def testMags(self):
"""
Test that the interpolated mags are similar to mags computed from interpolated spectra
"""
throughPath = os.path.join(getPackageDir('throughputs'), 'baseline')
filters = ['u', 'g', 'r', 'i', 'z', 'y']
bps = []
for filterName in filters:
bp = np.loadtxt(os.path.join(throughPath, 'filter_%s.dat' % filterName),
dtype=zip(['wave', 'trans'], [float]*2))
lsst_bp = Bandpass()
lsst_bp.setBandpass(bp['wave'], bp['trans'])
bps.append(lsst_bp)
sm1 = self.sm_spec
sm1.setRaDecMjd([36.], [-68.], 49353.18, degrees=True)
mags1 = []
for bp in bps:
mags1.append(sm1.returnMags(bandpass=bp))
mags1 = np.array(mags1)
sm2 = self.sm_mags
sm2.setRaDecMjd([36.], [-68.], 49353.18, degrees=True)
mag2 = sm2.returnMags()
for i, filtername in enumerate(filters):
np.testing.assert_allclose(mags1[i, :], mag2[filtername], rtol=1e-4)
def testMags(self):
"""
Test that the interpolated mags are similar to mags computed from interpolated spectra
"""
throughPath = os.path.join(getPackageDir('throughputs'),'baseline')
filters = ['u','g','r','i','z','y']
bps = []
for filterName in filters:
bp = np.loadtxt(os.path.join(throughPath, 'filter_%s.dat' % filterName),
dtype=zip(['wave','trans'],[float]*2 ))
lsst_bp = Bandpass()
lsst_bp.setBandpass(bp['wave'], bp['trans'])
bps.append(lsst_bp)
sm1 = sb.SkyModel()
sm1.setRaDecMjd([36.],[-68.],49353.18, degrees=True)
sm1.computeSpec()
mags1 = []
for bp in bps:
mags1.append(sm1.computeMags(bandpass=bp))
mags1 = np.array(mags1)
sm2 = sb.SkyModel(mags=True)
sm2.setRaDecMjd([36.],[-68.],49353.18, degrees=True)
sm2.computeSpec()
mag2 = sm2.computeMags()
np.testing.assert_allclose(mags1,mag2.T, rtol=1e-4)
def buildVendorDetector(vendorDir, addLosses=True):
"""
Builds a detector response from the files in vendorDir, by reading the *_QE.dat
and *_Losses subdirectory for a single version of the detector.
Returns a Bandpass object.
If addLosses is True, the QE curve is multiplied by the losses in the *Losses.dat files.
If addLosses is False, the QE curve does not have any losses included.
"""
# Read the QE file.
qefile = glob(os.path.join(vendorDir, '*_QE.dat'))
if len(qefile) != 1:
raise ValueError('Expected a single QE file in this directory, found: ', qefile)
qefile = qefile[0]
qe = Bandpass()
qe.readThroughput(qefile)
if addLosses:
loss = _readLosses(vendorDir)
wavelength, sb = qe.multiplyThroughputs(loss.wavelen, loss.sb)
qe.setBandpass(wavelength, sb)
# Verify that no values go significantly below zero.
belowzero = np.where(qe.sb < 0)
# If there are QE values significantly < 0, raise an exception.
if qe.sb[belowzero] < belowZeroThreshhold:
raise ValueError('Found values in QE response significantly below zero.')
# If they are just small errors in interpolation, set to zero.
qe.sb[belowzero] = 0
return qe
def __init__(self, m5Col='fiveSigmaDepth', metricName='ExgalM5', units='mag',
lsstFilter='r', wavelen_min=None , wavelen_max=None , **kwargs):
# Set the name for the dust map to use. This is gathered into the MetricBundle.
maps = ['DustMap']
# Set the default wavelength limits for the lsst filters. These are approximately correct.
waveMins = {'u':330.,'g':403.,'r':552.,'i':691.,'z':818.,'y':950.}
waveMaxes = {'u':403.,'g':552.,'r':691.,'i':818.,'z':922.,'y':1070.}
if lsstFilter is not None:
wavelen_min = waveMins[lsstFilter]
wavelen_max = waveMaxes[lsstFilter]
self.m5Col = m5Col
super().__init__(col=[self.m5Col], maps=maps, metricName=metricName, units=units, **kwargs)
# Set up internal values for the dust extinction.
testsed = Sed()
testsed.setFlatSED(wavelen_min=wavelen_min, wavelen_max=wavelen_max, wavelen_step=1.0)
testbandpass = Bandpass(wavelen_min=wavelen_min, wavelen_max=wavelen_max, wavelen_step=1.0)
testbandpass.setBandpass(wavelen=testsed.wavelen,
sb=np.ones(len(testsed.wavelen)))
self.R_v = 3.1
self.ref_ebv = 1.0
# Calculate non-dust-extincted magnitude
flatmag = testsed.calcMag(testbandpass)
# Add dust
self.a, self.b = testsed.setupCCM_ab()
testsed.addDust(self.a, self.b, ebv=self.ref_ebv, R_v=self.R_v)
# Calculate difference due to dust when EBV=1.0 (m_dust = m_nodust - Ax, Ax > 0)
self.Ax1 = testsed.calcMag(testbandpass) - flatmag
# We will call Coaddm5Metric to calculate the coadded depth. Set it up here.
self.Coaddm5Metric = Coaddm5Metric(m5Col=m5Col)
def buildMirror(mirrorDir, addLosses=True):
"""
Build a mirror throughput curve.
Assumes there are *Losses.dat subdirectory with loss files
and a m*_Ideal.dat file with the mirror throughput.
Returns a bandpass object.
If addLosses is True, the *_Ideal.dat file is multiplied by the *_Losses/*.dat files.
"""
# Read the mirror reflectance curve.
mirrorfile = glob(os.path.join(mirrorDir, 'm*Ideal.dat'))
if len(mirrorfile) != 1:
raise ValueError('Expected a single mirror file in directory %s, found: ' %mirrorDir, mirrorfile)
mirrorfile = mirrorfile[0]
mirror = Bandpass()
mirror.readThroughput(mirrorfile)
if addLosses:
loss = _readLosses(mirrorDir)
wavelen, sb = mirror.multiplyThroughputs(loss.wavelen, loss.sb)
mirror.setBandpass(wavelen, sb)
# Verify that no values go significantly below zero.
belowzero = np.where(mirror.sb < 0)
# If there are QE values significantly < 0, raise an exception.
if mirror.sb[belowzero] < belowZeroThreshhold:
raise ValueError('Found values in mirror response significantly below zero')
