def main():
np.set_printoptions(threshold=np.nan)
testPixelRow = 24
testPixelCol = 17
#obs_20120919-131142.h5,obs_20120919-131346.h5
#create a cal file from a twilight flat
cal = FlatCal('../../params/flatCal.dict')
#open another twilight flat as an observation and apply a wavelength cal and the new flat cal
# run='LICK2012'
# obsFileName = FileName(run=run,date='20120918',tstamp='20120919-131142').flat()
# flatCalFileName = FileName(run=run,date='20120918',tstamp='20120919-131448').flatSoln()
# wvlCalFileName = FileName(run=run,date='20120916',tstamp='20120917-072537').calSoln()
run = 'PAL2012'
obsFileName = FileName(run=run,date='20121211',tstamp='20121212-140003').obs()
flatCalFileName = FileName(run=run,date='20121210',tstamp='').flatSoln()
wvlCalFileName = FileName(run=run,date='20121210',tstamp='20121211-133056').calSoln()
flatCalPath = os.path.dirname(flatCalFileName)
ob = ObsFile(obsFileName)#('obs_20120919-131142.h5')
ob.loadWvlCalFile(wvlCalFileName)#('calsol_20120917-072537.h5')
ob.loadFlatCalFile(flatCalFileName)#('flatsol_20120919-131142.h5')
#plot some uncalibrated and calibrated spectra for one pixel
fig = plt.figure()
ax = fig.add_subplot(211)
ax2 = fig.add_subplot(212)
print ob.getPixelCount(testPixelRow,testPixelCol)
#flatSpectrum,wvlBinEdges = ob.getPixelSpectrum(testPixelRow,testPixelCol,weighted=False)
spectrum,wvlBinEdges = ob.getPixelSpectrum(testPixelRow,testPixelCol,wvlStart=cal.wvlStart,wvlStop=cal.wvlStop,wvlBinWidth=cal.wvlBinWidth,weighted=False,firstSec=0,integrationTime=-1)
weightedSpectrum,wvlBinEdges = ob.getPixelSpectrum(testPixelRow,testPixelCol,weighted=True)
#flatSpectrum,wvlBinEdges = cal.flatFile.getPixelSpectrum(testPixelRow,testPixelCol,wvlStart=cal.wvlStart,wvlStop=cal.wvlStop,wvlBinWidth=cal.wvlBinWidth,weighted=False,firstSec=0,integrationTime=-1)
flatSpectrum = cal.spectra[testPixelRow,testPixelCol]
x = wvlBinEdges[0:-1]
ax.plot(x,cal.wvlMedians,label='median spectrum',alpha=.5)
ax2.plot(x,cal.flatFactors[testPixelRow,testPixelCol,:],label='pixel weights',alpha=.5)
ax2.set_title('flat weights for pixel %d,%d'%(testPixelRow,testPixelCol))
ax.plot(x,spectrum+20,label='unweighted spectrum for pixel %d,%d'%(testPixelRow,testPixelCol),alpha=.5)
ax.plot(x,weightedSpectrum+10,label='weighted %d,%d'%(testPixelRow,testPixelCol),alpha=.5)
ax.plot(x,flatSpectrum+30,label='flatFile %d,%d'%(testPixelRow,testPixelCol),alpha=.5)
ax.legend(loc='upper center', bbox_to_anchor=(0.5, 1.3),fancybox=True,ncol=3)
plt.show()
#display a time-flattened image of the twilight flat as it is and after using itself as it's flat cal
#cal.flatFile.loadFlatCalFile(flatCalFileName)#('flatsol_20120919-131142.h5')
#cal.flatFile.displaySec(weighted=True,integrationTime=-1)
#ob.displaySec(integrationTime=-1)
#ob.displaySec(weighted=True,integrationTime=-1)
for idx in range(0,100,20):
factors10 = cal.flatFactors[:,:,idx]
plt.matshow(factors10,vmax=np.mean(factors10)+1.5*np.std(factors10))
plt.title('Flat weights at %d'%cal.wvlBinEdges[idx])
plt.colorbar()
plt.savefig('plots/factors%d.png'%idx)
plt.show()
class FluxCal:
def __init__(self,paramFile,plots=False,verbose=False):
"""
Opens flux file, prepares standard spectrum, and calculates flux factors for the file.
