def addObjects(self, inputlist='galaxies.dat'):
"""
Add object(s) from inputlist to the output image.
:param inputlist: name of the input list
:type inputlist: str
"""
self.log.info('Adding objects from %s to %s' %
(inputlist, self.settings['output']))
iraf.artdata.dynrange = self.settings['dynrange']
iraf.mkobjects(self.settings['output'],
output='',
ncols=self.settings['xdim'],
nlines=self.settings['ydim'],
background=self.settings['background'],
objects=inputlist,
xoffset=0.0,
yoffset=0.0,
star=self.settings['star'],
radius=self.settings['radius'],
beta=self.settings['beta'],
ar=self.settings['ar'],
pa=self.settings['pa'],
distance=1.0,
exptime=self.settings['exptime'],
magzero=self.settings['magzero'],
gain=self.settings['gain'],
rdnoise=self.settings['rdnoise'],
poisson=self.settings['poisson'],
seed=2,
comments=iraf.yes)
def addObjects(self, inputlist='galaxies.dat'):
"""
Add object(s) from inputlist to the output image.
:param inputlist: name of the input list
:type inputlist: str
"""
self.log.info('Adding objects from %s to %s' % (inputlist, self.settings['output']))
iraf.artdata.dynrange = self.settings['dynrange']
iraf.mkobjects(self.settings['output'],
output='',
ncols=self.settings['xdim'],
nlines=self.settings['ydim'],
background=self.settings['background'],
objects=inputlist,
xoffset=0.0,
yoffset=0.0,
star=self.settings['star'],
radius=self.settings['radius'],
beta=self.settings['beta'],
ar=self.settings['ar'],
pa=self.settings['pa'],
distance=1.0,
exptime=self.settings['exptime'],
magzero=self.settings['magzero'],
gain=self.settings['gain'],
rdnoise=self.settings['rdnoise'],
poisson=self.settings['poisson'],
seed=2,
comments=iraf.yes)
def makenoiselessimage(self, band, galfile, magz, psffile, save=0, gain=1.0):
"""
Creates a noiseless convolved image
"""
assert os.path.exists(psffile), "PSF image %s does not exist." % psffile
broot = self.root + '_%s' % band
outfile = broot + '_sim.fits'
outfile_nonoise = broot + '_sim_noiseless.fits'
# print outfile,xmax,ymax,galfile,magz,gain
iraf.unlearn('artdata')
iraf.unlearn('mkobjects')
iraf.artdata.dynrange=1.e5
print "Running iraf.mkobject for %s..." % band
iraf.mkobjects(outfile_nonoise, output="", title="", ncols=self.xmax,
nlines=self.ymax, header="", background=0.0, objects=galfile,
xoffset=0., yoffset=0., star="gaussian", radius=0.1,
beta=2.5, ar=1., pa=0., distance=1., exptime=1.,
magzero=magz, gain=gain, rdnoise=0., poisson=0,
seed=2, comments=1)
print "Convolving with PSF..."
if _hconvolve:
imhconvolve(outfile_nonoise, psffile, outfile, overwrite=True)
else:
print "No hconvolve..."
outimage = pyfits.getdata(outfile_nonoise)
psfimage = pyfits.getdata(psffile)
outimage2 = fftconvolve(outimage, psfimage, mode='same')
h = pyfits.open(outfile, mode='update')
h[0].data = outimage2
h.flush()
h.close()
self.noiselessimages[band] = outfile
os.remove(outfile_nonoise)
def makeObject(self, inObjectFile="mkobject.coo"):
"""IRAF routine: mkobjects. This places a star in the fits image that is the parent object of this class, at the given ra and dec. It takes as input a file of "ra dec magnitude" for a star type object.
