_equal(photon_array.y, 37.)
np.testing.assert_array_equal(photon_array.flux, 53.)
# Now create from shooting a profile
obj = galsim.Exponential(flux=1.7, scale_radius=2.3)
rng = galsim.UniformDeviate(1234)
photon_array = obj.shoot(nphotons, rng)
orig_x = photon_array.x.copy()
orig_y = photon_array.y.copy()
orig_flux = photon_array.flux.copy()
assert len(photon_array.x) == nphotons
assert len(photon_array.y) == nphotons
assert len(photon_array.flux) == nphotons
assert not photon_array.hasAllocatedWavelengths()
assert not photon_array.hasAllocatedAngles()
# Check arithmetic ops
photon_array.x *= 5
photon_array.y += 17
photon_array.flux /= 23
np.testing.assert_almost_equal(photon_array.x, orig_x * 5.)
np.testing.assert_almost_equal(photon_array.y, orig_y + 17.)
np.testing.assert_almost_equal(photon_array.flux, orig_flux / 23.)
# Check picklability again with non-zero values
do_pickle(photon_array)
# Now assign to the optional arrays
photon_array.dxdz = 0.17
assert photon_array.hasAllocatedAngles()
assert not photon_array.hasAllocatedWavelengths()
np.testing.assert_array_equal(photon_array.dxdz, 0.17)
np.testing.assert_array_equal(photon_array.dydz, 0.)
photon_array.dydz = 0.59
np.testing.assert_array_equal(photon_array.dxdz, 0.17)
np.testing.assert_array_equal(photon_array.dydz, 0.59)
# Start over to check that assigning to wavelength leaves dxdz, dydz alone.
photon_array = obj.shoot(nphotons, rng)
photon_array.wavelength = 500.
assert photon_array.hasAllocatedWavelengths()
assert not photon_array.hasAllocatedAngles()
np.testing.assert_array_equal(photon_array.wavelength, 500)
photon_array.dxdz = 0.23
photon_array.dydz = 0.88
photon_array.wavelength = 912.
assert photon_array.hasAllocatedWavelengths()
assert photon_array.hasAllocatedAngles()
np.testing.assert_array_equal(photon_array.dxdz, 0.23)
np.testing.assert_array_equal(photon_array.dydz, 0.88)
np.testing.assert_array_equal(photon_array.wavelength, 912)
# Check toggling is_corr
assert not photon_array.isCorrelated()
photon_array.setCorrelated()
assert photon_array.isCorrelated()
photon_array.setCorrelated(False)
assert not photon_array.isCorrelated()
photon_array.setCorrelated(True)
assert photon_array.isCorrelated()
# Check rescaling the total flux
flux = photon_array.flux.sum()
np.testing.assert_almost_equal(photon_array.getTotalFlux(), flux)
photon_array.scaleFlux(17)
np.testing.assert_almost_equal(photon_array.getTotalFlux(), 17 * flux)
photon_array.setTotalFlux(199)
np.testing.assert_almost_equal(photon_array.getTotalFlux(), 199)
# Check rescaling the positions
x = photon_array.x.copy()
y = photon_array.y.copy()
photon_array.scaleXY(1.9)
np.testing.assert_almost_equal(photon_array.x, 1.9 * x)
np.testing.assert_almost_equal(photon_array.y, 1.9 * y)
# Check ways to assign to photons
pa1 = galsim.PhotonArray(50)
pa1.x = photon_array.x[:50]
for i in range(50):
pa1.y[i] = photon_array.y[i]
pa1.flux[0:50] = photon_array.flux[:50]
pa1.dxdz = photon_array.dxdz[:50]
pa1.dydz = photon_array.dydz[:50]
pa1.wavelength = photon_array.wavelength[:50]
np.testing.assert_almost_equal(pa1.x, photon_array.x[:50])
np.testing.assert_almost_equal(pa1.y, photon_array.y[:50])
np.testing.assert_almost_equal(pa1.flux, photon_array.flux[:50])
np.testing.assert_almost_equal(pa1.dxdz, photon_array.dxdz[:50])
np.testing.assert_almost_equal(pa1.dydz, photon_array.dydz[:50])
np.testing.assert_almost_equal(pa1.wavelength,
photon_array.wavelength[:50])
# Check assignAt
pa2 = galsim.PhotonArray(100)
pa2.assignAt(0, pa1)
pa2.assignAt(50, pa1)
np.testing.assert_almost_equal(pa2.x[:50], pa1.x)
np.testing.assert_almost_equal(pa2.y[:50], pa1.y)
np.testing.assert_almost_equal(pa2.flux[:50], pa1.flux)
np.testing.assert_almost_equal(pa2.dxdz[:50], pa1.dxdz)
np.testing.assert_almost_equal(pa2.dydz[:50], pa1.dydz)
np.testing.assert_almost_equal(pa2.wavelength[:50], pa1.wavelength)
np.testing.assert_almost_equal(pa2.x[50:], pa1.x)
np.testing.assert_almost_equal(pa2.y[50:], pa1.y)
np.testing.assert_almost_equal(pa2.flux[50:], pa1.flux)
np.testing.assert_almost_equal(pa2.dxdz[50:], pa1.dxdz)
np.testing.assert_almost_equal(pa2.dydz[50:], pa1.dydz)
np.testing.assert_almost_equal(pa2.wavelength[50:], pa1.wavelength)