Method is provided in param file. If 'relative' is selected, an obs file with standard star defocused over
the entire array is expected, with accompanying sky file to do sky subtraction.
If any other method is provided, 'absolute' will be done by default, wherein a point source is assumed
to be present. The obs file is then broken into spectral frames with photometry (psf or aper) performed
on each frame to generate the ARCONS observed spectrum.
"""
self.verbose=verbose
self.plots = plots
self.params = readDict()
self.params.read_from_file(paramFile)
run = self.params['run']
sunsetDate = self.params['fluxSunsetLocalDate']
self.fluxTstamp = self.params['fluxTimestamp']
skyTstamp = self.params['skyTimestamp']
wvlSunsetDate = self.params['wvlCalSunsetLocalDate']
wvlTimestamp = self.params['wvlCalTimestamp']
flatCalFileName = self.params['flatCalFileName']
needTimeAdjust = self.params['needTimeAdjust']
self.deadtime = float(self.params['deadtime']) #from firmware pulse detection
self.timeSpacingCut = self.params['timeSpacingCut']
bLoadBeammap = self.params.get('bLoadBeammap',False)
self.method = self.params['method']
self.objectName = self.params['object']
self.r = float(self.params['energyResolution'])
self.photometry = self.params['photometry']
self.centroidRow = self.params['centroidRow']
self.centroidCol = self.params['centroidCol']
self.aperture = self.params['apertureRad']
self.annulusInner = self.params['annulusInner']
self.annulusOuter = self.params['annulusOuter']
self.collectingArea = self.params['collectingArea']
self.startTime = self.params['startTime']
self.intTime = self.params['integrationTime']
fluxFN = FileName(run=run,date=sunsetDate,tstamp=self.fluxTstamp)
self.fluxFileName = fluxFN.obs()
self.fluxFile = ObsFile(self.fluxFileName)
if self.plots:
self.plotSavePath = os.environ['MKID_PROC_PATH']+os.sep+'fluxCalSolnFiles'+os.sep+run+os.sep+sunsetDate+os.sep+'plots'+os.sep
if not os.path.exists(self.plotSavePath): os.mkdir(self.plotSavePath)
if self.verbose: print "Created directory %s"%self.plotSavePath
obsFNs = [fluxFN]
self.obsList = [self.fluxFile]
if self.startTime in ['',None]: self.startTime=0
if self.intTime in ['',None]: self.intTime=-1
if self.method=="relative":
try:
print "performing Relative Flux Calibration"
skyFN = FileName(run=run,date=sunsetDate,tstamp=skyTstamp)
self.skyFileName = skyFN.obs()
self.skyFile = ObsFile(self.skyFileName)
obsFNs.append(skyFN)
self.obsList.append(self.skyFile)
except:
print "For relative flux calibration a sky file must be provided in param file"
self.__del__()
else:
self.method='absolute'
print "performing Absolute Flux Calibration"
if self.photometry not in ['aperture','PSF']: self.photometry='PSF' #default to PSF fitting if no valid photometry selected
timeMaskFileNames = [fn.timeMask() for fn in obsFNs]
timeAdjustFileName = FileName(run=run).timeAdjustments()
#make filename for output fluxCalSoln file
self.fluxCalFileName = FileName(run=run,date=sunsetDate,tstamp=self.fluxTstamp).fluxSoln()
print "Creating flux cal: %s"%self.fluxCalFileName
if wvlSunsetDate != '':
wvlCalFileName = FileName(run=run,date=wvlSunsetDate,tstamp=wvlTimestamp).calSoln()
if flatCalFileName =='':
flatCalFileName=FileName(obsFile=self.fluxFile).flatSoln()
#load cal files for flux file and, if necessary, sky file
for iObs,obs in enumerate(self.obsList):
if bLoadBeammap:
print 'loading beammap',os.environ['MKID_BEAMMAP_PATH']
obs.loadBeammapFile(os.environ['MKID_BEAMMAP_PATH'])
if wvlSunsetDate != '':
obs.loadWvlCalFile(wvlCalFileName)
else:
obs.loadBestWvlCalFile()
obs.loadFlatCalFile(flatCalFileName)
