from __future__ import print_function
import numpy as np
import pylab as plt
import time
from astrometry.util.ttime import Time, CpuMeas
from astrometry.util.resample import resample_with_wcs, OverlapError
from astrometry.util.fits import fits_table
from astrometry.util.plotutils import dimshow
from tractor import Tractor, PointSource, Image, NanoMaggies, Catalog, Patch
from tractor.galaxy import DevGalaxy, ExpGalaxy, FixedCompositeGalaxy, SoftenedFracDev, FracDev, disable_galaxy_cache, enable_galaxy_cache
from tractor.patch import ModelMask
from legacypipe.survey import (SimpleGalaxy, RexGalaxy, GaiaSource,
LegacyEllipseWithPriors, get_rgb, IN_BLOB)
from legacypipe.runbrick import rgbkwargs, rgbkwargs_resid
from legacypipe.coadds import quick_coadds
from legacypipe.runbrick_plots import _plot_mods
[docs]def one_blob(X):
'''
Fits sources contained within a "blob" of pixels.
'''
if X is None:
return None
(nblob, iblob, Isrcs, brickwcs, bx0, by0, blobw, blobh, blobmask, timargs,
srcs, bands, plots, ps, simul_opt, use_ceres, rex, refs) = X
print('Fitting blob number', nblob, 'val', iblob, ':', len(Isrcs),
'sources, size', blobw, 'x', blobh, len(timargs), 'images')
if len(timargs) == 0:
return None
hasbright = refs is not None and np.any(refs.isbright)
hasmedium = refs is not None and np.any(refs.ismedium)
if plots:
plt.figure(2, figsize=(3,3))
plt.subplots_adjust(left=0.01, right=0.99, bottom=0.01, top=0.99)
plt.figure(1)
t0 = time.clock()
# A local WCS for this blob
blobwcs = brickwcs.get_subimage(bx0, by0, blobw, blobh)
# Per-source measurements for this blob
B = fits_table()
B.sources = srcs
B.Isrcs = Isrcs
B.iblob = iblob
B.blob_x0 = np.zeros(len(B), np.int16) + bx0
B.blob_y0 = np.zeros(len(B), np.int16) + by0
# Did sources start within the blob?
ok,x0,y0 = blobwcs.radec2pixelxy(
np.array([src.getPosition().ra for src in srcs]),
np.array([src.getPosition().dec for src in srcs]))
B.started_in_blob = blobmask[
np.clip(np.round(y0-1).astype(int), 0,blobh-1),
np.clip(np.round(x0-1).astype(int), 0,blobw-1)]
B.cpu_source = np.zeros(len(B), np.float32)
B.blob_width = np.zeros(len(B), np.int16) + blobw
B.blob_height = np.zeros(len(B), np.int16) + blobh
B.blob_npix = np.zeros(len(B), np.int32) + np.sum(blobmask)
B.blob_nimages= np.zeros(len(B), np.int16) + len(timargs)
B.blob_symm_width = np.zeros(len(B), np.int16)
B.blob_symm_height = np.zeros(len(B), np.int16)
B.blob_symm_npix = np.zeros(len(B), np.int32)
B.blob_symm_nimages = np.zeros(len(B), np.int16)
B.hit_limit = np.zeros(len(B), bool)
ob = OneBlob('%i'%(nblob+1), blobwcs, blobmask, timargs, srcs, bands,
plots, ps, simul_opt, use_ceres, hasbright, hasmedium, rex)
ob.run(B)
B.blob_totalpix = np.zeros(len(B), np.int32) + ob.total_pix
ok,x1,y1 = blobwcs.radec2pixelxy(
np.array([src.getPosition().ra for src in B.sources]),
np.array([src.getPosition().dec for src in B.sources]))
B.finished_in_blob = blobmask[
np.clip(np.round(y1-1).astype(int), 0, blobh-1),
np.clip(np.round(x1-1).astype(int), 0, blobw-1)]
assert(len(B.finished_in_blob) == len(B))
assert(len(B.finished_in_blob) == len(B.started_in_blob))
B.brightblob = np.zeros(len(B), np.int16)
if hasbright:
B.brightblob += IN_BLOB['BRIGHT']
if hasmedium:
B.brightblob += IN_BLOB['MEDIUM']
if refs is not None and 'iscluster' in refs.get_columns() and np.any(refs.iscluster):
B.brightblob += IN_BLOB['CLUSTER']
B.cpu_blob = np.zeros(len(B), np.float32)
t1 = time.clock()
B.cpu_blob[:] = t1 - t0
return B
class OneBlob(object):
def __init__(self, name, blobwcs, blobmask, timargs, srcs, bands,
plots, ps, simul_opt, use_ceres, hasbright, hasmedium, rex):
self.name = name
self.rex = rex
self.blobwcs = blobwcs
self.pixscale = self.blobwcs.pixel_scale()
self.blobmask = blobmask
self.srcs = srcs
self.bands = bands
self.plots = plots
self.plots_per_source = plots
self.plots_per_model = False
# blob-1-data.png, etc
self.plots_single = False
self.ps = ps
self.simul_opt = simul_opt
self.use_ceres = use_ceres
self.hasbright = hasbright
self.hasmedium = hasmedium
self.tims = self.create_tims(timargs)
self.total_pix = sum([np.sum(t.getInvError() > 0) for t in self.tims])
self.plots2 = False
alphas = [0.1, 0.3, 1.0]
self.optargs = dict(priors=True, shared_params=False, alphas=alphas,
print_progress=True)
self.blobh,self.blobw = blobmask.shape
self.bigblob = (self.blobw * self.blobh) > 100*100
if self.bigblob:
print('Big blob:', name)
self.trargs = dict()
# if use_ceres:
# from tractor.ceres_optimizer import CeresOptimizer
# ceres_optimizer = CeresOptimizer()
# self.optargs.update(scale_columns=False,
# scaled=False,
# dynamic_scale=False)
# self.trargs.update(optimizer=ceres_optimizer)
# else:
# self.optargs.update(dchisq = 0.1)
from legacypipe.constrained_optimizer import ConstrainedOptimizer
self.trargs.update(optimizer=ConstrainedOptimizer())
self.optargs.update(dchisq = 0.1)
def run(self, B):
# Not quite so many plots...
self.plots1 = self.plots
cat = Catalog(*self.srcs)
tlast = Time()
if self.plots:
self._initial_plots()
if not self.bigblob:
print('Fitting just fluxes using initial models...')
self._fit_fluxes(cat, self.tims, self.bands)
tr = self.tractor(self.tims, cat)
if self.plots:
self._plots(tr, 'Initial models')
# Optimize individual sources, in order of flux.
# First, choose the ordering...
Ibright = _argsort_by_brightness(cat, self.bands)
if len(cat) > 1:
self._optimize_individual_sources_subtract(
cat, Ibright, B.cpu_source)
else:
self._optimize_individual_sources(tr, cat, Ibright, B.cpu_source)
# Optimize all at once?
if len(cat) > 1 and len(cat) <= 10:
#tfit = Time()
cat.thawAllParams()
tr.optimize_loop(**self.optargs)
if self.plots:
self._plots(tr, 'After source fitting')
plt.clf()
self._plot_coadd(self.tims, self.blobwcs, model=tr)
plt.title('After source fitting')
self.ps.savefig()
if self.plots_single:
plt.figure(2)
mods = list(tr.getModelImages())
coimgs,cons = quick_coadds(self.tims, self.bands, self.blobwcs, images=mods,
fill_holes=False)
dimshow(get_rgb(coimgs,self.bands), ticks=False)
plt.savefig('blob-%s-initmodel.png' % (self.name))
res = [(tim.getImage() - mod) for tim,mod in zip(self.tims, mods)]
coresids,nil = quick_coadds(self.tims, self.bands, self.blobwcs, images=res)
dimshow(get_rgb(coresids, self.bands, **rgbkwargs_resid), ticks=False)
plt.savefig('blob-%s-initresid.png' % (self.name))
dimshow(get_rgb(coresids, self.bands), ticks=False)
plt.savefig('blob-%s-initsub.png' % (self.name))
plt.figure(1)
print('Blob', self.name, 'finished initial fitting:', Time()-tlast)
tlast = Time()
