def ReduceTwo(speclist, flatlist='', biaslist='', HeNeAr_file='',
stdstar='', trace_recenter=False, ntracesteps=15,
airmass_file='apoextinct.dat',
flat_mode='spline', flat_order=9, flat_response=True,
apwidth=8, skysep=3, skywidth=7, skydeg=0,
HeNeAr_prev=False, HeNeAr_interac=True,
HeNeAr_tol=20, HeNeAr_order=3, display_HeNeAr=False,
std_mode='spline', std_order=12, display_std=False,
trim=True, write_reduced=True,
display=True, display_final=True):
if (len(biaslist) > 0):
bias = pydis.biascombine(biaslist, trim=trim)
else:
bias = 0.0
if (len(biaslist) > 0) and (len(flatlist) > 0):
flat,fmask_out = pydis.flatcombine(flatlist, bias, trim=trim,
mode=flat_mode,display=False,
flat_poly=flat_order, response=flat_response)
else:
flat = 1.0
fmask_out = (1,)
if HeNeAr_prev is False:
prev = ''
else:
prev = HeNeAr_file+'.lines'
# do the HeNeAr mapping first, must apply to all science frames
if (len(HeNeAr_file) > 0):
wfit = pydis.HeNeAr_fit(HeNeAr_file, trim=trim, fmask=fmask_out,
interac=HeNeAr_interac, previous=prev,mode='poly',
display=display_HeNeAr, tol=HeNeAr_tol,
fit_order=HeNeAr_order)
# read in the list of target spectra
# assumes specfile is a list of file names of object
#-> wrap with array and flatten because Numpy sucks with one-element arrays...
specfile = np.array([np.loadtxt(speclist, dtype='string')]).flatten()
for i in range(len(specfile)):
spec = specfile[i]
print("> Processing file "+spec+" ["+str(i)+"/"+str(len(specfile))+"]")
# raw, exptime, airmass, wapprox = pydis.OpenImg(spec, trim=trim)
img = pydis.OpenImg(spec, trim=trim)
raw = img.data
exptime = img.exptime
airmass = img.airmass
wapprox = img.wavelength
# remove bias and flat, divide by exptime
data = ((raw - bias) / flat) / exptime
if display is True:
plt.figure()
plt.imshow(np.log10(data), origin = 'lower',aspect='auto',cmap=cm.Greys_r)
plt.title(spec+' (flat and bias corrected)')
plt.show()
# with reduced data, trace BOTH apertures
trace_1 = pydis.ap_trace(data,fmask=fmask_out, nsteps=ntracesteps,
recenter=trace_recenter, interac=True)
trace_2 = pydis.ap_trace(data,fmask=fmask_out, nsteps=ntracesteps,
recenter=trace_recenter, interac=True)
xbins = np.arange(data.shape[1])
if display is True:
plt.figure()
plt.imshow(np.log10(data), origin='lower',aspect='auto',cmap=cm.Greys_r)
plt.plot(xbins, trace_1,'b',lw=1)
plt.plot(xbins, trace_1-apwidth,'r',lw=1)
plt.plot(xbins, trace_1+apwidth,'r',lw=1)
plt.plot(xbins, trace_1-apwidth-skysep,'g',lw=1)
plt.plot(xbins, trace_1-apwidth-skysep-skywidth,'g',lw=1)
plt.plot(xbins, trace_1+apwidth+skysep,'g',lw=1)
plt.plot(xbins, trace_1+apwidth+skysep+skywidth,'g',lw=1)
plt.plot(xbins, trace_2,'b',lw=1)
plt.plot(xbins, trace_2-apwidth,'r',lw=1)
plt.plot(xbins, trace_2+apwidth,'r',lw=1)
plt.plot(xbins, trace_2-apwidth-skysep,'g',lw=1)
plt.plot(xbins, trace_2-apwidth-skysep-skywidth,'g',lw=1)
plt.plot(xbins, trace_2+apwidth+skysep,'g',lw=1)
plt.plot(xbins, trace_2+apwidth+skysep+skywidth,'g',lw=1)
plt.title('(Both Traces, with aperture and sky regions)')
plt.show()
t_indx = 1
# now do the processing for both traces as if separate stars
for trace in [trace_1, trace_2]:
tnum = '_' + str(t_indx)
t_indx = t_indx + 1
# extract the spectrum, measure sky values along trace, get flux errors
ext_spec, sky, fluxerr = pydis.ap_extract(data, trace, apwidth=apwidth,
skysep=skysep,skywidth=skywidth,
skydeg=skydeg,coaddN=1)
if (len(HeNeAr_file) > 0):
wfinal = pydis.mapwavelength(trace, wfit, mode='poly')
else:
# if no line lamp given, use approx from the img header
wfinal = wapprox
# subtract local sky level, divide by exptime to get flux units
# (counts / sec)
flux_red = (ext_spec - sky)
# now correct the spectrum for airmass extinction
flux_red_x = pydis.AirmassCor(wfinal, flux_red, airmass,
airmass_file=airmass_file)
