def GaussMoffatFit(pixels, projected_footprint, amplitude, x_0, gamma, alpha,
A, mu, sigma, residuals, i, plot):
g_init = models.Moffat1D(amplitude = amplitude, x_0 = x_0, gamma = gamma, alpha=alpha)\
+ models.Gaussian1D(amplitude=A, mean=mu, stddev=sigma)
g_init.stddev_1.min = 0.5
g_init.stddev_1.max = 3.
g_init.amplitude_0.min = 1.
g_init.amplitude_0.max = A / 10.
g_init.gamma_0.min = 1.
g_init.gamma_0.max = 2.
g_init.alpha_0.min = 1.
g_init.alpha_0.max = 2.
fit_g = fitting.LevMarLSQFitter()
psf = fit_g(g_init, pixels, projected_footprint)
start = psf.x_0_0 - 10 * psf.stddev_1
end = psf.x_0_0 + 10 * psf.stddev_1
integralGM = (integrate.quad(lambda pixels: psf(pixels), start, end))[0]
integralG = np.sqrt(2 * np.pi) * psf.stddev_1 * psf.amplitude_1
''' begin Control plot'''
if ((not i % 10) and (i < 400) and (plot == True)):
pl.plot(pixels, psf(pixels), label='Gauss+Moffat')
pl.yscale('log')
pl.ylim(1., 1E6)
pl.plot(pixels, projected_footprint)
pl.legend()
pl.show()
''' End control plot'''
'''Filling residuals'''
residuals[:, i] = psf(pixels) - projected_footprint
return integralGM, integralG, psf.amplitude_0.value, psf.x_0_0.value, psf.gamma_0.value, psf.alpha_0.value, psf.amplitude_1.value, psf.mean_1.value, psf.stddev_1.value
def test_moffat_fwhm(gamma):
ans = 34.641016151377542
kwargs = {'gamma': gamma, 'alpha': 0.5}
m1 = models.Moffat1D(**kwargs)
m2 = models.Moffat2D(**kwargs)
assert_allclose([m1.fwhm, m2.fwhm], ans)
assert_array_less(0, [m1.fwhm, m2.fwhm])
def make_2dspec_image(
nx=3000,
ny=1000,
background=5,
trace_center=None,
trace_order=3,
trace_coeffs={'c0': 0, 'c1': 50, 'c2': 100},
source_amplitude=10,
source_alpha=0.1
):
"""
Create synthetic 2D spectroscopic image with a single source. The spatial (y-axis) position
of the source along the dispersion (x-axis) direction is modeled using a Chebyshev polynomial.
The flux units are counts and the noise is modeled as Poisson.
Parameters
----------
nx : int (default=3000)
Size of image in X axis which is assumed to be the dispersion axis
ny : int (default=1000)
Size of image in Y axis which is assumed to be the spatial axis
background : int (default=5)
Level of constant background in counts
trace_center : int (default=None)
Zeropoint of the trace. If None, then use center of Y (spatial) axis.
trace_order : int (default=3)
Order of the Chebyshev polynomial used to model the source's trace
trace_coeffs : dict (default={'c0': 0, 'c1': 50, 'c2': 100})
Dict containing the Chebyshev polynomial coefficients to use in the trace model
source_amplitude : int (default=10)
Amplitude of modeled source in counts
source_alpha : float (default=0.1)
Power index of the source's Moffat profile. Use small number here to emulate
extended source.
Returns
-------
ccd_im : `~astropy.nddata.CCDData`
CCDData instance containing synthetic 2D spectroscopic image
"""
x = np.arange(nx)
y = np.arange(ny)
xx, yy = np.meshgrid(x, y)
profile = models.Moffat1D()
profile.amplitude = source_amplitude
profile.alpha = source_alpha
if trace_center is None:
trace_center = ny / 2
trace_mod = models.Chebyshev1D(degree=trace_order, **trace_coeffs)
trace = yy - trace_center + trace_mod(xx/nx)
z = background + profile(trace)
noisy_image = apply_poisson_noise(z)
ccd_im = CCDData(noisy_image, unit=u.count)
return ccd_im
def MoffatFit(pixels, projected_footprint, A, mu, sigma):
g_init = models.Moffat1D(amplitude=A, x_0=mu, gamma=sigma)
fit_g = fitting.LevMarLSQFitter()
psf = fit_g(g_init, pixels, projected_footprint)
start = psf.x_0 - 5 * psf.gamma
end = psf.x_0 + 5 * psf.gamma
integral = (integrate.quad(lambda pixels: psf(pixels), start, end))[0]
''' begin Control plot'''
#pl.plot(pixels, psf(pixels), label='Moffat')
#pl.yscale('log')
#pl.ylim(1., 1E6)
#pl.plot(projected_footprint)
''' End control plot'''
return
def model_data(self):
#Astropy Simplex LSQ Fitter for PSFs
fitter = fitting.SimplexLSQFitter()
#Try to fit Moffat in X direction
try:
moffatx_init = models.Moffat1D(1.2 * np.max(self.xdata), self.x,
1.0, 1.0)
moffatx_fit = fitter(moffatx_init, self.X[self.x0:self.x1],
self.xdata[self.x0:self.x1])
self.xmoff = moffatx_fit(self.Xs)
self.x_opt = moffatx_fit.x_0.value
except:
self.xmoff = np.zeros_like(self.Xs)
self.x_opt = self.x
#Try to fit Moffat in Y direction
try:
#self.ydata -= np.median(self.ydata)
moffaty_init = models.Moffat1D(1.2 * np.max(self.ydata), self.y,
1.0, 1.0)
moffaty_fit = fitter(moffaty_init, self.Y[self.y0:self.y1],
self.ydata[self.y0:self.y1])
self.ymoff = moffaty_fit(self.Ys)
self.y_opt = moffaty_fit.x_0.value
except:
self.ymoff = np.zeros_like(self.Ys)
self.y_opt = self.y
#Update upper and lower bounds for fitting PSF
self.x0 = max(0, self.x - self.dx)
self.x1 = min(self.X[-1] - 1, self.x + self.dx)
self.y0 = max(0, self.y - self.dy)
self.y1 = min(self.Y[-1] - 1, self.y + self.dy)
def fit_moffat_1d(data, gamma=2., alpha=1.):
"""Fit a 1D moffat profile to the data and return the fit."""
# data is assumed to already be chunked to a reasonable size
ldata = len(data)
x = np.arange(ldata)
# Fit model to data
fit = fitting.LevMarLSQFitter()
# Moffat1D
model = models.Moffat1D(amplitude=max(data), x_0=ldata/2, gamma=gamma, alpha=alpha)
with warnings.catch_warnings():
# Ignore model linearity warning from the fitter
warnings.simplefilter('ignore')
results = fit(model, x, data)
# previous yield amp, ycenter, xcenter, sigma, offset
return results
def fit_moffat_1d(x, y, gamma=2., alpha=1.):
"""Fit a 1D moffat profile to the data and return the fit."""