obs.setWvlCutoffs(-1,-1)
if needTimeAdjust:
obs.loadTimeAdjustmentFile(timeAdjustFileName)
timeMaskFileName = timeMaskFileNames[iObs]
print timeMaskFileName
if not os.path.exists(timeMaskFileName):
print 'Running hotpix for ',obs
hp.findHotPixels(obsFile=obs,outputFileName=timeMaskFileName,fwhm=np.inf,useLocalStdDev=True)
print "Flux cal/sky file pixel mask saved to %s"%(timeMaskFileName)
obs.loadHotPixCalFile(timeMaskFileName)
if self.verbose: print "Loaded hot pixel file %s"%timeMaskFileName
#get flat cal binning information since flux cal will need to match it
self.wvlBinEdges = self.fluxFile.flatCalFile.root.flatcal.wavelengthBins.read()
self.nWvlBins = self.fluxFile.flatWeights.shape[2]
self.binWidths = np.empty((self.nWvlBins),dtype=float)
self.binCenters = np.empty((self.nWvlBins),dtype=float)
for i in xrange(self.nWvlBins):
self.binWidths[i] = self.wvlBinEdges[i+1]-self.wvlBinEdges[i]
self.binCenters[i] = (self.wvlBinEdges[i]+(self.binWidths[i]/2.0))
if self.method=='relative':
print "Extracting ARCONS flux and sky spectra"
self.loadRelativeSpectrum()
print "Flux Spectrum loaded"
self.loadSkySpectrum()
print "Sky Spectrum loaded"
elif self.method=='absolute':
print "Extracting ARCONS point source spectrum"
self.loadAbsoluteSpectrum()
print "Loading standard spectrum"
try:
self.loadStdSpectrum(self.objectName)
except KeyError:
print "Invalid spectrum object name"
self.__del__()
sys.exit()
print "Generating sensitivity curve"
self.calculateFactors()
print "Sensitivity Curve calculated"
print "Writing fluxCal to file %s"%self.fluxCalFileName
self.writeFactors(self.fluxCalFileName)
if self.plots: self.makePlots()
print "Done"
def __del__(self):
try:
self.fluxFile.close()
self.calFile.close()
except AttributeError:#fluxFile was never defined
pass
def getDeadTimeCorrection(self, obs): #WRONG RIGHT NOW. NEEDS TO HAVE RAW COUNTS SUMMED, NOT CUBE WHICH EXCLUDES NOISE TAIL
if self.verbose: print "Making raw cube to get dead time correction"
cubeDict = obs.getSpectralCube(firstSec=self.startTime, integrationTime=self.intTime, weighted=False)
cube= np.array(cubeDict['cube'], dtype=np.double)
wvlBinEdges= cubeDict['wvlBinEdges']
effIntTime= cubeDict['effIntTime']
if self.verbose: print "median effective integration time = ", np.median(effIntTime)
nWvlBins=len(wvlBinEdges)-1
if self.verbose: print "cube shape ", np.shape(cube)
if self.verbose: print "effIntTime shape ", np.shape(effIntTime)
#add third dimension to effIntTime for broadcasting
effIntTime = np.reshape(effIntTime,np.shape(effIntTime)+(1,))
#put cube into counts/s in each pixel
cube /= effIntTime
#CALCULATE DEADTIME CORRECTION
#NEED TOTAL COUNTS PER SECOND FOR EACH PIXEL TO DO PROPERLY
#ASSUMES SAME CORRECTION FACTOR APPLIED FOR EACH WAVELENGTH, MEANING NO WL DEPENDANCE ON DEAD TIME EFFECT
DTCorr = np.zeros((np.shape(cube)[0],np.shape(cube)[1]),dtype=float)
for f in range(0,np.shape(cube)[2]):
#if self.verbose: print cube[:,:,f]
#if self.verbose: print '-----------------------'
DTCorr += cube[:,:,f]
#if self.verbose: print DTCorr
#if self.verbose: print '\n=====================\n'
#Correct for firmware dead time (100us in 2012 ARCONS firmware)
DTCorrNew=DTCorr/(1-DTCorr*self.deadtime)
CorrFactors = DTCorrNew/DTCorr #This is what the frames need to be multiplied by to get their true values
if self.verbose: print "Dead time correction factors: ", CorrFactors
#add third dimension to CorrFactors for broadcasting
CorrFactors = np.reshape(CorrFactors,np.shape(CorrFactors)+(1,))
return CorrFactors
def loadAbsoluteSpectrum(self):
'''
extract the ARCONS measured spectrum of the spectrophotometric standard by breaking data into spectral cube