# now get flux std IF stdstar is defined
# !! assume first object in list is std star !!
if (len(stdstar) > 0) and (i==0):
sens_flux = pydis.DefFluxCal(wfinal, flux_red_x, stdstar=stdstar,
mode=std_mode, polydeg=std_order, display=display_std)
sens_wave = wfinal
elif (len(stdstar) == 0) and (i==0):
# if 1st obj not the std, then just make array of 1's to multiply thru
sens_flux = np.ones_like(flux_red_x)
sens_wave = wfinal
# final step in reduction, apply sensfunc
ffinal,efinal = pydis.ApplyFluxCal(wfinal, flux_red_x, fluxerr,
sens_wave, sens_flux)
if write_reduced is True:
pydis._WriteSpec(spec+tnum, wfinal, ffinal, efinal, trace)
now = datetime.datetime.now()
lout = open(spec+tnum+'.log','w')
lout.write('# This file contains the reduction parameters \n'+
'# used in autoreduce for '+spec+'\n')
lout.write('DATE-REDUCED = '+str(now)+'\n')
lout.write('HeNeAr_tol = '+str(HeNeAr_tol)+'\n')
lout.write('HeNeAr_order = '+str(HeNeAr_order)+'\n')
lout.write('trace1 = '+str(False)+'\n')
lout.write('ntracesteps = '+str(ntracesteps)+'\n')
lout.write('trim = '+str(trim)+'\n')
lout.write('response = '+str(flat_response)+'\n')
lout.write('apwidth = '+str(apwidth)+'\n')
lout.write('skysep = '+str(skysep)+'\n')
lout.write('skywidth = '+str(skywidth)+'\n')
lout.write('skydeg = '+str(skydeg)+'\n')
lout.write('stdstar = '+str(stdstar)+'\n')
lout.write('airmass_file = '+str(airmass_file)+'\n')
lout.close()
if display_final is True:
# the final figure to plot
plt.figure()
# plt.plot(wfinal, ffinal)
plt.errorbar(wfinal, ffinal, yerr=efinal)
plt.xlabel('Wavelength')
plt.ylabel('Flux')
plt.title(spec)
#plot within percentile limits
plt.ylim( (np.percentile(ffinal,2),
np.percentile(ffinal,98)) )
plt.show()
return
def autoreduce(speclist, flatlist='', biaslist='', HeNeAr_file='',
stdstar='', trace_recenter=False, trace_interac=True,
trace1=False, ntracesteps=15,
airmass_file='apoextinct.dat',
flat_mode='spline', flat_order=9, flat_response=True,
apwidth=8, skysep=3, skywidth=7, skydeg=0,
HeNeAr_prev=False, HeNeAr_interac=True,
HeNeAr_tol=20, HeNeAr_order=3, display_HeNeAr=False,
std_mode='spline', std_order=12, display_std=False,
trim=True, write_reduced=True,
display=True, display_final=True,
silent=True):
"""
A wrapper routine to carry out the full steps of the spectral
reduction and calibration. Steps include:
1) combines bias and flat images
2) maps wavelength in the HeNeAr image
3) perform simple image reduction: Data = (Raw - Bias)/Flat
4) trace spectral aperture
5) extract spectrum
6) measure sky along extracted spectrum
7) apply flux calibration
8) write output files
Parameters
----------
speclist : str
Path to file containing list of science images.
flatlist : str
Path to file containing list of flat images.
biaslist : str
Path to file containing list of bias images.
HeNeAr_file : str
Path to the HeNeAr calibration image
stdstar : str
Name of the standard star to use for flux calibration. Currently
the IRAF library onedstds/spec50cal is used for flux calibration.
Assumes the first star in "speclist" is the standard star. If
nothing is entered for "stdstar", no flux calibration will be
computed. (Default is '')
trace1 : bool, optional
use trace1=True if only perform aperture trace on first object in
speclist. Useful if e.g. science targets are faint, and first
object is a bright standard star. Note: assumes star placed at
same position in spatial direction. (Default is False)
trace_recenter : bool, optional
If trace1=True, set this to True to allow for small linear
adjustments to the trace (default is False)
trace_interac : bool, optional
Set to True if user should interactively select aperture center
for each object spectrum. (Default is True)
ntracesteps : int, optional
Number of bins in X direction to chop image into. Use
fewer bins if ap_trace is having difficulty, such as with faint
targets (default here is 25, minimum is 4)
apwidth : int, optional
The width along the Y axis of the trace to extract. Note: a fixed
width is used along the whole trace. (default here is 3 pixels)
skysep : int, optional
The separation in pixels from the aperture to the sky window.
(Default is 25)
skywidth : int, optional
The width in pixels of the sky windows on either side of the
aperture. (Default is 75)
HeNeAr_interac : bool, optional
Should the HeNeAr identification be done interactively (manually)?