# If they are just small errors in interpolation, set to zero.
mirror.sb[belowzero] = 0
return mirror
def testMags(self):
"""
Test that the interpolated mags are similar to mags computed from interpolated spectra
"""
throughPath = os.path.join(getPackageDir('throughputs'), 'baseline')
filters = ['u', 'g', 'r', 'i', 'z', 'y']
bps = {}
for filterName in filters:
bp = np.loadtxt(os.path.join(throughPath,
'filter_%s.dat' % filterName),
dtype=list(zip(['wave', 'trans'], [float] * 2)))
lsst_bp = Bandpass()
lsst_bp.setBandpass(bp['wave'], bp['trans'])
bps[filterName] = lsst_bp
sm1 = self.sm_spec
sm1.setRaDecMjd([36.], [-68.], 49353.18, degrees=True)
mags1 = sm1.returnMags(bandpasses=bps)
sm2 = self.sm_mags
sm2.setRaDecMjd([36.], [-68.], 49353.18, degrees=True)
mag2 = sm2.returnMags()
for i, filtername in enumerate(filters):
np.testing.assert_allclose(mags1[filtername],
mag2[filtername],
rtol=1e-4)
def importBandpass(filename, name):
'''Given the name of a bandpass read it from file into Bandpass class
assumes filters are differentiated by #NAME filter_name filter comments'''
filter = Bandpass()
data = []
with open(filename, 'r') as input:
for line in input:
line = line.strip().split()
if (line[0].startswith("#NAME") and (line[1] == name)):
for line in input:
if line.startswith("#NAME"):
break
else:
data.append(map(float, line.split()))
data = np.asarray(data).T
# convert to nanometers and set limits for wavelength
filter.setWavelenLimits(data[0].min() / 10., data[0].max() / 10., 1.)
try:
filter.setBandpass(data[0] / 10., data[1])
except IndexError:
print "Unable to find data values for ", name
exit()
#resample to
filter.resampleBandpass(wavelen_min=300.0,
wavelen_max=1150.0,
wavelen_step=0.1)
return filter
def buildVendorDetector(vendorDir, addLosses=True):
"""
Builds a detector response from the files in vendorDir, by reading the *_QE.dat
and *_Losses subdirectory for a single version of the detector.
Returns a Bandpass object.
If addLosses is True, the QE curve is multiplied by the losses in the *Losses.dat files.
If addLosses is False, the QE curve does not have any losses included.
"""
# Read the QE file.
qefile = glob(os.path.join(vendorDir, '*_QE.dat'))
if len(qefile) != 1:
raise ValueError('Expected a single QE file in this directory, found: ', qefile)
qefile = qefile[0]
qe = Bandpass()
qe.readThroughput(qefile)
if addLosses:
loss = _readLosses(vendorDir)
wavelength, sb = qe.multiplyThroughputs(loss.wavelen, loss.sb)
qe.setBandpass(wavelength, sb)
# Verify that no values go significantly below zero.
belowzero = np.where(qe.sb < 0)
# If there are QE values significantly < 0, raise an exception.
if qe.sb[belowzero] < belowZeroThreshhold:
raise ValueError('Found values in QE response significantly below zero.')
# If they are just small errors in interpolation, set to zero.
qe.sb[belowzero] = 0
return qe
def buildMirror(mirrorDir, addLosses=True):
"""
Build a mirror throughput curve.
Assumes there are *Losses.dat subdirectory with loss files
and a m*_Ideal.dat file with the mirror throughput.
Returns a bandpass object.
If addLosses is True, the *_Ideal.dat file is multiplied by the *_Losses/*.dat files.
"""
# Read the mirror reflectance curve.
mirrorfile = glob(os.path.join(mirrorDir, 'm*Ideal.dat'))
if len(mirrorfile) != 1:
raise ValueError('Expected a single mirror file in directory %s, found: ' %mirrorDir, mirrorfile)
mirrorfile = mirrorfile[0]
mirror = Bandpass()
mirror.readThroughput(mirrorfile)
if addLosses:
loss = _readLosses(mirrorDir)
wavelen, sb = mirror.multiplyThroughputs(loss.wavelen, loss.sb)
mirror.setBandpass(wavelen, sb)
# Verify that no values go significantly below zero.
belowzero = np.where(mirror.sb < 0)
# If there are QE values significantly < 0, raise an exception.
if mirror.sb[belowzero] < belowZeroThreshhold:
raise ValueError('Found values in mirror response significantly below zero')
# If they are just small errors in interpolation, set to zero.
mirror.sb[belowzero] = 0
return mirror
def testMags(self):
"""
Test that the interpolated mags are similar to mags computed from interpolated spectra
"""
throughPath = os.path.join(getPackageDir("throughputs"), "baseline")
filters = ["u", "g", "r", "i", "z", "y"]
bps = []
for filterName in filters:
bp = np.loadtxt(
os.path.join(throughPath, "filter_%s.dat" % filterName), dtype=zip(["wave", "trans"], [float] * 2)
)
lsst_bp = Bandpass()
lsst_bp.setBandpass(bp["wave"], bp["trans"])
bps.append(lsst_bp)
sm1 = sb.SkyModel()
sm1.setRaDecMjd([36.0], [-68.0], 49353.18, degrees=True)
sm1.computeSpec()
mags1 = []
for bp in bps:
mags1.append(sm1.computeMags(bandpass=bp))
mags1 = np.array(mags1)
sm2 = sb.SkyModel(mags=True)
sm2.setRaDecMjd([36.0], [-68.0], 49353.18, degrees=True)
sm2.computeSpec()
mag2 = sm2.computeMags()
np.testing.assert_allclose(mags1, mag2.T, rtol=1e-4)
def lsst_filters():
throughPath = os.path.join(getPackageDir('throughputs'), 'baseline')
lsstKeys = ['u', 'g', 'r', 'i', 'z', 'y']
bps = {}
for key in lsstKeys:
bp = np.loadtxt(os.path.join(throughPath, 'total_'+key+'.dat'),
dtype=zip(['wave', 'trans'], [float]*2))
bpTemp = Bandpass()
good = np.where(bp['trans'] > 0.)
bpTemp.setBandpass(bp['wave'], bp['trans'], wavelen_min=bp['wave'][good].min(),
wavelen_max=bp['wave'][good].max())
bps[key] = bpTemp
return bps
def addAerosol(atmosphere, X, tau0=0.05, alpha=1.0, wavelen0=440.0, plotAtmosphere=True):
# Calculate the aerosol contribution -- sb with aerosols = sb*exp(-tau)
tau = tau0 * np.power((wavelen0/atmosphere.wavelen), alpha)
# Generate new atmosphere bandpass with aerosols.
atmosphere_aerosol = Bandpass()
atmosphere_aerosol.setBandpass(wavelen = atmosphere.wavelen,
sb = atmosphere.sb * np.exp(-tau*X))
if plotAtmosphere:
# Plot for a check:
atmodict = {'Original atmosphere':atmosphere,
'With aerosols': atmosphere_aerosol}
bu.plotBandpasses(atmodict)
return atmosphere_aerosol
def stubb_fitlers(wave_min=350., wave_max=1050):
"""
Define some narrow filters that overlap LSST u and y, and are in GAIA overlap.
