def LCO_PSF_PHOT(hdu,init_guesses): # im ~ np array dat, pixel [x0,y0] ~ float pixel position, sigma_psf ~ LCO-PSF sigma x0,y0=init_guesses im = hdu.data hdr = hdu.header fwhm = hdr['L1FWHM']/hdr['PIXSCALE'] # PSF FWHM in pixels, roughly ~ 5 pixels, ~ 2 arcsec sigma_psf = fwhm*gaussian_fwhm_to_sigma # PSF sigma in pixels psf_model = IntegratedGaussianPRF(sigma=sigma_psf) daogroup = DAOGroup(2.0*sigma_psf*gaussian_sigma_to_fwhm) mmm_bkg = MMMBackground() fitter = LevMarLSQFitter() psf_model.x_0.fixed = True psf_model.y_0.fixed = True pos = Table(names=['x_0', 'y_0'], data=[[x0],[y0]]) # optionally give flux_0 has good aperture method for guessing though photometry = BasicPSFPhotometry(group_maker=daogroup, bkg_estimator=mmm_bkg, psf_model=psf_model, fitter=LevMarLSQFitter(), fitshape=(11,11)) result_tab = photometry(image=im, init_guesses=pos) residual_image = photometry.get_residual_image() return result_tab
def photomyPSF(imgdata, position, sigma):
PSFdata = np.copy(imgdata)
sigma_psf = sigma
daogroup = DAOGroup(2.0 * sigma_psf * gaussian_sigma_to_fwhm)
mmm_bkg = MMMBackground()
#fitter = LevMarLSQFitter()
psf_model = IntegratedGaussianPRF(sigma=sigma_psf)
sources = Table()
sources['x_mean'] = position[:, 0].T
sources['y_mean'] = position[:, 1].T
psf_model.x_0.fixed = True
psf_model.y_0.fixed = True
pos = Table(names=['x_0', 'y_0'],
data=[sources['x_mean'], sources['y_mean']])
photometry = BasicPSFPhotometry(group_maker=daogroup,
bkg_estimator=mmm_bkg,
psf_model=psf_model,
fitter=LevMarLSQFitter(),
fitshape=(11, 11))
result_tab = photometry(image=PSFdata, init_guesses=pos)
positionflux = np.transpose(
(result_tab['x_fit'], result_tab['y_fit'], result_tab['flux_fit']))
magstar = 25 - 2.5 * np.log10(abs(result_tab['flux_fit'] / 1))
return positionflux, magstar
def PSF_photometry(data, coord_table, sigma_psf=10, scale=0.67, step=0.5):
FLUX = []
bkgrms = MADStdBackgroundRMS()
std = bkgrms(data)
iraffind = IRAFStarFinder(threshold=3.5 * std,
fwhm=sigma_psf * gaussian_sigma_to_fwhm,
minsep_fwhm=0.01,
roundhi=5.0,
roundlo=-5.0,
sharplo=0.0,
sharphi=2.0)
daogroup = DAOGroup(2.0 * sigma_psf * gaussian_sigma_to_fwhm)
mmm_bkg = MMMBackground()
fitter = LevMarLSQFitter()
psf_model = IntegratedGaussianPRF(sigma=sigma_psf)
# psf_model.x_0.fixed = True
# psf_model.y_0.fixed = True
pos = Table(names=['x_0', 'y_0'],
data=[coord_table['X'],
coord_table['Y']])[coord_table['good_star']]
photometry = IterativelySubtractedPSFPhotometry(finder=iraffind,
group_maker=daogroup,
bkg_estimator=mmm_bkg,
psf_model=psf_model,
fitter=LevMarLSQFitter(),
niters=1,
fitshape=(41, 41))
result_tab = photometry(image=data, init_guesses=pos)
return result_tab['flux_fit']
def psf_photometry(filepath, filename, show, sn_ra, sn_dec):
start = time.time()
warnings.simplefilter('ignore', category=FITSFixedWarning)
warnings.simplefilter('ignore', category=AstropyUserWarning)
print(f'Working on {filename}')
full_filepath = filepath + filename
image_data = getdata(full_filepath)
hdr = getheader(full_filepath)
fwhm = hdr['L1FWHM'] / hdr['PIXSCALE']
exptime = hdr['EXPTIME']
metadata = load_pickle(filename)
epsf_data = np.array(metadata['epsf'])
epsf = EPSFModel(epsf_data, fwhm=fwhm, oversampling=2)
# epsf.x_0.fixed = True
# epsf.y_0.fixed = True
daogroup = DAOGroup(2.0 * fwhm)
bkg = MMMBackground()
fitter = LevMarLSQFitter()
fitshape = 25
photometry = BasicPSFPhotometry(group_maker=daogroup,
bkg_estimator=bkg,
psf_model=epsf,
fitter=fitter,
fitshape=fitshape,
aperture_radius=fitshape)
psfmags = []
print('\tExtracting other stars . . .')
counter = 0
for star in metadata['psf_fitted_stars']:
counter += 1
(x, y) = star
psfmags = _do_phot(x, y, image_data, exptime, fitshape, photometry,
psfmags)
print(
f'\t\tStars extracted: {counter}/{len(metadata["psf_fitted_stars"])}',
end='\r')
print()
print('\tExtracting supernova . . .')
x, y = _get_sn_xy(filepath, filename, sn_ra, sn_dec)
psfmags = _do_phot(x, y, image_data, exptime, fitshape, photometry,
psfmags)
create_or_update_pickle(filename, key='psfmags', val=psfmags)
end = time.time()
print(f'Time to perform photometry (s): {end-start:.3f}')
if show:
checkmag(image_data, photometry.get_residual_image(), x, y, fitshape)
print()
def findFitVertical(img, x, trailSize):
parDist, perpDist = GT.getDistancesVertical(x, img.shape[1], img.shape[0])
median = np.median(img)
bkg = MMMBackground()
back = bkg(img)
return fit(img-median, perpDist, parDist, trailSize)
def astropy_psf_photometry(img,
sigma_psf,
aperture=3,
x0=None,
y0=None,
filter=True,
sigma_filter=1):
"""
performs PSF photometry on an image. If x0 and y0 are None will attempt to locate the target by searching for the
brightest PSF in the field
:param img: 2D array, image on which to perform PSF photometry
:param sigma_psf: float, standard deviation of the PSF
:param aperture: int, size of the paerture (pixels)
:param x0: x position of the target (pixels)
:param y0: y position of the target (pixels)
:param filter: If True will apply a gaussian filter to the image with standard deviation sigma_filter before
performing PSF photometry
:param sigma_filter: standard deviation of gaussian filter to apply to the image
:return: x0 column of photometry table, y0 column of photometry table, flux column of photometry table
"""
if filter:
image = ndimage.gaussian_filter(img, sigma=sigma_filter, order=0)
else:
image = img
bkgrms = MADStdBackgroundRMS()
std = bkgrms(image[image != 0])
iraffind = IRAFStarFinder(threshold=2 * std,
fwhm=sigma_psf * gaussian_sigma_to_fwhm,
minsep_fwhm=0.01,
roundhi=5.0,
roundlo=-5.0,
sharplo=0.0,
sharphi=2.0)
daogroup = DAOGroup(2.0 * sigma_psf * gaussian_sigma_to_fwhm)
mmm_bkg = MMMBackground()
fitter = LevMarLSQFitter()
psf_model = IntegratedGaussianPRF(sigma=sigma_psf)
if x0 and y0:
pos = Table(names=['x_0', 'y_0'], data=[x0, y0])
photometry = BasicPSFPhotometry(group_maker=daogroup,
bkg_estimator=mmm_bkg,
psf_model=psf_model,
fitter=LevMarLSQFitter(),
fitshape=(11, 11))
res = photometry(image=image, init_guesses=pos)
return res['x_fit'], res['y_fit'], res['flux_0']
photometry = BasicPSFPhotometry(finder=iraffind,
group_maker=daogroup,
bkg_estimator=mmm_bkg,
psf_model=psf_model,
fitter=fitter,
fitshape=(11, 11),
aperture_radius=aperture)
res = photometry(image=image)
return res['x_0'], res['y_0'], res['flux_0']
def __init__(self,
psfimfilename,
targetpixscale,
psfpixscale=0.03,
x_0=None,
y_0=None,
psf_recenter=False,
fix_target_pos=True,
fwhm_arcsec=_HST_WFC3_PSF_FWHM_ARCSEC):
"""
:param psfimfilename: full path for a .fits image file
:param targetpixscale: arcseconds per pixel of the target image
:param psfpixscale: arcseconds per pixel of the psf image (if not
provided in the image header). Defaults to 0.03" per pixel
:param xycenter: tuple, giving pixel coordinates of the star. If not
provided, we assume it is at the center of the image.
:param psf_recenter: execute a centroiding algorithm to locate the
center of the psf
:param fix_target_pos: execute "forced photometry" with the center of
the target fixed, and only the psf flux scaling as a free parameter.
"""
psfimage = fits.open(psfimfilename)
self.header = psfimage[0].header
self.psfimdat = psfimage[0].data
# TODO : check the header for pixel scale info
if x_0 is None:
self.xpsf = self.psfimdat.shape[0] / 2.,
self.ypsf = self.psfimdat.shape[1] / 2.