(Default here is False)
HeNeAr_tol : int, optional
When in automatic mode, the tolerance in pixel units between
linelist entries and estimated wavelengths for the first few
lines matched... use carefully. (Default here is 20)
HeNeAr_order : int, optional
The polynomial order to use to interpolate between identified
peaks in the HeNeAr (Default is 2)
display_HeNeAr : bool, optional
std_mode : str, optional
Fit mode to use with the flux standard star. Options are 'spline'
and 'poly' (Default is 'spline')
std_order : int, optional
The order of polynomial to fit, if std_mode='poly'. (Default is 12)
display_std : bool, optional
If set, display plots of the flux standard being fit (Default is
False)
trim : bool, optional
Trim the image using the DATASEC keyword in the header, assuming
has format of [0:1024,0:512] (Default is True)
write_reduced : bool, optional
Set to True to write output files, including the .spec file with
columns (wavelength, flux); the .trace file with columns
(X pixel number, Y pixel of trace); .log file with record of
settings used in this routine for reduction. (Default is True)
display : bool, optional
Set to True to display intermediate steps along the way.
(Default is True)
display_final : bool, optional
Set to False to suppress plotting the final reduced spectrum to
the screen. Useful for running in quiet batch mode. (Default is
True)
"""
if (len(biaslist) > 0):
bias = pydis.biascombine(biaslist, trim=trim, silent=silent)
else:
bias = 0.0
if (len(biaslist) > 0) and (len(flatlist) > 0):
flat,fmask_out = pydis.flatcombine(flatlist, bias, trim=trim,
mode=flat_mode,display=False,
flat_poly=flat_order, response=flat_response)
else:
flat = 1.0
fmask_out = (1,)
if HeNeAr_prev is False:
prev = ''
else:
prev = HeNeAr_file+'.lines'
# do the HeNeAr mapping first, must apply to all science frames
if (len(HeNeAr_file) > 0):
wfit = pydis.HeNeAr_fit(HeNeAr_file, trim=trim, fmask=fmask_out,
interac=HeNeAr_interac, previous=prev,mode='poly',
display=display_HeNeAr, tol=HeNeAr_tol,
fit_order=HeNeAr_order)
# read in the list of target spectra
# assumes specfile is a list of file names of object
specfile = np.array([np.loadtxt(speclist, dtype='string')]).flatten()
for i in range(len(specfile)):
spec = specfile[i]
if silent is False:
print("> Processing file "+spec+" ["+str(i)+"/"+str(len(specfile))+"]")
# raw, exptime, airmass, wapprox = pydis.OpenImg(spec, trim=trim)
img = pydis.OpenImg(spec, trim=trim)
raw = img.data
exptime = img.exptime
airmass = img.airmass
wapprox = img.wavelength
# remove bias and flat, divide by exptime
data = ((raw - bias) / flat) / exptime
if display is True:
plt.figure()
plt.imshow(np.log10(data), origin = 'lower',aspect='auto',cmap=cm.Greys_r)
plt.title(spec+' (flat and bias corrected)')
plt.show()
# with reduced data, trace the aperture
if (i==0) or (trace1 is False):
trace = pydis.ap_trace(data,fmask=fmask_out, nsteps=ntracesteps,
recenter=trace_recenter, interac=trace_interac)
# extract the spectrum, measure sky values along trace, get flux errors
ext_spec, sky, fluxerr = pydis.ap_extract(data, trace, apwidth=apwidth,
skysep=skysep,skywidth=skywidth,
skydeg=skydeg,coaddN=1)
xbins = np.arange(data.shape[1])
if display is True:
plt.figure()
plt.imshow(np.log10(data), origin='lower',aspect='auto',cmap=cm.Greys_r)
plt.plot(xbins, trace,'b',lw=1)
plt.plot(xbins, trace-apwidth,'r',lw=1)
plt.plot(xbins, trace+apwidth,'r',lw=1)
plt.plot(xbins, trace-apwidth-skysep,'g',lw=1)
plt.plot(xbins, trace-apwidth-skysep-skywidth,'g',lw=1)
plt.plot(xbins, trace+apwidth+skysep,'g',lw=1)
plt.plot(xbins, trace+apwidth+skysep+skywidth,'g',lw=1)
plt.title('(with trace, aperture, and sky regions)')
plt.show()
if (len(HeNeAr_file) > 0):
wfinal = pydis.mapwavelength(trace, wfit, mode='poly')
else:
# if no line lamp given, use approx from the img header
wfinal = wapprox
# plt.figure()
# plt.plot(wfinal,'r')
# plt.show()
# subtract local sky level, divide by exptime to get flux units
# (counts / sec)
flux_red = (ext_spec - sky)
# now correct the spectrum for airmass extinction
flux_red_x = pydis.AirmassCor(wfinal, flux_red, airmass,
airmass_file=airmass_file)