# Error if it doesn't fit.
assert_raises(ValueError, pa2.assignAt, 90, pa1)
# Test some trivial usage of makeFromImage
zero = galsim.Image(4, 4, init_value=0)
photons = galsim.PhotonArray.makeFromImage(zero)
print('photons = ', photons)
assert len(photons) == 16
np.testing.assert_array_equal(photons.flux, 0.)
ones = galsim.Image(4, 4, init_value=1)
photons = galsim.PhotonArray.makeFromImage(ones)
print('photons = ', photons)
assert len(photons) == 16
np.testing.assert_almost_equal(photons.flux, 1.)
tens = galsim.Image(4, 4, init_value=8)
photons = galsim.PhotonArray.makeFromImage(tens, max_flux=5.)
print('photons = ', photons)
assert len(photons) == 32
np.testing.assert_almost_equal(photons.flux, 4.)
assert_raises(ValueError,
galsim.PhotonArray.makeFromImage,
zero,
max_flux=0.)
assert_raises(ValueError,
galsim.PhotonArray.makeFromImage,
zero,
max_flux=-2)
# Check some other errors
undef = galsim.Image()
assert_raises(galsim.GalSimUndefinedBoundsError, pa2.addTo, undef)
# Check picklability again with non-zero values for everything
do_pickle(photon_array)
def test_add_flux_scaling():
"""Test flux scaling for Add.
"""
import time
t1 = time.time()
# decimal point to go to for parameter value comparisons
param_decimal = 12
# init with Gaussian and Exponential only (should be ok given last tests)
obj = galsim.Add([
galsim.Gaussian(sigma=test_sigma, flux=test_flux * .5),
galsim.Exponential(scale_radius=test_scale, flux=test_flux * .5)
])
obj *= 2.
np.testing.assert_almost_equal(
obj.getFlux(),
test_flux * 2.,
decimal=param_decimal,
err_msg="Flux param inconsistent after __imul__.")
obj = galsim.Add([
galsim.Gaussian(sigma=test_sigma, flux=test_flux * .5),
galsim.Exponential(scale_radius=test_scale, flux=test_flux * .5)
])
obj /= 2.
np.testing.assert_almost_equal(
obj.getFlux(),
test_flux / 2.,
decimal=param_decimal,
err_msg="Flux param inconsistent after __idiv__.")
obj = galsim.Add([
galsim.Gaussian(sigma=test_sigma, flux=test_flux * .5),
galsim.Exponential(scale_radius=test_scale, flux=test_flux * .5)
])
obj2 = obj * 2.
# First test that original obj is unharmed... (also tests that .copy() is working)
np.testing.assert_almost_equal(
obj.getFlux(),
test_flux,
decimal=param_decimal,
err_msg="Flux param inconsistent after __rmul__ (original).")
# Then test new obj2 flux
np.testing.assert_almost_equal(
obj2.getFlux(),
test_flux * 2.,
decimal=param_decimal,
err_msg="Flux param inconsistent after __rmul__ (result).")
obj = galsim.Add([
galsim.Gaussian(sigma=test_sigma, flux=test_flux * .5),
galsim.Exponential(scale_radius=test_scale, flux=test_flux * .5)
])
obj2 = 2. * obj
# First test that original obj is unharmed... (also tests that .copy() is working)
np.testing.assert_almost_equal(
obj.getFlux(),
test_flux,
decimal=param_decimal,
err_msg="Flux param inconsistent after __mul__ (original).")