# Fit model to data
fit = fitting.LevMarLSQFitter()
x_0 = x[0]
# Moffat1D
model = models.Moffat1D(amplitude=max(y),
x_0=x_0,
gamma=gamma,
alpha=alpha)
with warnings.catch_warnings():
# Ignore model linearity warning from the fitter
warnings.simplefilter('ignore')
results = fit(model, x, y)
# previous yield amp, ycenter, xcenter, sigma, offset
return results
def MoffatFit(pixels, projected_footprint, A, mu, sigma, residuals, i, plot):
g_init = models.Moffat1D(amplitude=A, x_0=mu, gamma=sigma)
fit_g = fitting.LevMarLSQFitter()
psf = fit_g(g_init, pixels, projected_footprint)
start = psf.x_0 - 5 * psf.gamma
end = psf.x_0 + 5 * psf.gamma
integral = (integrate.quad(lambda pixels: psf(pixels), start, end))[0]
''' begin Control plot'''
if ((not i % 10) and (i < 400) and (plot == True)):
pl.plot(pixels, psf(pixels), label='Moffat')
pl.yscale('log')
pl.ylim(1., 1E6)
pl.plot(pixels, projected_footprint)
pl.legend()
pl.show()
''' End control plot'''
'''Filling residuals'''
#residuals[:, i] = psf(pixels)-projected_footprint
return integral, psf.x_0.value, psf.gamma.value, psf.alpha.value
astmodels.Const1D(amplitude=5.),
astmodels.Const2D(amplitude=5.),
astmodels.Disk2D(amplitude=10., x_0=0.5, y_0=1.5, R_0=5.),
astmodels.Ellipse2D(amplitude=10., x_0=0.5, y_0=1.5, a=2., b=4.,
theta=0.1),
astmodels.Exponential1D(amplitude=10., tau=3.5),
astmodels.Gaussian1D(amplitude=10., mean=5., stddev=3.),
astmodels.Gaussian2D(amplitude=10.,
x_mean=5.,
y_mean=5.,
x_stddev=3.,
y_stddev=3.),
astmodels.KingProjectedAnalytic1D(amplitude=10., r_core=5., r_tide=2.),
astmodels.Logarithmic1D(amplitude=10., tau=3.5),
astmodels.Lorentz1D(amplitude=10., x_0=0.5, fwhm=2.5),
astmodels.Moffat1D(amplitude=10., x_0=0.5, gamma=1.2, alpha=2.5),
astmodels.Moffat2D(amplitude=10., x_0=0.5, y_0=1.5, gamma=1.2, alpha=2.5),
astmodels.Planar2D(slope_x=0.5, slope_y=1.2, intercept=2.5),
astmodels.RedshiftScaleFactor(z=2.5),
astmodels.RickerWavelet1D(amplitude=10., x_0=0.5, sigma=1.2),
astmodels.RickerWavelet2D(amplitude=10., x_0=0.5, y_0=1.5, sigma=1.2),
astmodels.Ring2D(amplitude=10., x_0=0.5, y_0=1.5, r_in=5., width=10.),
astmodels.Sersic1D(amplitude=10., r_eff=1., n=4.),
astmodels.Sersic2D(amplitude=10.,
r_eff=1.,
n=4.,
x_0=0.5,
y_0=1.5,
ellip=0.0,
theta=0.0),
astmodels.Sine1D(amplitude=10., frequency=0.5, phase=1.),
from astropy.modeling import Parameter, Fittable1DModel
from astropy.modeling.polynomial import PolynomialModel
registry = {
'Gaussian1D':
models.Gaussian1D(1.0, 1.0, 1.0),
'GaussianAbsorption1D':
models.GaussianAbsorption1D(1.0, 1.0, 1.0),
'Lorentz1D':
models.Lorentz1D(1.0, 1.0, 1.0),
'MexicanHat1D':
models.MexicanHat1D(1.0, 1.0, 1.0),
'Trapezoid1D':
models.Trapezoid1D(1.0, 1.0, 1.0, 1.0),
'Moffat1D':
models.Moffat1D(1.0, 1.0, 1.0, 1.0),
'ExponentialCutoffPowerLaw1D':
models.ExponentialCutoffPowerLaw1D(1.0, 1.0, 1.0, 1.0),
'BrokenPowerLaw1D':
models.BrokenPowerLaw1D(1.0, 1.0, 1.0, 1.0),
'LogParabola1D':
models.LogParabola1D(1.0, 1.0, 1.0, 1.0),
'PowerLaw1D':
models.PowerLaw1D(1.0, 1.0, 1.0),
'Linear1D':
models.Linear1D(1.0, 0.0),
'Const1D':
models.Const1D(0.0),
'Redshift':
models.Redshift(0.0),
'Scale':
def fit_ellipse_for_source(
friendid=None,
detectid=None,
coords=None,
shotid=None,
subcont=True,
convolve_image=False,
pixscale=pixscale,
imsize=imsize,
wave_range=None,
):
if detectid is not None:
global deth5
detectid_obj = detectid
if detectid_obj <= 2190000000:
det_info = deth5.root.Detections.read_where("detectid == detectid_obj")[0]
linewidth = det_info["linewidth"]
wave_obj = det_info["wave"]
redshift = wave_obj / (1216) - 1
else:
det_info = conth5.root.Detections.read_where("detectid == detectid_obj")[0]
redshift = 0
wave_obj = 4500
coords_obj = SkyCoord(det_info["ra"], det_info["dec"], unit="deg")
shotid_obj = det_info["shotid"]
fwhm = surveyh5.root.Survey.read_where("shotid == shotid_obj")["fwhm_virus"][0]
amp = det_info["multiframe"]
if wave_range is not None:
wave_range_obj = wave_range
else:
if detectid_obj <= 2190000000:
wave_range_obj = [wave_obj - 2 * linewidth, wave_obj + 2 * linewidth]
else:
wave_range_obj = [4100, 4200]
if coords is not None:
coords_obj = coords
if shotid is not None:
shotid_obj = shotid
fwhm = surveyh5.root.Survey.read_where("shotid == shotid_obj")[
"fwhm_virus"
][0]
try:
hdu = make_narrowband_image(
coords=coords_obj,
shotid=shotid_obj,
wave_range=wave_range_obj,
imsize=imsize * u.arcsec,
pixscale=pixscale * u.arcsec,
subcont=subcont,