# now get flux std IF stdstar is defined
# !! assume first object in list is std star !!
if (len(stdstar) > 0) and (i==0):
sens_flux = pydis.DefFluxCal(wfinal, flux_red_x, stdstar=stdstar,
mode=std_mode, polydeg=std_order, display=display_std)
sens_wave = wfinal
elif (len(stdstar) == 0) and (i==0):
# if 1st obj not the std, then just make array of 1's to multiply thru
sens_flux = np.ones_like(flux_red_x)
sens_wave = wfinal
# final step in reduction, apply sensfunc
ffinal,efinal = pydis.ApplyFluxCal(wfinal, flux_red_x, fluxerr,
sens_wave, sens_flux)
if write_reduced is True:
pydis._WriteSpec(spec, wfinal, ffinal, efinal, trace)
now = datetime.datetime.now()
lout = open(spec+'.log','w')
lout.write('# This file contains the reduction parameters \n'+
'# used in autoreduce for '+spec+'\n')
lout.write('DATE-REDUCED = '+str(now)+'\n')
lout.write('HeNeAr_tol = '+str(HeNeAr_tol)+'\n')
lout.write('HeNeAr_order = '+str(HeNeAr_order)+'\n')
lout.write('trace1 = '+str(trace1)+'\n')
lout.write('ntracesteps = '+str(ntracesteps)+'\n')
lout.write('trim = '+str(trim)+'\n')
lout.write('response = '+str(flat_response)+'\n')
lout.write('apwidth = '+str(apwidth)+'\n')
lout.write('skysep = '+str(skysep)+'\n')
lout.write('skywidth = '+str(skywidth)+'\n')
lout.write('skydeg = '+str(skydeg)+'\n')
lout.write('stdstar = '+str(stdstar)+'\n')
lout.write('airmass_file = '+str(airmass_file)+'\n')
lout.close()
if display_final is True:
# the final figure to plot
plt.figure()
# plt.plot(wfinal, ffinal)
plt.errorbar(wfinal, ffinal, yerr=efinal)
plt.xlabel('Wavelength')
plt.ylabel('Flux')
plt.title(spec)
#plot within percentile limits
plt.ylim( (np.percentile(ffinal,2),
np.percentile(ffinal,98)) )
plt.show()
return
def ReduceCoAdd(speclist, flatlist, biaslist, HeNeAr_file,
stdstar='', trace1=False, ntracesteps=15,
flat_mode='spline', flat_order=9, flat_response=True,
apwidth=6,skysep=1,skywidth=7, skydeg=0,
HeNeAr_prev=False, HeNeAr_interac=False,
HeNeAr_tol=20, HeNeAr_order=2, displayHeNeAr=False,
trim=True, write_reduced=True, display=True):
"""
A special version of autoreduce, that assumes all the target images
want to be median co-added and then extracted. All images have flat
and bias removed first, then are combined. Trace and Extraction
happens only on the final combined image.
Assumes file names in speclist are the standard star, followed by all the target
images you want to co-add.
"""
#-- the basic crap, used for all frames
bias = pydis.biascombine(biaslist, trim=trim)
flat,fmask_out = pydis.flatcombine(flatlist, bias, trim=trim, mode=flat_mode,display=False,
flat_poly=flat_order, response=flat_response)
if HeNeAr_prev is False:
prev = ''
else:
prev = HeNeAr_file+'.lines'
wfit = pydis.HeNeAr_fit(HeNeAr_file, trim=trim, fmask=fmask_out, interac=HeNeAr_interac,
previous=prev,mode='poly',
display=displayHeNeAr, tol=HeNeAr_tol, fit_order=HeNeAr_order)
#-- the standard star, set the stage
specfile = np.array([np.loadtxt(speclist, dtype='string')]).flatten()
spec = specfile[0]
# raw, exptime, airmass, wapprox = pydis.OpenImg(spec, trim=trim)
img = pydis.OpenImg(spec, trim=trim)
raw = img.data
exptime = img.exptime
airmass = img.airmass
wapprox = img.wavelength
data = ((raw - bias) / flat) / exptime
trace = pydis.ap_trace(data,fmask=fmask_out, nsteps=ntracesteps)
# extract the spectrum, measure sky values along trace, get flux errors
ext_spec, sky, fluxerr = pydis.ap_extract(data, trace, apwidth=apwidth,
skysep=skysep,skywidth=skywidth,
skydeg=skydeg,coaddN=1)
xbins = np.arange(data.shape[1])
wfinal = pydis.mapwavelength(trace, wfit, mode='poly')
flux_red_x = (ext_spec - sky)
sens_flux = pydis.DefFluxCal(wfinal, flux_red_x, stdstar=stdstar,
mode='spline',polydeg=12)
sens_wave = wfinal
ffinal,efinal = pydis.ApplyFluxCal(wfinal, flux_red_x, fluxerr, sens_wave, sens_flux)
#-- the target star exposures, stack and proceed
for i in range(1,len(specfile)):
spec = specfile[i]
# raw, exptime, airmass, wapprox = pydis.OpenImg(spec, trim=trim)
img = pydis.OpenImg(spec, trim=trim)
raw = img.data
exptime = img.exptime
airmass = img.airmass
wapprox = img.wavelength
data_i = ((raw - bias) / flat) / exptime
if (i==1):
all_data = data_i
elif (i>1):
all_data = np.dstack( (all_data, data_i))
data = np.median(all_data, axis=2)
# extract the spectrum, measure sky values along trace, get flux errors
ext_spec, sky, fluxerr = pydis.ap_extract(data, trace, apwidth=apwidth,
skysep=skysep,skywidth=skywidth,
skydeg=skydeg,coaddN=len(specfile))
xbins = np.arange(data.shape[1])
wfinal = pydis.mapwavelength(trace, wfit, mode='poly')
flux_red_x = (ext_spec - sky)
ffinal,efinal = pydis.ApplyFluxCal(wfinal, flux_red_x, fluxerr, sens_wave, sens_flux)
plt.figure()
plt.plot(wfinal, ffinal)
plt.title("CO-ADD DONE")
plt.ylim( (np.percentile(ffinal,5),
np.percentile(ffinal,95)) )
plt.show()
return wfinal, ffinal, efinal
def ReduceCoAdd(speclist, flatlist, biaslist, HeNeAr_file,
stdstar='', trace1=False, ntracesteps=15,
flat_mode='spline', flat_order=9, flat_response=True,
apwidth=6,skysep=1,skywidth=7, skydeg=0,
HeNeAr_prev=False, HeNeAr_interac=False,
HeNeAr_tol=20, HeNeAr_order=2, displayHeNeAr=False,
trim=True, write_reduced=True, display=True):
"""
A special version of autoreduce, that assumes all the target images
want to be median co-added and then extracted. All images have flat
and bias removed first, then are combined. Trace and Extraction
happens only on the final combined image.