# Next, model selections: point source vs dev/exp vs composite.
self.run_model_selection(cat, Ibright, B)
print('Blob', self.name, 'finished model selection:', Time()-tlast)
tlast = Time()
if self.plots:
self._plots(tr, 'After model selection')
if self.plots_single:
plt.figure(2)
mods = list(tr.getModelImages())
coimgs,cons = quick_coadds(self.tims, self.bands, self.blobwcs, images=mods,
fill_holes=False)
dimshow(get_rgb(coimgs,self.bands), ticks=False)
plt.savefig('blob-%s-model.png' % (self.name))
res = [(tim.getImage() - mod) for tim,mod in zip(self.tims, mods)]
coresids,nil = quick_coadds(self.tims, self.bands, self.blobwcs, images=res)
dimshow(get_rgb(coresids, self.bands, **rgbkwargs_resid), ticks=False)
plt.savefig('blob-%s-resid.png' % (self.name))
plt.figure(1)
# Cut down to just the kept sources
I = np.array([i for i,s in enumerate(cat) if s is not None])
B.cut(I)
cat = Catalog(*B.sources)
tr.catalog = cat
# Do another quick round of flux-only fitting?
# This does horribly -- fluffy galaxies go out of control because
# they're only constrained by pixels within this blob.
#_fit_fluxes(cat, tims, bands, use_ceres, alphas)
# ### Simultaneous re-opt?
# if simul_opt and len(cat) > 1 and len(cat) <= 10:
# #tfit = Time()
# cat.thawAllParams()
# #print('Optimizing:', tr)
# #tr.printThawedParams()
# max_cpu = 300.
# cpu0 = time.clock()
# for step in range(50):
# dlnp,X,alpha = tr.optimize(**optargs)
# cpu = time.clock()
# if cpu-cpu0 > max_cpu:
# print('Warning: Exceeded maximum CPU time for source')
# break
# if dlnp < 0.1:
# break
# #print('Simultaneous fit took:', Time()-tfit)
# Compute variances on all parameters for the kept model
B.srcinvvars = [None for i in range(len(B))]
cat.thawAllRecursive()
cat.freezeAllParams()
for isub in range(len(B.sources)):
cat.thawParam(isub)
src = cat[isub]
if src is None:
cat.freezeParam(isub)
continue
# Convert to "vanilla" ellipse parameterization
nsrcparams = src.numberOfParams()
_convert_ellipses(src)
assert(src.numberOfParams() == nsrcparams)
# print('Computing variances for source', src, ': N params:', nsrcparams)
# print('Source params:')
# src.printThawedParams()
# For Gaia sources, temporarily convert the GaiaPosition to a
# RaDecPos in order to compute the invvar it would have in our
# imaging? Or just plug in the Gaia-measured uncertainties??
# (going to implement the latter)
# Compute inverse-variances
allderivs = tr.getDerivs()
ivars = _compute_invvars(allderivs)
assert(len(ivars) == nsrcparams)
#print('Inverse-variances:', ivars)
B.srcinvvars[isub] = ivars
assert(len(B.srcinvvars[isub]) == cat[isub].numberOfParams())
cat.freezeParam(isub)
# Check for sources with zero inverse-variance -- I think these
# can be generated during the "Simultaneous re-opt" stage above --
# sources can get scattered outside the blob.
I, = np.nonzero([np.sum(iv) > 0 for iv in B.srcinvvars])
if len(I) < len(B):
print('Keeping', len(I), 'of', len(B),'sources with non-zero ivar')
B.cut(I)
cat = Catalog(*B.sources)
tr.catalog = cat
M = _compute_source_metrics(B.sources, self.tims, self.bands, tr)
for k,v in M.items():
B.set(k, v)
print('Blob', self.name, 'finished:', Time()-tlast)
def run_model_selection(self, cat, Ibright, B):
# We compute & subtract initial models for the other sources while
# fitting each source:
# -Remember the original images
# -Compute initial models for each source (in each tim)
# -Subtract initial models from images
# -During fitting, for each source:
# -add back in the source's initial model (to each tim)
# -fit, with Catalog([src])
# -subtract final model (from each tim)
# -Replace original images
models = SourceModels()
# Remember original tim images
models.save_images(self.tims)
# Create initial models for each tim x each source
models.create(self.tims, cat, subtract=True)
N = len(cat)
B.dchisq = np.zeros((N, 5), np.float32)
B.all_models = np.array([{} for i in range(N)])
B.all_model_ivs = np.array([{} for i in range(N)])
B.all_model_cpu = np.array([{} for i in range(N)])
B.all_model_hit_limit = np.array([{} for i in range(N)])
# Model selection for sources, in decreasing order of brightness
for numi,srci in enumerate(Ibright):
src = cat[srci]
print('Model selection for source %i of %i in blob %s; sourcei %i' %
(numi+1, len(Ibright), self.name, srci))
cpu0 = time.clock()
# Add this source's initial model back in.
models.add(srci, self.tims)
if self.plots_single:
plt.figure(2)
tr = self.tractor(self.tims, cat)
coimgs,cons = quick_coadds(self.tims, self.bands, self.blobwcs,
fill_holes=False)
rgb = get_rgb(coimgs,self.bands)
plt.imsave('blob-%s-%s-bdata.png' % (self.name, srci), rgb,
origin='lower')
plt.figure(1)
keepsrc = self.model_selection_one_source(src, srci, models, B)
B.sources[srci] = keepsrc
cat[srci] = keepsrc
# Re-remove the final fit model for this source.
models.update_and_subtract(srci, keepsrc, self.tims)
if self.plots_single:
plt.figure(2)
tr = self.tractor(self.tims, cat)
coimgs,cons = quick_coadds(self.tims, self.bands, self.blobwcs,
fill_holes=False)
dimshow(get_rgb(coimgs,self.bands), ticks=False)
plt.savefig('blob-%s-%i-sub.png' % (self.name, srci))
plt.figure(1)
cpu1 = time.clock()
B.cpu_source[srci] += (cpu1 - cpu0)
models.restore_images(self.tims)
del models
def model_selection_one_source(self, src, srci, models, B):
# Fit local constant sky background levels if we're in the
# same blob as a medium-brightness star.
fit_background = self.hasmedium
if self.bigblob:
mods = [mod[srci] for mod in models.models]
srctims,modelMasks = _get_subimages(self.tims, mods, src)
# Create a little local WCS subregion for this source, by
# resampling non-zero inverrs from the srctims into blobwcs
insrc = np.zeros((self.blobh,self.blobw), bool)
for tim in srctims:
try:
Yo,Xo,Yi,Xi,nil = resample_with_wcs(
self.blobwcs, tim.subwcs, [],2)
except:
continue
insrc[Yo,Xo] |= (tim.inverr[Yi,Xi] > 0)
if np.sum(insrc) == 0:
# No source pixels touching blob... this can
# happen when a source scatters outside the blob
# in the fitting stage. Drop the source here.
return None
yin = np.max(insrc, axis=1)
xin = np.max(insrc, axis=0)
yl,yh = np.flatnonzero(yin)[np.array([0,-1])]
xl,xh = np.flatnonzero(xin)[np.array([0,-1])]
del insrc
srcwcs = self.blobwcs.get_subimage(xl, yl, 1+xh-xl, 1+yh-yl)
srcwcs_x0y0 = (xl, yl)
# A mask for which pixels in the 'srcwcs' square are occupied.
srcblobmask = self.blobmask[yl:yh+1, xl:xh+1]
else:
modelMasks = models.model_masks(srci, src)
srctims = self.tims
srcwcs = self.blobwcs
srcwcs_x0y0 = (0, 0)
srcblobmask = self.blobmask
if self.plots_per_source:
# This is a handy blob-coordinates plot of the data
# going into the fit.
plt.clf()
nil,nil,coimgs,nil = quick_coadds(srctims, self.bands,self.blobwcs,
fill_holes=False, get_cow=True)
dimshow(get_rgb(coimgs, self.bands))
ax = plt.axis()
pos = src.getPosition()
ok,x,y = self.blobwcs.radec2pixelxy(pos.ra, pos.dec)
ix,iy = int(np.round(x-1)), int(np.round(y-1))
plt.plot(x-1, y-1, 'r+')
plt.axis(ax)
plt.title('Model selection: stage1 data')
self.ps.savefig()
# Mask out other sources while fitting this one, by
# finding symmetrized blobs of significant pixels
mask_others = True
if mask_others:
from legacypipe.detection import detection_maps
from astrometry.util.multiproc import multiproc
from scipy.ndimage.morphology import binary_dilation
from scipy.ndimage.measurements import label, find_objects
# Compute per-band detection maps
mp = multiproc()
detmaps,detivs,satmaps = detection_maps(
srctims, srcwcs, self.bands, mp)
# Compute the symmetric area that fits in this 'tim'
pos = src.getPosition()
ok,xx,yy = srcwcs.radec2pixelxy(pos.ra, pos.dec)
bh,bw = srcblobmask.shape
ix = int(np.clip(np.round(xx-1), 0, bw-1))
iy = int(np.clip(np.round(yy-1), 0, bh-1))
flipw = min(ix, bw-1-ix)
fliph = min(iy, bh-1-iy)
flipblobs = np.zeros(srcblobmask.shape, bool)
# Go through the per-band detection maps, marking significant pixels
for i,(detmap,detiv) in enumerate(zip(detmaps,detivs)):
sn = detmap * np.sqrt(detiv)
slc = (slice(iy-fliph, iy+fliph+1),
slice(ix-flipw, ix+flipw+1))
flipsn = np.zeros_like(sn)
# Symmetrize
flipsn[slc] = np.minimum(sn[slc],
np.flipud(np.fliplr(sn[slc])))
# just OR the detection maps per-band...
flipblobs |= (flipsn > 5.)
blobs,nb = label(flipblobs)
goodblob = blobs[iy,ix]
if goodblob != 0:
flipblobs = (blobs == goodblob)
dilated = binary_dilation(flipblobs, iterations=4)
if not np.any(dilated):
print('No pixels in dilated symmetric mask')
return None
yin = np.max(dilated, axis=1)
xin = np.max(dilated, axis=0)
yl,yh = np.flatnonzero(yin)[np.array([0,-1])]
xl,xh = np.flatnonzero(xin)[np.array([0,-1])]
#print('Dilated: good bounds x', xl,xh, 'y', yl,yh)
#oldshape = srcwcs.shape
(oldx0,oldy0) = srcwcs_x0y0
srcwcs = srcwcs.get_subimage(xl, yl, 1+xh-xl, 1+yh-yl)
srcwcs_x0y0 = (oldx0 + xl, oldy0 + yl)
srcblobmask = srcblobmask[yl:yh+1, xl:xh+1]
#print('Cut srcwcs from', oldshape, 'to', srcwcs.shape)
dilated = dilated[yl:yh+1, xl:xh+1]
flipblobs = flipblobs[yl:yh+1, xl:xh+1]
saved_srctim_ies = []
keep_srctims = []
mm = []
totalpix = 0
for tim in srctims:
# Zero out inverse-errors for all pixels outside
# 'dilated'.
try:
Yo,Xo,Yi,Xi,nil = resample_with_wcs(
tim.subwcs, srcwcs, [], 2)
except:
continue
ie = tim.getInvError()
newie = np.zeros_like(ie)
good, = np.nonzero(dilated[Yi,Xi] * (ie[Yo,Xo] > 0))
if len(good) == 0:
print('Tim has inverr all == 0')
continue
yy = Yo[good]
xx = Xo[good]
newie[yy,xx] = ie[yy,xx]
xl,xh = xx.min(), xx.max()
yl,yh = yy.min(), yy.max()
totalpix += len(xx)
d = { src: ModelMask(xl, yl, 1+xh-xl, 1+yh-yl) }
mm.append(d)
saved_srctim_ies.append(ie)
tim.inverr = newie
keep_srctims.append(tim)
srctims = keep_srctims
modelMasks = mm
B.blob_symm_nimages[srci] = len(srctims)
B.blob_symm_npix[srci] = totalpix
sh,sw = srcwcs.shape
B.blob_symm_width [srci] = sw
B.blob_symm_height[srci] = sh
if self.plots_per_source:
from legacypipe.detection import plot_boundary_map
plt.clf()
dimshow(get_rgb(coimgs, self.bands))
ax = plt.axis()
plt.plot(x-1, y-1, 'r+')
plt.axis(ax)
sx0,sy0 = srcwcs_x0y0
sh,sw = srcwcs.shape
ext = [sx0, sx0+sw, sy0, sy0+sh]
plot_boundary_map(flipblobs, rgb=(255,255,255), extent=ext)
plot_boundary_map(dilated, rgb=(0,255,0), extent=ext)
plt.title('symmetrized blobs')
self.ps.savefig()
nil,nil,coimgs,nil = quick_coadds(
srctims, self.bands, self.blobwcs,
fill_holes=False, get_cow=True)
# dimshow(get_rgb(coimgs, self.bands))
# ax = plt.axis()
# plt.plot(x-1, y-1, 'r+')
# plt.axis(ax)
# plt.title('Symmetric-blob masked')
# self.ps.savefig()
# plt.clf()
# for tim in srctims:
# ie = tim.getInvError()
# sigmas = (tim.getImage() * ie)[ie > 0]
# plt.hist(sigmas, range=(-5,5), bins=21, histtype='step')
# plt.axvline(np.mean(sigmas), alpha=0.5)
# plt.axvline(0., color='k', lw=3, alpha=0.5)
# plt.xlabel('Image pixels (sigma)')
# plt.title('Symmetrized pixel values')
# self.ps.savefig()
# # plot the modelmasks for each tim.
# plt.clf()
# R = int(np.floor(np.sqrt(len(srctims))))
# C = int(np.ceil(len(srctims) / float(R)))
# for i,tim in enumerate(srctims):
# plt.subplot(R, C, i+1)
# msk = modelMasks[i][src].mask
# print('Mask:', msk)
# if msk is None:
# continue
# plt.imshow(msk, interpolation='nearest', origin='lower', vmin=0, vmax=1)
# plt.title(tim.name)
# plt.suptitle('Model Masks')
# self.ps.savefig()
if self.bigblob and self.plots_per_source:
# This is a local source-WCS plot of the data going into the
# fit.
plt.clf()
coimgs,cons = quick_coadds(srctims, self.bands, srcwcs,
fill_holes=False)
dimshow(get_rgb(coimgs, self.bands))
plt.title('Model selection: stage1 data (srcwcs)')
self.ps.savefig()
#self._plots(srctractor, 'Model selection init')
srctractor = self.tractor(srctims, [src])
srctractor.setModelMasks(modelMasks)
srccat = srctractor.getCatalog()
ok,ix,iy = srcwcs.radec2pixelxy(src.getPosition().ra,
src.getPosition().dec)
ix = int(ix-1)
iy = int(iy-1)
# Start in blob
sh,sw = srcwcs.shape
if ix < 0 or iy < 0 or ix >= sw or iy >= sh or not srcblobmask[iy,ix]:
print('Source is starting outside blob -- skipping.')