# Then test new obj2 flux
np.testing.assert_almost_equal(
obj2.getFlux(),
test_flux * 2.,
decimal=param_decimal,
err_msg="Flux param inconsistent after __mul__ (result).")
obj = galsim.Add([
galsim.Gaussian(sigma=test_sigma, flux=test_flux * .5),
galsim.Exponential(scale_radius=test_scale, flux=test_flux * .5)
])
obj2 = obj / 2.
# First test that original obj is unharmed... (also tests that .copy() is working)
np.testing.assert_almost_equal(
obj.getFlux(),
test_flux,
decimal=param_decimal,
err_msg="Flux param inconsistent after __div__ (original).")
# Then test new obj2 flux
np.testing.assert_almost_equal(
obj2.getFlux(),
test_flux / 2.,
decimal=param_decimal,
err_msg="Flux param inconsistent after __div__ (result).")
t2 = time.time()
print 'time for %s = %.2f' % (funcname(), t2 - t1)
def main(argv):
"""
Make a fits image cube using parameters from an input catalog
- The number of images in the cube matches the number of rows in the catalog.
- Each image size is computed automatically by GalSim based on the Nyquist size.
- Only galaxies. No stars.
- PSF is Moffat
- Each galaxy is bulge plus disk: deVaucouleurs + Exponential.
- The catalog's columns are:
0 PSF beta (Moffat exponent)
1 PSF FWHM
2 PSF e1
3 PSF e2
4 PSF trunc
5 Disc half-light-radius
6 Disc e1
7 Disc e2
8 Bulge half-light-radius
9 Bulge e1
10 Bulge e2
11 Galaxy dx (the two components have same center)
12 Galaxy dy
- Applied shear is the same for each galaxy
- Noise is Poisson using a nominal sky value of 1.e6
"""
logging.basicConfig(format="%(message)s",
level=logging.INFO,
stream=sys.stdout)
logger = logging.getLogger("demo4")
# Define some parameters we'll use below and make directories if needed.
cat_file_name = os.path.join('input', 'galsim_default_input.asc')
if not os.path.isdir('output'):
os.mkdir('output')
multi_file_name = os.path.join('output', 'multi.fits')
random_seed = 8241573
sky_level = 1.e6 # ADU / arcsec^2
pixel_scale = 1.0 # arcsec / pixel (size units in input catalog are pixels)
gal_flux = 1.e6 # arbitrary choice, makes nice (not too) noisy images
gal_g1 = -0.009 #
gal_g2 = 0.011 #
xsize = 64 # pixels
ysize = 64 # pixels
logger.info('Starting demo script 4 using:')
logger.info(' - parameters taken from catalog %r', cat_file_name)
logger.info(' - Moffat PSF (parameters from catalog)')
logger.info(' - pixel scale = %.2f', pixel_scale)
logger.info(' - Bulge + Disc galaxies (parameters from catalog)')
logger.info(' - Applied gravitational shear = (%.3f,%.3f)', gal_g1,
gal_g2)
logger.info(' - Poisson noise (sky level = %.1e).', sky_level)
# Read in the input catalog
cat = galsim.Catalog(cat_file_name)
# save a list of the galaxy images in the "images" list variable:
images = []
for k in range(cat.nobjects):
# Initialize the (pseudo-)random number generator that we will be using below.
# Use a different random seed for each object to get different noise realizations.
# Using sequential random seeds here is safer than it sounds. We use Mersenne Twister
# random number generators that are designed to be used with this kind of seeding.
# However, to be extra safe, we actually initialize one random number generator with this
# seed, generate and throw away two random values with that, and then use the next value
# to seed a completely different Mersenne Twister RNG. The result is that successive
# RNGs created this way produce very independent random number streams.
rng = galsim.BaseDeviate(random_seed + k + 1)
# Take the Moffat beta from the first column (called 0) of the input catalog:
# Note: cat.get(k,col) returns a string. To get the value as a float, use either
# cat.getFloat(k,col) or float(cat.get(k,col))
beta = cat.getFloat(k, 0)