convolve_image=convolve_image,
include_error=True,
)
except:
print("Could not make narrowband image for {}".format(detectid))
return np.nan, np.nan
elif friendid is not None:
global friend_cat
sel = friend_cat["friendid"] == friendid
group = friend_cat[sel]
coords_obj = SkyCoord(ra=group["icx"][0] * u.deg, dec=group["icy"][0] * u.deg)
wave_obj = group["icz"][0]
redshift = wave_obj / (1216) - 1
linewidth = group["linewidth"][0]
shotid_obj = group["shotid"][0]
fwhm = group["fwhm"][0]
amp = group["multiframe"][0]
if wave_range is not None:
wave_range_obj = wave_range
else:
wave_range_obj = [wave_obj - 2 * linewidth, wave_obj + 2 * linewidth]
if shotid is not None:
shotid_obj = shotid
fwhm = surveyh5.root.Survey.read_where("shotid == shotid_obj")[
"fwhm_virus"
][0]
try:
hdu = make_narrowband_image(
coords=coords_obj,
shotid=shotid_obj,
wave_range=wave_range_obj,
imsize=imsize * u.arcsec,
pixscale=pixscale * u.arcsec,
subcont=subcont,
convolve_image=convolve_image,
include_error=True,
)
except:
print("Could not make narrowband image for {}".format(friendid))
return None
elif coords is not None:
coords_obj = coords
if wave_range is not None:
wave_range_obj = wave_range
else:
print(
"You need to supply wave_range=[wave_start, wave_end] for collapsed image"
)
if shotid is not None:
shotid_obj = shotid
fwhm = surveyh5.root.Survey.read_where("shotid == shotid_obj")[
"fwhm_virus"
][0]
else:
print("Enter the shotid to use (eg. 20200123003)")
hdu = make_narrowband_image(
coords=coords_obj,
shotid=shotid_obj,
wave_range=wave_range_obj,
imsize=imsize * u.arcsec,
pixscale=pixscale * u.arcsec,
subcont=subcont,
convolve_image=convolve_image,
include_error=True,
)
else:
print("You must provide a detectid, friendid or coords/wave_range/shotid")
return np.nan, np.nan
w = wcs.WCS(hdu[0].header)
if friendid is not None:
sel_friend_group = friend_cat["friendid"] == friendid
group = friend_cat[sel_friend_group]
eps = 1 - group["a2"][0] / group["b2"][0]
pa = group["pa"][0] * np.pi / 180.0 - 90
sma = group["a"][0] * 3600 / pixscale
coords = SkyCoord(ra=group["icx"][0] * u.deg, dec=group["icy"][0] * u.deg)
wave_obj = group["icz"][0]
redshift = wave_obj / (1216) - 1
linewidth = np.nanmedian(group["linewidth"])
shotid_obj = group["shotid"][0]
fwhm = group["fwhm"][0]
geometry = EllipseGeometry(
x0=w.wcs.crpix[0], y0=w.wcs.crpix[0], sma=sma, eps=eps, pa=pa
)
else:
geometry = EllipseGeometry(
x0=w.wcs.crpix[0], y0=w.wcs.crpix[0], sma=20, eps=0.2, pa=20.0
)
geometry = EllipseGeometry(
x0=w.wcs.crpix[0], y0=w.wcs.crpix[0], sma=20, eps=0.2, pa=20.0
)
# geometry.find_center(hdu.data)
# aper = EllipticalAperture((geometry.x0, geometry.y0), geometry.sma,
# geometry.sma*(1 - geometry.eps), geometry.pa)
# plt.imshow(hdu.data, origin='lower')
# aper.plot(color='white')
ellipse = Ellipse(hdu[0].data)
isolist = ellipse.fit_image()
iso_tab = isolist.to_table()
if len(iso_tab) == 0:
geometry.find_center(hdu[0].data, verbose=False, threshold=0.5)
ellipse = Ellipse(hdu[0].data, geometry)
isolist = ellipse.fit_image()
iso_tab = isolist.to_table()
if len(iso_tab) == 0:
return np.nan, np.nan, np.nan
try:
# compute iso's manually in steps of 3 pixels
ellipse = Ellipse(hdu[0].data) # reset ellipse
iso_list = []
for sma in np.arange(1, 60, 2):
iso = ellipse.fit_isophote(sma)
if np.isnan(iso.intens):
# print('break at {}'.format(sma))
break
else:
iso_list.append(iso)
isolist = IsophoteList(iso_list)
iso_tab = isolist.to_table()
except:
return np.nan, np.nan, np.nan
try:
model_image = build_ellipse_model(hdu[0].data.shape, isolist)
residual = hdu[0].data - model_image
except:
return np.nan, np.nan, np.nan
sma = iso_tab["sma"] * pixscale
const_arcsec_to_kpc = cosmo.kpc_proper_per_arcmin(redshift).value / 60.0
def arcsec_to_kpc(sma):
dist = const_arcsec_to_kpc * sma
return dist
def kpc_to_arcsec(dist):
sma = dist / const_arcsec_to_kpc
return sma
dist_kpc = (
sma * u.arcsec.to(u.arcmin) * u.arcmin * cosmo.kpc_proper_per_arcmin(redshift)
)
dist_arcsec = kpc_to_arcsec(dist_kpc)
# print(shotid_obj, fwhm)
# s_exp1d = models.Exponential1D(amplitude=0.2, tau=-50)
alpha = 3.5
s_moffat = models.Moffat1D(
amplitude=1,
gamma=(0.5 * fwhm) / np.sqrt(2 ** (1.0 / alpha) - 1.0),
x_0=0.0,
alpha=alpha,
fixed={"amplitude": False, "x_0": True, "gamma": True, "alpha": True},
)
s_init = models.Exponential1D(amplitude=0.2, tau=-50)
fit = fitting.LevMarLSQFitter()
s_r = fit(s_init, dist_kpc, iso_tab["intens"])