and performing photometry (aper or psf) on each spectral frame
'''
if self.verbose:print "Making spectral cube"
cubeDict = self.fluxFile.getSpectralCube(firstSec=self.startTime, integrationTime=self.intTime, weighted=True, fluxWeighted=False)
cube= np.array(cubeDict['cube'], dtype=np.double)
effIntTime= cubeDict['effIntTime']
if self.verbose: print "median effective integration time in flux file cube = ", np.median(effIntTime)
if self.verbose: print "cube shape ", np.shape(cube)
if self.verbose: print "effIntTime shape ", np.shape(effIntTime)
#add third dimension to effIntTime for broadcasting
effIntTime = np.reshape(effIntTime,np.shape(effIntTime)+(1,))
#put cube into counts/s in each pixel
cube /= effIntTime
#get dead time correction factors
DTCorr = self.getDeadTimeCorrection(self.fluxFile)
cube*=DTCorr #cube now in units of counts/s and corrected for dead time
if self.plots and not 'figureHeader' in sys.modules:
if self.verbose: print "Saving spectral frames as movie..."
movieCube = np.zeros((self.nWvlBins,np.shape(cube)[0],np.shape(cube)[1]),dtype=float)
for i in xrange(self.nWvlBins):
movieCube[i,:,:] = cube[:,:,i]
makeMovie(movieCube,frameTitles=self.binCenters,cbar=True,outName=self.plotSavePath+'FluxCal_Cube_%s.gif'%(self.objectName), normMin=0, normMax=50)
if self.verbose: print "Movie saved in %s"%self.plotSavePath
LCplot=False #light curve pop-ups not compatible with FLuxCal plotting 2/18/15
#if self.photometry=='PSF': LCplot = False
LC = LightCurve.LightCurve(verbose=self.verbose, showPlot=LCplot)
self.fluxSpectrum=np.empty((self.nWvlBins),dtype=float)
self.skySpectrum=np.zeros((self.nWvlBins),dtype=float)
for i in xrange(self.nWvlBins):
frame = cube[:,:,i]
if self.verbose: print "%s photometry on frame %i of cube, central wvl = %f Angstroms"%(self.photometry,i,self.binCenters[i])
if self.photometry == 'aperture':
fDict = LC.performPhotometry(self.photometry,frame,[[self.centroidCol,self.centroidRow]],expTime=None,aper_radius = self.aperture, annulus_inner = self.annulusInner, annulus_outer = self.annulusOuter, interpolation="linear")
self.fluxSpectrum[i] = fDict['flux']
self.skySpectrum[i] = fDict['skyFlux']
print "Sky estimate = ", fDict['skyFlux']
else:
fDict = LC.performPhotometry(self.photometry,frame,[[self.centroidCol,self.centroidRow]],expTime=None,aper_radius = self.aperture)
self.fluxSpectrum[i] = fDict['flux']
self.fluxSpectrum=self.fluxSpectrum/self.binWidths/self.collectingArea #spectrum now in counts/s/Angs/cm^2
self.skySpectrum=self.skySpectrum/self.binWidths/self.collectingArea
return self.fluxSpectrum, self.skySpectrum
def loadRelativeSpectrum(self):
self.fluxSpectra = [[[] for i in xrange(self.nCol)] for j in xrange(self.nRow)]
self.fluxEffTime = [[[] for i in xrange(self.nCol)] for j in xrange(self.nRow)]
for iRow in xrange(self.nRow):
for iCol in xrange(self.nCol):
count = self.fluxFile.getPixelCount(iRow,iCol)
fluxDict = self.fluxFile.getPixelSpectrum(iRow,iCol,weighted=True,firstSec=0,integrationTime=-1)
self.fluxSpectra[iRow][iCol],self.fluxEffTime[iRow][iCol] = fluxDict['spectrum'],fluxDict['effIntTime']
self.fluxSpectra = np.array(self.fluxSpectra)
self.fluxEffTime = np.array(self.fluxEffTime)
DTCorr = self.getDeadTimeCorrection(self.fluxFile)
#print "Bin widths = ",self.binWidths
self.fluxSpectra = self.fluxSpectra/self.binWidths/self.fluxEffTime*DTCorr
self.fluxSpectrum = self.calculateMedian(self.fluxSpectra) #find median of subtracted spectra across whole array
return self.fluxSpectrum
def loadSkySpectrum(self):