"""
throughPath = os.path.join(getPackageDir('throughputs'), 'baseline')
bps = {}
lsstKeys = ['u', 'y']
bps = {}
for key in lsstKeys:
bp = np.loadtxt(os.path.join(throughPath, 'total_'+key+'.dat'),
dtype=zip(['wave', 'trans'], [float]*2))
bpTemp = Bandpass()
good = np.where((bp['trans'] > 0.) & (bp['wave'] > wave_min) & (bp['wave'] < wave_max))
bpTemp.setBandpass(bp['wave'], bp['trans'], wavelen_min=bp['wave'][good].min(),
wavelen_max=bp['wave'][good].max())
bps[key+'_truncated'] = bpTemp
return bps
def calcWDColors():
"""
Calculate a few example WD colors. Values to go in stellarMags(). Here in case
values need to be regenerated (different stars, bandpasses change, etc.)
"""
try:
from lsst.utils import getPackageDir
import os
from lsst.sims.photUtils import Bandpass, Sed
except:
'Need to setup sims_photUtils to generate WD magnitudes.'
names = ['HeWD_25200_80', 'WD_11000_85', 'WD_3000_85']
fns = [
'bergeron_He_24000_80.dat_25200.gz', 'bergeron_10500_85.dat_11000.gz',
'bergeron_2750_85.dat_3000.gz'
]
wdDir = os.path.join(getPackageDir('sims_sed_library'), 'starSED/wDs/')
files = [os.path.join(wdDir, filename) for filename in fns]
# Read in the LSST bandpasses
bpNames = ['u', 'g', 'r', 'i', 'z', 'y']
bps = []
throughPath = os.path.join(getPackageDir('throughputs'), 'baseline')
for key in bpNames:
bp = np.loadtxt(os.path.join(throughPath, 'filter_' + key + '.dat'),
dtype=list(zip(['wave', 'trans'], [float] * 2)))
tempB = Bandpass()
tempB.setBandpass(bp['wave'], bp['trans'])
bps.append(tempB)
# Read in the SEDs and compute mags
mags = []
for filename in files:
star = Sed()
star.readSED_flambda(filename)
singleMags = [star.calcMag(band) for band in bps]
mags.append([singleMags[i - 1] - singleMags[i] for i in range(1, 6)])
for maglist, fn, name in zip(mags, fns, names):
format = (name, fn) + tuple(maglist)
print("['%s', '%s', %f, %f, %f, %f, %f]" % format)
def calcWDColors():
"""
Calculate a few example WD colors. Values to go in stellarMags(). Here in case
values need to be regenerated (different stars, bandpasses change, etc.)
"""
try:
from lsst.utils import getPackageDir
import os
from lsst.sims.photUtils import Bandpass, Sed
except:
'Need to setup sims_photUtils to generate WD magnitudes.'
names = ['HeWD_25200_80', 'WD_11000_85', 'WD_3000_85']
fns = ['bergeron_He_24000_80.dat_25200.gz',
'bergeron_10500_85.dat_11000.gz', 'bergeron_2750_85.dat_3000.gz']
wdDir = os.path.join(getPackageDir('sims_sed_library'), 'starSED/wDs/')
files = [os.path.join(wdDir, filename) for filename in fns]
# Read in the LSST bandpasses
bpNames = ['u', 'g', 'r', 'i', 'z', 'y']
bps = []
throughPath = os.path.join(getPackageDir('throughputs'), 'baseline')
for key in bpNames:
bp = np.loadtxt(os.path.join(throughPath, 'filter_' + key + '.dat'),
dtype=list(zip(['wave', 'trans'], [float] * 2)))
tempB = Bandpass()
tempB.setBandpass(bp['wave'], bp['trans'])
bps.append(tempB)
# Read in the SEDs and compute mags
mags = []
for filename in files:
star = Sed()
star.readSED_flambda(filename)
singleMags = [star.calcMag(band) for band in bps]
mags.append([singleMags[i - 1] - singleMags[i] for i in range(1, 6)])
for maglist, fn, name in zip(mags, fns, names):
format = (name, fn) + tuple(maglist)
print("['%s', '%s', %f, %f, %f, %f, %f]" % format)
def addAerosol(atmosphere,
X,
tau0=0.05,
alpha=1.0,
wavelen0=440.0,
plotAtmosphere=True):
# Calculate the aerosol contribution -- sb with aerosols = sb*exp(-tau)
tau = tau0 * np.power((wavelen0 / atmosphere.wavelen), alpha)
# Generate new atmosphere bandpass with aerosols.
atmosphere_aerosol = Bandpass()
atmosphere_aerosol.setBandpass(wavelen=atmosphere.wavelen,
sb=atmosphere.sb * np.exp(-tau * X))
if plotAtmosphere:
# Plot for a check:
atmodict = {
'Original atmosphere': atmosphere,
'With aerosols': atmosphere_aerosol
}
bu.plotBandpasses(atmodict)
return atmosphere_aerosol
def buildLens(lensDir, addLosses=True):
"""
Build the lens throughput curve from the files in lensDir.
Returns a bandpass object.
The coatings for the lens are in *_Coatings, the loss files are in *_Losses.
The borosilicate glass throughput is in l*_Glass.dat; this file is smoothed using the
savitzsky_golay function.
The glass response is multiplied by the coatings and (if addLosses is True),
also the loss curves.
"""
lens = Bandpass()
# Read the glass base file.
glassfile = glob(os.path.join(lensDir, 'l*_Glass.dat'))
if len(glassfile) != 1:
raise ValueError('Expected a single glass file in this directory, found: ', glassfile)
glassfile = glassfile[0]
glass = Bandpass()
glass.readThroughput(glassfile)
# Smooth the glass response.
smoothSb = savitzky_golay(glass.sb, 31, 3)
lens = Bandpass()
lens.setBandpass(glass.wavelen, smoothSb)
# Read the broad band antireflective (BBAR) coatings files.
bbars = _readCoatings(lensDir)
# Multiply the bbars by the glass.
wavelen, sb = lens.multiplyThroughputs(bbars.wavelen, bbars.sb)
lens.setBandpass(wavelen, sb)
# Add losses.
if addLosses:
loss = _readLosses(lensDir)
wavelen, sb = lens.multiplyThroughputs(loss.wavelen, loss.sb)
lens.setBandpass(wavelen, sb)
# Verify that no values go significantly below zero.
belowzero = np.where(lens.sb < 0)
# If there are QE values significantly < 0, raise an exception.
if lens.sb[belowzero] < belowZeroThreshhold:
raise ValueError('Found values in lens throughput significantly below zero.')
# If they are just small errors in interpolation, set to zero.
lens.sb[belowzero] = 0
return lens
def buildLens(lensDir, addLosses=True):
"""
Build the lens throughput curve from the files in lensDir.
Returns a bandpass object.
The coatings for the lens are in *_Coatings, the loss files are in *_Losses.
The borosilicate glass throughput is in l*_Glass.dat; this file is smoothed using the
savitzsky_golay function.
The glass response is multiplied by the coatings and (if addLosses is True),
also the loss curves.