# Fitting can be done using the uncertainties as weights.
# To get the standard weighting of 1/unc^2 for the case of
# Gaussian errors, the weights to pass to the fitting are 1/unc.
# fitted_line = fit(line_init, x, y, weights=1.0/yunc)
# s_r = fit(s_init, dist_kpc, iso_tab['intens'])#, weights=iso_tab['intens']/iso_tab['intens_err'] )
print(s_r)
try:
r_n = -1.0 * s_r.tau # _0 #* const_arcsec_to_kpc
except:
r_n = np.nan # r_n = -1. * s_r.tau_0
try:
sel_iso = np.where(dist_kpc >= 2 * r_n)[0][0]
except:
sel_iso = -1
aper = EllipticalAperture(
(isolist.x0[sel_iso], isolist.y0[sel_iso]),
isolist.sma[sel_iso],
isolist.sma[sel_iso] * (1 - isolist.eps[sel_iso]),
isolist.pa[sel_iso],
)
phottable = aperture_photometry(hdu[0].data, aper, error=hdu[1].data)
flux = phottable["aperture_sum"][0] * 10 ** -17 * u.erg / (u.cm ** 2 * u.s)
flux_err = phottable["aperture_sum_err"][0] * 10 ** -17 * u.erg / (u.cm ** 2 * u.s)
lum_dist = cosmo.luminosity_distance(redshift).to(u.cm)
lum = flux * 4.0 * np.pi * lum_dist ** 2
lum_err = flux_err * 4.0 * np.pi * lum_dist ** 2
if detectid:
name = detectid
elif friendid:
name = friendid
# Get Image data from Elixer
catlib = catalogs.CatalogLibrary()
try:
cutout = catlib.get_cutouts(
position=coords_obj,
side=imsize,
aperture=None,
dynamic=False,
filter=["r", "g", "f606W"],
first=True,
allow_bad_image=False,
allow_web=True,
)[0]
except:
print("Could not get imaging for " + str(name))
zscale = ZScaleInterval(contrast=0.5, krej=1.5)
vmin, vmax = zscale.get_limits(values=hdu[0].data)
fig = plt.figure(figsize=(20, 12))
fig.suptitle(
"{} ra={:3.2f}, dec={:3.2f}, wave={:5.2f}, z={:3.2f}, mf={}".format(
name, coords_obj.ra.value, coords_obj.dec.value, wave_obj, redshift, amp
),
fontsize=22,
)
ax1 = fig.add_subplot(231, projection=w)
plt.imshow(hdu[0].data, vmin=vmin, vmax=vmax)
plt.xlabel("RA")
plt.ylabel("Dec")
plt.colorbar()
plt.title("Image summed across 4*linewidth")
ax2 = fig.add_subplot(232, projection=w)
plt.imshow(model_image, vmin=vmin, vmax=vmax)
plt.xlabel("RA")
plt.ylabel("Dec")
plt.colorbar()
plt.title("model")
ax3 = fig.add_subplot(233, projection=w)
plt.imshow(residual, vmin=vmin, vmax=vmax)
plt.xlabel("RA")
plt.ylabel("Dec")
plt.colorbar()
plt.title("residuals (image-model)")
# fig = plt.figure(figsize=(10,5))
im_zscale = ZScaleInterval(contrast=0.5, krej=2.5)
im_vmin, im_vmax = im_zscale.get_limits(values=cutout["cutout"].data)
ax4 = fig.add_subplot(234, projection=cutout["cutout"].wcs)
plt.imshow(
cutout["cutout"].data,
vmin=im_vmin,
vmax=im_vmax,
origin="lower",
cmap=plt.get_cmap("gray"),
interpolation="none",
)
plt.text(
0.8,
0.9,
cutout["instrument"] + cutout["filter"],
transform=ax4.transAxes,
fontsize=20,
color="w",
)
plt.contour(hdu[0].data, transform=ax4.get_transform(w))
plt.xlabel("RA")
plt.ylabel("Dec")
aper.plot(
color="white", linestyle="dashed", linewidth=2, transform=ax4.get_transform(w)
)
ax5 = fig.add_subplot(235)
plt.errorbar(
dist_kpc.value,
iso_tab["intens"],
yerr=iso_tab["intens_err"] * iso_tab["intens"],
linestyle="none",
marker="o",
label="Lya SB profile",
)
plt.plot(dist_kpc, s_r(dist_kpc), color="r", label="Lya exp SB model", linewidth=2)
plt.xlabel("Semi-major axis (kpc)")
# plt.xlabel('Semi-major axis (arcsec)')
plt.ylabel("Flux ({})".format(10 ** -17 * (u.erg / (u.s * u.cm ** 2))))
plt.text(0.4, 0.7, "r_n={:3.2f}".format(r_n), transform=ax5.transAxes, fontsize=16)
plt.text(
0.4, 0.6, "L_lya={:3.2e}".format(lum), transform=ax5.transAxes, fontsize=16
)
secax = ax5.secondary_xaxis("top", functions=(kpc_to_arcsec, kpc_to_arcsec))
secax.set_xlabel("Semi-major axis (arcsec)")
# secax.set_xlabel('Semi-major axis (kpc)')
plt.xlim(0, 100)
# plt.plot(sma, s_r(sma), label='moffat psf')
# plt.plot(dist_kpc.value, s1(kpc_to_arcsec(dist_kpc.value)),
# linestyle='dashed', linewidth=2,
# color='green', label='PSF seeing:{:3.2f}'.format(fwhm))
# These two are the exact same
# s1 = models.Moffat1D()
# s1.amplitude = iso_tab['intens'][0]
# alpha=3.5
# s1.gamma = 0.5*(fwhm*const_arcsec_to_kpc)/ np.sqrt(2 ** (1.0 / alpha) - 1.0)
# s1.alpha = alpha
# plt.plot(r_1d, moffat_1d, color='orange')
# plt.plot(dist_kpc.value, (s1(dist_kpc.value)),
# linestyle='dashed', linewidth=2,
# color='blue', label='PSF seeing:{:3.2f}'.format(fwhm))
E = Extract()
E.load_shot(shotid_obj)
moffat_psf = E.moffat_psf(seeing=fwhm, boxsize=imsize, scale=pixscale)
moffat_shape = np.shape(moffat_psf)
xcen = int(moffat_shape[1] / 2)
ycen = int(moffat_shape[2] / 2)
moffat_1d = (
moffat_psf[0, xcen:-1, ycen] / moffat_psf[0, xcen, ycen] * iso_tab["intens"][0]
)
r_1d = moffat_psf[1, xcen:-1, ycen]
E.close()
plt.plot(
arcsec_to_kpc(pixscale * np.arange(80)),
iso_tab["intens"][0] * (moffat_psf[0, 80:-1, 80] / moffat_psf[0, 80, 80]),
linestyle="dashed",
color="green",
label="PSF seeing:{:3.2f}".format(fwhm),
)
plt.legend()
if friendid is not None:
ax6 = fig.add_subplot(236, projection=cutout["cutout"].wcs)
plot_friends(friendid, friend_cat, cutout, ax=ax6, label=False)
plt.savefig("fit2d_{}.png".format(name))
# filename = 'param_{}.txt'.format(name)
# np.savetxt(filename, (r_n.value, lum.value))
return r_n, lum, lum_err