self.skySpectra = [[[] for i in xrange(self.nCol)] for j in xrange(self.nRow)]
self.skyEffTime = [[[] for i in xrange(self.nCol)] for j in xrange(self.nRow)]
for iRow in xrange(self.nRow):
for iCol in xrange(self.nCol):
count = self.skyFile.getPixelCount(iRow,iCol)
skyDict = self.skyFile.getPixelSpectrum(iRow,iCol,weighted=True,firstSec=0,integrationTime=-1)
self.skySpectra[iRow][iCol],self.skyEffTime[iRow][iCol] = skyDict['spectrum'],skyDict['effIntTime']
self.skySpectra = np.array(self.skySpectra)
self.skyEffTime = np.array(self.skyEffTime)
DTCorr = self.getDeadTimeCorrection(self.skyFile)
self.skySpectra = self.skySpectra/self.binWidths/self.skyEffTime*DTCorr
self.skySpectrum = self.calculateMedian(self.skySpectra) #find median of subtracted spectra across whole array
return self.skySpectrum
def loadStdSpectrum(self, objectName="G158-100"):
#import the known spectrum of the calibrator and rebin to the histogram parameters given
#must be imported into array with dtype float so division later does not have error
std = MKIDStd.MKIDStd()
a = std.load(objectName)
a = std.countsToErgs(a) #convert std spectrum to ergs/s/Angs/cm^2 for BB fitting and cleaning
self.stdWvls = np.array(a[:,0])
self.stdFlux = np.array(a[:,1]) #std object spectrum in ergs/s/Angs/cm^2
if self.plots:
#create figure for plotting standard spectrum modifications
self.stdFig = plt.figure()
self.stdAx = self.stdFig.add_subplot(111)
plt.xlim(4000,11000)
plt.plot(self.stdWvls,self.stdFlux*1E15,linewidth=1,color='grey',alpha=0.75)
convX_rev,convY_rev = self.cleanSpectrum(self.stdWvls,self.stdFlux)
convX = convX_rev[::-1] #convolved spectrum comes back sorted backwards, from long wvls to low which screws up rebinning
convY = convY_rev[::-1]
#rebin cleaned spectrum to flat cal's wvlBinEdges
newa = rebin(convX,convY,self.wvlBinEdges)
rebinnedWvl = np.array(newa[:,0])
rebinnedFlux = np.array(newa[:,1])
if self.plots:
#plot final resampled spectrum
plt.plot(convX,convY*1E15,color='blue')
plt.step(rebinnedWvl,rebinnedFlux*1E15,color = 'black',where='mid')
plt.legend(['%s Spectrum'%self.objectName,'Blackbody Fit','Gaussian Convolved Spectrum','Rebinned Spectrum'],'upper right', numpoints=1)
plt.xlabel(ur"Wavelength (\r{A})")
plt.ylabel(ur"Flux (10$^{-15}$ ergs s$^{-1}$ cm$^{-2}$ \r{A}$^{-1}$)")
plt.ylim(1,5)
plt.savefig(self.plotSavePath+'FluxCal_StdSpectrum_%s.eps'%self.objectName,format='eps')
#convert standard spectrum back into counts/s/angstrom/cm^2
newa = std.ergsToCounts(newa)
self.binnedSpectrum = np.array(newa[:,1])
def cleanSpectrum(self,x,y):
##=============== BB Fit to extend spectrum beyond 11000 Angstroms ==================
fraction = 1.0/3.0
nirX = np.arange(int(x[(1.0-fraction)*len(x)]),20000)
T, nirY = fitBlackbody(x,y,fraction=fraction,newWvls=nirX,tempGuess=5600)
if self.plots: plt.plot(nirX,nirY*1E15,linestyle='--',linewidth=2, color="black",alpha=0.5)
extendedWvl = np.concatenate((x,nirX[nirX>max(x)]))
extendedFlux = np.concatenate((y,nirY[nirX>max(x)]))
##======= Gaussian convolution to smooth std spectrum to MKIDs median resolution ========
newX, newY = gaussianConvolution(extendedWvl,extendedFlux,xEnMin=0.005,xEnMax=6.0,xdE=0.001,fluxUnits = "lambda",r=self.r,plots=False)
return newX, newY
def calculateFactors(self):
"""
Calculate the sensitivity spectrum: the weighting factors that correct the flat calibrated spectra to the real spectra
For relative calibration:
First subtract sky spectrum from ARCONS observed spectrum. Then take median of this spectrum as it should be identical
across the array, assuming the flat cal has done its job. Then divide this into the known spectrum of the object.