else:
self.xpsf, self.ypsf = x_0, y_0
if psf_recenter:
self.xpsf, self.ypsf = centroid(self.psfimdat, x_0, y_0)
self.psfmodel = photutils.psf.models.FittableImageModel(
self.psfimdat,
x_0=self.xpsf,
y_0=self.ypsf,
oversampling=targetpixscale / psfpixscale)
# Fix the center of the psf for "forced photometry" -- no recentering
if fix_target_pos:
self.psfmodel.x_0.fixed = True
self.psfmodel.y_0.fixed = True
else:
self.psfmodel.x_0.fixed = False
self.psfmodel.y_0.fixed = False
# Set up the grouper, background estimator, and fitter objects:
self.grouper = DAOGroup(2.0 * fwhm_arcsec * psfpixscale)
self.bkg_estimator = MMMBackground()
self.fitter = LevMarLSQFitter()
def run(self, stars_coords):
stack_path = self.fits_explorer.get("stack")[0]
stack_fwhm = np.mean(self.fwhm_fit.run(fits.getdata(stack_path), stars_coords)[0:2])
print("{} global psf FWHM: {:.2f} (pixels)".format(INFO_LABEL, np.mean(stack_fwhm)))
n_stars = np.shape(stars_coords)[0]
n_images = len(self.files)
fluxes = np.zeros((n_stars, n_images))
pos = Table(
names=["x_0", "y_0"], data=[stars_coords[:, 0], stars_coords[:, 1]]
)
daogroup = DAOGroup(2.0 * stack_fwhm * gaussian_sigma_to_fwhm)
mmm_bkg = MMMBackground()
psf_model = IntegratedGaussianPRF(sigma=stack_fwhm)
psf_model.sigma.fixed = False
sky = []
psf_model.x_0.fixed = True
psf_model.y_0.fixed = True
photometry = BasicPSFPhotometry(
group_maker=daogroup,
bkg_estimator=mmm_bkg,
psf_model=psf_model,
fitter=LevMarLSQFitter(),
fitshape=(17, 17)
)
for i, image in enumerate(
tqdm(
self.files[0::],
desc="Photometry extraction",
unit="files",
ncols=80,
bar_format=TQDM_BAR_FORMAT,
)
):
image = fits.getdata(image)
result_tab = photometry(image=image, init_guesses=pos)
fluxes[:, i] = result_tab["flux_fit"]
sky.append(1)
return fluxes, np.ones_like(fluxes), {"sky": sky}
def __init__(self, fwhm, **kwargs):
super().__init__(**kwargs)
daogroup = DAOGroup(2.0 * fwhm * gaussian_sigma_to_fwhm)
mmm_bkg = MMMBackground()
psf_model = IntegratedGaussianPRF(sigma=fwhm)
psf_model.sigma.fixed = False
psf_model.x_0.fixed = True
psf_model.y_0.fixed = True
self.photometry = BasicPSFPhotometry(group_maker=daogroup,
bkg_estimator=mmm_bkg,
psf_model=psf_model,
fitter=LevMarLSQFitter(),
fitshape=(17, 17))
def do_photometry_basic(image: np.ndarray,
σ_psf: float) -> Tuple[Table, np.ndarray]:
"""
Find stars in an image with IRAFStarFinder
:param image: The image data you want to find stars in
:param σ_psf: expected deviation of PSF
:return: tuple result table, residual image
"""
bkgrms = MADStdBackgroundRMS()
std = bkgrms(image)
iraffind = IRAFStarFinder(threshold=3 * std,
sigma_radius=σ_psf,
fwhm=σ_psf * gaussian_sigma_to_fwhm,
minsep_fwhm=2,
roundhi=5.0,
roundlo=-5.0,
sharplo=0.0,
sharphi=2.0)
daogroup = DAOGroup(0.1 * σ_psf * gaussian_sigma_to_fwhm)
mmm_bkg = MMMBackground()
# my_psf = AiryDisk2D(x_0=0., y_0=0.,radius=airy_minimum)
# psf_model = prepare_psf_model(my_psf, xname='x_0', yname='y_0', fluxname='amplitude',renormalize_psf=False)
psf_model = IntegratedGaussianPRF(sigma=σ_psf)
# psf_model = AiryDisk2D(radius = airy_minimum)#prepare_psf_model(AiryDisk2D,xname ="x_0",yname="y_0")
# psf_model = Moffat2D([amplitude, x_0, y_0, gamma, alpha])
# photometry = IterativelySubtractedPSFPhotometry(finder=iraffind, group_maker=daogroup,
# bkg_estimator=mmm_bkg, psf_model=psf_model,
# fitter=LevMarLSQFitter(),
# niters=2, fitshape=(11,11))
photometry = BasicPSFPhotometry(finder=iraffind,
group_maker=daogroup,
bkg_estimator=mmm_bkg,
psf_model=psf_model,
fitter=LevMarLSQFitter(),
aperture_radius=11.0,
fitshape=(11, 11))
result_table = photometry.do_photometry(image)
return result_table, photometry.get_residual_image()
def __init__(self, imfit_io, config_file_or_dict={}):
if type(config_file_or_dict) == str:
logger.info(f'Loading config file {config_file_or_dict}')
config = load_config(config_file_or_dict)
else:
config = config_file_or_dict.copy()
self.input_config = config.copy()
self.imfit_io = config.pop('imfit_io', imfit_io)
self.sersic_fitter = SersicFitter(out_dir=self.imfit_io)
self.use_hsc_bright_mask = config.pop('use_hsc_bright_mask',
dict(phot=False, imfit=True))
self.residual_image_forced = None
self.residual_image = None
# daofinder parameters
self.threshold = config.pop('threshold', 3.0)
self.daofinder_opt = dict(
sigma_radius=config.pop('sigma_radius', 3.0),
sharphi=config.pop('sharphi', 2.0),
sharplo=config.pop('sharplo', 0.),
roundlo=config.pop('roundlo', -1.0),
roundhi=config.pop('roundhi', 1.0),
)
# daogroup parameter
self.crit_separation = config.pop('crit_separation', 1.5)
# TODO: make these bkgrd methods options
self.bkg = MMMBackground()
self.bkgrms = MADStdBackgroundRMS()
# phot parameters
self.aperture_radius = config.pop('aperture_radius', 1.0)
self.phot_opts = dict(
fitshape=config.pop('fitshape', (15, 15)),
niters=config.pop('niters', 3),
bkg_estimator=self.bkg,
)
self.master_band = config.pop('master_band', 'i')
self.max_match_sep = config.pop('max_match_sep', 1.0)
self.min_match_bands = config.pop('min_match_bands', 4)
def init_setup():
fitimage = fits.open('Serpens3/idxq28010_drz.fits')
imdata = fitimage[1].data
head = fitimage[0].header
bkgrms = MADStdBackgroundRMS()
std = bkgrms(imdata)
mean = np.mean(imdata)
sigma_psf = 2.0
iraffind = IRAFStarFinder(threshold=3.5 * std,
fwhm=sigma_psf * gaussian_sigma_to_fwhm,
minsep_fwhm=0.01,
roundhi=5.0,
roundlo=-5.0,
sharplo=0.0,
sharphi=2.0)
daogroup = DAOGroup(2.0 * sigma_psf * gaussian_sigma_to_fwhm)
mmm_bkg = MMMBackground()
return imdata, bkgrms, std, sigma_psf, iraffind, daogroup, mmm_bkg, mean
def _basic_psf_flux(self,
image,
fwhm,
x=None,
y=None,
return_residual_image=False):
w, h = image.shape
if x is None:
x = w / 2
if y is None:
y = h / 2
wfit = w if w % 2 == 1 else w - 1
hfit = h if h % 2 == 1 else h - 1
fitshape = (wfit, hfit)
daogroup = DAOGroup(2.0 * fwhm)
psf_model = IntegratedGaussianPRF(sigma=fwhm / 2.35)
photometry = BasicPSFPhotometry(group_maker=daogroup,
bkg_estimator=MMMBackground(),
psf_model=psf_model,
fitshape=fitshape)
psf_model.x_0.fixed = True
psf_model.y_0.fixed = True
pos = Table(names=['x_0', 'y_0'], data=[[x], [y]])
result = photometry(image=image, positions=pos)
flux = result["flux_fit"].data[0]
self.results = result
if return_residual_image:
return flux, photometry.get_residual_image()
else:
return flux
def onpress(event):
if event.key == 'p':
filename = d.get('file')
#hdu=fits.open(filename)
hdu = d.get_pyfits()
data = hdu[0].data
x = d.get('crosshair image')
x, y = x.split()
x, y = int(float(x)), int(float(y))
new_image_halfwidth = int(entry1.get())
aperture_radius = int(entry2.get())
inner_sky_radius = int(entry3.get())
outer_sky_radius = int(entry4.get())
new_image = data[y - new_image_halfwidth:y + new_image_halfwidth,
x - new_image_halfwidth:x + new_image_halfwidth]
x_grid = np.arange(x - new_image_halfwidth, x + new_image_halfwidth, 1)
y_grid = np.arange(y - new_image_halfwidth, y + new_image_halfwidth, 1)
x_grid, y_grid = np.meshgrid(x_grid, y_grid)
guess = (np.amax(new_image) - new_image[0, 0], x, y, 3, 3, 0,
new_image[0, 0])
popt, pcov = curve_fit(gauss2d, (x_grid, y_grid),
new_image.ravel(),
p0=guess)
#print popt
x = int(popt[1])
y = int(popt[2])
labeltext.set('X: ' + str(x))
label2text.set('Y: ' + str(y))
new_image = data[y - new_image_halfwidth:y + new_image_halfwidth,
x - new_image_halfwidth:x + new_image_halfwidth]
# for artist in ax1.get_children():
# if hasattr(artist,'get_label') and artist.get_label()=='centroid':
# artist.remove()
ax1.clear()
ax1.matshow(np.flip(new_image, axis=0),
cmap='gray',
origin='upper',
clim=zscale(new_image),
zorder=0)
ax1.scatter(
[new_image_halfwidth + 1], [new_image_halfwidth - 1],
marker='+',
s=120,
c='k',
zorder=1
) #ax1.scatter([popt[1]-x+new_image_halfwidth],[popt[2]-y+new_image_halfwidth],marker='+',s=120,c='k',zorder=1)
aperture_circle = plt.Circle((popt[1] - x + new_image_halfwidth,
popt[2] - y + new_image_halfwidth),
radius=aperture_radius,
linewidth=3,
color='hotpink',
fill=False,
lw=3,
zorder=2)
ax1.add_patch(aperture_circle)
inner_sky = plt.Circle((popt[1] - x + new_image_halfwidth,
popt[2] - y + new_image_halfwidth),
radius=inner_sky_radius,
linewidth=3,
color='lime',
fill=False,
zorder=2)
ax1.add_patch(inner_sky)
outer_sky = plt.Circle((popt[1] - x + new_image_halfwidth,
popt[2] - y + new_image_halfwidth),
radius=outer_sky_radius,
linewidth=3,
color='red',
fill=False,
zorder=2)
ax1.add_patch(outer_sky)
canvas.draw()
#update the radial plot
ax2.clear()
radial = radial_profile(new_image,
[new_image_halfwidth, new_image_halfwidth])
#perform the aperture photometry
#currently 2% different from IDL atv
aperture = CircularAperture((x, y), r=aperture_radius)
annulus = CircularAnnulus((x, y),
r_in=inner_sky_radius,
r_out=outer_sky_radius)
phot_table = aperture_photometry(data, [aperture, annulus])
#new background estimation
bkg_mask = np.ma.masked_outside(radial[0].reshape(new_image.shape),
inner_sky_radius, outer_sky_radius)
bkg_map = Background2D(new_image,
tuple(np.array(new_image.shape) / 4),
mask=bkg_mask.mask,
exclude_mesh_method='all')
bkg_map_med = MMMBackground().calc_background(
bkg_map.data) #bkg_map_med=np.median(bkg_map.background)
#print 'Map sky mean '+str(bkg_map_med)
#bkg_mean=phot_table['aperture_sum_1']/annulus.area()
#print 'Aperture sky mean '+str(bkg_mean)
#phot_table['residual_aperture_sum']=phot_table['aperture_sum_0']-bkg_mean*aperture.area()
phot_table['residual_aperture_sum'] = phot_table[
'aperture_sum_0'] - bkg_map_med * aperture.area()
#print 'Map sky result: '+str(phot_table['aperture_sum_0']-bkg_map_med*aperture.area())
#print "Aperture Photometry Result: "+str(phot_table['residual_aperture_sum'])
label8text.set('Sky Value: ' + str(int(bkg_map_med)))
label9text.set('Aperture Counts: ' +
str(int(phot_table['residual_aperture_sum'][0])))
label10text.set(
'Mag: ' +
str(-2.5 * np.log10(int(phot_table['residual_aperture_sum'][0])) +
25.)[:5])
ax2.scatter(radial[0], radial[1])