"""
lens = Bandpass()
# Read the glass base file.
glassfile = glob(os.path.join(lensDir, 'l*_Glass.dat'))
if len(glassfile) != 1:
raise ValueError('Expected a single glass file in this directory, found: ', glassfile)
glassfile = glassfile[0]
glass = Bandpass()
glass.readThroughput(glassfile)
# Smooth the glass response.
smoothSb = savitzky_golay(glass.sb, 31, 3)
lens = Bandpass()
lens.setBandpass(glass.wavelen, smoothSb)
# Read the broad band antireflective (BBAR) coatings files.
bbars = _readCoatings(lensDir)
# Multiply the bbars by the glass.
wavelen, sb = lens.multiplyThroughputs(bbars.wavelen, bbars.sb)
lens.setBandpass(wavelen, sb)
# Add losses.
if addLosses:
loss = _readLosses(lensDir)
wavelen, sb = lens.multiplyThroughputs(loss.wavelen, loss.sb)
lens.setBandpass(wavelen, sb)
# Verify that no values go significantly below zero.
belowzero = np.where(lens.sb < 0)
# If there are QE values significantly < 0, raise an exception.
if lens.sb[belowzero] < belowZeroThreshhold:
raise ValueError('Found values in lens throughput significantly below zero.')
# If they are just small errors in interpolation, set to zero.
lens.sb[belowzero] = 0
return lens
sb = f(wavelen)*0.01
#alternatively we could do (only for >10 QE measurements)
#amp_point = amp.getBBox().getCenter()
#sb = qe_curve.evaluate(det, amp_point, wavelen* u.nm, kind='quadratic').value*.01 #unit was percent in CALIB data
sb[np.isnan(sb)] = 0
if np.max(sb)>1.5:
print('These seem too LARGE ', k)
print(np.max(sb))
sb = 0
if np.max(sb)<0.2: #3 dead channels, 1 out of each of R01, R10, and R30; see camera confluence page table
print('dead channel: %s, max sb = %.2f'%(key, np.max(sb)))
continue;
detector.setBandpass(wavelen, sb)
#detector losses
#os.listdir(vendorDir)
detLosses = Bandpass()
detLosses.readThroughput(os.path.join(vendorDir, '%s_Losses/det_Losses.dat' % (vendor)))
#build hardware and system
hardware = {}
system = {}
for f in filters:
sb = mirror1.sb * mirror2.sb *mirror3.sb
sb *= lens1.sb * lens2.sb * lens3.sb * filters[f].sb
sb *= detector.sb * detLosses.sb
hardware[f] = Bandpass()
def packageLowerAtm():
dataDir = getPackageDir('SIMS_SKYBRIGHTNESS_DATA')
outDir = os.path.join(dataDir, 'ESO_Spectra/LowerAtm')
# Read in all the spectra from ESO call and package into a single npz file
files = glob.glob('LowerAtm/skytable*.fits')
temp = pyfits.open(files[0])
wave = temp[1].data['lam'].copy()*1e3
airmasses = []
nightTimes = []
specs = []
for i,filename in enumerate(files):
fits = pyfits.open(filename)
if np.max(fits[1].data['flux']) > 0:
specs.append(fits[1].data['flux'].copy())
header = fits[0].header['comment']
for card in header:
if 'SKYMODEL.TARGET.AIRMASS' in card:
airmasses.append(float(card.split('=')[-1]))
elif 'SKYMODEL.TIME' in card:
nightTimes.append(float(card.split('=')[-1]))
airmasses = np.array(airmasses)
nigtTimes = np.array(nightTimes)
nrec = airmasses.size
nwave = wave.size
dtype = [('airmass', 'float'),
('nightTimes', 'float'),
('spectra', 'float', (nwave)), ('mags', 'float', (6))]
Spectra = np.zeros(nrec, dtype=dtype)
Spectra['airmass'] = airmasses
Spectra['nightTimes'] = nightTimes
Spectra['spectra'] = specs
hPlank = 6.626068e-27 # erg s
cLight = 2.99792458e10 # cm/s
# Convert spectra from ph/s/m2/micron/arcsec2 to erg/s/cm2/nm/arcsec2
Spectra['spectra'] = Spectra['spectra']/(100.**2)*hPlank*cLight/(wave*1e-7)/1e3
# Sort things since this might be helpful later
Spectra.sort(order=['airmass','nightTimes'])
# Load LSST filters
throughPath = os.path.join(getPackageDir('throughputs'),'baseline')
keys = ['u','g','r','i','z','y']
nfilt = len(keys)
filters = {}
for filtername in keys:
bp = np.loadtxt(os.path.join(throughPath, 'filter_'+filtername+'.dat'),
dtype=zip(['wave','trans'],[float]*2 ))
tempB = Bandpass()
tempB.setBandpass(bp['wave'],bp['trans'])
filters[filtername] = tempB
filterWave = np.array([filters[f].calcEffWavelen()[0] for f in keys ])
for i,spectrum in enumerate(Spectra['spectra']):
tempSed = Sed()
tempSed.setSED(wave,flambda=spectrum)
for j,filtName in enumerate(keys):
try:
Spectra['mags'][i][j] = tempSed.calcMag(filters[filtName])
except:
pass
np.savez(os.path.join(outDir,'Spectra.npz'), wave = wave, spec=Spectra, filterWave=filterWave)
def packageZodiacal():
dataDir = getPackageDir('SIMS_SKYBRIGHTNESS_DATA')
outDir = os.path.join(dataDir, 'ESO_Spectra/Zodiacal')
nside = 4
# Read in all the spectra from ESO call and package into a single npz file
files = glob.glob('Zodiacal/skytable*.fits')
temp = pyfits.open(files[0])
wave = temp[1].data['lam'].copy()*1e3
airmasses = []
eclLon = []
eclLat = []
specs = []
for i,filename in enumerate(files):
fits = pyfits.open(filename)
if np.max(fits[1].data['flux']) > 0:
specs.append(fits[1].data['flux'].copy())
header = fits[0].header['comment']
for card in header:
if 'SKYMODEL.TARGET.AIRMASS' in card:
airmasses.append(float(card.split('=')[-1]))
elif 'SKYMODEL.ECL.LON' in card:
eclLon.append(float(card.split('=')[-1]))
elif 'SKYMODEL.ECL.LAT' in card:
eclLat.append(float(card.split('=')[-1]))
airmasses = np.array(airmasses)
eclLon = np.array(eclLon)
eclLat = np.array(eclLat)
wrapA = np.where(eclLon < 0.)
eclLon[wrapA] = eclLon[wrapA]+360.