1. Get info from the header files if you want noise
2. Get FWHM for size of the star for the given image
3. Generate the star
radius = FWHM / scale, from statistics, scale = 2*sqrt(2*ln(2))
"""
# 1.
self.loadHeader()
INFODICT = {
"RON": self.getHeader("RON"), \
"GAIN": self.getHeader("GAIN"), \
"EXPTIME": self.getHeader("EXPTIME"), \
"MAGZP": self._ZPDICT[self.getHeader("FILTER")], \
"POISSON": "no", \
"STAR": "gaussian", \
}
# 2.
scale = 2*scipy.sqrt(2*scipy.log(2))
self.getMyMedianFWHM()
INFODICT["RADIUS"] = self._MEDFWHM / scale
# 3.
outputname = self._Name.replace(".fits", "_mko.fits")
iraf.noao(_doprint=0)
iraf.artdata(_doprint=0)
iraf.mkobjects(input=self._Name, \
output=outputname, \
# When creating new images
#title="",\
#ncols=self.xdim, \
#nlines=self.ydim, \
#header=self.hdrfile, \
#background=0.0, \
# When creating objects
objects=inObjectFile, \
xoffset=0.0, \
yoffset=0.0, \
star=INFODICT["STAR"], \
radius=INFODICT["RADIUS"], # this is fwhm/scale (pixels), where scale = 2sqrt(2ln2)\
#beta=2.5, # for star=moffat profile\
ar=1.0, \
pa=0.0, \
distance=1.0, \
exptime=INFODICT["EXPTIME"], \
magzero=INFODICT["MAGZP"], \
# Noise parameters
gain=INFODICT["GAIN"], \
rdnoise=INFODICT["RON"], \
poisson=INFODICT["POISSON"], \
seed=1, \
comments=1)
return outputname
def makenoiselessimage_galfit(self,
band,
galfile,
magz,
psffile,
save=0,
gain=1.0):
"""
Creates a noiseless convolved image
"""
assert os.path.exists(
psffile), "PSF image %s does not exist." % psffile
broot = self.root + '_%s' % band
outfile = broot + '_sim.fits'
outfile_nonoise = broot + '_sim_noiseless.fits'
if os.path.exists(outfile):
os.remove(outfile)
# print outfile,xmax,ymax,galfile,magz,gain
iraf.unlearn('artdata')
iraf.unlearn('mkobjects')
iraf.artdata.dynrange = 1.e5
print "Running iraf.mkobject in %s for GALFIT..." % band
iraf.mkobjects(outfile_nonoise,
output="",
title="",
ncols=self.xmax_galfit,
nlines=self.ymax_galfit,
header="",
background=0.0,
objects=galfile,
xoffset=0.,
yoffset=0.,
star="gaussian",
radius=0.1,
beta=2.5,
ar=1.,
pa=0.,
distance=1.,
exptime=1.,
magzero=magz,
gain=gain,
rdnoise=0.,
poisson=0,
seed=2,
comments=1)
imhconvolve(outfile_nonoise, psffile, outfile, overwrite=True)
self.noiselessimages[band] = outfile
os.remove(outfile_nonoise)
def addgalaxies(self, simimage, objectcat='stars.coords.dat'):
if os.path.exists(simimage):
os.remove(simimage)
os.system('cp /Applications/mopex/cal/mips24_prf_mosaic_2.45_4x.fits .'
) #convolve star w/SSC PRF
iraf.mkobjects(input=self.inputimage,
output=simimage,
objects=objectcat,
radius=15.875,
star='mips24_prf_mosaic_2.45_4x.fits',
magzero=zp,
background=0.,
gain=5.,
rdnoise=0.,
poisson='no')
def quick_insert_gaussian(input_image, ra, dec, mags, zeropoint, gain=1):
"""
A quick function that inserts point sources with Moffat profile into the
specified RA & DEC locations.