Assumes file names in speclist are the standard star, followed by all the target
images you want to co-add.
"""
#-- the basic crap, used for all frames
bias = pydis.biascombine(biaslist, trim=trim)
flat,fmask_out = pydis.flatcombine(flatlist, bias, trim=trim, mode=flat_mode,display=False,
flat_poly=flat_order, response=flat_response)
# Going to need to add in something HERE for that multi henear stuffs!
if HeNeAr_prev is False:
prev = ''
else:
prev = HeNeAr_file+'.lines'
wfit = pydis.HeNeAr_fit(HeNeAr_file, trim=trim, fmask=fmask_out, interac=HeNeAr_interac,
previous=prev,mode='poly',
display=displayHeNeAr, tol=HeNeAr_tol, fit_order=HeNeAr_order)
#-- the standard star, set the stage
specfile = np.loadtxt(speclist,dtype='string')
spec = specfile[0]
# raw, exptime, airmass, wapprox = pydis.OpenImg(spec, trim=trim)
img = pydis.OpenImg(spec, trim=trim)
raw = img.data
exptime = img.exptime
airmass = img.airmass
wapprox = img.wavelength
data = ((raw - bias) / flat) / exptime
trace = pydis.ap_trace(data,fmask=fmask_out, nsteps=ntracesteps)
# extract the spectrum, measure sky values along trace, get flux errors
ext_spec, sky, fluxerr = pydis.ap_extract(data, trace, apwidth=apwidth,
skysep=skysep,skywidth=skywidth,
skydeg=skydeg,coaddN=1)
xbins = np.arange(data.shape[1])
wfinal = pydis.mapwavelength(trace, wfit, mode='poly')
flux_red_x = (ext_spec - sky)
sens_flux = pydis.DefFluxCal(wfinal, flux_red_x, stdstar=stdstar,
mode='spline',polydeg=12)
sens_wave = wfinal
ffinal,efinal = pydis.ApplyFluxCal(wfinal, flux_red_x, fluxerr, sens_wave, sens_flux)
#-- the target star exposures, stack and proceed
for i in range(1,len(specfile)):
spec = specfile[i]
# raw, exptime, airmass, wapprox = pydis.OpenImg(spec, trim=trim)
img = pydis.OpenImg(spec, trim=trim)
raw = img.data
exptime = img.exptime
airmass = img.airmass
wapprox = img.wavelength
data_i = ((raw - bias) / flat) / exptime
if (i==1):
all_data = data_i
elif (i>1):
all_data = np.dstack( (all_data, data_i))
data = np.median(all_data, axis=2)
# extract the spectrum, measure sky values along trace, get flux errors
ext_spec, sky, fluxerr = pydis.ap_extract(data, trace, apwidth=apwidth,
skysep=skysep,skywidth=skywidth,
skydeg=skydeg,coaddN=len(specfile))
xbins = np.arange(data.shape[1])
wfinal = pydis.mapwavelength(trace, wfit, mode='poly')
flux_red_x = (ext_spec - sky)
ffinal,efinal = pydis.ApplyFluxCal(wfinal, flux_red_x, fluxerr, sens_wave, sens_flux)
plt.figure()
plt.plot(wfinal, ffinal)
plt.title("CO-ADD DONE")
plt.ylim( (np.percentile(ffinal,5),
np.percentile(ffinal,95)) )
plt.show()
return wfinal, ffinal, efinal
def autoreduce(speclist, flatlist='', biaslist='', HeNeAr_file='',
stdstar='', trace_recenter=False, trace_interac=True,
trace1=False, ntracesteps=15,
airmass_file='apoextinct.dat',
flat_mode='spline', flat_order=9, flat_response=True,
apwidth=8, skysep=3, skywidth=7, skydeg=0,
HeNeAr_prev=False, HeNeAr_interac=True,
HeNeAr_tol=20, HeNeAr_order=3, display_HeNeAr=False,
std_mode='spline', std_order=12, display_std=False,
trim=True, write_reduced=True,
display=True, display_final=True):
"""
A wrapper routine to carry out the full steps of the spectral
reduction and calibration. Steps include:
1) combines bias and flat images
2) maps wavelength in the HeNeAr image
3) perform simple image reduction: Data = (Raw - Bias)/Flat
4) trace spectral aperture
5) extract spectrum
6) measure sky along extracted spectrum
7) apply flux calibration
8) write output files
Parameters
----------
speclist : str
Path to file containing list of science images.
flatlist : str
Path to file containing list of flat images.
biaslist : str
Path to file containing list of bias images.