Image_Data_All2 = Image_Data_All[300:400]
Image_Data_All2= np.nan_to_num(Image_Data_All2)
#Define a running median calculator
def RunMedian(x,N):
idx = np.arange(N) + np.arange(len(x)-N+1)[:,None]
b = [row[row>0] for row in x[idx]]
return np.array(map(np.median,b))
#Create the Gaussian and Moffat fits and creates Fit_Data and Fit_Data2
#which contains the parameters for the two models (Moffat still does not work correct)
x = np.linspace(-50,50,100)
Gauss_Model = models.Gaussian1D(amplitude = 1000., mean = 0, stddev = 1., )
Gauss_Model.mean.fixed = False
Moffat_Model = models.Moffat1D(amplitude = 1000, x_0 = 0, gamma = 1, alpha = 2)
Fitting_Model = fitting.LevMarLSQFitter()
Fit_Data_1 = []
Fit_Data_2 = []
for i in range(0, Image_Data_All2.shape[1]):
Fit_Data_1.append(Fitting_Model(Gauss_Model, x, Image_Data_All2[:,i]))
x2 = np.empty((1024,3))
for n in range(1024):
x2[n,:] = Fit_Data_1[n].parameters
Amp_Data_1 = x2[:,0]
def RunMedian(x, N):
idx = np.arange(N) + np.arange(len(x) - N + 1)[:, None]
b = [row[row > 0] for row in x[idx]]
return np.array(map(np.median, b))
#Create the Gaussian and Moffat fits and creates Fit_Data and Fit_Data2
#which contains the parameters for the two models (Moffat still does not work correct)
x = np.linspace(-50, 50, 100)
Gauss_Model = models.Gaussian1D(
amplitude=1000.,
mean=0,
stddev=1.,
)
Gauss_Model.mean.fixed = False
Moffat_Model = models.Moffat1D(amplitude=1000, x_0=0, gamma=1, alpha=2)
Fitting_Model = fitting.LevMarLSQFitter()
Fit_Data_1 = []
Fit_Data_2 = []
#Normal Gauss Model Fitting
for i in range(0, Image_Data_All2.shape[1]):
Fit_Data_1.append(Fitting_Model(Gauss_Model, x, Image_Data_All2[:, i]))
x2 = np.empty((1024, 3))
for n in range(1024):
x2[n, :] = Fit_Data_1[n].parameters
else:
print('Sigma Clipping Complete')
Mean_Poly_Fit = np.ma.polyfit(Mean_Range, Mean_Data_Clipped, Polydegree)
Mean_Range_Fit = np.linspace(0, Image_Pixel_Data.shape[1] - 1,
Image_Pixel_Data.shape[1])
Mean_Data_Fit = Mean_Poly_Fit[0] * Mean_Range_Fit**2 + Mean_Poly_Fit[
1] * Mean_Range_Fit**1 + Mean_Poly_Fit[2]
plt.plot(Mean_Data_1)
plt.plot(Mean_Data_Fit)
plt.show()
#Normal Moffat Model Fitting
Moffat_Model = models.Moffat1D(amplitude=1000, x_0=0, gamma=1, alpha=2)
Fit_Data_2 = []
for i in range(0, Image_Pixel_Data.shape[1]):
if Fit_Data_2: # true if not an empty list
Moffat_Model = models.Moffat1D(amplitude=Ampl_Data_1[-1],
x_0=Mean_Data_Fit[i],
gamma=1.3,
alpha=0.9)
Moffat_Model.x_0.fixed = True
Fit_Data_2.append(Fitting_Model(Moffat_Model, x, Image_Pixel_Data[:, i]))
Fit_Data_2[0] = Fitting_Model(
models.Moffat1D(amplitude=Ampl_Data_1[0],
x_0=Mean_Data_Fit[0],
gamma=1.3,
def moffatModel(pars):
amp, mu, sigma = pars
moff = models.Moffat1D(amplitude=amp, x_0=mu, gamma=sigma)
return moff
fit = fitting.LevMarLSQFitter()
gaus_1 = models.Gaussian1D(amplitude=np.amax(c1_height), mean=0.5*np.pi, stddev=0.05*np.pi)
gaus_2 = models.Gaussian1D(amplitude=np.amax(c2_height), mean=0.5*np.pi, stddev=0.05*np.pi)
th_fit = 0.5 * (c1_th[1:] + c1_th[:-1]) # np.linspace(c_min,c_max,len(c1_height))
th_plot = np.linspace(c_min,c_max,10000)
gausfit_1 = fit(gaus_1, th_fit, c1_height)
# ax_CC[0].plot(th_plot, gausfit_1(th_plot), ls=':', lw=0.9, color='black')
gausfit_2 = fit(gaus_2, th_fit, c2_height)
# ax_CC[1].plot(th_plot, gausfit_2(th_plot), ls=':', lw=0.9, color='black')
c1_stddev = 1. * gausfit_1.stddev # * 2.355 se fwhm
c2_stddev = 1. * gausfit_2.stddev
print('c1_stddev = {:.3f} pi'.format(c1_stddev / np.pi))
print('c2_stddev = {:.3f} pi'.format(c2_stddev / np.pi))
moff_1 = models.Moffat1D(amplitude=np.amax(c1_height), x_0=0.5*np.pi, gamma=1, alpha=1)
moff_2 = models.Moffat1D(amplitude=np.amax(c2_height), x_0=0.5*np.pi, gamma=1, alpha=1)
th_fit = 0.5 * (c1_th[1:] + c1_th[:-1]) # np.linspace(c_min,c_max,len(c1_height))
th_plot = np.linspace(c_min,c_max,10000)
moffit_1 = fit(moff_1, th_fit, c1_height)
ax_CC[0].plot(th_plot, moffit_1(th_plot), ls='--', lw=0.9, color='black')
moffit_2 = fit(moff_2, th_fit, c2_height)
ax_CC[1].plot(th_plot, moffit_2(th_plot), ls='--', lw=0.9, color='black')
# fig_CC.tight_layout()
for i in range(2):
ax_CC[i].grid(ls=':',which='both')
ax_CC[i].set_xlim(c_min,c_max)
# ax_CC[i].xaxis.set_major_locator(tck.MultipleLocator(0.15 / 2 * np.pi))
ax_CC[i].set_xticks(np.array([0.350, 0.425, 0.500, 0.575, 0.650]) * np.pi)
def psfSubtract(fits,
pos,
redshift=None,
vwindow=1000,
radius=5,
mode='scale2D',
errLimit=3,
inst='PCWI'):
global lines, skylines
##### EXTRACT DATA FROM FITS
data = fits[0].data #data cube
head = fits[0].header #header
#ROTATE (TEMPORARILY) SO THAT AXIS 2 IS 'IN-SLICE' for KCWI DATA
if instrument == 'KCWI':
data_rot = np.zeros((data.shape[0], data.shape[2], data.shape[1]))
for wi in range(len(data)):
data_rot[wi] = np.rot90(data[wi], k=1)
data = data_rot
pos = (pos[1], pos[0])
w, y, x = data.shape #Cube dimensions
X = np.arange(x) #Create domains X,Y and W
Y = np.arange(y)
W = np.array([
head["CRVAL3"] + head["CD3_3"] * (i - head["CRPIX3"]) for i in range(w)
])
##### CREATE USEFUl VARIABLES & DATA STRUCTURES
cmodel = np.zeros_like(data) #Cube to store 3D continuum model
usewav = np.ones_like(
W, dtype=bool