uAM = np.unique(airmasses)
nAM = uAM.size
nwave = wave.size
dtype = [('airmass', 'float'),
('hpid', 'int' ),
('spectra', 'float', (nwave)), ('mags', 'float', (6))]
npix = hp.nside2npix(nside)
Spectra = np.zeros(nAM*npix, dtype=dtype)
for i,am in enumerate(uAM):
Spectra['airmass'][i*npix:i*npix+npix] = am
Spectra['hpid'][i*npix:i*npix+npix] = np.arange(npix)
for am, lat, lon, spec in zip(airmasses,eclLat, eclLon, specs):
hpid = hp.ang2pix(nside, np.radians(lat+90.), np.radians(lon) )
good = np.where( (Spectra['airmass'] == am) & (Spectra['hpid'] == hpid))
Spectra['spectra'][good] = spec.copy()
hPlank = 6.626068e-27 # erg s
cLight = 2.99792458e10 # cm/s
# Convert spectra from ph/s/m2/micron/arcsec2 to erg/s/cm2/nm/arcsec2
Spectra['spectra'] = Spectra['spectra']/(100.**2)*hPlank*cLight/(wave*1e-7)/1e3
# Sort things since this might be helpful later
Spectra.sort(order=['airmass', 'hpid'])
# Load LSST filters
throughPath = os.path.join(getPackageDir('throughputs'),'baseline')
keys = ['u','g','r','i','z','y']
nfilt = len(keys)
filters = {}
for filtername in keys:
bp = np.loadtxt(os.path.join(throughPath, 'filter_'+filtername+'.dat'),
dtype=zip(['wave','trans'],[float]*2 ))
tempB = Bandpass()
tempB.setBandpass(bp['wave'],bp['trans'])
filters[filtername] = tempB
filterWave = np.array([filters[f].calcEffWavelen()[0] for f in keys ])
for i,spectrum in enumerate(Spectra['spectra']):
tempSed = Sed()
tempSed.setSED(wave,flambda=spectrum)
for j,filtName in enumerate(keys):
try:
Spectra['mags'][i][j] = tempSed.calcMag(filters[filtName])
except:
pass
#span this over multiple files to store in github
nbreak = 3
nrec = np.size(Spectra)
for i in np.arange(nbreak):
np.savez(os.path.join(outDir,'zodiacalSpectra_'+str(i)+'.npz'), wave = wave,
spec=Spectra[i*nrec/nbreak:(i+1)*nrec/nbreak], filterWave=filterWave)
def packageMoon():
dataDir = getPackageDir('SIMS_SKYBRIGHTNESS_DATA')
outDir = os.path.join(dataDir, 'ESO_Spectra/Moon')
# Read in all the spectra from ESO call and package into a single npz file
files = glob.glob('Moon/skytable*.fits')
temp = pyfits.open(files[0])
moonWave = temp[1].data['lam'].copy()*1e3
moonSpec = []
moonAM = [] # Actually target airmass
moonAlt=[] # altitude of the moon
moonSunSep=[] # moon Phase
moonTargetSep=[]
hpid=[]
for i,filename in enumerate(files):
fits = pyfits.open(filename)
try:
if np.max(fits[1].data['flux']) > 0:
moonSpec.append(fits[1].data['flux'].copy())
header = fits[0].header['comment']
for card in header:
if 'SKYMODEL.MOON.SUN.SEP' in card:
moonSunSep.append(float(card.split('=')[-1]))
elif 'SKYMODEL.TARGET.AIRMASS' in card:
#moonAM.append( 1./np.cos(np.radians(90.-float(card.split('=')[-1]))) )
moonAM.append( float(card.split('=')[-1]) )
elif 'SKYMODEL.MOON.TARGET.SEP' in card:
moonTargetSep.append(float(card.split('=')[-1]))
elif 'SKYMODEL.MOON.ALT' in card:
moonAlt.append(float(card.split('=')[-1]))
except:
print filename, ' Failed'
import healpy as hp
from lsst.sims.utils import haversine
nside = 4
lat, az = hp.pix2ang(nside, np.arange(hp.nside2npix(nside)))
alt = np.pi/2.-lat
airmass = 1./np.cos(np.pi/2.-alt)
# Only need low airmass and then 1/2 to sky
good = np.where( (az >= 0) & (az <= np.pi) & (airmass <=2.6) & (airmass >= 1.) )
airmass = airmass[good]
alt=alt[good]
az = az[good]
moonAM = np.array(moonAM)
moonAlt = np.array(moonAlt)
moonSunSep = np.array(moonSunSep)
moonTargetSep = np.array(moonTargetSep)
moonAzDiff = moonTargetSep*0
targetAlt = np.pi/2.-np.arccos(1./moonAM)
# Compute the azimuth difference given the moon-target-seperation
# Let's just do a stupid loop:
for i in np.arange(targetAlt.size):
possibleDistances = haversine(0., np.radians(moonAlt[i]), az, az*0+targetAlt[i])
diff = np.abs(possibleDistances - np.radians(moonTargetSep[i]))
good = np.where(diff == diff.min())
moonAzDiff[i] = az[good][0]
# ok, now I have an alt and az, I can convert that back to a healpix id.
hpid.append(hp.ang2pix(nside, np.pi/2.-targetAlt[i], moonAzDiff[i]))
nrec = moonAM.size
nwave = moonWave.size
dtype = [('hpid', 'int'),
('moonAltitude', 'float'),
('moonSunSep', 'float'),
('spectra', 'float', (nwave)), ('mags', 'float', (6))]
moonSpectra = np.zeros(nrec, dtype=dtype)
moonSpectra['hpid'] = hpid
moonSpectra['moonAltitude'] = moonAlt
moonSpectra['moonSunSep'] = moonSunSep
moonSpectra['spectra'] = moonSpec
hPlank = 6.626068e-27 # erg s
cLight = 2.99792458e10 # cm/s
# Convert spectra from ph/s/m2/micron/arcsec2 to erg/s/cm2/nm/arcsec2
moonSpectra['spectra'] = moonSpectra['spectra']/(100.**2)*hPlank*cLight/(moonWave*1e-7)/1e3
# Sort things since this might be helpful later
moonSpectra.sort(order=['moonSunSep','moonAltitude', 'hpid'])
# Crop off the incomplete ones
good =np.where((moonSpectra['moonAltitude'] >= 0) & (moonSpectra['moonAltitude'] < 89.) )
moonSpectra = moonSpectra[good]
# Load LSST filters
throughPath = os.path.join(getPackageDir('throughputs'),'baseline')
keys = ['u','g','r','i','z','y']
nfilt = len(keys)
filters = {}
for filtername in keys:
bp = np.loadtxt(os.path.join(throughPath, 'filter_'+filtername+'.dat'),
dtype=zip(['wave','trans'],[float]*2 ))
tempB = Bandpass()
tempB.setBandpass(bp['wave'],bp['trans'])
filters[filtername] = tempB
filterWave = np.array([filters[f].calcEffWavelen()[0] for f in keys ])
for i,spectrum in enumerate(moonSpectra['spectra']):
tempSed = Sed()
tempSed.setSED(moonWave,flambda=spectrum)
for j,filtName in enumerate(keys):
try:
moonSpectra['mags'][i][j] = tempSed.calcMag(filters[filtName])
except:
pass
nbreak=5
nrec = np.size(moonSpectra)
for i in np.arange(nbreak):
np.savez(os.path.join(outDir,'moonSpectra_'+str(i)+'.npz'), wave = moonWave, spec=moonSpectra[i*nrec/nbreak:(i+1)*nrec/nbreak], filterWave=filterWave)
import lsst.sims.photUtils.Bandpass as Bandpass
import numpy as np
import os
# Check and see what the model returns for a dark sky at zenith
# Load LSST filters
throughPath = os.getenv('LSST_THROUGHPUTS_BASELINE')
keys = ['u', 'g', 'r', 'i', 'z', 'y']
overview_vals = [22.9, 22.3, 21.2, 20.5, 19.6, 18.6]
filters = {}
for filtername in keys:
bp = np.loadtxt(os.path.join(throughPath, 'filter_' + filtername + '.dat'),
dtype=zip(['wave', 'trans'], [float] * 2))
tempB = Bandpass()
tempB.setBandpass(bp['wave'], bp['trans'])