return None
if fit_background:
for tim in srctims:
tim.freezeAllBut('sky')
srctractor.thawParam('images')
skyparams = srctractor.images.getParams()
enable_galaxy_cache()
# Compute the log-likehood without a source here.
srccat[0] = None
if fit_background:
#print('Fitting no-source model (sky)')
srctractor.optimize_loop(**self.optargs)
#srctractor.images.printThawedParams()
chisqs_none = _per_band_chisqs(srctractor, self.bands)
nparams = dict(ptsrc=2, simple=2, rex=3, exp=5, dev=5, comp=9)
# This is our "upgrade" threshold: how much better a galaxy
# fit has to be versus ptsrc, and comp versus galaxy.
galaxy_margin = 3.**2 + (nparams['exp'] - nparams['ptsrc'])
# *chisqs* is actually chi-squared improvement vs no source;
# larger is a better fit.
chisqs = dict(none=0)
oldmodel, ptsrc, simple, dev, exp, comp = _initialize_models(
src, self.rex)
if self.rex:
simname = 'rex'
rex = simple
else:
simname = 'simple'
trymodels = [('ptsrc', ptsrc)]
if oldmodel == 'ptsrc':
forced = False
if isinstance(src, GaiaSource):
print('Gaia source', src)
if src.isForcedPointSource():
forced = True
if forced:
print('Gaia source is forced to be a point source -- not trying other models')
elif self.hasbright:
print('Not computing galaxy models: bright star in blob')
else:
trymodels.append((simname, simple))
# Try galaxy models if simple > ptsrc, or if bright.
# The 'gals' model is just a marker
trymodels.append(('gals', None))
else:
trymodels.extend([('dev', dev), ('exp', exp), ('comp', comp)])
cputimes = {}
for name,newsrc in trymodels:
cpum0 = time.clock()
if name == 'gals':
# If 'simple' was better than 'ptsrc', or the source is
# bright, try the galaxy models.
chi_sim = chisqs.get(simname, 0)
chi_psf = chisqs.get('ptsrc', 0)
if chi_sim > chi_psf or max(chi_psf, chi_sim) > 400:
trymodels.extend([
('dev', dev), ('exp', exp), ('comp', comp)])
continue
if name == 'comp' and newsrc is None:
# Compute the comp model if exp or dev would be accepted
smod = _select_model(chisqs, nparams, galaxy_margin, self.rex)
if smod not in ['dev', 'exp']:
continue
newsrc = comp = FixedCompositeGalaxy(
src.getPosition(), src.getBrightness(),
SoftenedFracDev(0.5), exp.getShape(),
dev.getShape()).copy()
srccat[0] = newsrc
#print('Starting optimization for', name)
# Set maximum galaxy model sizes
# FIXME -- could use different fractions for deV vs exp (or comp)
fblob = 0.8
sh,sw = srcwcs.shape
rmax = np.log(fblob * max(sh, sw) * self.pixscale)
if name in ['exp', 'rex', 'dev']:
newsrc.shape.setMaxLogRadius(rmax)
elif name in ['comp']:
newsrc.shapeExp.setMaxLogRadius(rmax)
newsrc.shapeDev.setMaxLogRadius(rmax)
### FIXME -- also set model rendering limits here??
# Use the same modelMask shapes as the original source ('src').
# Need to create newsrc->mask mappings though:
mm = remap_modelmask(modelMasks, src, newsrc)
srctractor.setModelMasks(mm)
enable_galaxy_cache()
# Save these modelMasks for later...
newsrc_mm = mm
#lnp = srctractor.getLogProb()
#print('Initial log-prob:', lnp)
#print('vs original src: ', lnp - lnp0)
# if self.plots and False:
# # Grid of derivatives.
# _plot_derivs(tims, newsrc, srctractor, ps)
# if self.plots:
# mods = list(srctractor.getModelImages())
# plt.clf()
# coimgs,cons = quick_coadds(srctims, bands, srcwcs,
# images=mods, fill_holes=False)
# dimshow(get_rgb(coimgs, bands))
# plt.title('Initial: ' + name)
# self.ps.savefig()
if fit_background:
#print('Resetting sky params.')
srctractor.images.setParams(skyparams)
srctractor.thawParam('images')
# First-round optimization (during model selection)
#print('Optimizing: first round for', name, ':', len(srctims))
#print(newsrc)
cpustep0 = time.clock()
R = srctractor.optimize_loop(**self.optargs)
#print('Optimizing first round', name, 'took',
# time.clock()-cpustep0)
print('Fit result:', newsrc)
hit_limit = R.get('hit_limit', False)
if hit_limit:
if name in ['exp', 'rex', 'dev']:
print('Hit limit: r %.2f vs %.2f' %
(newsrc.shape.re, np.exp(rmax)))
elif name in ['comp']:
print('Hit limit: r %.2f, %.2f vs %.2f' %
(newsrc.shapeExp.re, newsrc.shapeDev.re,
np.exp(rmax)))
#srctractor.printThawedParams()
ok,ix,iy = srcwcs.radec2pixelxy(newsrc.getPosition().ra,
newsrc.getPosition().dec)
ix = int(ix-1)
iy = int(iy-1)
sh,sw = srcblobmask.shape
if ix < 0 or iy < 0 or ix >= sw or iy >= sh or not srcblobmask[iy,ix]:
# Exited blob!
print('Source exited sub-blob!')
# FIXME -- do we want to save any of the fitting results?
# Or flag this??
continue
disable_galaxy_cache()
# Compute inverse-variances for each source.
# Convert to "vanilla" ellipse parameterization
# (but save old shapes first)
# we do this (rather than making a copy) because we want to
# use the same modelMask maps.
if isinstance(newsrc, (DevGalaxy, ExpGalaxy)):
oldshape = newsrc.shape
elif isinstance(newsrc, FixedCompositeGalaxy):
oldshape = (newsrc.shapeExp, newsrc.shapeDev,newsrc.fracDev)
if fit_background:
# We have to freeze the sky here before computing
# uncertainties
srctractor.freezeParam('images')
nsrcparams = newsrc.numberOfParams()
_convert_ellipses(newsrc)
assert(newsrc.numberOfParams() == nsrcparams)
# Compute inverse-variances
# This uses the second-round modelMasks.
allderivs = srctractor.getDerivs()
ivars = _compute_invvars(allderivs)
assert(len(ivars) == nsrcparams)
B.all_model_ivs[srci][name] = np.array(ivars).astype(np.float32)
B.all_models[srci][name] = newsrc.copy()
assert(B.all_models[srci][name].numberOfParams() == nsrcparams)
# Now revert the ellipses!
if isinstance(newsrc, (DevGalaxy, ExpGalaxy)):
newsrc.shape = oldshape
elif isinstance(newsrc, FixedCompositeGalaxy):
(newsrc.shapeExp, newsrc.shapeDev,newsrc.fracDev) = oldshape
# Use the original 'srctractor' here so that the different
# models are evaluated on the same pixels.
# ---> AND with the same modelMasks as the original source...
#
srctractor.setModelMasks(newsrc_mm)
ch = _per_band_chisqs(srctractor, self.bands)
chisqs[name] = _chisq_improvement(newsrc, ch, chisqs_none)
cpum1 = time.clock()
B.all_model_cpu[srci][name] = cpum1 - cpum0
cputimes[name] = cpum1 - cpum0
B.all_model_hit_limit[srci][name] = hit_limit
if mask_others:
for ie,tim in zip(saved_srctim_ies, srctims):
tim.inverr = ie
# After model selection, revert the sky
# (srctims=tims when not bigblob)
if fit_background:
srctractor.images.setParams(skyparams)
# Actually select which model to keep. This "modnames"
# array determines the order of the elements in the DCHISQ
# column of the catalog.
modnames = ['ptsrc', simname, 'dev', 'exp', 'comp']
keepmod = _select_model(chisqs, nparams, galaxy_margin, self.rex)
keepsrc = {'none':None, 'ptsrc':ptsrc, simname:simple,
'dev':dev, 'exp':exp, 'comp':comp}[keepmod]
bestchi = chisqs.get(keepmod, 0.)