if var10.get() == 1:
ax2.plot(np.linspace(0, new_image_halfwidth, num=50),
gauss1d(np.linspace(0, new_image_halfwidth, num=50),
popt[0], 0, np.mean([popt[3], popt[4]]), popt[6]),
c='k',
lw=2)
ax2.text(0.5,
0.93,
'Gaussian FWHM: ' +
str(2.35482 * np.mean([popt[3], popt[4]]))[:5],
transform=ax2.transAxes,
fontsize=int(15 * scaling))
if var11.get() == 1:
moffat1d_guess = (np.amax(new_image) - bkg_map_med, 0, 3, 1,
bkg_map_med)
popt2, pcov2 = curve_fit(moffat1d,
radial[0],
radial[1],
p0=moffat1d_guess)
ax2.plot(np.linspace(0, new_image_halfwidth, num=50),
moffat1d(np.linspace(0, new_image_halfwidth,
num=50), popt2[0], popt2[1],
popt2[2], popt2[3], popt2[4]),
c='r',
lw=2)
ax2.text(
0.5,
0.85,
'Moffat FWHM: ' +
str(2.0 * popt2[2] * np.sqrt(2.0**(1. / popt2[3]) - 1.))[:5],
transform=ax2.transAxes,
fontsize=int(15 * scaling))
ax2.grid(True, color='white', linestyle='-', linewidth=1)
ax2.set_axisbelow(True)
ax2.autoscale(False)
ax2.set_xlim([0, new_image_halfwidth])
ax2.set_xlabel('Radius (Pixels)')
ax2.set_ylim([np.amin(radial[1]), np.amax(radial[1])])
ax2.set_axis_bgcolor('0.85')
ax2.axvline(aperture_radius, linewidth=2, color='hotpink')
ax2.axvline(inner_sky_radius, linewidth=2, color='lime')
ax2.axvline(outer_sky_radius, linewidth=2, color='red')
ax2.axhline(bkg_map_med, linewidth=2, color='yellow')
canvas2.draw()
radial = radial_profile(new_image, [new_image_halfwidth, new_image_halfwidth])
#perform the aperture photometry
#currently 2% different from IDL atv
aperture = CircularAperture((x, y), r=aperture_radius)
annulus = CircularAnnulus((x, y),
r_in=inner_sky_radius,
r_out=outer_sky_radius)
phot_table = aperture_photometry(data, [aperture, annulus])
#new background estimation
bkg_mask = np.ma.masked_outside(radial[0].reshape(new_image.shape),
inner_sky_radius, outer_sky_radius)
bkg_map = Background2D(new_image,
tuple(np.array(new_image.shape) / 4),
mask=bkg_mask.mask,
exclude_mesh_method='all')
bkg_map_med = MMMBackground().calc_background(
bkg_map.data) #bkg_map_med=np.median(bkg_map.background)
#print 'Map sky mean '+str(bkg_map_med)
#bkg_mean=phot_table['aperture_sum_1']/annulus.area()
#print 'Aperture sky mean '+str(bkg_mean)
#phot_table['residual_aperture_sum']=phot_table['aperture_sum_0']-bkg_mean*aperture.area()
phot_table['residual_aperture_sum'] = phot_table[
'aperture_sum_0'] - bkg_map_med * aperture.area()
#print 'Map sky result: '+str(phot_table['aperture_sum_0']-bkg_map_med*aperture.area())
#print "Aperture Photometry Result: "+str(phot_table['residual_aperture_sum'])
fig2 = Figure(figsize=(int(6 * scaling), int(6 * scaling)))
fig2.set_facecolor('0.85')
ax2 = fig2.add_axes([0.1, 0.1, .9, .9])
ax2.grid(True, color='white', linestyle='-', linewidth=1)
ax2.set_axisbelow(True)
ax2.scatter(radial[0], radial[1])
ax2.plot(np.linspace(0, new_image_halfwidth, num=50),
r'/Users/phystastical/Desktop/BB2/script/twomass-j.fits') as hdul:
image = hdul[0].data
bkgrms = MADStdBackgroundRMS()
std = bkgrms(image)
iraffind = IRAFStarFinder(threshold=3.5 * std,
fwhm=sigma_psf * gaussian_sigma_to_fwhm,
minsep_fwhm=0.01,
roundhi=5.0,
roundlo=-5.0,
sharplo=0.0,
sharphi=2.0)
daogroup = DAOGroup(2.0 * sigma_psf * gaussian_sigma_to_fwhm)
mmm_bkg = MMMBackground()
fitter = LevMarLSQFitter()
psf_model = IntegratedGaussianPRF(sigma=sigma_psf)
photometry = IterativelySubtractedPSFPhotometry(finder=iraffind,
group_maker=daogroup,
bkg_estimator=mmm_bkg,
psf_model=psf_model,
fitter=LevMarLSQFitter(),
niters=1,
fitshape=(11, 11))
result_tab = photometry(image=image)
residual_image = photometry.get_residual_image()
#Plot images made#
plt.subplot(1, 2, 1)
plt.imshow(image,
image = fits.getdata('./cutout_BS90_V.fits').astype(np.float64)
epsf_file = 'epsf.pkl'
if not os.path.exists(epsf_file):
mean, median, std = sigma_clipped_stats(image)
threshold = median + 10 * std
finder = IRAFStarFinder(threshold=threshold, fwhm=4, minsep_fwhm=5, peakmax=image.max() / 0.8)
star_table = finder(image)
star_table.rename_columns(('xcentroid', 'ycentroid'),('x','y'))
sigma_clip = SigmaClip(sigma=5.0)
bkg_estimator = MMMBackground()
bkg = Background2D(image, 5, filter_size=(3, 3),
sigma_clip=sigma_clip, bkg_estimator=bkg_estimator)
nddata = NDData(image-bkg.background)
stars = extract_stars(nddata, star_table, size=51)
epsf, fitted_stars = EPSFBuilder(oversampling=4, maxiters=3, progress_bar=True, smoothing_kernel='quadratic')(stars)
epsf_model = prepare_psf_model(epsf, renormalize_psf=False)
with open(epsf_file,'wb') as f:
pickle.dump([epsf_model, finder], f)
else:
with open(epsf_file, 'rb') as f:
epsf_model, finder = pickle.load(f)
def basic_psf_phot(target, centroided_sources, plots=False):
def hmsm_to_days(hour=0,min=0,sec=0,micro=0):
"""
Convert hours, minutes, seconds, and microseconds to fractional days.
"""
days = sec + (micro / 1.e6)
days = min + (days / 60.)
days = hour + (days / 60.)
return days / 24.
def date_to_jd(year,month,day):
"""
Convert a date to Julian Day.
Algorithm from 'Practical Astronomy with your Calculator or Spreadsheet',
4th ed., Duffet-Smith and Zwart, 2011.
"""
if month == 1 or month == 2:
yearp = year - 1
monthp = month + 12
else:
yearp = year
monthp = month
# this checks where we are in relation to October 15, 1582, the beginning
# of the Gregorian calendar.
if ((year < 1582) or
(year == 1582 and month < 10) or
(year == 1582 and month == 10 and day < 15)):
# before start of Gregorian calendar
B = 0
else:
# after start of Gregorian calendar
A = math.trunc(yearp / 100.)
B = 2 - A + math.trunc(A / 4.)
if yearp < 0:
C = math.trunc((365.25 * yearp) - 0.75)
else:
C = math.trunc(365.25 * yearp)
D = math.trunc(30.6001 * (monthp + 1))
jd = B + C + D + day + 1720994.5
return jd
def gaussian(p, x, y):
height, center_x, center_y, width_x, width_y, rotation = p
rotation = np.deg2rad(rotation)
x_0 = center_x * np.cos(rotation) - center_y * np.sin(rotation)
y_0 = center_x * np.sin(rotation) + center_y * np.cos(rotation)
def rotgauss(x,y):
xp = x * np.cos(rotation) - y * np.sin(rotation)
yp = x * np.sin(rotation) + y * np.cos(rotation)
g = height*np.exp(
-(((x_0-xp)/width_x)**2+
((y_0-yp)/width_y)**2)/2.)
return g
g = rotgauss(x,y)
return g
def moments(data):
total = np.nansum(data)
X, Y = np.indices(data.shape)
center_x = int(np.shape(data)[1]/2)
center_y = int(np.shape(data)[0]/2)
row = data[int(center_x), :]
col = data[:, int(center_y)]
width_x = np.nansum(np.sqrt(abs((np.arange(col.size)-center_y)**2*col))
/np.nansum(col))
width_y = np.nansum(np.sqrt(abs((np.arange(row.size)-center_x)**2*row))
/np.nansum(row))
height = np.nanmax(data)
rotation = 0.0
return height, center_x, center_y, width_x, width_y, rotation
def errorfunction(p, x, y, data):
return gaussian(p, x, y) - data
def fitgaussian(data):
params = moments(data)
X, Y = np.indices(data.shape)
mask = ~np.isnan(data)
x = X[mask]
y = Y[mask]
data = data[mask]
p, success = optimize.leastsq(errorfunction, params, args=(x, y, data))
return p
pines_path = pines_dir_check()
short_name = short_name_creator(target)
reduced_path = pines_path/('Objects/'+short_name+'/reduced/')
reduced_files = np.array(natsort.natsorted([x for x in reduced_path.glob('*.fits')]))
centroided_sources.columns = centroided_sources.columns.str.strip()
source_names = natsort.natsorted(list(set([i[0:-2].replace('X','').replace('Y','').rstrip().lstrip() for i in centroided_sources.keys()])))
#Declare a new dataframe to hold the information for all targets for this .
columns = ['Filename', 'Time UT', 'Time JD', 'Airmass', 'Seeing']
for i in range(0, len(source_names)):
columns.append(source_names[i]+' Flux')
columns.append(source_names[i]+' Flux Error')
psf_df = pd.DataFrame(index=range(len(reduced_files)), columns=columns)
output_filename = pines_path/('Objects/'+short_name+'/psf_phot/'+short_name+'_psf_phot.csv')
for i in range(len(reduced_files)):
#Read in image data/header.
file = reduced_files[i]
data = fits.open(file)[0].data
header = fits.open(file)[0].header
print('{}, image {} of {}.'.format(file.name, i+1, len(reduced_files)))
#Read in some supporting information.
log_path = pines_path/('Logs/'+file.name.split('.')[0]+'_log.txt')
log = pines_log_reader(log_path)
date_obs = header['DATE-OBS']
#Catch a case that can cause datetime strptime to crash; Mimir headers sometimes have DATE-OBS with seconds specified as 010.xx seconds, when it should be 10.xx seconds.
if len(date_obs.split(':')[-1].split('.')[0]) == 3:
date_obs = date_obs.split(':')[0] + ':' + date_obs.split(':')[1] + ':' + date_obs.split(':')[-1][1:]
#Keep a try/except clause here in case other unknown DATE-OBS formats pop up.
try:
date = datetime.datetime.strptime(date_obs, '%Y-%m-%dT%H:%M:%S.%f')
except:
print('Header DATE-OBS format does not match the format code in strptime! Inspect/correct the DATE-OBS value.')
pdb.set_trace()
days = date.day + hmsm_to_days(date.hour,date.minute,date.second,date.microsecond)
jd = date_to_jd(date.year,date.month,days)
psf_df['Filename'][i] = file.name
psf_df['Time UT'][i] = header['DATE-OBS']
psf_df['Time JD'][i] = jd
psf_df['Airmass'][i] = header['AIRMASS']
psf_df['Seeing'][i] = log['X seeing'][np.where(log['Filename'] == file.name.split('_')[0]+'.fits')[0][0]]
#Read in source centroids for this image
x = np.zeros(len(source_names))
y = np.zeros(len(source_names))
seeing = psf_df['Seeing'][i]
for j in range(len(source_names)):
source = source_names[j]
x[j] = centroided_sources[source+' X'][i]
y[j] = centroided_sources[source+' Y'][i]
#The extract_stars() function requires the input data as an NDData object.
nddata = NDData(data=data)
#Create table of good star positions
stars_tbl = Table()
stars_tbl['x'] = x
stars_tbl['y'] = y
size = 25
x, y = np.meshgrid(np.arange(0,size), np.arange(0,size))
#Extract star cutouts.
stars = extract_stars(nddata, stars_tbl, size=size)
fitter = fitting.LevMarLSQFitter()
fig, ax = plt.subplots(nrows=len(stars), ncols=3, sharex=True, sharey=True, figsize=(12,40))
#Fit a 2D Gaussian to each star.
