def getSpecNorms(self, sedfile, mag, filtstr):
band = Bandpass()
band.readThroughput(os.path.join(self.tpath, "total_%s.dat"%(filtstr)))
imsimband = Bandpass()
imsimband.imsimBandpass()
sed = Sed()
sed.readSED_flambda(self.spath+"/"+sedfile)
fluxNorm = sed.calcFluxNorm(mag, band)
sed.multiplyFluxNorm(fluxNorm)
magNorm = sed.calcMag(imsimband)
return magNorm, fluxNorm
def calcLSSTMags(self, sedfile, fluxnorm):
sed = Sed()
sed.readSED_flambda(self.spath+"/"+sedfile)
sed.multiplyFluxNorm(fluxnorm)
mags = []
for filtstr in ('u', 'g', 'r', 'i', 'z', 'y'):
band = Bandpass()
band.readThroughput(os.path.join(self.tpath, "total_%s.dat"%(filtstr)))
imsimband = Bandpass()
imsimband.imsimBandpass()
mags.append(sed.calcMag(band))
return mags
def getSpecNorms(self, sedfile, mag, filtstr):
band = Bandpass()
band.readThroughput(
os.path.join(self.tpath, "total_%s.dat" % (filtstr)))
imsimband = Bandpass()
imsimband.imsimBandpass()
sed = Sed()
sed.readSED_flambda(self.spath + "/" + sedfile)
fluxNorm = sed.calcFluxNorm(mag, band)
sed.multiplyFluxNorm(fluxNorm)
magNorm = sed.calcMag(imsimband)
return magNorm, fluxNorm
def calcLSSTMags(self, sedfile, fluxnorm):
sed = Sed()
sed.readSED_flambda(self.spath + "/" + sedfile)
sed.multiplyFluxNorm(fluxnorm)
mags = []
for filtstr in ('u', 'g', 'r', 'i', 'z', 'y'):
band = Bandpass()
band.readThroughput(
os.path.join(self.tpath, "total_%s.dat" % (filtstr)))
imsimband = Bandpass()
imsimband.imsimBandpass()
mags.append(sed.calcMag(band))
return mags
def mkGalPhot(self):
ifh = open(self.mfile)
lnum = 0
k = None
for l in ifh:
flds = l.rstrip().split()
if l.startswith("Opsim_filter"):
self.filter = self.filtmap[int(flds[1])]
k = self.filter
ifh.close()
ifh = open(self.tfile)
for l in ifh:
flds = l.rstrip().split()
if not flds[0] == "object":
continue
otype = flds[12]
if otype != "sersic2D":
continue
id = float(flds[1])
if not self.centdata.has_key(id):
continue
magNorm = float(flds[4])
spec = flds[5]
redshift = float(flds[6])
ind = float(flds[16])
mwav = float(flds[21])
av = float(flds[18])
sed = Sed()
sed.readSED_flambda(self.spath+"/"+spec)
a_int, b_int = sed.setupCCMab()
self.outdata['id'].append(id)
if lnum > self.donum and self.donum is not None:
break
if lnum%10000 == 0:
print id
fluxNorm = sed.calcFluxNorm(magNorm, self.imsimband)
sed.multiplyFluxNorm(fluxNorm/(1+redshift))
sed.addCCMDust(a_int, b_int, A_v=av)
sed.redshiftSED(redshift, dimming=False)
a_mw, b_mw = sed.setupCCMab()
sed.addCCMDust(a_mw, b_mw, A_v=mwav)
line = {'flux':None, 'mag':None}
mag = sed.calcMag(self.bands[k])
flux = sed.calcADU(self.bands[k], gain=1.0)
line['mag'] = mag
line['flux'] = flux
self.outdata[k].append(line)
lnum += 1
ifh.close()
def calcAbsMag(self, mag, D_L, spec, redshift, filter='i'): """Calculate an absolute magnitude given a filter, luminosity distance, apparent magnitude, sed, and redshift """ #Get default locations for filters and seds #Set up filters and sed imsimband = Bandpass() imsimband.imsimBandpass() sed = Sed() sed.readSED_flambda(os.path.join(self.spath,spec)) #Calculate rest frame magnitude magr = sed.calcMag(self.bands[filter]) #redshift spectrum sed.redshiftSED(redshift, dimming=False) #calculate observed frame magnitude mago = sed.calcMag(self.bands[filter]) #SED portion of the K-correction Kcorr = mago-magr #Cosmological portion of the K-correction due to the dilation of the #filter Kcorrz = 2.5*numpy.log10(1+redshift) #D_L is in Mpc so the normal relation goes 5.(log(D_L) +6.-1.) absMag = mag - (5.*(numpy.log10(D_L) + 5.)) - Kcorr - Kcorrz return absMag
def calcAbsMag(self, mag, D_L, spec, redshift, filter='i'):
"""Calculate an absolute magnitude given a filter, luminosity distance,
apparent magnitude, sed, and redshift
"""
#Get default locations for filters and seds
#Set up filters and sed
imsimband = Bandpass()
imsimband.imsimBandpass()
sed = Sed()
sed.readSED_flambda(os.path.join(self.spath, spec))
#Calculate rest frame magnitude
magr = sed.calcMag(self.bands[filter])
#redshift spectrum
sed.redshiftSED(redshift, dimming=False)
#calculate observed frame magnitude
mago = sed.calcMag(self.bands[filter])
#SED portion of the K-correction
Kcorr = mago - magr
#Cosmological portion of the K-correction due to the dilation of the
#filter
Kcorrz = 2.5 * numpy.log10(1 + redshift)
#D_L is in Mpc so the normal relation goes 5.(log(D_L) +6.-1.)
absMag = mag - (5. * (numpy.log10(D_L) + 5.)) - Kcorr - Kcorrz
return absMag
def mkStarPhot(self):
ifh = open(self.mfile)
lnum = 0
k = None
for l in ifh:
flds = l.rstrip().split()
if l.startswith("Opsim_filter"):
self.filter = self.filtmap[int(flds[1])]
k = self.filter
ifh.close()
ifh = open(self.tfile)
for l in ifh:
flds = l.rstrip().split()
if not flds[0] == "object":
continue
otype = flds[12]
if otype != "point":
continue
id = float(flds[1])
if not self.centdata.has_key(id):
continue
magNorm = float(flds[4])
spec = flds[5]
av = float(flds[14])
sed = Sed()
self.outdata['id'].append(id)
if re.search("kurucz", spec):
sed.readSED_flambda(self.spath+"/"+spec)
else:
sed.readSED_flambda(self.spath+"/"+spec)
fluxNorm = sed.calcFluxNorm(magNorm, self.imsimband)
sed.multiplyFluxNorm(fluxNorm)
a, b = sed.setupCCMab()
sed.addCCMDust(a, b, A_v=av)
line = {'flux':None, 'mag':None}
mag = sed.calcMag(self.bands[k])
flux = sed.calcADU(self.bands[k], gain=1.)
line['mag'] = mag
line['flux'] = flux
self.outdata[k].append(line)
lnum += 1
ifh.close()