B.dchisq[srci, :] = np.array([chisqs.get(k,0) for k in modnames])
if keepsrc is not None and bestchi == 0.:
# Weird edge case, or where some best-fit fluxes go
# negative. eg
# https://github.com/legacysurvey/legacypipe/issues/174
print('Best dchisq is 0 -- dropping source')
keepsrc = None
B.hit_limit[srci] = B.all_model_hit_limit[srci].get(keepmod, False)
# This is the model-selection plot
if self.plots_per_source:
from collections import OrderedDict
subplots = []
plt.clf()
rows,cols = 3, 6
mods = OrderedDict([
('none',None), ('ptsrc',ptsrc), (simname,simple),
('dev',dev), ('exp',exp), ('comp',comp)])
for imod,modname in enumerate(mods.keys()):
if modname != 'none' and not modname in chisqs:
continue
srccat[0] = mods[modname]
srctractor.setModelMasks(None)
axes = []
plt.subplot(rows, cols, imod+1)
if modname == 'none':
# In the first panel, we show a coadd of the data
coimgs, cons = quick_coadds(srctims, self.bands,srcwcs)
rgbims = coimgs
rgb = get_rgb(coimgs, self.bands)
dimshow(rgb, ticks=False)
subplots.append(('data', rgb))
axes.append(plt.gca())
ax = plt.axis()
ok,x,y = srcwcs.radec2pixelxy(
src.getPosition().ra, src.getPosition().dec)
plt.plot(x-1, y-1, 'r+')
plt.axis(ax)
tt = 'Image'
chis = [((tim.getImage()) * tim.getInvError())**2
for tim in srctims]
res = [tim.getImage() for tim in srctims]
else:
modimgs = list(srctractor.getModelImages())
comods,nil = quick_coadds(srctims, self.bands, srcwcs,
images=modimgs)
rgbims = comods
rgb = get_rgb(comods, self.bands)
dimshow(rgb, ticks=False)
axes.append(plt.gca())
subplots.append(('mod'+modname, rgb))
tt = modname #+ '\n(%.0f s)' % cputimes[modname]
chis = [((tim.getImage() - mod) * tim.getInvError())**2
for tim,mod in zip(srctims, modimgs)]
res = [(tim.getImage() - mod) for tim,mod in
zip(srctims, modimgs)]
# Second row: same rgb image with arcsinh stretch
plt.subplot(rows, cols, imod+1+cols)
dimshow(get_rgb(rgbims, self.bands, **rgbkwargs), ticks=False)
axes.append(plt.gca())
plt.title(tt)
# residuals
coresids,nil = quick_coadds(srctims, self.bands, srcwcs,
images=res)
plt.subplot(rows, cols, imod+1+2*cols)
rgb = get_rgb(coresids, self.bands, **rgbkwargs_resid)
dimshow(rgb, ticks=False)
axes.append(plt.gca())
subplots.append(('res'+modname, rgb))
plt.title('chisq %.0f' % chisqs[modname], fontsize=8)
# Highlight the model to be kept
if modname == keepmod:
for ax in axes:
for spine in ax.spines.values():
spine.set_edgecolor('red')
spine.set_linewidth(2)
plt.suptitle('Blob %s, source %i: keeping %s\nwas: %s' %
(self.name, srci, keepmod, str(src)), fontsize=10)
self.ps.savefig()
if self.plots_single:
for name,rgb in subplots:
plt.figure(2)
plt.subplots_adjust(left=0.01, right=0.99, bottom=0.01, top=0.99)
dimshow(rgb, ticks=False)
fn = 'blob-%s-%i-%s.png' % (self.name, srci, name)
plt.savefig(fn)
print('Wrote', fn)
plt.figure(1)
return keepsrc
def _optimize_individual_sources(self, tr, cat, Ibright, cputime):
# Single source (though this is coded to handle multiple sources)
# Fit sources one at a time, but don't subtract other models
cat.freezeAllParams()
models = SourceModels()
models.create(self.tims, cat)
enable_galaxy_cache()
for numi,i in enumerate(Ibright):
cpu0 = time.clock()
#print('Fitting source', i, '(%i of %i in blob)' %
# (numi, len(Ibright)))
cat.freezeAllBut(i)
modelMasks = models.model_masks(0, cat[i])
tr.setModelMasks(modelMasks)
tr.optimize_loop(**self.optargs)
#print('Fitting source took', Time()-tsrc)
# print(cat[i])
cpu1 = time.clock()
cputime[i] += (cpu1 - cpu0)
tr.setModelMasks(None)
disable_galaxy_cache()
def tractor(self, tims, cat):
tr = Tractor(tims, cat, **self.trargs)
tr.freezeParams('images')
return tr
def _optimize_individual_sources_subtract(self, cat, Ibright,
cputime):
# -Remember the original images
# -Compute initial models for each source (in each tim)
# -Subtract initial models from images
# -During fitting, for each source:
# -add back in the source's initial model (to each tim)
# -fit, with Catalog([src])
# -subtract final model (from each tim)
# -Replace original images
models = SourceModels()
# Remember original tim images
models.save_images(self.tims)
# Create & subtract initial models for each tim x each source
models.create(self.tims, cat, subtract=True)
# For sources, in decreasing order of brightness
for numi,srci in enumerate(Ibright):
cpu0 = time.clock()
print('Fitting source', srci, '(%i of %i in blob %s)' %
(numi+1, len(Ibright), self.name))
src = cat[srci]
# Add this source's initial model back in.
models.add(srci, self.tims)
if self.bigblob:
# Create super-local sub-sub-tims around this source
# Make the subimages the same size as the modelMasks.
#tbb0 = Time()
mods = [mod[srci] for mod in models.models]
srctims,modelMasks = _get_subimages(self.tims, mods, src)
#print('Creating srctims:', Time()-tbb0)
# We plots only the first & last three sources
if self.plots_per_source and (numi < 3 or numi >= len(Ibright)-3):
plt.clf()
# Recompute coadds because of the subtract-all-and-readd shuffle
coimgs,cons = quick_coadds(self.tims, self.bands, self.blobwcs,
fill_holes=False)
rgb = get_rgb(coimgs, self.bands)
dimshow(rgb)
#dimshow(self.rgb)
ax = plt.axis()
for tim in srctims:
h,w = tim.shape
tx,ty = [0,0,w,w,0], [0,h,h,0,0]
rd = [tim.getWcs().pixelToPosition(xi,yi)
for xi,yi in zip(tx,ty)]
ra = [p.ra for p in rd]
dec = [p.dec for p in rd]
ok,x,y = self.blobwcs.radec2pixelxy(ra, dec)
plt.plot(x, y, 'b-')
ra,dec = tim.subwcs.pixelxy2radec(tx, ty)
ok,x,y = self.blobwcs.radec2pixelxy(ra, dec)
plt.plot(x, y, 'c-')
plt.title('source %i of %i' % (numi, len(Ibright)))
plt.axis(ax)
self.ps.savefig()
else:
srctims = self.tims
modelMasks = models.model_masks(srci, src)
srctractor = self.tractor(srctims, [src])
#print('Setting modelMasks:', modelMasks)
srctractor.setModelMasks(modelMasks)
# if plots and False:
# spmods,spnames = [],[]
# spallmods,spallnames = [],[]
# if numi == 0:
# spallmods.append(list(tr.getModelImages()))
# spallnames.append('Initial (all)')
# spmods.append(list(srctractor.getModelImages()))
# spnames.append('Initial')
# First-round optimization
#print('First-round initial log-prob:', srctractor.getLogProb())
srctractor.optimize_loop(**self.optargs)
#print('First-round final log-prob:', srctractor.getLogProb())