For absolute calibration:
self.fluxSpectra already has sky subtraction included. Simply divide this spectrum into the known standard spectrum.
"""
self.subtractedSpectrum = self.fluxSpectrum - self.skySpectrum
self.subtractedSpectrum = np.array(self.subtractedSpectrum,dtype=float) #cast as floats so division does not fail later
if self.method=='relative':
normWvl = 5500 #Angstroms. Choose an arbitrary wvl to normalize the relative correction at
ind = np.where(self.wvlBinEdges >= normWvl)[0][0]-1
self.subtractedSpectrum = self.subtractedSpectrum/(self.subtractedSpectrum[ind]) #normalize
self.binnedSpectrum = self.binnedSpectrum/(self.binnedSpectrum[ind]) #normalize treated Std spectrum while we are at it
#Calculate FluxCal factors
self.fluxFactors = self.binnedSpectrum/self.subtractedSpectrum
#self.fluxFlags = np.zeros(np.shape(self.fluxFactors),dtype='int')
self.fluxFlags = np.empty(np.shape(self.fluxFactors),dtype='int')
self.fluxFlags.fill(pipelineFlags.fluxCal['good']) #Initialise flag array filled with 'good' flags. JvE 5/1/2013.
#set factors that will cause trouble to 1
#self.fluxFlags[self.fluxFactors == np.inf] = 1
self.fluxFlags[self.fluxFactors == np.inf] = pipelineFlags.fluxCal['infWeight'] #Modified to use flag dictionary - JvE 5/1/2013
self.fluxFactors[self.fluxFactors == np.inf]=1.0
self.fluxFlags[np.isnan(self.fluxFactors)] = pipelineFlags.fluxCal['nanWeight'] #Modified to use flag dictionary - JvE 5/1/2013
self.fluxFactors[np.isnan(self.fluxFactors)]=1.0
self.fluxFlags[self.fluxFactors <= 0]=pipelineFlags.fluxCal['LEzeroWeight'] #Modified to use flag dictionary - JvE 5/1/2013
self.fluxFactors[self.fluxFactors <= 0]=1.0
def calculateMedian(self, spectra):
spectra2d = np.reshape(spectra,[self.nRow*self.nCol,self.nWvlBins])
wvlMedian = np.empty(self.nWvlBins,dtype=float)
for iWvl in xrange(self.nWvlBins):
spectrum = spectra2d[:,iWvl]
goodSpectrum = spectrum[spectrum != 0]#dead pixels need to be taken out before calculating medians
wvlMedian[iWvl] = np.median(goodSpectrum)
return wvlMedian
def makePlots(self):
"""
Output all debugging plots of ARCONS sky and object spectra, known calibrator spectrum, and sensitivity curve
"""
scratchDir = os.getenv('MKID_PROC_PATH')
fluxDir = self.plotSavePath
fluxCalBase = 'FluxCal_%s'%self.objectName
plotFileName = fluxCalBase+".pdf"
fullFluxPlotFileName = os.path.join(fluxDir,plotFileName)
#uncomment to make some plots for the paper. Proper formatting Will also require figureheader to be imported and for movie making to be turned off
self.paperFig = plt.figure()
self.paperAx = self.paperFig.add_subplot(111)
plt.xlim(4000,11000)
plt.plot(self.binCenters,self.fluxFactors,linewidth=3,color='black')
plt.xlabel(ur"Wavelength (\r{A})")
plt.ylabel(ur"Spectral Calibration Curve")
plt.ylim(0,150)
plt.savefig(self.plotSavePath+'FluxCal_Sensitivity_%s.eps'%self.objectName,format='eps')
#save throughput as a .npz file that other code uses when making paper plots