"""
# Define image parameters
hdr = fits.getheader(input_image)
xmax = hdr['naxis1']
ymax = hdr['naxis2']
outfile_nonoise = os.path.splitext(input_image)[0] + '_sim_noiseless.fits'
if os.path.exists(outfile_nonoise):
os.remove(outfile_nonoise)
wcs_in = wcs.WCS(hdr)
# Figure out the x, y coordinates of fake sources
radec_input = np.array([ra, dec])
xy_input = wcs_in.wcs_world2pix(ra, dec, 1)
x_input, y_input = xy_input
nobj = len(ra)
print "There are {} objects in total.".format(nobj)
# write the input list of objects
f = open('fake_sources.in', 'w')
for i in range(nobj):
f.write('{:.2f} {:.2f} {:.2f}\n'.format(x_input[i], y_input[i], mags[i]))
f.close()
iraf.mkobjects(outfile_nonoise, output="", title="", ncols=xmax,
nlines=ymax, header="", background=0.0, objects='fake_sources.in',
xoffset=0., yoffset=0., star="gaussian", radius=2.5,
beta=2.5, ar=1., pa=0., distance=1., exptime=1.,
magzero=zeropoint, gain=gain, rdnoise=0., poisson=0,
seed=2, comments=1)
# Combine noiseless fake image with input image
output_image = os.path.splitext(input_image)[0] + '_sim.fits'
if os.path.exists(output_image):
os.remove(output_image)
noiseless_data = fits.getdata(outfile_nonoise)
os.system('cp {} {}'.format(input_image, output_image))
h = fits.open(output_image, mode='update')
h[0].data = h[0].data + noiseless_data
h.flush()
h.close()
print "Image {} written!".format(output_image)
def mkobjects_iraf(inimage, outimage, objfile, radius, magzero):
from pyraf import iraf
iraf.noao(_doprint=0)
iraf.artdata(_doprint=0)
if os.path.exists(
outimage) == True: # If the file exists already, IRAF doesn't tell you but just doesn't write the new file
os.remove(outimage)
print 'Deleted ' + outimage + ' first'
iraf.mkobjects(input=inimage,
output=outimage,
objects=objfile,
radius=radius,
magzero=magzero)
return None
def makenoiselessimage(self,
galfile,
simroot,
magz=99.0,
save=0,
gain=1.0,
psffile=""):
"""
Creates a noiseless convolved image
"""
assert os.path.exists(
psffile), "PSF image %s does not exist." % psffile
if magz >= 99.0:
magz = self.calc_zeropoint()
outfile = simroot + '_sim.fits'
print outfile, xmax, ymax, galfile, magz, gain
iraf.unlearn('artdata')
iraf.unlearn('mkobjects')
iraf.artdata.dynrange = 1.e5
iraf.mkobjects(outfile,
output="",
title="",
ncols=self.hdr['naxis1'],
nlines=self.hdr['naxis2'],
header="",
background=0.0,
objects=galfile,
xoffset=0.,
yoffset=0.,
star="gaussian",
radius=0.1,
beta=2.5,
ar=1.,
pa=0.,
distance=1.,
exptime=1.,
magzero=magz,
gain=gain,
rdnoise=0.,
poisson=0,
seed=2,
comments=1)
imhconvolve(outfile, psffile, outfile, overwrite=True)
self.noiseless = outfile
def completeness():#measure completeness on final image
#combinepath=bcdpath+'pbcd/Combine/output_apex_step2'
combinepath=bcdpath+'pbcd/Combine/apex_1frame_step2'
os.chdir(combinepath)
file='mosaic_extract_final.tbl'
input=open(file,'r')
xgal=[]#positions of previous detections with snr > 3
ygal=[]
fap4gal=[]
for line in input:
if line.find('#') > -1: #skip lines with '#' in them
continue
if line.find('\\') > -1: #skip lines with '#' in them
continue
if line.find('|') > -1: #skip lines with '#' in them
continue
t=line.split()
xgal.append(float(t[8]))
ygal.append(float(t[10]))
fap4gal.append(float(t[28]))
input.close()
xgal=N.array(xgal,'f')
ygal=N.array(ygal,'f')
fsimall=[]
matchflagsimall=[]
f2all=[]
f3all=[]
f4all=[]
deblendsimall=[]
snrsimall=[]
myminmag=24.75
mymaxmag=27.4
myfmin=10.**((25.-mymaxmag)/2.5)#ZP=25
myfmax=10.**((25.-myminmag)/2.5)#ZP=25
#below is loop to create image w/artificial sources, extract, and compare
for k in range(100):
createflag=1.#create image w/artificial sources?
detectflag=1.#detect sources in image?