# if plots and False:
# spmods.append(list(srctractor.getModelImages()))
# spnames.append('Fit')
# spallmods.append(list(tr.getModelImages()))
# spallnames.append('Fit (all)')
#
# if plots and False:
# plt.figure(1, figsize=(8,6))
# plt.subplots_adjust(left=0.01, right=0.99, top=0.95,
# bottom=0.01, hspace=0.1, wspace=0.05)
# #plt.figure(2, figsize=(3,3))
# #plt.subplots_adjust(left=0.005, right=0.995,
# # top=0.995,bottom=0.005)
# #_plot_mods(tims, spmods, spnames, bands, None, None, bslc,
# # blobw, blobh, ps, chi_plots=plots2)
# plt.figure(2, figsize=(3,3.5))
# plt.subplots_adjust(left=0.005, right=0.995,
# top=0.88, bottom=0.005)
# plt.suptitle('Blob %i' % iblob)
# tempims = [tim.getImage() for tim in tims]
#
# _plot_mods(list(srctractor.getImages()), spmods, spnames,
# bands, None, None, bslc, blobw, blobh, ps,
# chi_plots=plots2, rgb_plots=True, main_plot=False,
# rgb_format=('spmods Blob %i, src %i: %%s' %
# (iblob, i)))
# _plot_mods(tims, spallmods, spallnames, bands, None, None,
# bslc, blobw, blobh, ps,
# chi_plots=plots2, rgb_plots=True, main_plot=False,
# rgb_format=('spallmods Blob %i, src %i: %%s' %
# (iblob, i)))
#
# models.restore_images(tims)
# _plot_mods(tims, spallmods, spallnames, bands, None, None,
# bslc, blobw, blobh, ps,
# chi_plots=plots2, rgb_plots=True, main_plot=False,
# rgb_format='Blob %i, src %i: %%s' % (iblob, i))
# for tim,im in zip(tims, tempims):
# tim.data = im
# Re-remove the final fit model for this source
models.update_and_subtract(srci, src, self.tims)
srctractor.setModelMasks(None)
disable_galaxy_cache()
#print('Fitting source took', Time()-tsrc)
#print(src)
cpu1 = time.clock()
cputime[srci] += (cpu1 - cpu0)
models.restore_images(self.tims)
del models
def _fit_fluxes(self, cat, tims, bands):
cat.thawAllRecursive()
for src in cat:
src.freezeAllBut('brightness')
for b in bands:
for src in cat:
src.getBrightness().freezeAllBut(b)
# Images for this band
btims = [tim for tim in tims if tim.band == b]
btr = self.tractor(btims, cat)
btr.optimize_forced_photometry(shared_params=False, wantims=False)
cat.thawAllRecursive()
def _plots(self, tr, title):
plotmods = []
plotmodnames = []
plotmods.append(list(tr.getModelImages()))
plotmodnames.append(title)
for tim in tr.images:
if hasattr(tim, 'resamp'):
del tim.resamp
_plot_mods(tr.images, plotmods, self.blobwcs, plotmodnames, self.bands,
None, None, None,
self.blobw, self.blobh, self.ps, chi_plots=False)
for tim in tr.images:
if hasattr(tim, 'resamp'):
del tim.resamp
def _plot_coadd(self, tims, wcs, model=None, resid=None):
if resid is not None:
mods = list(resid.getChiImages())
coimgs,cons = quick_coadds(tims, self.bands, wcs, images=mods,
fill_holes=False)
dimshow(get_rgb(coimgs,self.bands, **rgbkwargs_resid))
return
mods = None
if model is not None:
mods = list(model.getModelImages())
coimgs,cons = quick_coadds(tims, self.bands, wcs, images=mods,
fill_holes=False)
dimshow(get_rgb(coimgs,self.bands))
def _initial_plots(self):
print('Plotting blob image for blob', self.name)
coimgs,cons = quick_coadds(self.tims, self.bands, self.blobwcs,
fill_holes=False)
self.rgb = get_rgb(coimgs, self.bands)
plt.clf()
dimshow(self.rgb)
plt.title('Blob: %s' % self.name)
self.ps.savefig()
if self.plots_single:
plt.figure(2)
dimshow(self.rgb, ticks=False)
plt.savefig('blob-%s-data.png' % (self.name))
plt.figure(1)
ok,x0,y0 = self.blobwcs.radec2pixelxy(
np.array([src.getPosition().ra for src in self.srcs]),
np.array([src.getPosition().dec for src in self.srcs]))
ax = plt.axis()
plt.plot(x0-1, y0-1, 'r.')
plt.axis(ax)
plt.title('initial sources')
self.ps.savefig()
# plt.clf()
# ccmap = dict(g='g', r='r', z='m')
# for tim in tims:
# chi = (tim.data * tim.inverr)[tim.inverr > 0]
# plt.hist(chi.ravel(), range=(-5,10), bins=100, histtype='step',
# color=ccmap[tim.band])
# plt.xlabel('signal/noise per pixel')
# self.ps.savefig()
def create_tims(self, timargs):
# In order to make multiprocessing easier, the one_blob method
# is passed all the ingredients to make local tractor Images
# rather than the Images themselves. Here we build the
# 'tims'.
tims = []
for (img, inverr, twcs, wcs, pcal, sky, psf, name, sx0, sx1, sy0, sy1,
band, sig1, modelMinval, imobj) in timargs:
# Mask out inverr for pixels that are not within the blob.
subwcs = wcs.get_subimage(int(sx0), int(sy0),
int(sx1-sx0), int(sy1-sy0))
try:
Yo,Xo,Yi,Xi,rims = resample_with_wcs(subwcs, self.blobwcs,
[], 2)
except OverlapError:
continue
if len(Yo) == 0:
continue
inverr2 = np.zeros_like(inverr)
I = np.flatnonzero(self.blobmask[Yi,Xi])
inverr2[Yo[I],Xo[I]] = inverr[Yo[I],Xo[I]]
inverr = inverr2
# If the subimage (blob) is small enough, instantiate a
# constant PSF model in the center.
if sy1-sy0 < 400 and sx1-sx0 < 400:
subpsf = psf.constantPsfAt((sx0+sx1)/2., (sy0+sy1)/2.)
else:
# Otherwise, instantiate a (shifted) spatially-varying
# PsfEx model.
subpsf = psf.getShifted(sx0, sy0)
tim = Image(data=img, inverr=inverr, wcs=twcs,
psf=subpsf, photocal=pcal, sky=sky, name=name)
tim.band = band
tim.sig1 = sig1
tim.modelMinval = modelMinval
tim.subwcs = subwcs
tim.meta = imobj
tim.psf_sigma = imobj.fwhm / 2.35
tim.dq = None
tims.append(tim)
return tims
def _convert_ellipses(src):
if isinstance(src, (DevGalaxy, ExpGalaxy)):
#print('Converting ellipse for source', src)
src.shape = src.shape.toEllipseE()
#print('--->', src.shape)
if isinstance(src, RexGalaxy):
src.shape.freezeParams('e1', 'e2')
elif isinstance(src, FixedCompositeGalaxy):
src.shapeExp = src.shapeExp.toEllipseE()
src.shapeDev = src.shapeDev.toEllipseE()
src.fracDev = FracDev(src.fracDev.clipped())
def _compute_invvars(allderivs):
ivs = []
for iparam,derivs in enumerate(allderivs):
chisq = 0
for deriv,tim in derivs:
h,w = tim.shape
deriv.clipTo(w,h)
ie = tim.getInvError()
slc = deriv.getSlice(ie)
chi = deriv.patch * ie[slc]
chisq += (chi**2).sum()
ivs.append(chisq)
return ivs
def _argsort_by_brightness(cat, bands):
fluxes = []
for src in cat:
# HACK -- here we just *sum* the nanomaggies in each band. Bogus!
br = src.getBrightness()
flux = sum([br.getFlux(band) for band in bands])
fluxes.append(flux)
Ibright = np.argsort(-np.array(fluxes))
return Ibright
def _compute_source_metrics(srcs, tims, bands, tr):
# rchi2 quality-of-fit metric
rchi2_num = np.zeros((len(srcs),len(bands)), np.float32)
rchi2_den = np.zeros((len(srcs),len(bands)), np.float32)
# fracflux degree-of-blending metric
fracflux_num = np.zeros((len(srcs),len(bands)), np.float32)
fracflux_den = np.zeros((len(srcs),len(bands)), np.float32)
# fracin flux-inside-blob metric
fracin_num = np.zeros((len(srcs),len(bands)), np.float32)
fracin_den = np.zeros((len(srcs),len(bands)), np.float32)
# fracmasked: fraction of masked pixels metric
fracmasked_num = np.zeros((len(srcs),len(bands)), np.float32)
fracmasked_den = np.zeros((len(srcs),len(bands)), np.float32)
for iband,band in enumerate(bands):
for tim in tims:
if tim.band != band:
continue
mod = np.zeros(tim.getModelShape(), tr.modtype)
srcmods = [None for src in srcs]
counts = np.zeros(len(srcs))
pcal = tim.getPhotoCal()