) #Boolean array for whether or not to use wavelengths in fitting
Xs = np.linspace(X[0], X[-1],
10 * x) #Smooth X-Y domains for PSF modelling
Ys = np.linspace(Y[0], Y[-1], 10 * y)
ydist = 3600 * np.sqrt(
np.cos(head["CRVAL2"] * np.pi / 180) * head["CD1_2"]**2 +
head["CD2_2"]**2) #X & Y pixel sizes in arcseconds
xdist = 3600 * np.sqrt(
np.cos(head["CRVAL2"] * np.pi / 180) * head["CD1_1"]**2 +
head["CD2_1"]**2)
ry = int(round(radius / ydist)) #X and Y 'radius' extent in pixels
rx = int(round(radius / xdist))
##### EXCLUDE EMISSION LINE WAVELENGTHS
usewav[W < head["WAVGOOD0"]] = 0
usewav[W > head["WAVGOOD1"]] = 0
if redshift != None:
for line in lines:
wc = (redshift + 1) * line
dw = (vwindow * 1e5 / 3e10) * wc
a, b = params.getband(wc - dw, wc + dw, head)
usewav[a:b] = 0
##### OPTIMIZE CENTROID
xc, yc = pos #Take input position tuple
x0, x1 = max(0, xc - rx), min(x,
xc + rx + 1) #Get bounding box for PSF fit
y0, y1 = max(0, yc - ry), min(y, yc + ry + 1)
img = np.sum(data[usewav, y0:y1, x0:x1], axis=0) #Create white light image
xdomain, xdata = range(x1 - x0), np.sum(
img, axis=0) #Get X and Y PSF profiles/domains
ydomain, ydata = range(y1 - y0), np.sum(img, axis=1)
fit = fitting.SimplexLSQFitter() #Get astropy fitter class
moffat_bounds = {'amplitude': (0, float("inf"))}
xMoffInit = models.Moffat1D(max(xdata), x_0=xc - x0,
bounds=moffat_bounds) #Initial guesses
yMoffInit = models.Moffat1D(max(ydata), x_0=yc - y0, bounds=moffat_bounds)
xMoffFit = fit(xMoffInit, xdomain, xdata) #Fit Moffat1Ds to each axis
yMoffFit = fit(yMoffInit, ydomain, ydata)
xc_new = xMoffFit.x_0.value + x0
yc_new = yMoffFit.x_0.value + y0
#If the new centroid is beyond our anticipated error range away... just use scale method
if abs(xc - xc_new) * xdist > errLimit or abs(yc -
yc_new) * ydist > errLimit:
mode = 'scale2D'
#Otherwise, update the box to center better on our continuum source
else:
xc, yc = int(round(xc_new)), int(
round(yc_new)) #Round to nearest integer
x0, x1 = max(0, xc - rx), min(x, xc + rx + 1) #Get new ranges
y0, y1 = max(0, yc - ry), min(y, yc + ry + 1)
xc = max(0, min(x - 1, xc)) #Bound new variables to within image
yc = max(0, min(y - 1, yc))
#This method creates a 2D continuum image and scales it at each wavelength.
if mode == 'scale2D':
print 'scale2D',
##### CREATE CROPPED CUBE
cube = data[:, y0:y1, x0:x1].copy(
) #Create smaller working cube to isolate continuum source
##### CREATE 2D CONTINUUM IMAGE
cont2d = np.mean(cube[usewav], axis=0) #Create 2D continuum image
fitter = fitting.LinearLSQFitter()
##### BUILD 3D CONTINUUM MODEL
for i in range(cube.shape[0]):
A0 = max(0,
float(np.sum(cube[i])) /
np.sum(cont2d)) #Initial guess for scaling factor
scale_init = models.Scale()
scale_fit = fitter(scale_init, np.ndarray.flatten(cont2d),
np.ndarray.flatten(cube[i]))
model = scale_fit.factor.value * cont2d #Add this wavelength layer to the model
data[i, y0:y1, x0:x1] -= model #Subtract from data cube
cmodel[i, y0:y1, x0:x1] += model #Add to larger model cube
#This method just fits a simple line to the spectrum each spaxel; for flat continuum sources.
elif mode == 'lineFit':
print 'lineFit',
#Define custom astropy model class (just a line)
@custom_model
def line(xx, m=0, c=0):
return m * xx + c
#Run through pixels in 2D region
for yi in range(y0, y1):
for xi in range(x0, x1):
m_init = line() #Create initial guess model
m = fit(m_init, W[usewav], data[usewav, yi,
xi]) #Optimize model
model = m(W)
cmodel[:, yi, xi] += model
data[:, yi, xi] -= model
#This method extracts a central spectrum and fits it to each spaxel
elif mode == 'specFit':
print 'specFit',
#Define custom astropy model class (just a line)
@custom_model
def line(xx, m=0, c=0):
return m * xx + c
##### GET QSO SPECTRUM
q_spec = data[:, yc, xc].copy()
q_spec_fit = q_spec[usewav == 1]
#Run through slices
for yi in range(y0, y1):
print yi,
sys.stdout.flush()
#If this not the main QSO slice
if yi != yc:
#Extract QSO spectrum for this slice
s_spec = data[:, yi, xc].copy()
s_spec_fit = s_spec[usewav == 1]
#Estimate wavelength shift needed
corr = scipy.signal.correlate(s_spec, q_spec)
corrs = scipy.ndimage.filters.gaussian_filter1d(corr, 5.0)
w_offset = (np.nanargmax(corrs) - len(corrs) / 2) / 2.0
#Find wavelength offset (px) for this slice
chisq = lambda x: s_spec_fit[10:-10] - x[
0] * scipy.ndimage.interpolation.shift(
q_spec_fit, x[1], order=4, mode='reflect')[10:-10]
p0 = [np.max(s_spec) / np.max(q_spec), w_offset]
lbound = [0.0, -5]
ubound = [5.1, 5]
for j in range(len(p0)):
if p0[j] < lbound[j]: p0[j] = lbound[j]
elif p0[j] > ubound[j]: p0[j] = ubound[j]
p_fit = scipy.optimize.least_squares(chisq,
p0,
bounds=(lbound, ubound),
jac='3-point')
A0, dw0 = p_fit.x
q_spec_shifted = scipy.ndimage.interpolation.shift(
q_spec_fit, dw0, order=3, mode='reflect')
else:
q_spec_shifted = q_spec_fit
A0 = 0.5
dw0 = 0
lbound = [0.0, -5]
ubound = [20.0, 5]
for xi in range(x0, x1):
spec = data[:, yi, xi]
spec_fit = spec[usewav == 1]
#First fit to find wav offset for this slice
chisq = lambda x: spec_fit - x[
0] * scipy.ndimage.interpolation.shift(
q_spec_fit, x[1], order=3, mode='reflect')
p0 = [A0, dw0]