for j in range(len(stars)):
star = stars[j]
source = source_names[j]
mmm_bkg = MMMBackground()
cutout = star.data - mmm_bkg(star.data)
#Get the star's centroid position in the cutout.
dtype = [('x_0', 'f8'), ('y_0', 'f8')]
pos = Table(data=np.zeros(1, dtype=dtype))
source_x = stars_tbl['x'][j]
source_y = stars_tbl['y'][j]
pos['x_0'] = source_x - int(source_x - size/2 + 1)
pos['y_0'] = source_y - int(source_y - size/2 + 1)
parameters = fitgaussian(cutout)
g2d_fit = gaussian(parameters, x, y)
avg, med, std = sigma_clipped_stats(cutout)
im = ax[j,0].imshow(cutout, origin='lower', vmin=med-std, vmax=med+8*std)
divider = make_axes_locatable(ax[j,0])
cax = divider.append_axes('right', size='5%', pad=0.05)
fig.colorbar(im, cax=cax, orientation='vertical')
ax[j,0].plot(pos['x_0'], pos['y_0'], 'rx')
ax[j,0].set_ylabel(source)
ax[j,0].text(pos['x_0'], pos['y_0']+1, '('+str(np.round(source_x,1))+', '+str(np.round(source_y,1))+')', color='r', ha='center')
ax[j,0].axis('off')
axins = ax[j,0].inset_axes([0.75, 0.75, 0.25, 0.25])
axins.set_yticklabels([])
axins.set_yticks([])
axins.set_xticklabels([])
axins.set_xticks([])
axins.imshow(data, origin='lower', vmin=med-std, vmax=med+8*std)
axins.plot(source_x, source_y, 'rx')
im = ax[j,1].imshow(g2d_fit, origin='lower', vmin=med-std, vmax=med+8*std)
divider = make_axes_locatable(ax[j,1])
cax = divider.append_axes('right', size='5%', pad=0.05)
fig.colorbar(im, cax=cax, orientation='vertical')
ax[j,1].axis('off')
avg, med, std = sigma_clipped_stats(cutout - g2d_fit)
im = ax[j,2].imshow(cutout - g2d_fit, origin='lower', vmin=med-std, vmax=med+8*std)
divider = make_axes_locatable(ax[j,2])
cax = divider.append_axes('right', size='5%', pad=0.05)
fig.colorbar(im, cax=cax, orientation='vertical')
ax[j,2].axis('off')
if j == 0:
ax[j,0].set_title('Data')
ax[j,1].set_title('2D Gaussian Model')
ax[j,2].set_title('Data - Model')
plt.tight_layout()
output_filename = pines_path/('Objects/'+short_name+'/basic_psf_phot/'+reduced_files[i].name.split('_')[0]+'_'+'source_modeling.pdf')
plt.savefig(output_filename)
plt.close()
return
def extractFlux(cnam, ccd, rccd, read, gain, ccdwin, rfile, store):
"""This extracts the flux of all apertures of a given CCD.
The steps are (1) creation of PSF model, (2) PSF fitting, (3)
flux extraction. The apertures are assumed to be correctly positioned.
It returns the results as a dictionary keyed on the aperture label. Each
entry returns a list:
[x, ex, y, ey, fwhm, efwhm, beta, ebeta, counts, countse, sky, esky,
nsky, nrej, flag]
flag = bitmask. See hipercam.core to see all the options which are
referred to by name in the code e.g. ALL_OK. The various flags can
signal that there no sky pixels (NO_SKY), the sky aperture was off
the edge of the window (SKY_AT_EDGE), etc.
This code::
>> bset = flag & TARGET_SATURATED
determines whether the data saturation flag is set for example.
Arguments::
cnam : string
CCD identifier label
ccd : CCD
the debiassed, flat-fielded CCD.
rccd : CCD
corresponding raw CCD, used to work out whether data are
saturated in target aperture.
read : CCD
readnoise divided by the flat-field
gain : CCD
gain multiplied by the flat field
ccdwin : dictionary of strings
the Window label corresponding to each Aperture
rfile : Rfile
reduce file configuration parameters
store : dict of dicts
see moveApers for what this contains.
"""
# initialise flag
flag = hcam.ALL_OK
ccdaper = rfile.aper[cnam]
results = {}
# get profile params from aperture store
mfwhm = store["mfwhm"]
mbeta = store["mbeta"]
method = "m" if mbeta > 0.0 else "g"
if mfwhm <= 0:
# die hard, die soon as there's nothing we can do.
print((" *** WARNING: CCD {:s}: no measured FWHM to create PSF model"
"; no extraction possible").format(cnam))
# set flag to indicate no FWHM
flag = hcam.NO_FWHM
for apnam, aper in ccdaper.items():
info = store[apnam]
results[apnam] = {
"x": aper.x,
"xe": info["xe"],
"y": aper.y,
"ye": info["ye"],
"fwhm": info["fwhm"],
"fwhme": info["fwhme"],
"beta": info["beta"],
"betae": info["betae"],
"counts": 0.0,
"countse": -1,
"sky": 0.0,
"skye": 0.0,
"nsky": 0,
"nrej": 0,
"flag": flag,
}
return results
# all apertures have to be in the same window, or we can't easily make a
# postage stamp of the data
wnames = set(ccdwin.values())
if len(wnames) != 1:
print((" *** WARNING: CCD {:s}: not all apertures"
" lie within the same window; no extraction possible"
).format(cnam))
# set flag to indicate no extraction
flag = hcam.NO_EXTRACTION
# return empty results
for apnam, aper in ccdaper.items():
info = store[apnam]
results[apnam] = {
"x": aper.x,
"xe": info["xe"],
"y": aper.y,
"ye": info["ye"],
"fwhm": info["fwhm"],
"fwhme": info["fwhme"],
"beta": info["beta"],
"betae": info["betae"],
"counts": 0.0,
"countse": -1,
"sky": 0.0,
"skye": 0.0,
"nsky": 0,
"nrej": 0,
"flag": flag,
}
return results
wnam = wnames.pop()
# PSF params are in binned pixels, so find binning
bin_fac = ccd[wnam].xbin
# create PSF model
if method == "m":
psf_model = MoffatPSF(beta=mbeta, fwhm=mfwhm / bin_fac)
else:
psf_model = IntegratedGaussianPRF(sigma=mfwhm *
gaussian_fwhm_to_sigma / bin_fac)
# force photometry only at aperture positions
# this means PSF shape and positions are fixed, we are only fitting flux
if rfile["psf_photom"]["positions"] == "fixed":
psf_model.x_0.fixed = True
psf_model.y_0.fixed = True
# create instances for PSF photometry
gfac = float(rfile["psf_photom"]["gfac"])
sclip = float(rfile["sky"]["thresh"])
daogroup = DAOGroup(gfac * mfwhm / bin_fac)
mmm_bkg = MMMBackground(sigma_clip=SigmaClip(sclip))
fitter = LevMarLSQFitter()
fitshape_box_size = int(2 * int(rfile["psf_photom"]["fit_half_width"]) + 1)
fitshape = (fitshape_box_size, fitshape_box_size)
photometry_task = BasicPSFPhotometry(
group_maker=daogroup,
bkg_estimator=mmm_bkg,
psf_model=psf_model,
fitter=fitter,
fitshape=fitshape,
)
# initialise flag
flag = hcam.ALL_OK
# extract Windows relevant for these apertures
wdata = ccd[wnam]
wraw = rccd[wnam]
# extract sub-windows that include all of the apertures, plus a little
# extra around the edges.
x1 = min([ap.x - ap.rsky2 - wdata.xbin for ap in ccdaper.values()])
x2 = max([ap.x + ap.rsky2 + wdata.xbin for ap in ccdaper.values()])
y1 = min([ap.y - ap.rsky2 - wdata.ybin for ap in ccdaper.values()])
y2 = max([ap.y + ap.rsky2 + wdata.ybin for ap in ccdaper.values()])
# extract sub-Windows
swdata = wdata.window(x1, x2, y1, y2)
swraw = wraw.window(x1, x2, y1, y2)
# compute pixel positions of apertures in windows
xpos, ypos = zip(*((swdata.x_pixel(ap.x), swdata.y_pixel(ap.y))
for ap in ccdaper.values()))
positions = Table(names=["x_0", "y_0"], data=(xpos, ypos))
# do the PSF photometry
photom_results = photometry_task(swdata.data, init_guesses=positions)
slevel = mmm_bkg(swdata.data)
# unpack the results and check apertures
for apnam, aper in ccdaper.items():
try:
# reset flag
flag = hcam.ALL_OK
result_row = photom_results[photom_results["id"] == int(apnam)]
if len(result_row) == 0:
flag |= hcam.NO_DATA
raise hcam.HipercamError(
"no source in PSF photometry for this aperture")
elif len(result_row) > 1:
flag |= hcam.NO_EXTRACTION
raise hcam.HipercamError(
"ambiguous lookup for this aperture in PSF photometry")
else:
result_row = result_row[0]
# compute X, Y arrays over the sub-window relative to the centre
# of the aperture and the distance squared from the centre (Rsq)
# to save a little effort.
x = swdata.x(np.arange(swdata.nx)) - aper.x
y = swdata.y(np.arange(swdata.ny)) - aper.y
X, Y = np.meshgrid(x, y)
Rsq = X**2 + Y**2
# size of a pixel which is used to taper pixels as they approach
# the edge of the aperture to reduce pixellation noise
size = np.sqrt(wdata.xbin * wdata.ybin)
# target selection, accounting for extra apertures and allowing
# pixels to contribute if their centres are as far as size/2 beyond
# the edge of the circle (but with a tapered weight)
dok = Rsq < (aper.rtarg + size / 2.0)**2
if not dok.any():
# check there are some valid pixels
flag |= hcam.NO_DATA
raise hcam.HipercamError("no valid pixels in aperture")
# check for saturation and nonlinearity
if cnam in rfile.warn:
if swraw.data[dok].max() >= rfile.warn[cnam]["saturation"]:
flag |= hcam.TARGET_SATURATED
if swraw.data[dok].max() >= rfile.warn[cnam]["nonlinear"]:
flag |= hcam.TARGET_NONLINEAR
else:
warnings.warn(
"CCD {:s} has no nonlinearity or saturation levels set")
counts = result_row["flux_fit"]
countse = result_row["flux_unc"]
info = store[apnam]
results[apnam] = {
"x": aper.x,
"xe": info["xe"],
"y": aper.y,
"ye": info["ye"],
"fwhm": info["fwhm"],
"fwhme": info["fwhme"],
"beta": info["beta"],
"betae": info["betae"],
"counts": counts,
"countse": countse,
"sky": slevel,
"skye": 0,
"nsky": 0,
"nrej": 0,
"flag": flag,
}
except hcam.HipercamError as err:
info = store[apnam]
flag |= hcam.NO_EXTRACTION
results[apnam] = {
"x": aper.x,
"xe": info["xe"],
"y": aper.y,
"ye": info["ye"],
"fwhm": info["fwhm"],
"fwhme": info["fwhme"],
"beta": info["beta"],
"betae": info["betae"],
"counts": 0.0,
"countse": -1,
"sky": 0.0,
"skye": 0.0,
"nsky": 0,
"nrej": 0,
"flag": flag,
}
# finally, we are done
return results
def Flux(self,x,y):
x = int(x)
y = int(y)
r = 25
data = self.hdulist[self.fz].data[x-r:x+r,y-r:y+r]
data = (lacosmic.lacosmic(data,2,10,10, effective_gain = self.gain, readnoise = self.readnoise))[0]
bkgrms = MADStdBackgroundRMS()
std = bkgrms(data)
iraffind = IRAFStarFinder(threshold=self.limit*std,
fwhm=self.sigma_psf*gaussian_sigma_to_fwhm,
minsep_fwhm=0.01, roundhi=5.0, roundlo=-5.0,
sharplo=0.0, sharphi=2.0)
daogroup = DAOGroup(2.0*self.sigma_psf*gaussian_sigma_to_fwhm)
mmm_bkg = MMMBackground()
psf_model = IntegratedGaussianPRF(sigma=self.sigma_psf)
from photutils.psf import IterativelySubtractedPSFPhotometry
photometry = IterativelySubtractedPSFPhotometry(finder=iraffind,
group_maker=daogroup,
bkg_estimator=mmm_bkg,
psf_model=psf_model,
fitter=LevMarLSQFitter(),
niters=1, fitshape=(21,21))
result_tab = photometry(image=data)
"""
if plot == 1:
residual_image = photometry.get_residual_image()
print(result_tab['x_fit','y_fit'])
plt.figure(self.filename+' data')
plt.imshow(data, cmap='viridis',
aspect=1, interpolation='nearest', origin='lower')
plt.show()
plt.figure(self.filename+' residual')
plt.imshow(residual_image, cmap='viridis',
aspect=1, interpolation='nearest', origin='lower')
plt.show()
plt.figure(self.filename+' PSF')
plt.imshow(data-residual_image, cmap='viridis',
aspect=1, interpolation='nearest', origin='lower')
plt.show()
"""
if len(result_tab) > 5:
return(0,0)
if len(result_tab) ==0:
print('None')
return(0,0)
result_tab['Minus'] = np.zeros(len(result_tab))
for i in range(len(result_tab)):
if 18.5 < result_tab['x_fit'][i] < 28.5 and 18.5 < result_tab['y_fit'][i] < 28.5:
#if 15 < result_tab['x_fit'][i] < 25 and 15 < result_tab['y_fit'][i] < 25:
result_tab['Minus'][i] = 1
else:
result_tab['Minus'][i] = 0
mask = result_tab['Minus'] == 1.0
result_tab = result_tab[mask]
if len(result_tab) != 1:
return(0,0)
flux_counts = float(result_tab['flux_fit'][0])
flux_unc = float(result_tab['flux_unc'][0])
flux_unc = flux_unc/flux_counts
return(flux_counts,flux_unc)
def run_iterative_PSF_photometry(setup,
reduction_metadata,
image_path,
log,
diagnostics=False):
"""Function to perform PSF-fitting photometry to all objects detected
in an image, using DAOphot-standard routines from photutils.