# For each source, compute its model and record its flux
# in this image. Also compute the full model *mod*.
for isrc,src in enumerate(srcs):
patch = tr.getModelPatch(tim, src, minsb=tim.modelMinval)
if patch is None or patch.patch is None:
continue
counts[isrc] = np.sum([np.abs(pcal.brightnessToCounts(b))
for b in src.getBrightnesses()])
if counts[isrc] == 0:
continue
H,W = mod.shape
patch.clipTo(W,H)
srcmods[isrc] = patch
patch.addTo(mod)
# Now compute metrics for each source
for isrc,patch in enumerate(srcmods):
if patch is None:
continue
if patch.patch is None:
continue
if counts[isrc] == 0:
continue
if np.sum(patch.patch**2) == 0:
continue
slc = patch.getSlice(mod)
patch = patch.patch
# print('fracflux: band', band, 'isrc', isrc, 'tim', tim.name)
# print('src:', srcs[isrc])
# print('patch sum', np.sum(patch),'abs',np.sum(np.abs(patch)))
# print('counts:', counts[isrc])
# print('mod slice sum', np.sum(mod[slc]))
# print('mod[slc] - patch:', np.sum(mod[slc] - patch))
# (mod - patch) is flux from others
# (mod - patch) / counts is normalized flux from others
# We take that and weight it by this source's profile;
# patch / counts is unit profile
# But this takes the dot product between the profiles,
# so we have to normalize appropriately, ie by
# (patch**2)/counts**2; counts**2 drops out of the
# denom. If you have an identical source with twice the flux,
# this results in fracflux being 2.0
# fraction of this source's flux that is inside this patch.
# This can be < 1 when the source is near an edge, or if the
# source is a huge diffuse galaxy in a small patch.
fin = np.abs(np.sum(patch) / counts[isrc])
# print('fin:', fin)
# print('fracflux_num: fin *',
# np.sum((mod[slc] - patch) * np.abs(patch)) /
# np.sum(patch**2))
fracflux_num[isrc,iband] += (fin *
np.sum((mod[slc] - patch) * np.abs(patch)) /
np.sum(patch**2))
fracflux_den[isrc,iband] += fin
fracmasked_num[isrc,iband] += (
np.sum((tim.getInvError()[slc] == 0) * np.abs(patch)) /
np.abs(counts[isrc]))
fracmasked_den[isrc,iband] += fin
fracin_num[isrc,iband] += np.abs(np.sum(patch))
fracin_den[isrc,iband] += np.abs(counts[isrc])
tim.getSky().addTo(mod)
chisq = ((tim.getImage() - mod) * tim.getInvError())**2
for isrc,patch in enumerate(srcmods):
if patch is None or patch.patch is None:
continue
if counts[isrc] == 0:
continue
slc = patch.getSlice(mod)
# We compute numerator and denom separately to handle
# edge objects, where sum(patch.patch) < counts.
# Also, to normalize by the number of images. (Being
# on the edge of an image is like being in half an
# image.)
rchi2_num[isrc,iband] += (np.sum(chisq[slc] * patch.patch) /
counts[isrc])
# If the source is not near an image edge,
# sum(patch.patch) == counts[isrc].
rchi2_den[isrc,iband] += np.sum(patch.patch) / counts[isrc]
#print('Fracflux_num:', fracflux_num)
#print('Fracflux_den:', fracflux_den)
fracflux = fracflux_num / fracflux_den
rchi2 = rchi2_num / rchi2_den
fracmasked = fracmasked_num / fracmasked_den
# Eliminate NaNs (these happen when, eg, we have no coverage in one band but
# sources detected in another band, hence denominator is zero)
fracflux [ fracflux_den == 0] = 0.
rchi2 [ rchi2_den == 0] = 0.
fracmasked[fracmasked_den == 0] = 0.
# fracin_{num,den} are in flux * nimages units
tinyflux = 1e-9
fracin = fracin_num / np.maximum(tinyflux, fracin_den)
return dict(fracin=fracin, fracflux=fracflux, rchisq=rchi2,
fracmasked=fracmasked)
def _initialize_models(src, rex):
if isinstance(src, PointSource):
ptsrc = src.copy()
if rex:
from legacypipe.survey import LogRadius
simple = RexGalaxy(src.getPosition(), src.getBrightness(),
LogRadius(-1.)).copy()
#print('Created Rex:', simple)
else:
simple = SimpleGalaxy(src.getPosition(), src.getBrightness()).copy()
# logr, ee1, ee2
shape = LegacyEllipseWithPriors(-1., 0., 0.)
dev = DevGalaxy(src.getPosition(), src.getBrightness(), shape).copy()
exp = ExpGalaxy(src.getPosition(), src.getBrightness(), shape).copy()
comp = None
oldmodel = 'ptsrc'
elif isinstance(src, DevGalaxy):
ptsrc = PointSource(src.getPosition(), src.getBrightness()).copy()
simple = SimpleGalaxy(src.getPosition(), src.getBrightness()).copy()
dev = src.copy()
exp = ExpGalaxy(src.getPosition(), src.getBrightness(),
src.getShape()).copy()
comp = None
oldmodel = 'dev'
elif isinstance(src, ExpGalaxy):
ptsrc = PointSource(src.getPosition(), src.getBrightness()).copy()
simple = SimpleGalaxy(src.getPosition(), src.getBrightness()).copy()
dev = DevGalaxy(src.getPosition(), src.getBrightness(),
src.getShape()).copy()
exp = src.copy()
comp = None
oldmodel = 'exp'
elif isinstance(src, FixedCompositeGalaxy):
ptsrc = PointSource(src.getPosition(), src.getBrightness()).copy()
simple = SimpleGalaxy(src.getPosition(), src.getBrightness()).copy()
frac = src.fracDev.clipped()
if frac > 0:
shape = src.shapeDev
else:
shape = src.shapeExp
dev = DevGalaxy(src.getPosition(), src.getBrightness(), shape).copy()
if frac < 1:
shape = src.shapeExp
else:
shape = src.shapeDev
exp = ExpGalaxy(src.getPosition(), src.getBrightness(), shape).copy()
comp = src.copy()
oldmodel = 'comp'
return oldmodel, ptsrc, simple, dev, exp, comp
def _get_subimages(tims, mods, src):
subtims = []
modelMasks = []
#print('Big blob: trimming:')
for tim,mod in zip(tims, mods):
if mod is None:
continue
mh,mw = mod.shape
if mh == 0 or mw == 0:
continue
# for modelMasks
d = { src: ModelMask(0, 0, mw, mh) }
modelMasks.append(d)
x0,y0 = mod.x0 , mod.y0
x1,y1 = x0 + mw, y0 + mh
subtim = _get_subtim(tim, x0, x1, y0, y1)
if subtim.shape != (mh,mw):
print('Subtim was not the shape expected:', subtim.shape,
'image shape', tim.getImage().shape, 'slice y', y0,y1,
'x', x0,x1, 'mod shape', mh,mw)
subtims.append(subtim)
return subtims, modelMasks
def _get_subtim(tim, x0, x1, y0, y1):
slc = slice(y0,y1), slice(x0, x1)
subimg = tim.getImage()[slc]
subpsf = tim.psf.constantPsfAt((x0+x1)/2., (y0+y1)/2.)
subtim = Image(data=subimg,
inverr=tim.getInvError()[slc],
wcs=tim.wcs.shifted(x0, y0),
psf=subpsf,
photocal=tim.getPhotoCal(),
sky=tim.sky.shifted(x0, y0),
name=tim.name)
sh,sw = subtim.shape
subtim.subwcs = tim.subwcs.get_subimage(x0, y0, sw, sh)
subtim.band = tim.band
subtim.sig1 = tim.sig1
subtim.modelMinval = tim.modelMinval
subtim.x0 = x0
subtim.y0 = y0
subtim.meta = tim.meta
subtim.psf_sigma = tim.psf_sigma
if tim.dq is not None:
subtim.dq = tim.dq[slc]
else:
subtim.dq = None
return subtim
[docs]class SourceModels(object):
'''
This class maintains a list of the model patches for a set of sources
in a set of images.