if createflag > 0.1:
xnoise=[]
ynoise=[]
infile=open('noisecoords.dat','r')
for line in infile:
t=line.split()
xnoise.append(float(t[0]))
ynoise.append(float(t[1]))
infile.close()
nstar=10
xsim=N.zeros(nstar,'d')
ysim=N.zeros(nstar,'d')
msim=N.zeros(nstar,'d')
outfile=open('stars.coords.dat','w')
for i in range(nstar):
#j=int(round(1.*len(xnoise)*random.uniform(0,1)))
#xsim[i]=xnoise[j]
#ysim[i]=ynoise[j]
j=0
for j in range(10000):
xt=int(round(random.uniform(5.,125.)))
yt=int(round(random.uniform(5.,140.)))
d=pylab.sqrt((xt-xgal)**2+(yt-ygal)**2)#make sure sim galaxies are not near real galaxies
if min(d) > -1.:
d2=pylab.sqrt((xt-xsim)**2+(yt-ysim)**2)#make sure sim points are not on top of each other
if min(d2) > 5.:
print i,'got a good point after ',j,' tries',xt,yt
break
j=j+1
xsim[i]=xt
ysim[i]=yt
k=random.uniform(myfmin,myfmax)
msim[i]=25.-2.5*pylab.log10(k)
#print k,msim[i]
s='%8.2f %8.2f %8.2f \n' % (xsim[i],ysim[i],msim[i])
outfile.write(s)
outfile.close()
#os.system('rm stars.coords.dat')
#iraf.starlist('stars.coords.dat',nstars=100,spatial='uniform',xmax=130,ymax=145,luminosity='uniform',minmag=22.,maxmag=30.0,mzero=22.0,sseed='INDEF',power=0.6,alpha=0.74,lseed='INDEF')
os.system('rm mosaic-completeness.fits')
#iraf.mkobjects(input='mosaic_minus_median_extract.fits',output='mosaic-completeness.fits',objects='stars.coords.dat',radius=1.13,magzero=25.,background=0.,gain=5.,rdnoise=0.,poisson='no')#don't convolve w/PRF
#os.system('cp ../cal/MIPS24_PRF_HD_center.fits .')#convolve star w/SSC PRF
os.system('cp ../cal/mips24_prf_mosaic_2.45_4x.fits .')#convolve star w/SSC PRF
iraf.mkobjects(input='mosaic_minus_median_extract.fits',output='mosaic-completeness.fits',objects='stars.coords.dat',radius=14,star='mips24_prf_mosaic_2.45_4x.fits',magzero=25.,background=0.,gain=5.,rdnoise=0.,poisson='no')
#os.system('cp ../cal/PRF_estimate.fits .')#convolve gaussian w/measured PRF
#iraf.mkobjects(input='mosaic_minus_median_extract.fits',output='mosaic-completeness.fits',objects='stars.coords.dat',radius=15,star='PRF_estimate.fits',magzero=25.,background=0.,gain=5.,rdnoise=0.,poisson='no')
os.system('ls *.fits')
os.system('pwd')
iraf.display('mosaic_minus_median_extract.fits',1,contrast=0.01)
iraf.display('mosaic-completeness.fits',2,contrast=0.01)
iraf.tvmark(1,'stars.coords.dat')
iraf.tvmark(2,'stars.coords.dat')
fsim=10.**((25.-msim)/2.5)#ZP=25
if createflag < .1:#read in positions and magnitudes of artdata sources
xsim=[]
ysim=[]
msim=[]
infile=open('stars.coords.dat','r')
for line in infile:
if line.find('#') > -1:
continue
t=line.split()
xsim.append(float(t[0]))
ysim.append(float(t[1]))
msim.append(float(t[2]))
infile.close()
xsim=N.array(xsim,'f')
ysim=N.array(ysim,'f')
msim=N.array(msim,'f')
fsim=10.**((25.-msim)/2.5)#ZP=25
if detectflag > 0.1:#now run detection on mosaic-completeness.fits
combinepath=bcdpath+'pbcd/Combine/'
os.chdir(combinepath)
print combinepath