"""
iterate = False
log.info('Performing PSF-fitting photometry on ' +
os.path.basename(image_path))
image_data = fits.getdata(image_path)
psf_size = reduction_metadata.reduction_parameters[1]['PSF_SIZE'][0]
image_idx = reduction_metadata.images_stats[1]['IM_NAME'].tolist().index(
os.path.basename(image_path))
fwhm = reduction_metadata.images_stats[1]['FWHM_X'][image_idx]
log.info('Applying psf size = ' + str(psf_size))
log.info(' fwhm = ' + str(fwhm))
psf_radius = psf_size * fwhm
log.info(' psf size = ' + str(psf_radius))
star_finder = starfind.build_star_finder(reduction_metadata, image_path,
log)
daogroup = DAOGroup(2.0 * fwhm)
log.info(' -> Build star grouping object')
sigma_clip = SigmaClip(sigma=3.0)
mmm_bkg = MMMBackground(sigma_clip=sigma_clip)
log.info(' -> Build sky background model')
fitter = LevMarLSQFitter()
psf_model = IntegratedGaussianPRF(sigma=fwhm)
log.info(' -> Build PSF model')
psf_x = calc_psf_dimensions(psf_size, fwhm, log)
if iterate:
photometer = IterativelySubtractedPSFPhotometry(finder=star_finder,
group_maker=daogroup,
bkg_estimator=mmm_bkg,
psf_model=psf_model,
fitter=fitter,
niters=3,
fitshape=(psf_x,
psf_x))
else:
photometer = BasicPSFPhotometry(finder=star_finder,
group_maker=daogroup,
bkg_estimator=mmm_bkg,
psf_model=psf_model,
fitter=fitter,
fitshape=(psf_x, psf_x))
photometry = photometer(image=image_data)
print photometry.colnames
print photometry['flux_unc'].data
log.info('Photometry warnings, if any: ' +
repr(fitter.fit_info['message']))
log.info('Executed photometry of ' + str(len(photometry)) + ' stars')
if diagnostics:
store_residual_image(setup, photometer, image_path, log)
return photometry
def daophot(cnam, ccd, xlo, xhi, ylo, yhi, niters, method, fwhm, beta, gfac,
thresh, rejthresh):
"""
Perform iterative PSF photometry and star finding on region of CCD
"""
print(xlo, ylo, xhi, yhi)
# first check we are within a single window
wnam1 = ccd.inside(xlo, ylo, 2)
wnam2 = ccd.inside(xhi, yhi, 2)
if wnam1 != wnam2:
raise hcam.HipercamError(
'PSF photometry cannot currently be run across seperate windows')
wnam = wnam1
print(wnam)
# background stats from whole windpw
# estimate background RMS
wind = ccd[wnam]
rms_func = MADStdBackgroundRMS(sigma_clip=SigmaClip(sigma=rejthresh))
bkg_rms = rms_func(wind.data)
bkg_func = MMMBackground(sigma_clip=SigmaClip(sigma=rejthresh))
bkg = bkg_func(wind.data)
print(' Background estimate = {}, BKG RMS = {}'.format(bkg, bkg_rms))
# crop window to ROI
wind = ccd[wnam].window(xlo, xhi, ylo, yhi)
# correct FWHM for binning
fwhm /= wind.xbin
if method == 'm':
psf_model = MoffatPSF(fwhm, beta)
print(' FWHM = {:.1f}, BETA={:.1f}'.format(fwhm, beta))
else:
psf_model = IntegratedGaussianPRF(sigma=fwhm * gaussian_fwhm_to_sigma)
print(' FWHM = {:.1f}'.format(fwhm))
# region to extract around positions for fits
fitshape = int(5 * fwhm)
# ensure odd
if fitshape % 2 == 0:
fitshape += 1
photometry_task = DAOPhotPSFPhotometry(gfac * fwhm,
thresh * bkg_rms,
fwhm,
psf_model,
fitshape,
niters=niters,
sigma=rejthresh)
with warnings.catch_warnings():
warnings.simplefilter('ignore')
results = photometry_task(wind.data - bkg)
# filter out junk fits
tiny = 1e-30
bad_errs = (results['flux_unc'] < tiny) | (results['x_0_unc'] < tiny) | (
results['y_0_unc'] < tiny)
results = results[~bad_errs]
results.write('table_{}.fits'.format(cnam))
print(' found {} stars'.format(len(results)))
xlocs, ylocs = results['x_fit'], results['y_fit']
# convert to device coordinates
xlocs = wind.x(xlocs)
ylocs = wind.y(ylocs)
return xlocs, ylocs
def epsf_phot(target, centroided_sources, plots=False):
def hmsm_to_days(hour=0,min=0,sec=0,micro=0):
"""
Convert hours, minutes, seconds, and microseconds to fractional days.
"""
days = sec + (micro / 1.e6)
days = min + (days / 60.)
days = hour + (days / 60.)
return days / 24.
def date_to_jd(year,month,day):
"""
Convert a date to Julian Day.
Algorithm from 'Practical Astronomy with your Calculator or Spreadsheet',
4th ed., Duffet-Smith and Zwart, 2011.
"""
if month == 1 or month == 2:
yearp = year - 1
monthp = month + 12
else:
yearp = year
monthp = month
# this checks where we are in relation to October 15, 1582, the beginning
# of the Gregorian calendar.
if ((year < 1582) or
(year == 1582 and month < 10) or
(year == 1582 and month == 10 and day < 15)):
# before start of Gregorian calendar
B = 0
else:
# after start of Gregorian calendar
A = math.trunc(yearp / 100.)
B = 2 - A + math.trunc(A / 4.)
if yearp < 0:
C = math.trunc((365.25 * yearp) - 0.75)
else:
C = math.trunc(365.25 * yearp)
D = math.trunc(30.6001 * (monthp + 1))
jd = B + C + D + day + 1720994.5
return jd
pines_path = pines_dir_check()
short_name = short_name_creator(target)
reduced_path = pines_path/('Objects/'+short_name+'/reduced/')
reduced_filenames = natsort.natsorted([x.name for x in reduced_path.glob('*.fits')])
reduced_files = np.array([reduced_path/i for i in reduced_filenames])
centroided_sources.columns = centroided_sources.columns.str.strip()
source_names = natsort.natsorted(list(set([i.split(' ')[0]+' '+i.split(' ')[1] for i in centroided_sources.keys() if (i[0] == '2') or (i[0] == 'R')])))
#Create output plot directories for each source.
if plots:
for name in source_names:
#If the folders are already there, delete them.
source_path = (pines_path/('Objects/'+short_name+'/psf_phot/'+name+'/'))
if source_path.exists():
shutil.rmtree(source_path)
#Create folders.
os.mkdir(source_path)
#Declare a new dataframe to hold the information for all targets for this .
columns = ['Filename', 'Time UT', 'Time JD', 'Airmass', 'Seeing']
for i in range(0, len(source_names)):
columns.append(source_names[i]+' Flux')
columns.append(source_names[i]+' Flux Error')
psf_df = pd.DataFrame(index=range(len(reduced_files)), columns=columns)
output_filename = pines_path/('Objects/'+short_name+'/psf_phot/'+short_name+'_psf_phot.csv')
for i in range(0, len(reduced_files)):
#Read in image data/header.
file = reduced_files[i]
data = fits.open(file)[0].data
header = fits.open(file)[0].header
print('{}, image {} of {}.'.format(file.name, i+1, len(reduced_files)))
#Read in some supporting information.
log_path = pines_path/('Logs/'+file.name.split('.')[0]+'_log.txt')
log = pines_log_reader(log_path)
date_obs = header['DATE-OBS']
#Catch a case that can cause datetime strptime to crash; Mimir headers sometimes have DATE-OBS with seconds specified as 010.xx seconds, when it should be 10.xx seconds.
if len(date_obs.split(':')[-1].split('.')[0]) == 3:
date_obs = date_obs.split(':')[0] + ':' + date_obs.split(':')[1] + ':' + date_obs.split(':')[-1][1:]
#Keep a try/except clause here in case other unknown DATE-OBS formats pop up.
try:
date = datetime.datetime.strptime(date_obs, '%Y-%m-%dT%H:%M:%S.%f')
except:
print('Header DATE-OBS format does not match the format code in strptime! Inspect/correct the DATE-OBS value.')
pdb.set_trace()
days = date.day + hmsm_to_days(date.hour,date.minute,date.second,date.microsecond)
jd = date_to_jd(date.year,date.month,days)
psf_df['Filename'][i] = file.name
psf_df['Time UT'][i] = header['DATE-OBS']
psf_df['Time JD'][i] = jd
psf_df['Airmass'][i] = header['AIRMASS']
psf_df['Seeing'][i] = log['X seeing'][np.where(log['Filename'] == file.name.split('_')[0]+'.fits')[0][0]]
#Read in source centroids for this image
x = np.zeros(len(source_names))
y = np.zeros(len(source_names))
for j in range(len(source_names)):
source = source_names[j]
x[j] = centroided_sources[source+' X'][i]
y[j] = centroided_sources[source+' Y'][i]
#Extract pixel cutouts of our stars, so let’s explicitly exclude stars that are too close to the image boundaries (because they cannot be extracted).
size = 13
hsize = (size - 1) / 2
#mask = ((x > hsize) & (x < (data.shape[1] -1 - hsize)) & (y > hsize) & (y < (data.shape[0] -1 - hsize)) & (y > 100) & (y < 923))
#Create table of good star positions
stars_tbl = Table()
stars_tbl['x'] = x
stars_tbl['y'] = y
#Subtract background (star cutouts from which we build the ePSF must have background subtracted).
mean_val, median_val, std_val = sigma_clipped_stats(data, sigma=2.)
data -= median_val
#Replace nans in data using Gaussian.