'''
def __init__(self):
self.filledModelMasks = True
def save_images(self, tims):
self.orig_images = [tim.getImage() for tim in tims]
for tim,img in zip(tims, self.orig_images):
tim.data = img.copy()
def restore_images(self, tims):
for tim,img in zip(tims, self.orig_images):
tim.data = img
[docs] def create(self, tims, srcs, subtract=False):
'''
Note that this modifies the *tims* if subtract=True.
'''
self.models = []
for tim in tims:
mods = []
sh = tim.shape
ie = tim.getInvError()
for src in srcs:
mod = src.getModelPatch(tim)
if mod is not None and mod.patch is not None:
if not np.all(np.isfinite(mod.patch)):
print('Non-finite mod patch')
print('source:', src)
print('tim:', tim)
print('PSF:', tim.getPsf())
assert(np.all(np.isfinite(mod.patch)))
mod = _clip_model_to_blob(mod, sh, ie)
if subtract and mod is not None:
mod.addTo(tim.getImage(), scale=-1)
mods.append(mod)
self.models.append(mods)
[docs] def add(self, i, tims):
'''
Adds the models for source *i* back into the tims.
'''
for tim,mods in zip(tims, self.models):
mod = mods[i]
if mod is not None:
mod.addTo(tim.getImage())
def update_and_subtract(self, i, src, tims):
for tim,mods in zip(tims, self.models):
#mod = srctractor.getModelPatch(tim, src)
if src is None:
mod = None
else:
mod = src.getModelPatch(tim)
if mod is not None:
mod.addTo(tim.getImage(), scale=-1)
mods[i] = mod
def model_masks(self, i, src):
modelMasks = []
for mods in self.models:
d = dict()
modelMasks.append(d)
mod = mods[i]
if mod is not None:
if self.filledModelMasks:
mh,mw = mod.shape
d[src] = ModelMask(mod.x0, mod.y0, mw, mh)
else:
d[src] = ModelMask(mod.x0, mod.y0, mod.patch != 0)
return modelMasks
def remap_modelmask(modelMasks, oldsrc, newsrc):
mm = []
for mim in modelMasks:
d = dict()
mm.append(d)
try:
d[newsrc] = mim[oldsrc]
except KeyError:
pass
return mm
def _clip_model_to_blob(mod, sh, ie):
'''
mod: Patch
sh: tim shape
ie: tim invError
Returns: new Patch
'''
mslc,islc = mod.getSlices(sh)
sy,sx = mslc
patch = mod.patch[mslc] * (ie[islc]>0)
if patch.shape == (0,0):
return None
mod = Patch(mod.x0 + sx.start, mod.y0 + sy.start, patch)
# Check
mh,mw = mod.shape
assert(mod.x0 >= 0)
assert(mod.y0 >= 0)
ph,pw = sh
assert(mod.x0 + mw <= pw)
assert(mod.y0 + mh <= ph)
return mod
def _select_model(chisqs, nparams, galaxy_margin, rex):
'''
Returns keepmod
'''
keepmod = 'none'
# This is our "detection threshold": 5-sigma in
# *parameter-penalized* units; ie, ~5.2-sigma for point sources
cut = 5.**2
# Take the best of all models computed
diff = max([chisqs[name] - nparams[name] for name in chisqs.keys()
if name != 'none'] + [-1])
if diff < cut:
return keepmod
# We're going to keep this source!
if rex:
simname = 'rex'
else:
simname = 'simple'
if not simname in chisqs:
# bright stars / reference stars: we don't test the simple model.
return 'ptsrc'
# Now choose between point source and simple model (SIMP/REX)
if chisqs.get('ptsrc',0)-nparams['ptsrc'] > chisqs.get(simname,0)-nparams[simname]:
#print('Keeping source; PTSRC is better than SIMPLE')
keepmod = 'ptsrc'
else:
#print('Keeping source; SIMPLE is better than PTSRC')
#print('REX is better fit. Radius', simplemod.shape.re)
keepmod = simname
# For REX, we also demand a fractionally better fit
if simname == 'rex':
dchisq_psf = chisqs.get('ptsrc',0)
dchisq_rex = chisqs.get('rex',0)
if dchisq_psf > 0 and (dchisq_rex - dchisq_psf) < (0.01 * dchisq_psf):
keepmod = 'ptsrc'
if not ('exp' in chisqs or 'dev' in chisqs):
return keepmod
# This is our "upgrade" threshold: how much better a galaxy
# fit has to be versus ptsrc, and comp versus galaxy.
cut = galaxy_margin
# This is the "fractional" upgrade threshold for ptsrc/simple->dev/exp:
# 1% of ptsrc vs nothing
fcut = 0.01 * chisqs.get('ptsrc', 0)
#print('Cut: max of', cut, 'and', fcut, ' (fraction of chisq_psf=%.1f)'
# % chisqs['ptsrc'])
cut = max(cut, fcut)
expdiff = chisqs.get('exp', 0) - chisqs[keepmod]
devdiff = chisqs.get('dev', 0) - chisqs[keepmod]
#print('EXP vs', keepmod, ':', expdiff)
#print('DEV vs', keepmod, ':', devdiff)
if not (expdiff > cut or devdiff > cut):
#print('Keeping', keepmod)
return keepmod
if expdiff > devdiff:
#print('Upgrading from PTSRC to EXP: diff', expdiff)
keepmod = 'exp'
else:
#print('Upgrading from PTSRC to DEV: diff', expdiff)
keepmod = 'dev'
if not 'comp' in chisqs:
return keepmod
diff = chisqs['comp'] - chisqs[keepmod]
#print('Comparing', keepmod, 'to comp. cut:', cut, 'comp:', diff)
if diff < cut:
return keepmod
#print('Upgrading from dev/exp to composite.')
keepmod = 'comp'
return keepmod
def _chisq_improvement(src, chisqs, chisqs_none):
'''
chisqs, chisqs_none: dict of band->chisq
'''
bright = src.getBrightness()
bands = chisqs.keys()
fluxes = dict([(b, bright.getFlux(b)) for b in bands])
dchisq = 0.
for b in bands:
flux = fluxes[b]
if flux == 0:
continue
# this will be positive for an improved model
d = chisqs_none[b] - chisqs[b]
if flux > 0:
dchisq += d
else:
dchisq -= np.abs(d)
return dchisq
def _per_band_chisqs(tractor, bands):
chisqs = dict([(b,0) for b in bands])
for i,img in enumerate(tractor.images):
chi = tractor.getChiImage(img=img)
chisqs[img.band] = chisqs[img.band] + (chi ** 2).sum()
return chisqs
def _limit_galaxy_stamp_size(src, tim, maxhalf=128):
from tractor.galaxy import ProfileGalaxy
if isinstance(src, ProfileGalaxy):
px,py = tim.wcs.positionToPixel(src.getPosition())
h = src._getUnitFluxPatchSize(tim, px, py, tim.modelMinval)
if h > maxhalf:
#print('halfsize', h, 'for', src, '-> setting to', maxhalf)
src.halfsize = maxhalf
RetroSearch is an open source project built by @garambo | Open a GitHub Issue
Search and Browse the WWW like it's 1997 | Search results from DuckDuckGo
HTML:
3.2
| Encoding:
UTF-8
| Version:
0.7.4