#os.system('apex_1frame.pl -n apex_1frame_MIPS24_step2.nl -i output_apex_step2/mosaic-completeness.fits')
#combinepath=bcdpath+'pbcd/Combine/output_apex_step2'
os.system('apex_1frame.pl -n apex_1frame_step2all.nl -i apex_1frame_step2/mosaic-completeness.fits')
combinepath=bcdpath+'pbcd/Combine/apex_1frame_step2'
os.chdir(combinepath)
print combinepath
file='mosaic-completeness_extract_raw.tbl'
input=open(file,'r')
ngal=0
for line in input:
if line.find('Conversion') > -1:
t=line.split('=')
convfactor=float(t[1])#conversion from ADU to uJy
#aperr=aveaperr*convfactor #convert noise in ADU to uJy using conv factor from apex
print "Conversion Factor = ",convfactor
#print "aveaperr = ",aveaperr
#print "aperr = ",aperr
continue
if line.find('#') > -1: #skip lines with '#' in them
continue
if line.find('\\') > -1: #skip lines with '#' in them
continue
if line.find('|') > -1: #skip lines with '#' in them
continue
ngal=ngal+1
input.close()
id24 = N.zeros(ngal,'f')
imagex24 = N.zeros(ngal,'f')
imagey24 = N.zeros(ngal,'f')
ra24 = N.zeros(ngal,'f')
dec24 = N.zeros(ngal,'f')
f24 = N.zeros(ngal,'d')#flux
errf24 = N.zeros(ngal,'d')
fap1 = N.zeros(ngal,'d')#flux in aperture 1 (1,1.5,2,2.6,3,3.5,4,4.5,5.,5.5) pixels
fap2 = N.zeros(ngal,'d')#flux
fap3 = N.zeros(ngal,'d')#flux
fap4 = N.zeros(ngal,'d')#flux in ap 4 - this is one w/ap cor of 1.67 (Calzetti et al 2007)
fap5 = N.zeros(ngal,'d')#flux
fap6 = N.zeros(ngal,'d')#flux
fap7 = N.zeros(ngal,'d')#flux
fap8 = N.zeros(ngal,'d')#flux
fap9 = N.zeros(ngal,'d')#flux
fap10 = N.zeros(ngal,'d')#flux
snr24 = N.zeros(ngal,'d')#SNR calculated by mopex
deblend = N.zeros(ngal,'f')#SNR calculated by mopex
input=open(file,'r')
i=0
output=open('xy24raw.dat','w')
for line in input:
if line.find('#') > -1: #skip lines with '#' in them
continue
if line.find('\\') > -1: #skip lines with '#' in them
continue
if line.find('|') > -1: #skip lines with '#' in them
continue
t=line.split()
#print "length of t = ",len(t)
#print (t[8]),(t[10]),(t[13]),(t[14]),(t[18]),(t[2]),(t[23]),(t[24]),(t[25]),(t[26]),(t[27]),(t[28]),(t[29]),(t[30]),(t[31]),(t[32])
(imagex24[i],imagey24[i],f24[i],errf24[i],snr24[i],deblend[i],fap1[i],fap2[i],fap3[i],fap4[i],fap5[i],fap6[i],fap7[i],fap8[i],fap9[i],fap10[i])=(float(t[8]),float(t[10]),float(t[13]),float(t[14]),float(t[18]),float(t[2]),float(t[25]),float(t[26]),float(t[27]),float(t[28]),float(t[29]),float(t[30]),float(t[31]),float(t[32]),float(t[33]),float(t[34]))
s='%6.2f %6.2f \n'%(imagex24[i],imagey24[i])
output.write(s)
i=i+1
input.close()#44 -> 43
output.close()
iraf.tvmark(1,'xy24raw.dat',color=204,radi=2)
iraf.tvmark(2,'xy24raw.dat',color=204,radi=2)
delta=1.#max number of pixels for a match
#get rid of objects that were detected in original image. Otherwise, matching will think any object near a sim galaxy is the sim galaxy. A faint galaxy placed on type of a pre-existing bright galaxy will be detected.