HeNeAr_file : str
Path to the HeNeAr calibration image
stdstar : str
Name of the standard star to use for flux calibration. Currently
the IRAF library onedstds/spec50cal is used for flux calibration.
Assumes the first star in "speclist" is the standard star. If
nothing is entered for "stdstar", no flux calibration will be
computed. (Default is '')
trace1 : bool, optional
use trace1=True if only perform aperture trace on first object in
speclist. Useful if e.g. science targets are faint, and first
object is a bright standard star. Note: assumes star placed at
same position in spatial direction. (Default is False)
trace_recenter : bool, optional
If trace1=True, set this to True to allow for small linear
adjustments to the trace (default is False)
trace_interac : bool, optional
Set to True if user should interactively select aperture center
for each object spectrum. (Default is True)
ntracesteps : int, optional
Number of bins in X direction to chop image into. Use
fewer bins if ap_trace is having difficulty, such as with faint
targets (default here is 25, minimum is 4)
apwidth : int, optional
The width along the Y axis of the trace to extract. Note: a fixed
width is used along the whole trace. (default here is 3 pixels)
skysep : int, optional
The separation in pixels from the aperture to the sky window.
(Default is 25)
skywidth : int, optional
The width in pixels of the sky windows on either side of the
aperture. (Default is 75)
HeNeAr_interac : bool, optional
Should the HeNeAr identification be done interactively (manually)?
(Default here is False)
HeNeAr_tol : int, optional
When in automatic mode, the tolerance in pixel units between
linelist entries and estimated wavelengths for the first few
lines matched... use carefully. (Default here is 20)
HeNeAr_order : int, optional
The polynomial order to use to interpolate between identified
peaks in the HeNeAr (Default is 2)
display_HeNeAr : bool, optional
trim : bool, optional
Trim the image using the DATASEC keyword in the header, assuming
has format of [0:1024,0:512] (Default is True)
write_reduced : bool, optional
Set to True to write output files, including the .spec file with
columns (wavelength, flux); the .trace file with columns
(X pixel number, Y pixel of trace); .log file with record of
settings used in this routine for reduction. (Default is True)
display : bool, optional
Set to True to display intermediate steps along the way.
(Default is True)
display_final : bool, optional
Set to False to suppress plotting the final reduced spectrum to
the screen. Useful for running in quiet batch mode. (Default is
True)
"""
if (len(biaslist) > 0):
bias = pydis.biascombine(biaslist, trim=trim)
else:
bias = 0.0
if (len(biaslist) > 0) and (len(flatlist) > 0):
flat,fmask_out = pydis.flatcombine(flatlist, bias, trim=trim,
mode=flat_mode,display=False,
flat_poly=flat_order, response=flat_response)
else:
flat = 1.0
fmask_out = (1,)
#something here will definately change or be added:
if HeNeAr_prev is False:
prev = ''
else:
prev = HeNeAr_file+'.lines'
# do the HeNeAr mapping first, must apply to all science frames
if (len(HeNeAr_file) > 0):
wfit = pydis.HeNeAr_fit(HeNeAr_file, trim=trim, fmask=fmask_out,
interac=HeNeAr_interac, previous=prev,mode='poly',
display=display_HeNeAr, tol=HeNeAr_tol,
fit_order=HeNeAr_order)
def ReduceTwo(speclist,
flatlist='',
biaslist='',
HeNeAr_file='',
stdstar='',
trace_recenter=False,
ntracesteps=15,
airmass_file='apoextinct.dat',
flat_mode='spline',
flat_order=9,
flat_response=True,
apwidth=8,
skysep=3,
skywidth=7,
skydeg=0,
HeNeAr_prev=False,
HeNeAr_interac=True,
HeNeAr_tol=20,
HeNeAr_order=3,
display_HeNeAr=False,
std_mode='spline',
std_order=12,
display_std=False,
trim=True,
write_reduced=True,
display=True,
display_final=True):
if (len(biaslist) > 0):
bias = pydis.biascombine(biaslist, trim=trim)
else:
bias = 0.0
if (len(biaslist) > 0) and (len(flatlist) > 0):
flat, fmask_out = pydis.flatcombine(flatlist,
bias,
trim=trim,
mode=flat_mode,
display=False,
flat_poly=flat_order,
response=flat_response)
else:
flat = 1.0
fmask_out = (1, )
if HeNeAr_prev is False:
prev = ''
else:
prev = HeNeAr_file + '.lines'
# do the HeNeAr mapping first, must apply to all science frames
if (len(HeNeAr_file) > 0):
wfit = pydis.HeNeAr_fit(HeNeAr_file,
trim=trim,
fmask=fmask_out,
interac=HeNeAr_interac,
previous=prev,
mode='poly',
display=display_HeNeAr,
tol=HeNeAr_tol,
fit_order=HeNeAr_order)
# read in the list of target spectra
# assumes specfile is a list of file names of object
#-> wrap with array and flatten because Numpy sucks with one-element arrays...