filters[filtername] = tempB
# XXX--hmm, the zodiacal seems to be fairly important here!
sm = sb.SkyModel(moon=False, twilight=False) #, zodiacal=False)
sm2 = sb.SkyModel(moon=False, twilight=False, zodiacal=False)
mjd = 56948.05174
sm.setRaDecMjd(np.array([0.]), np.array([90.]), mjd, azAlt=True, degrees=True)
sm2.setRaDecMjd(np.array([0.]), np.array([90.]), mjd, azAlt=True, degrees=True)
sm.computeSpec()
sm2.computeSpec()
print 'filter ESO model ESO(no Z) Overview Paper'
for i, key in enumerate(keys):
print key + ' %.2f & %.2f & %.2f \\\\' % (sm.computeMags(
filters[key])[0], sm2.computeMags(filters[key])[0], overview_vals[i])
# Crop off the incomplete ones
good = np.where((moonSpectra['moonAltitude'] >= 0)
& (moonSpectra['moonAltitude'] < 89.))
moonSpectra = moonSpectra[good]
# Load LSST filters
throughPath = os.getenv('LSST_THROUGHPUTS_BASELINE')
keys = ['u', 'g', 'r', 'i', 'z', 'y']
nfilt = len(keys)
filters = {}
for filtername in keys:
bp = np.loadtxt(os.path.join(throughPath, 'filter_' + filtername + '.dat'),
dtype=zip(['wave', 'trans'], [float] * 2))
tempB = Bandpass()
tempB.setBandpass(bp['wave'], bp['trans'])
filters[filtername] = tempB
filterWave = np.array([filters[f].calcEffWavelen()[0] for f in keys])
for i, spectrum in enumerate(moonSpectra['spectra']):
tempSed = Sed()
tempSed.setSED(moonWave, flambda=spectrum)
for j, filtName in enumerate(keys):
try:
moonSpectra['mags'][i][j] = tempSed.calcMag(filters[filtName])
except:
pass
nbreak = 5
nrec = np.size(moonSpectra)
def __init__(self, mags=False, darkSkyMags=None, fitResults=None):
"""
Read the Solar spectrum into a handy object and compute mags in different filters
mags: If true, only return the LSST filter magnitudes, otherwise return the full spectrum
darkSkyMags = dict of the zenith dark sky values to be assumed. The twilight fits are
done relative to the dark sky level.
fitResults = dict of twilight parameters based on twilightFunc. Keys should be filter names.
"""
if darkSkyMags is None:
darkSkyMags = {'u': 22.8, 'g': 22.3, 'r': 21.2,
'i': 20.3, 'z': 19.3, 'y': 18.0,
'B': 22.35, 'G': 21.71, 'R': 21.3}
self.mags = mags
dataDir = getPackageDir('sims_skybrightness_data')
solarSaved = np.load(os.path.join(dataDir, 'solarSpec/solarSpec.npz'))
self.solarSpec = Sed(wavelen=solarSaved['wave'], flambda=solarSaved['spec'])
solarSaved.close()
canonFilters = {}
fnames = ['blue_canon.csv', 'green_canon.csv', 'red_canon.csv']
# Filter names, from bluest to reddest.
self.filterNames = ['B', 'G', 'R']
for fname, filterName in zip(fnames, self.filterNames):
bpdata = np.genfromtxt(os.path.join(dataDir, 'Canon/', fname), delimiter=', ',
dtype=list(zip(['wave', 'through'], [float]*2)))
bpTemp = Bandpass()
bpTemp.setBandpass(bpdata['wave'], bpdata['through'])
canonFilters[filterName] = bpTemp
# Tack on the LSST filters
throughPath = os.path.join(getPackageDir('throughputs'), 'baseline')
lsstKeys = ['u', 'g', 'r', 'i', 'z', 'y']
for key in lsstKeys:
bp = np.loadtxt(os.path.join(throughPath, 'filter_'+key+'.dat'),
dtype=list(zip(['wave', 'trans'], [float]*2)))
tempB = Bandpass()
tempB.setBandpass(bp['wave'], bp['trans'])
canonFilters[key] = tempB
self.filterNames.append(key)
# MAGIC NUMBERS from fitting the all-sky camera:
# Code to generate values in sims_skybrightness/examples/fitTwiSlopesSimul.py
# Which in turn uses twilight maps from sims_skybrightness/examples/buildTwilMaps.py
# values are of the form:
# 0: ratio of f^z_12 to f_dark^z
# 1: slope of curve wrt sun alt
# 2: airmass term (10^(arg[2]*(X-1)))
# 3: azimuth term.
# 4: zenith dark sky flux (erg/s/cm^2)
# For z and y, just assuming the shape parameter fits are similar to the other bands.
# Looks like the diode is not sensitive enough to detect faint sky.
# Using the Patat et al 2006 I-band values for z and modeified a little for y as a temp fix.
if fitResults is None:
self.fitResults = {'B': [7.56765633e+00, 2.29798055e+01, 2.86879956e-01,
3.01162143e-01, 2.58462036e-04],
'G': [2.38561156e+00, 2.29310648e+01, 2.97733083e-01,
3.16403197e-01, 7.29660095e-04],
'R': [1.75498017e+00, 2.22011802e+01, 2.98619033e-01,
3.28880254e-01, 3.24411056e-04],
'z': [2.29, 24.08, 0.3, 0.3, -666],
'y': [2.0, 24.08, 0.3, 0.3, -666]}
# XXX-completely arbitrary fudge factor to make things brighter in the blue
# Just copy the blue and say it's brighter.
self.fitResults['u'] = [16., 2.29622121e+01, 2.85862729e-01,
2.99902574e-01, 2.32325117e-04]
else:
self.fitResults = fitResults
# Take out any filters that don't have fit results
self.filterNames = [key for key in self.filterNames if key in self.fitResults]
self.effWave = []
self.solarMag = []
for filterName in self.filterNames:
self.effWave.append(canonFilters[filterName].calcEffWavelen()[0])
self.solarMag.append(self.solarSpec.calcMag(canonFilters[filterName]))
ord = np.argsort(self.effWave)
self.filterNames = np.array(self.filterNames)[ord]
self.effWave = np.array(self.effWave)[ord]
self.solarMag = np.array(self.solarMag)[ord]
# update the fit results to be zeropointed properly
for key in self.fitResults:
f0 = 10.**(-0.4*(darkSkyMags[key]-np.log10(3631.)))