newgalflag=N.ones(len(imagex24),'i')
for i in range(len(imagex24)):
(imatch, matchflag,nmatch)=findnearest(imagex24[i],imagey24[i],xgal,ygal,delta)
if matchflag > 0.:
dflux=abs(fap4gal[imatch] - fap4[i])/fap4[i]
if dflux < .1:#position of real galaxy, flux difference less than 10% -> not a new galaxy
newgalflag[i] = 0
#keep only galaxies that are new
imagex24 = N.compress(newgalflag,imagex24)
imagey24 = N.compress(newgalflag,imagey24)
fap1 = N.compress(newgalflag,fap1)
fap2 = N.compress(newgalflag,fap2)
fap3 = N.compress(newgalflag,fap3)
fap4 = N.compress(newgalflag,fap4)
fap5 = N.compress(newgalflag,fap5)
fap6 = N.compress(newgalflag,fap6)
fap7 = N.compress(newgalflag,fap7)
fap8 = N.compress(newgalflag,fap8)
fap9 = N.compress(newgalflag,fap9)
fap10 =N.compress(newgalflag,fap10)
snr24 =N.compress(newgalflag,snr24)
deblend = N.compress(newgalflag,deblend)
delta=2.#max number of pixels for a match
matchflagsim=N.zeros(len(xsim),'i')
fmeas1=N.zeros(len(xsim),'f')
fmeas2=N.zeros(len(xsim),'f')
fmeas3=N.zeros(len(xsim),'f')
fmeas4=N.zeros(len(xsim),'f')
fmeas5=N.zeros(len(xsim),'f')
fmeas6=N.zeros(len(xsim),'f')
fmeas7=N.zeros(len(xsim),'f')
fmeas8=N.zeros(len(xsim),'f')
fmeas9=N.zeros(len(xsim),'f')
fmeas10=N.zeros(len(xsim),'f')
fmeas24=N.zeros(len(xsim),'f')
deblendsim=N.zeros(len(xsim),'f')
snrsim=N.zeros(len(xsim),'f')
for i in range(len(xsim)):
(imatch, matchflag,nmatch)=findnearest(xsim[i],ysim[i],imagex24,imagey24,delta)
matchflagsim[i]=matchflag
if matchflag > .1:
fmeas1[i]=fap1[int(imatch)]
fmeas2[i]=fap2[int(imatch)]
fmeas3[i]=fap3[int(imatch)]
fmeas4[i]=fap4[int(imatch)]
fmeas5[i]=fap5[int(imatch)]
fmeas6[i]=fap6[int(imatch)]
fmeas7[i]=fap7[int(imatch)]
fmeas8[i]=fap8[int(imatch)]
fmeas9[i]=fap9[int(imatch)]
fmeas10[i]=fap10[int(imatch)]
fmeas24[i]=f24[int(imatch)]
deblendsim[i]=deblend[int(imatch)]
snrsim[i]=snr24[int(imatch)]
fsimall=fsimall+list(fsim)
matchflagsimall=matchflagsimall+list(matchflagsim)
f2all=f2all+list(fmeas2)
f3all=f3all+list(fmeas3)
f4all=f4all+list(fmeas4)
deblendsimall=deblendsimall+list(deblendsim)
snrsimall=snrsimall+list(snrsim)
fsim=N.array(fsimall,'f')
matchflagsim=N.array(matchflagsimall,'f')
fmeas2=N.array(f2all,'f')
fmeas3=N.array(f3all,'f')
fmeas4=N.array(f4all,'f')
deblendsim=N.array(deblendsimall,'f')
snrsim=N.array(snrsimall,'f')
#make plots using all realizations
pylab.cla()
pylab.clf()
fsim=fsim*convfactor
fs=pylab.compress((matchflagsim > 0.1) & (deblendsim < 1.5),fsim)
#f1=pylab.compress((matchflagsim > 0.1) & (deblendsim < 1.5),fmeas1)
f2=pylab.compress((matchflagsim > 0.1) & (deblendsim < 1.5),fmeas2)