np.savez(self.plotSavePath+'%s_%s_throughput.npz'%(self.objectName.strip(),self.fluxTstamp),throughput=1.0/self.fluxFactors,wvls=self.binCenters)
pp = PdfPages(fullFluxPlotFileName)
#plt.rcParams['font.size'] = 2
wvls = self.binCenters
plt.figure()
ax1 = plt.subplot(111)
ax1.set_title('ARCONS median flat cal\'d flux in counts')
plt.plot(wvls,self.fluxSpectrum)
pp.savefig()
plt.figure()
ax2 = plt.subplot(111)
ax2.set_title('ARCONS median flat cal\'d sky in counts')
plt.plot(wvls,self.skySpectrum)
pp.savefig()
plt.figure()
ax3 = plt.subplot(111)
ax3.set_title('Flux data minus sky in counts')
plt.plot(wvls,self.subtractedSpectrum)
pp.savefig()
plt.figure()
ax4 = plt.subplot(111)
ax4.set_title('Std Spectrum of %s'%(self.objectName))
plt.plot(self.stdWvls,self.stdFlux)
pp.savefig()
plt.figure()
ax5 = plt.subplot(111)
ax5.set_title('Binned Std Spectrum')
plt.plot(wvls,self.binnedSpectrum)
pp.savefig()
plt.figure()
ax6 = plt.subplot(111)
ax6.set_title('Median Sensitivity Spectrum')
ax6.set_xlim((3000,13000))
#ax6.set_ylim((0,5))
plt.plot(wvls,self.fluxFactors)
pp.savefig()
plt.figure()
ax7 = plt.subplot(111)
ax7.set_title('1/Sensitivity (Throughput)')
ax7.set_xlim((4000,11000))
plt.plot(wvls,1.0/self.fluxFactors)
pp.savefig()
plt.figure()
ax8 = plt.subplot(111)
ax8.set_title('Flux Cal\'d ARCONS Spectrum of Std')
plt.plot(wvls,self.fluxFactors*self.subtractedSpectrum)
pp.savefig()
pp.close()
print "Saved Flux Cal plots to %s"%(fullFluxPlotFileName)
def writeFactors(self,fluxCalFileName):
"""
Write flux cal weights to h5 file
"""
if os.path.isabs(fluxCalFileName) == True:
fullFluxCalFileName = fluxCalFileName
else:
scratchDir = os.getenv('MKID_PROC_PATH')
fluxDir = os.path.join(scratchDir,'fluxCalSolnFiles')
fullFluxCalFileName = os.path.join(fluxDir,fluxCalFileName)
try:
fluxCalFile = tables.openFile(fullFluxCalFileName,mode='w')
except:
print 'Error: Couldn\'t create flux cal file, ',fullFluxCalFileName
return
calgroup = fluxCalFile.createGroup(fluxCalFile.root,'fluxcal','Table of flux calibration weights by wavelength')
caltable = tables.Array(calgroup,'weights',object=self.fluxFactors,title='Flux calibration Weights indexed by wavelengthBin')
flagtable = tables.Array(calgroup,'flags',object=self.fluxFlags,title='Flux cal flags indexed by wavelengthBin. 0 is Good')
bintable = tables.Array(calgroup,'wavelengthBins',object=self.wvlBinEdges,title='Wavelength bin edges corresponding to third dimension of weights array')
fluxCalFile.flush()
fluxCalFile.close()
print "Finished Flux Cal, written to %s"%(fullFluxCalFileName)
def cleanSpectrum_old(self,x,y,objectName):
'''
function to take high resolution spectrum of standard star, extend IR coverage with
an exponential tail, then rebin down to ARCONS resolution. This function has since been
deprecated with the current cleanSpectrum which uses a BB fit to extend IR coverage,
and does the rebinning using a gaussian convolution. This is left in for reference.