# A Moffat's size may be either scale_radius, fwhm, or half_light_radius.
# Here we use fwhm, taking from the catalog as well.
fwhm = cat.getFloat(k, 1)
# A Moffat profile may be truncated if desired
# The units for this are expected to be arcsec (or specifically -- whatever units
# you are using for all the size values as defined by the pixel_scale).
trunc = cat.getFloat(k, 4)
# Note: You may omit the flux, since the default is flux=1.
psf = galsim.Moffat(beta=beta, fwhm=fwhm, trunc=trunc)
# Take the (e1, e2) shape parameters from the catalog as well.
psf = psf.shear(e1=cat.getFloat(k, 2), e2=cat.getFloat(k, 3))
# Galaxy is a bulge + disk with parameters taken from the catalog:
disk = galsim.Exponential(flux=0.6,
half_light_radius=cat.getFloat(k, 5))
disk = disk.shear(e1=cat.getFloat(k, 6), e2=cat.getFloat(k, 7))
bulge = galsim.DeVaucouleurs(flux=0.4,
half_light_radius=cat.getFloat(k, 8))
bulge = bulge.shear(e1=cat.getFloat(k, 9), e2=cat.getFloat(k, 10))
# The flux of an Add object is the sum of the component fluxes.
# Note that in demo3.py, a similar addition was performed by the binary operator "+".
gal = galsim.Add([disk, bulge])
# This flux may be overridden by withFlux. The relative fluxes of the components
# remains the same, but the total flux is set to gal_flux.
gal = gal.withFlux(gal_flux)
gal = gal.shear(g1=gal_g1, g2=gal_g2)
# The center of the object is normally placed at the center of the postage stamp image.
# You can change that with shift:
gal = gal.shift(dx=cat.getFloat(k, 11), dy=cat.getFloat(k, 12))
final = galsim.Convolve([psf, gal])
# Draw the profile
image = galsim.ImageF(xsize, ysize)
final.drawImage(image, scale=pixel_scale)
# Add Poisson noise to the image:
image.addNoise(galsim.PoissonNoise(rng, sky_level * pixel_scale**2))
logger.info('Drew image for object at row %d in the input catalog' % k)
# Add the image to our list of images
images.append(image)
# Now write the images to a multi-extension fits file. Each image will be in its own HDU.
galsim.fits.writeMulti(images, multi_file_name)
logger.info('Images written to multi-extension fits file %r',
multi_file_name)
def test_hlr():
"""Test the calculateHLR method.
"""
import time
t1 = time.time()
# Compare the calculation for a simple Gaussian.
g1 = galsim.Gaussian(sigma=5, flux=1.7)
print 'g1 native hlr = ',g1.half_light_radius
print 'g1.calculateHLR = ',g1.calculateHLR()
print 'nyquist scale = ',g1.nyquistScale()
# These should be exactly equal.
np.testing.assert_equal(g1.half_light_radius, g1.calculateHLR(),
err_msg="Gaussian.calculateHLR() returned wrong value.")
# Check for a convolution of two Gaussians. Should be equivalent, but now will need to
# do the calculation.
g2 = galsim.Convolve(galsim.Gaussian(sigma=3, flux=1.3), galsim.Gaussian(sigma=4, flux=23))
test_hlr = g2.calculateHLR()
print 'g2.calculateHLR = ',test_hlr
print 'ratio - 1 = ',test_hlr/g1.half_light_radius-1
np.testing.assert_almost_equal(test_hlr/g1.half_light_radius, 1.0, decimal=1,
err_msg="Gaussian.calculateHLR() is not accurate.")
# The default scale is only accurate to around 1 dp. Using scale = 0.1 is accurate to 3 dp.
# Note: Nyquist scale is about 4.23 for this profile.
test_hlr = g2.calculateHLR(scale=0.1)
print 'g2.calculateHLR(scale=0.1) = ',test_hlr
print 'ratio - 1 = ',test_hlr/g1.half_light_radius-1
np.testing.assert_almost_equal(test_hlr/g1.half_light_radius, 1.0, decimal=3,
err_msg="Gaussian.calculateHLR(scale=0.1) is not accurate.")
# Finally, we don't expect this to be accurate, but make sure the code can handle having
# more than half the flux in the central pixel.
test_hlr = g2.calculateHLR(scale=15)
print 'g2.calculateHLR(scale=15) = ',test_hlr
print 'ratio - 1 = ',test_hlr/g1.half_light_radius-1
np.testing.assert_almost_equal(test_hlr/g1.half_light_radius/10, 0.1, decimal=1,
err_msg="Gaussian.calculateHLR(scale=15) is not accurate.")