f3=pylab.compress((matchflagsim > 0.1) & (deblendsim < 1.5),fmeas3)
f4=pylab.compress((matchflagsim > 0.1) & (deblendsim < 1.5),fmeas4)
#f242=pylab.compress((matchflagsim > 0.1) & (deblendsim < 1.5),fmeas24)
r4=pylab.median(fs/f4)
r3=pylab.median(fs/f3)
r2=pylab.median(fs/f2)
print "average ratios ap 4",pylab.average(fs/f4),r4,pylab.std((fs/f4)/pylab.average(fs/f2))
print "average ratios ap 3",pylab.average(fs/f3),pylab.median(fs/f3),pylab.std((fs/f3)/pylab.average(fs/f3))
print "average ratios ap 2",pylab.average(fs/f2),pylab.median(fs/f2),pylab.std((fs/f2)/pylab.average(fs/f2))
s='f4 w/apcor = %3.2f(%4.2f)'%(r4,pylab.average(abs(fs-f4*r4)/fs))
pylab.plot(fs,f4*r4,'b.',label=s)
pylab.plot(fs,f4,'bo',label='f4')
s='f3 w/apcor = %3.2f(%4.2f)'%(r3,pylab.average(abs(fs-f3*r3)/fs))
pylab.plot(fs,f3*r3,'g.',label=s)
pylab.plot(fs,f3,'go',label='f3')
s='f2 w/apcor = %3.2f(%4.2f)'%(r2,pylab.average(abs(fs-f2*r2)/fs))
pylab.plot(fs,f2*r2,'r.',label=s)
pylab.plot(fs,f2,'ro',label='f2')
#pylab.plot(fs,f1,'co',label='f1')
#pylab.plot(fs,f242,'k.',label='f24')
pylab.legend(loc='best')
x=N.arange(0.,max(fs),10.)
y=x
pylab.plot(x,y,'k-')
#y=2.*x
#pylab.plot(x,y,'k--')
#y=3.*x
#pylab.plot(x,y,'k--')
#y=4.*x
#pylab.plot(x,y,'k--')
#y=5.*x
#pylab.plot(x,y,'k--')
pylab.xlabel('F(24) Input')
pylab.ylabel('F(24) measured')
#pylab.axis([0.,50.,0.,50.])
s=str(prefix)+'fluxcomp.eps'
pylab.savefig(s)
pylab.cla()
pylab.clf()
nbins=20
fmin=10.#min(fsim)
fmax=max(fsim)
df=5.#(fmax-fmin)/(1.*nbins)
bins=N.arange(fmin,(fmax+df),df)
(xbin,ybin,ybinerr)=mystuff.completeness(bins,fsim,matchflagsim)
s=str(prefix)+'FracComplvsFlux.dat'
outdat=open(s,'w')
print "Completeness vs Input Flux"
for i in range(len(xbin)):
print i, xbin[i],ybin[i],ybinerr[i]
t='%8.2f %8.4f %8.4f\n'%(xbin[i],ybin[i],ybinerr[i])
outdat.write(t)
outdat.close()
#for i in range(len(fsim)):
#if snrsim[i] > 3.:
# print i, fsim[i],matchflagsim[i],deblendsim[i],abs(fsim[i]-fmeas4[i]*1.67)/fsim[i],snrsim[i]
#(xbin,ybin2,ybin2err)=mystuff.scipyhist2(bins,fmeas4)
#pylab.plot(xbin,ybin,'bo')
#pylab.plot(xbin,ybin2,'ro')
#s=str(prefix)+'NDetectvsFlux.eps'
#pylab.savefig(s)
pylab.cla()
pylab.clf()
pylab.plot(xbin,ybin,'ko')
pylab.errorbar(xbin,ybin,yerr=ybinerr,fmt=None,ecolor='k')
s=str(prefix)+'FracComplvsFlux.eps'
pylab.axhline(y=1.0,ls='-')
pylab.axhline(y=.8,ls='--')
pylab.axvline(x=80.0,ls=':',color='b')
pylab.xlabel('Input Flux (uJy)')
pylab.ylabel('Completeness')
pylab.axis([0.,max(xbin)+df,-.05,1.05])
pylab.savefig(s)
os.system('cp *.eps /Users/rfinn/clusters/spitzer/completeness/.')
os.system('cp *vsFlux.dat /Users/rfinn/clusters/spitzer/completeness/.')