specfile = np.array([np.loadtxt(speclist, dtype='string')]).flatten()
for i in range(len(specfile)):
spec = specfile[i]
print("> Processing file " + spec + " [" + str(i) + "/" +
str(len(specfile)) + "]")
# raw, exptime, airmass, wapprox = pydis.OpenImg(spec, trim=trim)
img = pydis.OpenImg(spec, trim=trim)
raw = img.data
exptime = img.exptime
airmass = img.airmass
wapprox = img.wavelength
# remove bias and flat, divide by exptime
data = ((raw - bias) / flat) / exptime
if display is True:
plt.figure()
plt.imshow(np.log10(data),
origin='lower',
aspect='auto',
cmap=cm.Greys_r)
plt.title(spec + ' (flat and bias corrected)')
plt.show()
# with reduced data, trace BOTH apertures
trace_1 = pydis.ap_trace(data,
fmask=fmask_out,
nsteps=ntracesteps,
recenter=trace_recenter,
interac=True)
trace_2 = pydis.ap_trace(data,
fmask=fmask_out,
nsteps=ntracesteps,
recenter=trace_recenter,
interac=True)
xbins = np.arange(data.shape[1])
if display is True:
plt.figure()
plt.imshow(np.log10(data),
origin='lower',
aspect='auto',
cmap=cm.Greys_r)
plt.plot(xbins, trace_1, 'b', lw=1)
plt.plot(xbins, trace_1 - apwidth, 'r', lw=1)
plt.plot(xbins, trace_1 + apwidth, 'r', lw=1)
plt.plot(xbins, trace_1 - apwidth - skysep, 'g', lw=1)
plt.plot(xbins, trace_1 - apwidth - skysep - skywidth, 'g', lw=1)
plt.plot(xbins, trace_1 + apwidth + skysep, 'g', lw=1)
plt.plot(xbins, trace_1 + apwidth + skysep + skywidth, 'g', lw=1)
plt.plot(xbins, trace_2, 'b', lw=1)
plt.plot(xbins, trace_2 - apwidth, 'r', lw=1)
plt.plot(xbins, trace_2 + apwidth, 'r', lw=1)
plt.plot(xbins, trace_2 - apwidth - skysep, 'g', lw=1)
plt.plot(xbins, trace_2 - apwidth - skysep - skywidth, 'g', lw=1)
plt.plot(xbins, trace_2 + apwidth + skysep, 'g', lw=1)
plt.plot(xbins, trace_2 + apwidth + skysep + skywidth, 'g', lw=1)
plt.title('(Both Traces, with aperture and sky regions)')
plt.show()
t_indx = 1
# now do the processing for both traces as if separate stars
for trace in [trace_1, trace_2]:
tnum = '_' + str(t_indx)
t_indx = t_indx + 1
# extract the spectrum, measure sky values along trace, get flux errors
ext_spec, sky, fluxerr = pydis.ap_extract(data,
trace,
apwidth=apwidth,
skysep=skysep,
skywidth=skywidth,
skydeg=skydeg,
coaddN=1)
if (len(HeNeAr_file) > 0):
wfinal = pydis.mapwavelength(trace, wfit, mode='poly')
else:
# if no line lamp given, use approx from the img header
wfinal = wapprox
# subtract local sky level, divide by exptime to get flux units
# (counts / sec)
flux_red = (ext_spec - sky)
# now correct the spectrum for airmass extinction
flux_red_x = pydis.AirmassCor(wfinal,
flux_red,
airmass,
airmass_file=airmass_file)