# Next, use an Exponential profile
e1 = galsim.Exponential(scale_radius=5, flux=1.7)
print 'e1 native hlr = ',e1.half_light_radius
print 'e1.calculateHLR = ',e1.calculateHLR()
print 'nyquist scale = ',e1.nyquistScale()
# These should be exactly equal.
np.testing.assert_equal(e1.half_light_radius, e1.calculateHLR(),
err_msg="Exponential.calculateHLR() returned wrong value.")
# Check for a convolution with a delta function. Should be equivalent, but now will need to
# do the calculation.
e2 = galsim.Convolve(galsim.Exponential(scale_radius=5, flux=1.3),
galsim.Gaussian(sigma=1.e-4, flux=23))
test_hlr = e2.calculateHLR()
print 'e2.calculateHLR = ',test_hlr
print 'ratio - 1 = ',test_hlr/e1.half_light_radius-1
np.testing.assert_almost_equal(test_hlr/e1.half_light_radius, 1.0, decimal=1,
err_msg="Exponential.calculateHLR() is not accurate.")
# The default scale is only accurate to around 1 dp. Using scale = 0.1 is accurate to 3 dp.
# Note: Nyquist scale is about 1.57 for this profile.
# We can also decrease the size, which should still be accurate, but maybe a little faster.
# Go a bit more that 2*hlr in units of the pixels.
size = int(2.2 * e1.half_light_radius / 0.1)
test_hlr = e2.calculateHLR(scale=0.1, size=size)
print 'e2.calculateHLR(scale=0.1) = ',test_hlr
print 'ratio - 1 = ',test_hlr/e1.half_light_radius-1
np.testing.assert_almost_equal(test_hlr/e1.half_light_radius, 1.0, decimal=3,
err_msg="Exponential.calculateHLR(scale=0.1) is not accurate.")
# Check that it works if the centroid is not at the origin
e3 = e2.shift(2,3)
test_hlr = e3.calculateHLR(scale=0.1)
print 'e3.calculateHLR(scale=0.1) = ',test_hlr
print 'ratio - 1 = ',test_hlr/e1.half_light_radius-1
np.testing.assert_almost_equal(test_hlr/e1.half_light_radius, 1.0, decimal=3,
err_msg="shifted Exponential HLR is not accurate.")
# Can set a centroid manually. This should be equivalent to the default.
print 'e3.centroid = ',e3.centroid()
test_hlr = e3.calculateHLR(scale=0.1, centroid=e3.centroid())
np.testing.assert_almost_equal(test_hlr/e1.half_light_radius, 1.0, decimal=3,
err_msg="shifted HLR with explicit centroid is not accurate.")
# The calculateHLR method can also return other radii like r90, rather than r50 using the
# parameter flux_fraction. This is also analytic for Exponential
r90 = 3.889720170 * e1.scale_radius
test_r90 = e2.calculateHLR(scale=0.1, flux_frac=0.9)
print 'r90 = ',r90
print 'e2.calculateHLR(scale=0.1, flux_frac=0.9) = ',test_r90
print 'ratio - 1 = ',test_r90/r90-1
np.testing.assert_almost_equal(test_r90/r90, 1.0, decimal=3,
err_msg="Exponential r90 calculation is not accurate.")
# Check the image version.
im = e1.drawImage(scale=0.1)
test_hlr = im.calculateHLR(flux=e1.flux)
print 'im.calculateHLR() = ',test_hlr
print 'ratio - 1 = ',test_hlr/e1.half_light_radius-1
np.testing.assert_almost_equal(test_hlr/e1.half_light_radius, 1.0, decimal=3,
err_msg="image.calculateHLR is not accurate.")