'''
#locations and widths of absorption features in Angstroms
#features = [3890,3970,4099,4340,4860,6564,6883,7619]
#widths = [50,50,50,50,50,50,50,50]
#for i in xrange(len(features)):
# #check for absorption feature in std spectrum
# ind = np.where((x<(features[i]+15)) & (x>(features[i]-15)))[0]
# if len(ind)!=0:
# ind = ind[len(ind)/2]
# #if feature is found (flux is higher on both sides of the specified wavelength where the feature should be)
# if y[ind]<y[ind+1] and y[ind]<y[ind-1]:
# #cut out width[i] around feature[i]
# inds = np.where((x >= features[i]+widths[i]) | (x <= features[i]-widths[i]))
# x = x[inds]
# y = y[inds]
#fit a tail to the end of the spectrum to interpolate out to desired wavelength in angstroms
fraction = 3.0/4.0
newx = np.arange(int(x[fraction*len(x)]),20000)
slopeguess = (np.log(y[-1])-np.log(y[fraction*len(x)]))/(x[-1]-x[fraction*len(x)])
print "Guess at exponential slope is %f"%(slopeguess)
guess_a, guess_b, guess_c = float(y[fraction*len(x)]), x[fraction*len(x)], slopeguess
guess = [guess_a, guess_b, guess_c]
fitx = x[fraction*len(x):]
fity = y[fraction*len(x):]
exp_decay = lambda fx, A, x0, t: A * np.exp((fx-x0) * t)
params, cov = curve_fit(exp_decay, fitx, fity, p0=guess, maxfev=2000)
A, x0, t= params
print "A = %s\nx0 = %s\nt = %s\n"%(A, x0, t)
best_fit = lambda fx: A * np.exp((fx-x0)*t)
calcx = np.array(newx,dtype=float)
newy = best_fit(calcx)
#func = interpolate.splrep(x[fration*len(x):],y[fraction*len(x):],s=smooth)
#newx = np.arange(int(x[fraction*len(x)]),self.wvlBinEdges[-1])
#newy = interpolate.splev(newx,func)
wl = np.concatenate((x,newx[newx>max(x)]))
flux = np.concatenate((y,newy[newx>max(x)]))
#new method, rebin data to grid of wavelengths generated from a grid of evenly spaced energy bins
#R=7.0 at 4500
#R=E/dE -> dE = R/E
dE = 0.3936 #eV
start = 1000 #Angs
stop = 20000 #Angs
enBins = ObsFile.makeWvlBins(dE,start,stop)
rebinned = rebin(wl,flux,enBins)
re_wl = rebinned[:,0]
re_flux = rebinned[:,1]
#plt.plot(re_wl,re_flux,color='r')
re_wl = re_wl[np.isnan(re_flux)==False]
re_flux = re_flux[np.isnan(re_flux)==False]
start1 = self.wvlBinEdges[0]
stop1 = self.wvlBinEdges[-1]
#regrid downsampled data
new_wl = np.arange(start1,stop1)
#print re_wl
#print re_flux
#print new_wl
#weight=1.0/(re_flux)**(2/1.00)
print len(re_flux)
weight = np.ones(len(re_flux))
#decrease weights near peak
ind = np.where(re_flux == max(re_flux))[0]
weight[ind] = 0.3
for p in [1,2,3]:
if p==1:
wt = 0.3
elif p==2:
wt = 0.6
elif p==3:
wt = 0.7
try:
weight[ind+p] = wt
except IndexError:
pass
try:
if ind-p >= 0:
weight[ind-p] = wt
except IndexError:
pass
weight[-4:] = 1.0
#weight = [0.7,1,0.3,0.3,0.5,0.7,1,1,1]
#print len(weight)
#weight = re_flux/min(re_flux)
#weight = 1.0/weight
#weight = weight/max(weight)
#print weight
f = interpolate.splrep(re_wl,re_flux,w=weight,k=3,s=max(re_flux)**1.71)
new_flux = interpolate.splev(new_wl,f,der=0)
return new_wl, new_flux