# kernel = Gaussian2DKernel(x_stddev=0.5)
# data = interpolate_replace_nans(data, kernel)
#The extract_stars() function requires the input data as an NDData object.
nddata = NDData(data=data)
#Extract star cutouts.
stars = extract_stars(nddata, stars_tbl, size=size)
#Plot.
nrows = 5
ncols = 5
fig, ax = plt.subplots(nrows=nrows, ncols=ncols, figsize=(10, 10), squeeze=True)
ax = ax.ravel()
for j in range(len(stars)):
norm = simple_norm(stars[j], 'log', percent=99.)
ax[j].imshow(stars[j].data, norm=norm, origin='lower', cmap='viridis')
pdb.set_trace()
#Construct the ePSF using the star cutouts.
epsf_fitter = EPSFFitter()
epsf_builder = EPSFBuilder(maxiters=4, progress_bar=False, fitter=epsf_fitter)
try:
epsf, fitted_stars = epsf_builder(stars)
output_filename = pines_path/('Objects/'+short_name+'/psf_phot/'+short_name+'_psf_phot.csv')
for j in range(len(stars)):
star = stars[j]
source_name = source_names[j]
sigma_psf = 1.85
dtype = [('x_0', 'f8'), ('y_0', 'f8')]
pos = Table(data=np.zeros(1, dtype=dtype))
source_x = stars_tbl['x'][j]
source_y = stars_tbl['y'][j]
pos['x_0'] = source_x - int(source_x - size/2 + 1)
pos['y_0'] = source_y - int(source_y - size/2 + 1)
daogroup = DAOGroup(4.0*sigma_psf*gaussian_sigma_to_fwhm)
mmm_bkg = MMMBackground()
photometry = BasicPSFPhotometry(group_maker=daogroup,
bkg_estimator=mmm_bkg,
psf_model=epsf,
fitter=LevMarLSQFitter(),
fitshape=(13,13),
aperture_radius=4.)
result_tab = photometry(image=star, init_guesses=pos)
residual_image = photometry.get_residual_image()
psf_df[source_name+' Flux'][i] = result_tab['flux_fit'][0]
psf_df[source_name+' Flux Error'][i] = result_tab['flux_unc'][0]
if plots:
fig, ax = plt.subplots(nrows=1, ncols=3, figsize=(12,4))
im = ax[0].imshow(star, origin='lower')
divider = make_axes_locatable(ax[0])
cax = divider.append_axes('right', size='5%', pad=0.05)
fig.colorbar(im, cax=cax, orientation='vertical')
ax[0].plot(result_tab['x_fit'][0], result_tab['y_fit'][0], 'rx')
ax[0].set_title('Data')
im2 = ax[1].imshow(epsf.data, origin='lower')
ax[1].set_title('EPSF Model')
divider = make_axes_locatable(ax[1])
cax = divider.append_axes('right', size='5%', pad=0.05)
fig.colorbar(im2, cax=cax, orientation='vertical')
im3 = ax[2].imshow(residual_image, origin='lower')
ax[2].set_title('Residual Image')
divider = make_axes_locatable(ax[2])
cax = divider.append_axes('right', size='5%', pad=0.05)
fig.colorbar(im3, cax=cax, orientation='vertical')
plt.suptitle(source_name+'\n'+reduced_files[i].name+', image '+str(i+1)+' of '+str(len(reduced_files)))
plt.subplots_adjust(wspace=0.5, top=0.95, bottom = 0.05)
plot_output_name = pines_path/('Objects/'+short_name+'/psf_phot/'+source_name+'/'+str(i).zfill(4)+'.jpg')
plt.savefig(plot_output_name)
plt.close()
except:
print('')
print('EPSF BUILDER FAILED, SKIPPING IMAGE.')
print('')
#Plot the ePSF.
# plt.figure()
# norm = simple_norm(epsf.data, 'log', percent=99.)
# plt.imshow(epsf.data, norm=norm, origin='lower', cmap='viridis')
# cb = plt.colorbar()
# plt.tight_layout()
print('Saving psf photometry output to {}.'.format(output_filename))
with open(output_filename, 'w') as f:
for j in range(len(psf_df)):
if j == 0:
f.write('{:>21s}, {:>22s}, {:>17s}, {:>7s}, {:>7s}, '.format('Filename', 'Time UT', 'Time JD', 'Airmass', 'Seeing'))
for i in range(len(source_names)):
if i != len(source_names) - 1:
f.write('{:>20s}, {:>26s}, '.format(source_names[i]+' Flux', source_names[i]+' Flux Error'))
else:
f.write('{:>20s}, {:>26s}\n'.format(source_names[i]+' Flux', source_names[i]+' Flux Error'))
format_string = '{:21s}, {:22s}, {:17.9f}, {:7.2f}, {:7.1f}, '
#If the seeing value for this image is 'nan' (a string), convert it to a float.
#TODO: Not sure why it's being read in as a string, fix that.
if type(psf_df['Seeing'][j]) == str:
psf_df['Seeing'][j] = float(psf_df['Seeing'][j])
#Do a try/except clause for writeout, in case it breaks in the future.
try:
f.write(format_string.format(psf_df['Filename'][j], psf_df['Time UT'][j], psf_df['Time JD'][j], psf_df['Airmass'][j], psf_df['Seeing'][j]))
except:
print('Writeout failed! Inspect quantities you are trying to write out.')
pdb.set_trace()
for i in range(len(source_names)):
if i != len(source_names) - 1:
format_string = '{:20.11f}, {:26.11f}, '
else:
format_string = '{:20.11f}, {:26.11f}\n'
f.write(format_string.format(psf_df[source_names[i]+' Flux'][j], psf_df[source_names[i]+' Flux Error'][j]))
print('')
return
def jwst_camera_fpa_data(data_dir,
pattern,
standardized_data_dir,
parameters,
overwrite_source_extraction=False):
"""Generate standardized focal plane alignment (fpa) data
based on JWST camera image.
"""
save_plot = parameters['save_plot']
file_list = glob.glob(os.path.join(data_dir, '*{}'.format(pattern)))
if len(file_list) == 0:
raise RuntimeError('No data found')
file_list.sort()
for f in file_list:
plt.close('all')
print()
print('Data directory: {}'.format(data_dir))
print('Image being processed: {}'.format(f))
im = datamodels.open(f)
if hasattr(im, 'data') is False:
im.data = fits.getdata(f)
#im.dq = np.zeros(im.data.shape)
header_info = OrderedDict()
for attribute in 'telescope'.split():
header_info[attribute] = getattr(im.meta, attribute)
# observations
for attribute in 'date time visit_number visit_id visit_group activity_id program_number'.split(
):
header_info['observation_{}'.format(attribute)] = getattr(
im.meta.observation, attribute)
header_info['epoch_isot'] = '{}T{}'.format(
header_info['observation_date'], header_info['observation_time'])
# instrument
for attribute in 'name filter pupil detector'.split():
header_info['instrument_{}'.format(attribute)] = getattr(
im.meta.instrument, attribute)
# subarray
for attribute in 'name'.split():
header_info['subarray_{}'.format(attribute)] = getattr(
im.meta.subarray, attribute)
# aperture
for attribute in 'name position_angle pps_name'.split():
try:
value = getattr(im.meta.aperture, attribute)
except AttributeError:
value = None
header_info['aperture_{}'.format(attribute)] = value
header_info['INSTRUME'] = header_info['instrument_name']
header_info['SIAFAPER'] = header_info['aperture_name']
instrument_name = getattr(im.meta.instrument, 'name')
instrument_detector = getattr(im.meta.instrument, 'detector')
instrument_filter = getattr(im.meta.instrument, 'filter')
# temporary solution, this should come from populated aperture attributes
#if header_info['subarray_name'] == 'FULL':
# master_apertures = pysiaf.read.read_siaf_detector_layout()
# if header_info['instrument_name'].lower() in ['niriss', 'miri']:
# header_info['SIAFAPER'] = master_apertures['AperName'][np.where(master_apertures['InstrName']==header_info['instrument_name'])[0][0]]
# elif header_info['instrument_name'].lower() in ['fgs']:
# header_info['SIAFAPER'] = 'FGS{}_FULL'.format(header_info['instrument_detector'][-1])
# elif header_info['instrument_name'].lower() in ['nircam']:
# header_info['SIAFAPER'] = header_info['aperture_name']
#else:
# sys.exit('Only FULL arrays are currently supported.')
# target
for attribute in 'ra dec catalog_name proposer_name'.split():
header_info['target_{}'.format(attribute)] = getattr(
im.meta.target, attribute)
# pointing
for attribute in 'ra_v1 dec_v1 pa_v3'.split():
try:
value = getattr(im.meta.pointing, attribute)
except AttributeError:
value = None
header_info['pointing_{}'.format(attribute)] = value
# add HST style keywords
header_info['PROGRAM_VISIT'] = '{}_{}'.format(
header_info['observation_program_number'],
header_info['observation_visit_id'])
header_info['PROPOSID'] = header_info['observation_program_number']
header_info['DATE-OBS'] = header_info['observation_date']
header_info['TELESCOP'] = header_info['telescope']
header_info['INSTRUME'] = header_info['instrument_name']
try:
header_info['APERTURE'] = header_info['SIAFAPER']
except KeyError:
header_info['APERTURE'] = None
header_info['CHIP'] = 0
# TBD: Need to remove making yet another directory
#extracted_sources_dir = os.path.join(standardized_data_dir, 'extraction')
#if os.path.isdir(extracted_sources_dir) is False:
# os.makedirs(extracted_sources_dir)
extracted_sources_file = os.path.join(
standardized_data_dir, #extracted_sources_dir,
'{}_extracted_sources.fits'.format(
os.path.basename(f).split('.')[0]))
mask_extreme_slope_values = False
parameters['maximum_slope_value'] = 1000.