# Check that a non-square image works correctly. Also, not centered anywhere in particular.
#bounds = galsim.BoundsI(-1234, -1234+size*2, 8234, 8234+size)
bounds = galsim.BoundsI(1, 1+size*2, 1, 1+size)
#offset = galsim.PositionD(29,1)
offset = galsim.PositionD(0,0)
im = e1.drawImage(scale=0.1, bounds=bounds, offset=offset)
test_hlr = im.calculateHLR(flux=e1.flux, center=im.trueCenter()+offset)
print 'im.calculateHLR() = ',test_hlr
print 'ratio - 1 = ',test_hlr/e1.half_light_radius-1
np.testing.assert_almost_equal(test_hlr/e1.half_light_radius, 1.0, decimal=3,
err_msg="non-square image.calculateHLR is not accurate.")
t2 = time.time()
print 'time for %s = %.2f'%(funcname(),t2-t1)
def test_hsmparams_nodefault():
"""Test that when non-default hsmparams are used, the results change."""
import time
# First make some profile
bulge = galsim.DeVaucouleurs(half_light_radius=0.3)
disk = galsim.Exponential(half_light_radius=0.5)
disk = disk.shear(e1=0.2, e2=-0.3)
psf = galsim.Kolmogorov(fwhm=0.6)
gal = bulge + disk # equal weighting, i.e., B/T=0.5
tot_gal = galsim.Convolve(gal, psf)
tot_gal_image = tot_gal.drawImage(scale=0.18)
tot_psf_image = psf.drawImage(scale=0.18)
# Check that recompute_flux changes give results that are as expected
test_t = time.time()
res = galsim.hsm.EstimateShear(tot_gal_image, tot_psf_image)
dt = time.time() - test_t
res2 = galsim.hsm.EstimateShear(tot_gal_image,
tot_psf_image,
recompute_flux='sum')
assert (res.moments_amp <
res2.moments_amp), 'Incorrect behavior with recompute_flux=sum'
res3 = galsim.hsm.EstimateShear(tot_gal_image,
tot_psf_image,
recompute_flux='none')
assert (
res3.moments_amp == 0), 'Incorrect behavior with recompute_flux=none'
# Check that results, timing change as expected with nsig_rg
# For this, use Gaussian as galaxy and for ePSF, i.e., no extra pixel response
p = galsim.Gaussian(fwhm=10.)
g = galsim.Gaussian(fwhm=20.)
g = g.shear(g1=0.5)
obj = galsim.Convolve(g, p)
# HSM allows a slop of 1.e-8 on nsig_rg, which means that default float32 images don't
# actually end up with different result when using nsig_rg=0. rather than 3.
im = obj.drawImage(scale=1., method='no_pixel', dtype=float)
psf_im = p.drawImage(scale=1., method='no_pixel', dtype=float)
test_t1 = time.time()
g_res = galsim.hsm.EstimateShear(im, psf_im)
test_t2 = time.time()
g_res2 = galsim.hsm.EstimateShear(
im, psf_im, hsmparams=galsim.hsm.HSMParams(nsig_rg=0.))
dt2 = time.time() - test_t2
dt1 = test_t2 - test_t1
if test_timing:
assert (
dt2 > dt1
), 'Should take longer to estimate shear without truncation of galaxy'
assert (not equal_hsmshapedata(
g_res, g_res2)), 'Results should differ with diff nsig_rg'
assert g_res != g_res2, 'Results should differ with diff nsig_rg'
# Check that results, timing change as expected with max_moment_nsig2
test_t2 = time.time()
res2 = galsim.hsm.EstimateShear(
tot_gal_image,
tot_psf_image,
hsmparams=galsim.hsm.HSMParams(max_moment_nsig2=9.))
dt2 = time.time() - test_t2
if test_timing:
assert (
dt2 < dt
), 'Should be faster to estimate shear with lower max_moment_nsig2'
assert (not equal_hsmshapedata(
res, res2)), 'Outputs same despite change in max_moment_nsig2'
assert res != res2, 'Outputs same despite change in max_moment_nsig2'
assert (res.moments_sigma >
res2.moments_sigma), 'Sizes do not change as expected'
assert (res.moments_amp >
res2.moments_amp), 'Amplitudes do not change as expected'
# Check that max_amoment, max_ashift work as expected
assert_raises(galsim.GalSimError,
galsim.hsm.EstimateShear,
tot_gal_image,
tot_psf_image,
hsmparams=galsim.hsm.HSMParams(max_amoment=10.))
assert_raises(galsim.GalSimError,
galsim.hsm.EstimateShear,
tot_gal_image,
tot_psf_image,
guess_centroid=galsim.PositionD(47.,
tot_gal_image.true_center.y),
hsmparams=galsim.hsm.HSMParams(max_ashift=0.1))