self.fitResults[key][-1] = f0
self.solarWave = self.solarSpec.wavelen
self.solarFlux = self.solarSpec.flambda
# This one isn't as bad as the model grids, maybe we could get away with computing the magnitudes
# in the __call__ each time.
if mags:
# Load up the LSST filters and convert the solarSpec.flabda and solarSpec.wavelen to fluxes
throughPath = os.path.join(getPackageDir('throughputs'), 'baseline')
self.lsstFilterNames = ['u', 'g', 'r', 'i', 'z', 'y']
self.lsstEquations = np.zeros((np.size(self.lsstFilterNames),
np.size(self.fitResults['B'])), dtype=float)
self.lsstEffWave = []
fits = np.empty((np.size(self.effWave), np.size(self.fitResults['B'])), dtype=float)
for i, fn in enumerate(self.filterNames):
fits[i, :] = self.fitResults[fn]
for filtername in self.lsstFilterNames:
bp = np.loadtxt(os.path.join(throughPath, 'filter_'+filtername+'.dat'),
dtype=list(zip(['wave', 'trans'], [float]*2)))
tempB = Bandpass()
tempB.setBandpass(bp['wave'], bp['trans'])
self.lsstEffWave.append(tempB.calcEffWavelen()[0])
# Loop through the parameters and interpolate to new eff wavelengths
for i in np.arange(self.lsstEquations[0, :].size):
interp = InterpolatedUnivariateSpline(self.effWave, fits[:, i])
self.lsstEquations[:, i] = interp(self.lsstEffWave)
# Set the dark sky flux
for i, filterName in enumerate(self.lsstFilterNames):
self.lsstEquations[i, -1] = 10.**(-0.4*(darkSkyMags[filterName]-np.log10(3631.)))
self.filterNameDict = {'u': 0, 'g': 1, 'r': 2, 'i': 3, 'z': 4, 'y': 5}
# Crop off the incomplete ones
good = np.where((moonSpectra['moonAltitude'] >= 0) & (moonSpectra['moonAltitude'] < 89.))
moonSpectra = moonSpectra[good]
# Load LSST filters
throughPath = os.getenv('LSST_THROUGHPUTS_BASELINE')
keys = ['u', 'g', 'r', 'i', 'z', 'y']
nfilt = len(keys)
filters = {}
for filtername in keys:
bp = np.loadtxt(os.path.join(throughPath, 'filter_'+filtername+'.dat'),
dtype=list(zip(['wave', 'trans'], [float]*2)))
tempB = Bandpass()
tempB.setBandpass(bp['wave'], bp['trans'])
filters[filtername] = tempB
filterWave = np.array([filters[f].calcEffWavelen()[0] for f in keys])
for i, spectrum in enumerate(moonSpectra['spectra']):
tempSed = Sed()
tempSed.setSED(moonWave, flambda=spectrum)
for j, filtName in enumerate(keys):
try:
moonSpectra['mags'][i][j] = tempSed.calcMag(filters[filtName])
except:
pass
nbreak = 5
fitDict = {}
canonDict = {}
canonFiles = {
'R': 'red_canon.csv',
'G': 'green_canon.csv',
'B': 'blue_canon.csv'
}
path = os.path.join(os.environ.get('SIMS_SKYBRIGHTNESS_DATA_DIR'), 'Canon')
for key in canonFiles.keys():
data = np.loadtxt(os.path.join(path, canonFiles[key]),
delimiter=',',
dtype=zip(['wave', 'throughput'], [float, float]))
band = Bandpass()
band.setBandpass(data['wave'], data['throughput'])
canonDict[key] = band
# Dict to save the fitted mag zeropoints
cannonZPs = {}
for filterName in filters:
twi = np.load('TwilightMaps/twiMaps_' + filterName + '.npz')
# set the surface brightness limits to try and fit.
brightLimit = brightLimits[filterName]
#faintLimit = faintLimits[filterName]
sunAlts = twi['sunAlts'].copy()
magMaps = twi['magMap'].copy()
rmsMaps = twi['rmsMap'].copy()
paramList = []
fitDict = {}
canonDict = {}
canonFiles = {'R':'red_canon.csv','G':'green_canon.csv','B':'blue_canon.csv'}
path = os.path.join(os.environ.get('SIMS_SKYBRIGHTNESS_DATA_DIR'), 'Canon')
for key in canonFiles.keys():
data = np.loadtxt(os.path.join(path,canonFiles[key]), delimiter=',',
dtype=zip(['wave','throughput'],[float,float]))
band = Bandpass()
band.setBandpass(data['wave'], data['throughput'])
canonDict[key]=band
# Dict to save the fitted mag zeropoints
cannonZPs = {}
for filterName in filters:
twi = np.load('TwilightMaps/twiMaps_'+filterName+'.npz')
# set the surface brightness limits to try and fit.
brightLimit = brightLimits[filterName]
#faintLimit = faintLimits[filterName]
sunAlts = twi['sunAlts'].copy()
magMaps = twi['magMap'].copy()
rmsMaps = twi['rmsMap'].copy()
def __init__(self, mags=False, darkSkyMags=None, fitResults=None):
"""
Read the Solar spectrum into a handy object and compute mags in different filters
mags: If true, only return the LSST filter magnitudes, otherwise return the full spectrum
darkSkyMags = dict of the zenith dark sky values to be assumed. The twilight fits are
done relative to the dark sky level.
fitResults = dict of twilight parameters based on twilightFunc. Keys should be filter names.
"""
if darkSkyMags is None:
darkSkyMags = {
'u': 22.8,
'g': 22.3,
'r': 21.2,
'i': 20.3,
'z': 19.3,
'y': 18.0,
'B': 22.35,
'G': 21.71,
'R': 21.3
}
self.mags = mags
dataDir = getPackageDir('sims_skybrightness_data')
solarSaved = np.load(os.path.join(dataDir, 'solarSpec/solarSpec.npz'))
self.solarSpec = Sed(wavelen=solarSaved['wave'],
flambda=solarSaved['spec'])
solarSaved.close()
canonFilters = {}
fnames = ['blue_canon.csv', 'green_canon.csv', 'red_canon.csv']
# Filter names, from bluest to reddest.
self.filterNames = ['B', 'G', 'R']
for fname, filterName in zip(fnames, self.filterNames):
bpdata = np.genfromtxt(os.path.join(dataDir, 'Canon/', fname),
delimiter=', ',
dtype=list(
zip(['wave', 'through'], [float] * 2)))
bpTemp = Bandpass()
bpTemp.setBandpass(bpdata['wave'], bpdata['through'])
canonFilters[filterName] = bpTemp
# Tack on the LSST filters
throughPath = os.path.join(getPackageDir('throughputs'), 'baseline')
lsstKeys = ['u', 'g', 'r', 'i', 'z', 'y']
for key in lsstKeys:
bp = np.loadtxt(os.path.join(throughPath,
'filter_' + key + '.dat'),
dtype=list(zip(['wave', 'trans'], [float] * 2)))
tempB = Bandpass()
tempB.setBandpass(bp['wave'], bp['trans'])
canonFilters[key] = tempB
self.filterNames.append(key)