# Check if extracted_sources_file exists, or overwrite_source_extraction is set to True
if (not os.path.isfile(extracted_sources_file)) or (
overwrite_source_extraction):
data = copy.deepcopy(im.data)
#dq = copy.deepcopy(im.dq)
# Convert image data to counts per second
photmjsr = getattr(im.meta.photometry, 'conversion_megajanskys')
data_cps = data / photmjsr
if mask_extreme_slope_values:
# clean up extreme slope values
bad_index = np.where(
np.abs(data) > parameters['maximum_slope_value'])
data[bad_index] = 0.
dq[bad_index] = -1
bkgrms = MADStdBackgroundRMS()
mmm_bkg = MMMBackground()
bgrms = bkgrms(data_cps)
bgavg = mmm_bkg(data_cps)
# Default parameters that generally works for NIRCam/NIRISS images
sigma_factor = 10
round_lo, round_hi = 0.0, 0.6
sharp_lo, sharp_hi = 0.3, 1.4
fwhm_lo, fwhm_hi = 1.0, 20.0
fwhm = 2.0
minsep_fwhm = 7 # NOTE: minsep_fwhm>5 to reject artifacts around saturated stars
flux_percent_lo, flux_percent_hi = 10, 99
# if 'sharp_lo' in parameters:
# sharp_lo = parameters['sharp_lo']
###
### TBD1: Relocate params below to config parts/files
###
# Use different criteria for selecting good stars
if parameters['nominalpsf']:
# If using Nominal PSF models
if instrument_name == 'NIRISS':
#fwhm_lo, fwhm_hi = 1.0, 2.0
sharp_lo, sharp_hi = 0.6, 1.4
elif instrument_name == 'FGS':
#fwhm_lo, fwhm_hi = 1.0, 1.4
sharp_lo, sharp_hi = 0.6, 1.4
elif instrument_name == 'NIRCAM':
sharp_lo, sharp_hi = 0.6, 1.4
elif instrument_name == 'MIRI':
sharp_lo, sharp_hi = 0.8, 1.0
fwhm_lo, fwhm_hi = 1.5, 2.2
sigma_factor = 3
elif instrument_name == 'NIRSPEC':
sharp_lo, sharp_hi = 0.6, 0.8
round_lo, round_hi = 0.0, 0.3
fwhm_lo, fwhm_hi = 1.0, 1.75
else:
###
### For OTE commissioning, tweak the params below after finding
### the correct ranges by runnin the photometry notebook.
###
# If using Commissioning (non-phased) PSF models
if instrument_name == 'NIRISS':
sharp_lo, sharp_hi = 0.6, 1.4
fwhm_lo, fwhm_hi = 1.4, 2.4
################################################################################
################################################################################
################################################################################
elif instrument_name == 'FGS':
sigma_factor = 10
minsep_fwhm = 2.5
sharp_lo, sharp_hi = 0.45, 0.7
round_lo, round_hi = 0.0, 0.3
flux_percent_lo, flux_percent_hi = 2, 99
fwhm = 4
################################################################################
################################################################################
################################################################################
# Below works well for F200W and F356W images
elif instrument_name == 'NIRCAM':
sigma_factor = 3
minsep_fwhm = 2.5
sharp_lo, sharp_hi = 0.5, 0.7
round_lo, round_hi = 0.0, 0.2
flux_percent_lo, flux_percent_hi = 2, 99
if 'F200W' in instrument_filter:
fwhm = 10
elif 'F356W' in instrument_filter:
fwhm = 8
elif 'F090W' in instrument_filter:
fwhm = 5.5
elif 'F277W' in instrument_filter:
fwhm = 6.5
else:
fwhm = 3
################################################################################
################################################################################
################################################################################
elif instrument_name == 'MIRI':
sharl_lo, sharp_hi = 0.5, 1.0
fwhm_lo, fwhm_hi = 1.5, 2.2
sigma_factor = 3
elif instrument_name == 'NIRSPEC':
sharp_lo, sharp_hi = 0.5, 0.8
round_lo, round_hi = 0.0, 0.3
fwhm_lo, fwhm_hi = 1.0, 1.75
# Use IRAFStarFinder for source detection
iraffind = IRAFStarFinder(threshold=sigma_factor * bgrms + bgavg,
fwhm=fwhm,
minsep_fwhm=minsep_fwhm,
roundlo=round_lo,
roundhi=round_hi,
sharplo=sharp_lo,
sharphi=sharp_hi)
# Create default mask with all False values
datamask = np.zeros(
data_cps.shape,
dtype=bool) # This creates an array with all False
# Mask the left (for NRS1) and right regions (for NRS2) for NIRSpec
if instrument_detector == 'NRS1':
datamask[:, :1023] = True # Mask everything on the left side
elif instrument_detector == 'NRS2':
datamask[:, 1024:] = True # Mask everything on the right side
iraf_extracted_sources = iraffind(data_cps, mask=datamask)
# Perform some basic filtering
# Remove sources based on flux percentile
# 10-99% works well for filtering out too faint or saturated sources
flux_min = np.percentile(iraf_extracted_sources['flux'],
flux_percent_lo)
flux_max = np.percentile(iraf_extracted_sources['flux'],
flux_percent_hi)
iraf_extracted_sources.remove_rows(
np.where(iraf_extracted_sources['flux'] < flux_min))
iraf_extracted_sources.remove_rows(
np.where(iraf_extracted_sources['flux'] > flux_max))
# Also remove sources based on fwhm
###
### Don't use below for now - 2/23/2022 (Don't use it unless we get lots of bad sources)
###
#iraf_extracted_sources.remove_rows(np.where(iraf_extracted_sources['fwhm']<fwhm_lo))
#iraf_extracted_sources.remove_rows(np.where(iraf_extracted_sources['fwhm']>fwhm_hi))
# Now improve the positions by re-running centroiding algorithm if necessary.
# NOTE: For now, re-centroiding will be turned off
###
### TBD2: Add re-centroiding algorithm adopted from Paul here
###
#xarr = sources_masked['xcentroid']
#yarr = sources_masked['ycentroid']
#newx, newy = centroid_sources(data_cps, xarr, yarr, box_size=5, centroid_func=centroid_2dg)
#coords = np.column_stack((newx, newy))
#srcaper = CircularAnnulus(coords, r_in=1, r_out=3)
#srcaper_masks = srcaper.to_mask(method='center')
#satflag = np.zeros((len(newx),),dtype=int)
#i = 0
#for mask in srcaper_masks:
# srcaper_dq = mask.multiply(dqarr)
# srcaper_dq_1d = srcaper_dq[mask.data>0]
# badpix = np.logical_and(srcaper_dq_1d>2, srcaper_dq_1d<7)
# reallybad = np.where(srcaper_dq_1d==1)
# if ((len(srcaper_dq_1d[badpix]) > 1) or (len(srcaper_dq_1d[reallybad]) > 0)):
# satflag[i] = 1
# i =+1
#goodx = newx[np.where(satflag==0)]
#goody = newy[np.where(satflag==0)]
#print('Number of sources before removing saturated or bad pixels: ', len(xarr))
#print('Number of sources without saturated or bad pixels: ', len(goodx))
#print(' ')
#coords = np.column_stack((goodx,goody))
print('Number of extracted sources after filtering: {} sources'.
format(len(iraf_extracted_sources)))
if parameters['use_epsf'] is True:
size = 25
hsize = (size - 1) / 2
x = iraf_extracted_sources['xcentroid']
y = iraf_extracted_sources['ycentroid']
mask = ((x > hsize) & (x < (data_cps.shape[1] - 1 - hsize)) &
(y > hsize) & (y < (data_cps.shape[0] - 1 - hsize)))
stars_tbl = Table()
stars_tbl['x'] = x[mask]
stars_tbl['y'] = y[mask]
print('Using {} stars to build epsf'.format(len(stars_tbl)))
data_cps_bkgsub = data_cps.copy()
data_cps_bkgsub -= bgavg
nddata = NDData(data=data_cps_bkgsub)
stars = extract_stars(nddata, stars_tbl, size=size)
#
# Figure - PSF stars
#
nrows = 10
ncols = 10
fig, ax = plt.subplots(nrows=nrows,
ncols=ncols,
figsize=(20, 20),
squeeze=True)
ax = ax.ravel()
for i in range(nrows * ncols):
if i <= len(stars) - 1:
norm = simple_norm(stars[i], 'log', percent=99.)
ax[i].imshow(stars[i],
norm=norm,
origin='lower',
cmap='viridis')
plt.title('{} sample stars for epsf'.format(
header_info['APERTURE']))
if save_plot:
figname = os.path.join(
extracted_sources_dir, '{}_sample_psfs.pdf'.format(
os.path.basename(f).split('.')[0]))
plt.savefig(figname)
if parameters['show_extracted_sources']:
plt.show()
#
# Timer for ePSF construction
#
tic = time.perf_counter()
epsf_builder = EPSFBuilder(oversampling=4,
maxiters=3,
progress_bar=False)
print("Building ePSF ...")
epsf, fitted_stars = epsf_builder(stars)
toc = time.perf_counter()
print("Time elapsed for building ePSF:", toc - tic)
#
# Figure - ePSF plot
#
norm_epsf = simple_norm(epsf.data, 'log', percent=99.)
plt.figure()
plt.imshow(epsf.data,
norm=norm_epsf,
origin='lower',
cmap='viridis')
plt.colorbar()
plt.title('{} epsf using {} stars'.format(
header_info['APERTURE'], len(stars_tbl)))
if save_plot:
figname = os.path.join(
extracted_sources_dir, '{}_epsf.pdf'.format(
os.path.basename(f).split('.')[0]))
plt.savefig(figname)
if parameters['show_extracted_sources']:
plt.show()
daogroup = DAOGroup(5.0 * 2.0)
psf_model = epsf.copy()
tic = time.perf_counter()
photometry = IterativelySubtractedPSFPhotometry(
finder=iraffind,
group_maker=daogroup,
bkg_estimator=mmm_bkg,
psf_model=psf_model,
fitter=LevMarLSQFitter(),
niters=1,
fitshape=(11, 11),
aperture_radius=5)
print('Performing source extraction and photometry ...')
epsf_extracted_sources = photometry(data_cps)
toc = time.perf_counter()
print("Time elapsed for PSF photometry:", toc - tic)
print('Final source extraction with epsf: {} sources'.format(
len(epsf_extracted_sources)))
epsf_extracted_sources['xcentroid'] = epsf_extracted_sources[
'x_fit']
epsf_extracted_sources['ycentroid'] = epsf_extracted_sources[
'y_fit']
extracted_sources = epsf_extracted_sources
extracted_sources.write(extracted_sources_file, overwrite=True)
norm = simple_norm(data_cps, 'sqrt', percent=99.)
diff = photometry.get_residual_image()
plt.figure()
ax1 = plt.subplot(1, 2, 1)
plt.xlabel("X [pix]")
plt.ylabel("Y [pix]")
ax1.imshow(data_cps, norm=norm, cmap='Greys')
ax2 = plt.subplot(1, 2, 2)
plt.xlabel("X [pix]")
plt.ylabel("Y [pix]")
ax2.imshow(diff, norm=norm, cmap='Greys')
plt.title('PSF subtracted image for {}'.format(
os.path.basename(f)))
if save_plot:
figname = os.path.join(
extracted_sources_dir,
'{}_psfsubtracted_image.pdf'.format(
os.path.basename(f).split('.')[0]))
plt.savefig(figname)
if parameters['show_psfsubtracted_image']:
plt.show()
else:
extracted_sources = iraf_extracted_sources
extracted_sources.write(extracted_sources_file, overwrite=True)
positions = np.transpose((extracted_sources['xcentroid'],
extracted_sources['ycentroid']))
apertures = CircularAperture(positions, r=10)
norm = simple_norm(data_cps, 'sqrt', percent=99.)