for j in range(len(p0)):
if p0[j] < lbound[j]: p0[j] = lbound[j]
elif p0[j] > ubound[j]: p0[j] = ubound[j]
#elif abs(p0[j]<1e-6): p0[j]=0
sys.stdout.flush()
p_fit = scipy.optimize.least_squares(chisq,
p0,
bounds=(lbound, ubound),
jac='3-point')
A, dw = p_fit.x
m_spec = A * scipy.ndimage.interpolation.shift(
q_spec, dw, order=4, mode='reflect')
#Do a linear fit to residual and correct linear errors
residual = data[:, yi, xi] - m_spec
ydata = residual[usewav == 1]
xdata = W[usewav == 1]
#m_init = line() #Create initial guess model
#m = fit(m_init, xdata, ydata) #Optimize model
#linefit = m(W)
model = m_spec
#residual = data[:,yi,xi] - model
if 0 and abs(yi - yc) < 1 and abs(xi - xc) < 1:
plt.figure(figsize=(16, 8))
plt.subplot(311)
plt.title(r"$A=%.4f,d\lambda=%.3fpx$" % (A, dw))
plt.plot(W, spec, 'bx', alpha=0.5)
plt.plot(W[usewav == 1], spec[usewav == 1], 'kx')
plt.plot(W, A * q_spec, 'g-', alpha=0.8)
plt.plot(W, model, 'r-')
plt.xlim([W[0], W[-1]])
plt.ylim([1.5 * min(spec), max(spec) * 1.5])
plt.subplot(312)
plt.xlim([W[0], W[-1]])
plt.plot(W, residual, 'gx')
plt.ylim([1.5 * min(residual), max(spec) * 1.5])
plt.subplot(313)
plt.hist(residual)
plt.tight_layout()
plt.show()
cmodel[:, yi, xi] += model
data[:, yi, xi] -= model
#ROTATE BACK IF ROTATED AT START
if instrument == 'KCWI':
data_rot = np.zeros((data.shape[0], data.shape[2], data.shape[1]))
cmodel_rot = np.zeros((data.shape[0], data.shape[2], data.shape[1]))
for wi in range(len(data)):
data_rot[wi] = np.rot90(data[wi], k=3)
cmodel_rot[wi] = np.rot90(cmodel[wi], k=3)
data = data_rot
cmodel = cmodel_rot
return data, cmodel
fitsimage_1.info()
fits1 = fitsimage_1[0]
#print(fits1.data.shape)
#print(fits1.header)
Image_Data_0 = fits1.data[:,0]
Image_Data2_0 = Image_Data_0[325:375]
Image_Data_All = fits1.data[:,:]
Image_Data_All2 = Image_Data_All[325:375]
x = np.linspace(-50,50,50)
Gauss_Model = models.Gaussian1D(amplitude = 1000., mean = 0, stddev = 1.)
Moffat_Model = models.Moffat1D(amplitude = 1000., x_0 = 0, gamma = 2., alpha = 1.)
Fitting_Model = fitting.LevMarLSQFitter()
Fit_Data = []
Fit_Data_2 = []
for i in range(0, Image_Data_All2.shape[1]):
Fit_Data.append(Fitting_Model(Gauss_Model, x, Image_Data_All2[:,i]))
for i in range(0, Image_Data_All2.shape[1]):
Fit_Data_2.append(Fitting_Model(Moffat_Model, x, Image_Data_All2[:,i]))
def get_mask(fits, regfile):
print "\tGenerating 2D mask from region file"
#EXTRACT/CREATE USEFUL VARS############
data3D = fits[0].data
head3D = fits[0].header
W, Y, X = data3D.shape #Dimensions
mask = np.zeros((Y, X), dtype=int) #Mask to be filled in
x, y = np.arange(X), np.arange(Y) #Create X/Y image coordinate domains
xx, yy = np.meshgrid(x, y) #Create meshgrid of X, Y
ww = np.array([
head3D["CRVAL3"] + head3D["CD3_3"] * (i - head3D["CRPIX3"])
for i in range(W)
])
yPS = np.sqrt(
np.cos(head3D["CRVAL2"] * np.pi / 180) * head3D["CD1_2"]**2 +
head3D["CD2_2"]**2) #X & Y plate scales (deg/px)
xPS = np.sqrt(
np.cos(head3D["CRVAL2"] * np.pi / 180) * head3D["CD1_1"]**2 +
head3D["CD2_1"]**2)
fit = fitting.SimplexLSQFitter() #Get astropy fitter class
Lfit = fitting.LinearLSQFitter()
usewav = np.ones_like(ww, dtype=bool)
usewav[ww < head3D["WAVGOOD0"]] = 0
usewav[ww > head3D["WAVGOOD1"]] = 0
data2D = np.sum(data3D[usewav], axis=0)
med = np.median(data2D)
#BUILD MASK############################
if regfile[0].coord_format == 'image':
rr = np.sqrt((xx - x0)**2 + (yy - y0)**2)
mask[rr <= R] = i + 1
elif regfile[0].coord_format == 'fk5':
#AIC = 2k + n Log(RSS/n) [ - (2k**2 +2k )/(n-k-1) ]
def AICc(dat, mod, k):
RSS = np.sum((dat - mod)**2)
n = np.size(dat)
return 2 * k + n * np.log(RSS / n) #+ (2*k**2 + 2*k)/(n-k-1)
head2D = head3D.copy() #Create a 2D header by modifying 3D header
for key in [
"NAXIS3", "CRPIX3", "CD3_3", "CRVAL3", "CTYPE3", "CNAME3",
"CUNIT3"
]:
head2D.remove(key)
head2D["NAXIS"] = 2
head2D["WCSDIM"] = 2
wcs = WCS(head2D)
ra, dec = wcs.wcs_pix2world(xx, yy, 0) #Get meshes of RA/DEC
for i, reg in enumerate(regfile):
ra0, dec0, R = reg.coord_list #Extract location and default radius
rr = np.sqrt(
(np.cos(dec * np.pi / 180) * (ra - ra0))**2 +
(dec - dec0)**2) #Create meshgrid of distance to source
if np.min(rr) > R:
continue #Skip any sources more than one default radius outside the FOV
else:
yc, xc = np.where(rr == np.min(rr)) #Take input position tuple
xc, yc = xc[0], yc[0]
rx = 2 * int(round(
R / xPS)) #Convert angular radius to distance in pixels
ry = 2 * int(round(R / yPS))
x0, x1 = max(0, xc - rx), min(X, xc + rx +
1) #Get bounding box for PSF fit
y0, y1 = max(0, yc - ry), min(Y, yc + ry + 1)
img = np.mean(data3D[usewav, y0:y1, x0:x1],
axis=0) #Not strictly a white-light image
img -= np.median(img) #Correct in case of bad sky subtraction
xdomain, xdata = range(x1 - x0), np.mean(
img, axis=0) #Get X and Y domains/data
ydomain, ydata = range(y1 - y0), np.mean(img, axis=1)
moffat_bounds = {'amplitude': (0, float("inf"))}
xMoffInit = models.Moffat1D(
max(xdata), x_0=xc - x0,
bounds=moffat_bounds) #Initial guess Moffat profiles
yMoffInit = models.Moffat1D(max(ydata),
x_0=yc - y0,
bounds=moffat_bounds)
xLineInit = models.Linear1D(slope=0, intercept=np.mean(xdata))