# MAGIC NUMBERS from fitting the all-sky camera:
# Code to generate values in sims_skybrightness/examples/fitTwiSlopesSimul.py
# Which in turn uses twilight maps from sims_skybrightness/examples/buildTwilMaps.py
# values are of the form:
# 0: ratio of f^z_12 to f_dark^z
# 1: slope of curve wrt sun alt
# 2: airmass term (10^(arg[2]*(X-1)))
# 3: azimuth term.
# 4: zenith dark sky flux (erg/s/cm^2)
# For z and y, just assuming the shape parameter fits are similar to the other bands.
# Looks like the diode is not sensitive enough to detect faint sky.
# Using the Patat et al 2006 I-band values for z and modeified a little for y as a temp fix.
if fitResults is None:
self.fitResults = {
'B': [
7.56765633e+00, 2.29798055e+01, 2.86879956e-01,
3.01162143e-01, 2.58462036e-04
],
'G': [
2.38561156e+00, 2.29310648e+01, 2.97733083e-01,
3.16403197e-01, 7.29660095e-04
],
'R': [
1.75498017e+00, 2.22011802e+01, 2.98619033e-01,
3.28880254e-01, 3.24411056e-04
],
'z': [2.29, 24.08, 0.3, 0.3, -666],
'y': [2.0, 24.08, 0.3, 0.3, -666]
}
# XXX-completely arbitrary fudge factor to make things brighter in the blue
# Just copy the blue and say it's brighter.
self.fitResults['u'] = [
16., 2.29622121e+01, 2.85862729e-01, 2.99902574e-01,
2.32325117e-04
]
else:
self.fitResults = fitResults
# Take out any filters that don't have fit results
self.filterNames = [
key for key in self.filterNames if key in self.fitResults
]
self.effWave = []
self.solarMag = []
for filterName in self.filterNames:
self.effWave.append(canonFilters[filterName].calcEffWavelen()[0])
self.solarMag.append(
self.solarSpec.calcMag(canonFilters[filterName]))
ord = np.argsort(self.effWave)
self.filterNames = np.array(self.filterNames)[ord]
self.effWave = np.array(self.effWave)[ord]
self.solarMag = np.array(self.solarMag)[ord]
# update the fit results to be zeropointed properly
for key in self.fitResults:
f0 = 10.**(-0.4 * (darkSkyMags[key] - np.log10(3631.)))
self.fitResults[key][-1] = f0
self.solarWave = self.solarSpec.wavelen
self.solarFlux = self.solarSpec.flambda
# This one isn't as bad as the model grids, maybe we could get away with computing the magnitudes
# in the __call__ each time.
if mags:
# Load up the LSST filters and convert the solarSpec.flabda and solarSpec.wavelen to fluxes
throughPath = os.path.join(getPackageDir('throughputs'),
'baseline')
self.lsstFilterNames = ['u', 'g', 'r', 'i', 'z', 'y']
self.lsstEquations = np.zeros(
(np.size(self.lsstFilterNames), np.size(self.fitResults['B'])),
dtype=float)
self.lsstEffWave = []
fits = np.empty(
(np.size(self.effWave), np.size(self.fitResults['B'])),
dtype=float)
for i, fn in enumerate(self.filterNames):
fits[i, :] = self.fitResults[fn]
for filtername in self.lsstFilterNames:
bp = np.loadtxt(os.path.join(throughPath,
'filter_' + filtername + '.dat'),
dtype=list(zip(['wave', 'trans'],
[float] * 2)))
tempB = Bandpass()
tempB.setBandpass(bp['wave'], bp['trans'])
self.lsstEffWave.append(tempB.calcEffWavelen()[0])
# Loop through the parameters and interpolate to new eff wavelengths
for i in np.arange(self.lsstEquations[0, :].size):
interp = InterpolatedUnivariateSpline(self.effWave, fits[:, i])
self.lsstEquations[:, i] = interp(self.lsstEffWave)
# Set the dark sky flux
for i, filterName in enumerate(self.lsstFilterNames):
self.lsstEquations[i, -1] = 10.**(
-0.4 * (darkSkyMags[filterName] - np.log10(3631.)))
self.filterNameDict = {'u': 0, 'g': 1, 'r': 2, 'i': 3, 'z': 4, 'y': 5}
wd = Sed()
wd.readSED_flambda(filepath)
magnorm = 16
fNorm = wd.calcFluxNorm(magnorm, imsimBand)
wd.multiplyFluxNorm(fNorm)
throughPath = os.path.join(getPackageDir('throughputs'), 'baseline')
lsstKeys = ['u', 'g', 'r', 'i', 'z', 'y']
# lsstKeys = ['r']
bps = {}
for key in lsstKeys:
bp = np.loadtxt(os.path.join(throughPath, 'total_'+key+'.dat'),
dtype=zip(['wave', 'trans'], [float]*2))
bpTemp = Bandpass()
good = np.where(bp['trans'] > 0.)
bpTemp.setBandpass(bp['wave'], bp['trans'], wavelen_min=bp['wave'][good].min(),
wavelen_max=bp['wave'][good].max())
bps[key] = bpTemp
# Generate a GAIA observation
gaia_obs = SED2GAIA(wd)
# Read it in as an SED object
final_sed = ulysses2SED(data=gaia_obs, noisy=False, response=response)
print 're-binned mag, orignal mag, diff'
for key in lsstKeys:
print key, final_sed.calcMag(bps[key]), wd.calcMag(bps[key]), \
final_sed.calcMag(bps[key])-wd.calcMag(bps[key])
import numpy as np
import os
# Check and see what the model returns for a dark sky at zenith
# Load LSST filters
throughPath = os.getenv('LSST_THROUGHPUTS_BASELINE')
keys = ['u','g','r','i','z','y']
overview_vals = [22.9,22.3,21.2,20.5,19.6,18.6]
filters = {}
for filtername in keys:
bp = np.loadtxt(os.path.join(throughPath, 'filter_'+filtername+'.dat'),
dtype=zip(['wave','trans'],[float]*2 ))
tempB = Bandpass()
tempB.setBandpass(bp['wave'],bp['trans'])
filters[filtername] = tempB
# XXX--hmm, the zodiacal seems to be fairly important here!
sm = sb.SkyModel( moon=False, twilight=False)#, zodiacal=False)
sm2 = sb.SkyModel( moon=False, twilight=False, zodiacal=False)
mjd = 56948.05174
sm.setRaDecMjd(np.array([0.]), np.array([90.]), mjd,azAlt=True, degrees=True)
sm2.setRaDecMjd(np.array([0.]), np.array([90.]), mjd,azAlt=True, degrees=True)
sm.computeSpec()
sm2.computeSpec()
print 'filter ESO model ESO(no Z) Overview Paper'
for i,key in enumerate(keys):
print key+' %.2f & %.2f & %.2f \\\\' %(sm.computeMags(filters[key])[0], sm2.computeMags(filters[key])[0],overview_vals[i])