plt.figure(figsize=(12, 12))
plt.xlabel("X [pix]")
plt.ylabel("Y [pix]")
plt.imshow(data_cps, norm=norm, cmap='Greys', origin='lower')
apertures.plot(color='blue', lw=1.5, alpha=0.5)
title_string = '{}: {} selected sources'.format(
os.path.basename(f), len(extracted_sources))
plt.title(title_string)
plt.tight_layout()
if save_plot:
figname = os.path.join(
standardized_data_dir, '{}_extracted_sources.pdf'.format(
os.path.basename(f).split('.')[0]))
plt.savefig(figname)
if parameters['show_extracted_sources']:
plt.show()
plt.close()
else:
extracted_sources = Table.read(extracted_sources_file)
print('Extracted {} sources from {}'.format(len(extracted_sources), f))
impose_positive_flux = True
if impose_positive_flux and parameters['use_epsf']:
extracted_sources.remove_rows(
np.where(extracted_sources['flux_fit'] < 0)[0])
print('Only {} sources have positve flux'.format(
len(extracted_sources)))
astrometry_uncertainty_mas = 5
if len(extracted_sources) > 0:
# Cal images are in DMS coordinates which correspond to the SIAF Science (SCI) frame
extracted_sources['x_SCI'], extracted_sources[
'y_SCI'] = extracted_sources['xcentroid'], extracted_sources[
'ycentroid']
# For now, astrometric uncertainty defaults to 5 mas for each source.
extracted_sources['sigma_x_mas'] = np.ones(
len(extracted_sources)) * astrometry_uncertainty_mas
extracted_sources['sigma_y_mas'] = np.ones(
len(extracted_sources)) * astrometry_uncertainty_mas
# transfer info to astropy table header
for key, value in header_info.items():
extracted_sources.meta[key] = value
extracted_sources.meta['DATAFILE'] = os.path.basename(f)
extracted_sources.meta['DATAPATH'] = os.path.dirname(f)
extracted_sources.meta['EPOCH'] = header_info['epoch_isot']
out_file = os.path.join(
standardized_data_dir, '{}_FPA_data.fits'.format(
extracted_sources.meta['DATAFILE'].split('.')[0]))
print('Writing {}'.format(out_file))
with warnings.catch_warnings():
warnings.simplefilter('ignore', AstropyWarning, append=True)
extracted_sources.write(out_file, overwrite=True)
return im
bkgrms = MADStdBackgroundRMS ()
std = bkgrms (imageSumBV)
# On donne les paramètres du finder pour déterminer les étoiles de base dans l'image
iraffind = IRAFStarFinder (threshold = 10 * std,
fwhm = fwhm,
minsep_fwhm = 0.01, roundhi = 1.0, roundlo = -1.0,
sharplo = 0.1, sharphi = 0.8)
# On donne un critère de groupage des étoiles
daogroup = DAOGroup (2.0 * fwhm)
# On détermine le fond de ciel et la procédure de fitting
mmm_bkg = MMMBackground ()
#fitter = LevMarLSQFitter ()
fitter = SLSQPLSQFitter ()
psf_model = IntegratedGaussianPRF (sigma = fwhm / 2.35)
# On met tout ça dans une boîte noire qui fait des itérations soustractives
photometry = IterativelySubtractedPSFPhotometry (finder = iraffind,
group_maker = daogroup,
bkg_estimator = mmm_bkg,
psf_model = psf_model,
fitter = LevMarLSQFitter (),
niters = 1, fitshape = (fshape, fshape))
# On exécute le tout et on extrait des résultats !
result_tabBV = photometry (image = imageSumBV)
residual_imageBV = photometry.get_residual_image ()
bkgrms = MADStdBackgroundRMS ()
std = bkgrms (imageSumBV)
# On donne les paramètres du finder pour déterminer les étoiles de base dans l'image
iraffind = IRAFStarFinder (threshold = 10 * std,
fwhm = fwhm,
minsep_fwhm = 0.01, roundhi = 1.0, roundlo = -1.0,
sharplo = 0.1, sharphi = 0.8)
# On donne un critère de groupage des étoiles
daogroup = DAOGroup (2.0 * fwhm)
# On détermine le fond de ciel et la procédure de fitting
mmm_bkg = MMMBackground ()
fitter = LevMarLSQFitter ()
psf_model = IntegratedGaussianPRF (sigma = fwhm / 2.35)
# On met tout ça dans une boîte noire qui fait des itérations soustractives
photometry = IterativelySubtractedPSFPhotometry (finder = iraffind,
group_maker = daogroup,
bkg_estimator = mmm_bkg,
psf_model = psf_model,
fitter = LevMarLSQFitter(),
niters = 1, fitshape = (2 * fwhm - 1, 2 * fwhm - 1))
# On exécute le tout et on extrait des résultats !
result_tabBV = photometry (image = imageSumBV)
residual_imageBV = photometry.get_residual_image ()
#result_tabBV.write ('result_tabBV.2.5s.dat', format = 'ascii')
def SubmitEvent(self):
#Not a fan of globals but this is the easiest way to grab the file location
global fileLocation
#sigma_psf = 2.88
#Grab the Sigma from the Entry box in the GUI
SigmaPSF = SigmaPSFentry.get()
#Turn the string into a float
sigma_psf = float(SigmaPSF)
#Grab the number of iterations from Entry box in GUI
N_iters1 = nitersEntry.get()
#Turn the string into a float
N_iters = float(N_iters1)
#Test cases to make sure that information was flowing from the GUI to the program
#print(SigmaPSF)
#print(N_iters)
#Open the file as a fits (allows us to handle it) then turn that into readable data.
with fits.open(fileLocation) as hdul:
image = hdul[0].data
#automatically gathered information needed to run the Star Finder
bkgrms = MADStdBackgroundRMS()
std = bkgrms(image)
#Find the stars
iraffind = IRAFStarFinder(threshold=3.5 * std,
fwhm=sigma_psf * gaussian_sigma_to_fwhm,
minsep_fwhm=0.01,
roundhi=5.0,
roundlo=-5.0,
sharplo=0.0,
sharphi=2.0)
#Group the stars
daogroup = DAOGroup(2.0 * sigma_psf * gaussian_sigma_to_fwhm)
#More automatically gathered info needed for IS-PSFPhotometry to take places
mmm_bkg = MMMBackground()
fitter = LevMarLSQFitter()
#Grabbed from the user input
psf_model = IntegratedGaussianPRF(sigma=sigma_psf)
#Run IS-PSFPhotometry
photometry = IterativelySubtractedPSFPhotometry(
finder=iraffind,
group_maker=daogroup,
bkg_estimator=mmm_bkg,
psf_model=psf_model,
fitter=LevMarLSQFitter(),
niters=N_iters,
fitshape=(11, 11))
#Do photometry on the image
result_tab = photometry(image=image)
#grab the resiudal image
residual_image = photometry.get_residual_image()
#Get the results of the photometry and print the aspects we want.
phot_results = photometry(image)
with open("output.txt", "w") as text_file:
print(phot_results['x_fit', 'y_fit', 'flux_fit'],
file=text_file)
print(phot_results['x_fit', 'y_fit', 'flux_fit'])
print("Sum of pixels: {}".format(sum(sum(residual_image))))
#Plot images made#
#Start by creating plots.
plt.subplot(1, 5, 1)
#Show the first plot (which is just the raw image)
plt.imshow(image,
cmap='viridis',
aspect=1,
interpolation='nearest',
origin='lower')
plt.title('Raw')
plt.colorbar(orientation='horizontal', fraction=0.046, pad=0.04)
#Create the second plot
plt.subplot(1, 5, 2)
#Show the residual_image
plt.imshow(residual_image,
cmap='viridis',
aspect=1,
interpolation='nearest',
origin='lower')
plt.title('PSF')
plt.colorbar(orientation='horizontal', fraction=0.046, pad=0.04)
#Draw in the sum of pixels.
plt.text(0,
65,
"Sum of pixels: {}".format(sum(sum(residual_image))),
fontsize=7)
#Create the third plot which is the subtracted images combined.
sb = image - residual_image
plt.subplot(1, 5, 3)
plt.imshow(sb,
cmap='viridis',
aspect=1,
interpolation='nearest',
origin='lower')
plt.title('PSF-S')
plt.colorbar(orientation='horizontal', fraction=0.046, pad=0.04)
with open("AP_RI.txt", "w") as f:
for _ in range(len(residual_image)):
f.write(str(residual_image[_]))
with open("AP_BS.txt", "w") as f:
for _ in range(len(sb)):
f.write(str(sb[_]))
print("Starting creation of CSV")
subprocess.run(['py', 'create_CSV.py'], shell=False)
print("Starting creation of Stats")
subprocess.run(['py', 'create_info.py'], shell=False)
print("Starting Threshold")
subprocess.run(['py', 'threshold.py'], shell=False)
with open("APC_Res.csv", "r") as f:
APC_Res = f.read()
APC_Res = APC_Res.split(",")
APC_Res = [float(i) for i in APC_Res]
#Every (SquareRoot of the Pixels) datapoints create a new array. Into a 2D Array.
#I'm going to use the Correct_Res list as the main list and store the temp list every Sqrt(pix) in it,
#then reset that list and continue until the pixel count is met.
#Have an internal counter. Reset that every Sqrt(Pix)
temp_list = np.array([])
SqrPixels = math.sqrt(len(APC_Res))
internal_counter = 0
#print(SqrPixels)
#print(len(APC_Res))
Corrected_Res = np.array([[]])
for _ in range(len(APC_Res)):
if internal_counter <= SqrPixels - 2:
try:
temp_list = np.append(temp_list, APC_Res[_ - 1])
#print(_)
if _ + 1 == (int(SqrPixels) * int(SqrPixels)):
Corrected_Res = np.append(Corrected_Res, temp_list)
except:
print("Not right 2.0")
internal_counter = internal_counter + 1
else:
internal_counter = 0
#print(temp_list)
Corrected_Res = np.append(Corrected_Res, temp_list)
temp_list = []
temp_list = np.append(temp_list, APC_Res[_ - 1])
#print("Resetting Counter & List {}".format(_))
if _ + 1 == (int(SqrPixels) * int(SqrPixels)):
Corrected_Res = np.append(Corrected_Res, temp_list)
#print(_+1)
#print("Iteration {}".format(_))
#print(residual_image)
#print("\n")
#print(Corrected_Res)
Corrected_Res = np.reshape(Corrected_Res,
(int(SqrPixels), int(SqrPixels)))
Correct_BS = image - Corrected_Res
plt.subplot(1, 5, 4)
plt.imshow(Corrected_Res,
cmap='viridis',
aspect=1,
interpolation='nearest',
origin='lower')
plt.title('CPSF')
plt.colorbar(orientation='horizontal', fraction=0.046, pad=0.04)
plt.subplot(1, 5, 5)
plt.imshow(Correct_BS,
cmap='viridis',
aspect=1,
interpolation='nearest',
origin='lower')
plt.title('CPSF-S')
plt.colorbar(orientation='horizontal', fraction=0.046, pad=0.04)
#Number of bins
n_bins = 20
#Not super sure why this works the way that it does if I’m being truthful, took tinkering to work, and lots of documentation examples.
fig, axs = plt.subplots(1, 2)
# We can set the number of bins with the `bins` kwarg
axs[0].hist(residual_image, bins=n_bins)
plt.title('Residual Image Hist')
axs[1].hist(sb, bins=n_bins)
plt.title('Background Subtracted Hist')
#plt.colorbar(orientation='horizontal', fraction=0.046, pad=0.04)
#All Pixels from residual image
fig = plt.figure()
ax = fig.add_subplot(111, projection='3d')
delta = (6 * (1 / len(sb)))
nx = ny = np.arange(-3.0, 3.0, delta)
X, Y = np.meshgrid(nx, ny)
#print(X)
#print(Y)
x, y, z = X * len(sb), Y * len(sb), sb
ax.plot_surface(x, y, z, rstride=1, cstride=1, cmap='viridis')
figi = plt.figure()
axi = figi.add_subplot(111, projection='3d')
deltai = (6 * (1 / len(sb)))
nxi = nyi = np.arange(-3.0, 3.0, deltai)
Xi, Yi = np.meshgrid(nxi, nyi)
#print(X)
#print(Y)
xi, yi, zi = Xi * len(Correct_BS), Yi * len(Correct_BS), Correct_BS
axi.plot_surface(xi, yi, zi, rstride=1, cstride=1, cmap='viridis')
plt.show()