yLineInit = models.Linear1D(slope=0, intercept=np.mean(ydata))
xMoffFit = fit(xMoffInit, xdomain,
xdata) #Fit Moffat1Ds to each axis
yMoffFit = fit(yMoffInit, ydomain, ydata)
xLineFit = Lfit(xLineInit, xdomain,
xdata) #Fit Linear1Ds to each axis
yLineFit = Lfit(yLineInit, ydomain, ydata)
kMoff = len(xMoffFit.parameters
) #Get number of parameters in each model
kLine = len(xLineFit.parameters)
xMoffAICc = AICc(
xdata, xMoffFit(xdomain),
kMoff) #Get Akaike Information Criterion for each
xLineAICc = AICc(xdata, xLineFit(xdomain), kLine)
yMoffAICc = AICc(ydata, yMoffFit(ydomain), kMoff)
yLineAICc = AICc(ydata, yLineFit(ydomain), kLine)
xIsMoff = xMoffAICc < xLineAICc # Determine if Moffat is a better fit than a simple line
yIsMoff = yMoffAICc < yLineAICc
if xIsMoff and yIsMoff: #If source has detectable moffat profile (i.e. bright source) expand mask
xfwhm = xMoffFit.gamma.value * 2 * np.sqrt(
2**(1 / xMoffFit.alpha.value) - 1) #Get FWHMs
yfwhm = yMoffFit.gamma.value * 2 * np.sqrt(
2**(1 / yMoffFit.alpha.value) - 1)
R = 2 * max(xfwhm * xPS, yfwhm * yPS)
mask[rr < R] = i + 1
return mask
# ------Gaussian smoothing for tip-tilt uncertainties----------
final_kernel = con.convolve(added_kernel, gaussian_kernel, normalize_kernel=True)
if not plot_breakdown: final_kernel.normalize(mode='integral')
if plot2d: fig = plot_kernel(final_kernel, 'Convolved')
# ------plotting 1D cross-sections of the 2D kernels----------
portion = int(fraction_to_plot * (size/2)) + 1
if plot_breakdown:
ax.plot(np.arange(portion), airy_kernel.array[size/2][size/2 : size/2 + portion], c='r', lw=1, label='Airy (%.2F")'%radius_arcsec)
ax.plot(np.arange(portion), moffat_kernel.array[size/2][size/2 : size/2 + portion], c='brown', lw=1, label='Moffat (%.2F")'%fwhm_arcsec)
ax.plot(np.arange(portion), added_kernel.array[size/2][size/2 : size/2 + portion], c='gray', lw=1, label='Airy + Moffat', linestyle='--')
ax.plot(np.arange(portion), gaussian_kernel.array[size/2][size/2 : size/2 + portion], c='g', lw=1, label='Gaussian (%.2F")'%gaussian_blur_arcsec)
fwhm_guess = 0.1#fwhm_arcsec / 4.
gamma_guess = (fwhm_guess/arcsec_per_pixel)/(2 * np.sqrt(np.power(2, 1./beta) - 1))
fitted_moffat = fitting.LevMarLSQFitter()(models.Moffat1D(x_0=0, alpha=beta, gamma=gamma_guess, \
fixed={'alpha':True, 'x_0':True, 'gamma':False, 'amplitude':False}), \
np.arange(portion), final_kernel.array[size / 2][size / 2: size / 2 + portion])
print fitted_moffat #
fitted_moffat_fwhm_pix = fitted_moffat.gamma * (2 * np.sqrt(np.power(2, 1./fitted_moffat.alpha) - 1))
fitted_moffat_fwhm_arcsec = fitted_moffat_fwhm_pix * arcsec_per_pixel
ax.plot(np.arange(portion), fitted_moffat(np.arange(portion)), c='goldenrod', lw=1, label='Fitted Moffat (%.2F")'%fitted_moffat_fwhm_arcsec)
rms = np.sqrt(np.sum((fitted_moffat(np.arange(portion)) - final_kernel.array[size / 2][size / 2: size / 2 + portion])**2))
print 'RMS = %.3E'%rms #
label = 'Convolved: Strehl %.1F'%strehl
else:
label = '%s band: Strehl %.1F'%(band, strehl)
ax.plot(np.arange(portion), final_kernel.array[size/2][size/2 : size/2 + portion], lw=2, label=label)
ax.legend()
ax.set_xlim(0, 0.2 / arcsec_per_pixel)
ax.set_xticklabels(['%.2F' % (float(item) * arcsec_per_pixel) for item in ax.get_xticks()])
def gausMoffatModel(pars):
moffatAmp, x0, gamma, alpha, gausAmp, mu, gausSigma = pars
moff = models.Moffat1D(amplitude=moffatAmp, x_0=x0, gamma=gamma, alpha=alpha)
gaus = models.Gaussian1D(amplitude=gausAmp, mean=mu, stddev=gausSigma)
model = gaus + moff
return model
def fit_moffat_1d(data,
gamma=2.,
alpha=1.,
sigma_factor=0.,
center_at=None,
weighted=False):
"""Fit a 1D moffat profile to the data and return the fit.
Parameters
----------
data: 2D data array
The input sigma to use
gamma: float (optional)
The input gamma to use
alpha: float (optional)
The input alpha to use
sigma_factor: float (optional)
If sigma>0 then sigma clipping of the data is performed
at that level
center_at: float or None
None by default, set to value to use as center
weighted: bool
if weighted is True, then weight the values by basic
uncertainty hueristic
Returns
-------
The fitted 1D moffat model for the data
"""
# data is assumed to already be chunked to a reasonable size
ldata = len(data)
# guesstimate mean
if center_at:
x0 = 0
else:
x0 = int(ldata / 2.)
# assumes negligable background
if weighted:
z = np.nan_to_num(1. / np.sqrt(data)) # use as weight
x = np.arange(ldata)
# Initialize the fitter
fitter = fitting.LevMarLSQFitter()
if sigma_factor > 0:
fit = fitting.FittingWithOutlierRemoval(fitter,
sigma_clip,
niter=3,
sigma=sigma_factor)
else:
fit = fitter
# Moffat1D + constant
model = (models.Moffat1D(
amplitude=max(data), x_0=x0, gamma=gamma, alpha=alpha) +
models.Polynomial1D(c0=data.min(), degree=0))
with warnings.catch_warnings():
# Ignore model linearity warning from the fitter
warnings.simplefilter('ignore')
if weighted:
results = fit(model, x, data, weights=z)
else:
results = fit(model, x, data)
# previous yield amp, ycenter, xcenter, sigma, offset
# if sigma clipping is used, results is a tuple of data, model
if sigma_factor > 0:
return results[1]
else:
return results