# now get flux std IF stdstar is defined
# !! assume first object in list is std star !!
if (len(stdstar) > 0) and (i == 0):
sens_flux = pydis.DefFluxCal(wfinal,
flux_red_x,
stdstar=stdstar,
mode=std_mode,
polydeg=std_order,
display=display_std)
sens_wave = wfinal
elif (len(stdstar) == 0) and (i == 0):
# if 1st obj not the std, then just make array of 1's to multiply thru
sens_flux = np.ones_like(flux_red_x)
sens_wave = wfinal
# final step in reduction, apply sensfunc
ffinal, efinal = pydis.ApplyFluxCal(wfinal, flux_red_x, fluxerr,
sens_wave, sens_flux)
if write_reduced is True:
pydis._WriteSpec(spec + tnum, wfinal, ffinal, efinal, trace)
now = datetime.datetime.now()
lout = open(spec + tnum + '.log', 'w')
lout.write(
'# This file contains the reduction parameters \n' +
'# used in autoreduce for ' + spec + '\n')
lout.write('DATE-REDUCED = ' + str(now) + '\n')
lout.write('HeNeAr_tol = ' + str(HeNeAr_tol) + '\n')
lout.write('HeNeAr_order = ' + str(HeNeAr_order) + '\n')
lout.write('trace1 = ' + str(False) + '\n')
lout.write('ntracesteps = ' + str(ntracesteps) + '\n')
lout.write('trim = ' + str(trim) + '\n')
lout.write('response = ' + str(flat_response) + '\n')
lout.write('apwidth = ' + str(apwidth) + '\n')
lout.write('skysep = ' + str(skysep) + '\n')
lout.write('skywidth = ' + str(skywidth) + '\n')
lout.write('skydeg = ' + str(skydeg) + '\n')
lout.write('stdstar = ' + str(stdstar) + '\n')
lout.write('airmass_file = ' + str(airmass_file) + '\n')
lout.close()
if display_final is True:
# the final figure to plot
plt.figure()
# plt.plot(wfinal, ffinal)
plt.errorbar(wfinal, ffinal, yerr=efinal)
plt.xlabel('Wavelength')
plt.ylabel('Flux')
plt.title(spec)
#plot within percentile limits
plt.ylim((np.percentile(ffinal, 2), np.percentile(ffinal, 98)))
plt.show()
return
def autoreduce(speclist,
flatlist='',
biaslist='',
HeNeAr_file='',
stdstar='',
trace_recenter=False,
trace_interac=True,
trace1=False,
ntracesteps=15,
airmass_file='apoextinct.dat',
flat_mode='spline',
flat_order=9,
flat_response=True,
apwidth=8,
skysep=3,
skywidth=7,
skydeg=0,
HeNeAr_prev=False,
HeNeAr_interac=True,
HeNeAr_tol=20,
HeNeAr_order=3,
display_HeNeAr=False,
std_mode='spline',
std_order=12,
display_std=False,
trim=True,
write_reduced=True,
display=True,
display_final=True,
silent=True):
"""
A wrapper routine to carry out the full steps of the spectral
reduction and calibration. Steps include:
1) combines bias and flat images
2) maps wavelength in the HeNeAr image
3) perform simple image reduction: Data = (Raw - Bias)/Flat
4) trace spectral aperture
5) extract spectrum
6) measure sky along extracted spectrum
7) apply flux calibration
8) write output files
Parameters
----------
speclist : str
Path to file containing list of science images.
flatlist : str
Path to file containing list of flat images.
biaslist : str
Path to file containing list of bias images.
HeNeAr_file : str
Path to the HeNeAr calibration image
stdstar : str
Name of the standard star to use for flux calibration. If
nothing is entered for "stdstar", no flux calibration will be
computed. (Default is '').
NOTE1: must include the subdir for the star, e.g. 'spec50cal/feige34'.
NOTE2: Assumes the first star in "speclist" is the standard star.
trace1 : bool, optional
use trace1=True if only perform aperture trace on first object in
speclist. Useful if e.g. science targets are faint, and first
object is a bright standard star. Note: assumes star placed at
same position in spatial direction. (Default is False)
trace_recenter : bool, optional
If trace1=True, set this to True to allow for small linear
adjustments to the trace (default is False)
trace_interac : bool, optional
Set to True if user should interactively select aperture center
for each object spectrum. (Default is True)
ntracesteps : int, optional
Number of bins in X direction to chop image into. Use
fewer bins if ap_trace is having difficulty, such as with faint
targets (default here is 25, minimum is 4)
apwidth : int, optional
The width along the Y axis of the trace to extract. Note: a fixed
width is used along the whole trace. (default here is 3 pixels)
skysep : int, optional
The separation in pixels from the aperture to the sky window.
(Default is 25)
skywidth : int, optional
The width in pixels of the sky windows on either side of the
aperture. (Default is 75)
HeNeAr_interac : bool, optional
Should the HeNeAr identification be done interactively (manually)?
(Default here is False)
HeNeAr_tol : int, optional
When in automatic mode, the tolerance in pixel units between
linelist entries and estimated wavelengths for the first few
lines matched... use carefully. (Default here is 20)
HeNeAr_order : int, optional
The polynomial order to use to interpolate between identified
peaks in the HeNeAr (Default is 2)
display_HeNeAr : bool, optional
std_mode : str, optional
Fit mode to use with the flux standard star. Options are 'spline'
and 'poly' (Default is 'spline')
std_order : int, optional
The order of polynomial to fit, if std_mode='poly'. (Default is 12)
display_std : bool, optional
If set, display plots of the flux standard being fit (Default is
False)
trim : bool, optional
Trim the image using the DATASEC keyword in the header, assuming
has format of [0:1024,0:512] (Default is True)
write_reduced : bool, optional
Set to True to write output files, including the .spec file with
columns (wavelength, flux); the .trace file with columns
(X pixel number, Y pixel of trace); .log file with record of
settings used in this routine for reduction. (Default is True)
display : bool, optional
Set to True to display intermediate steps along the way.
(Default is True)
display_final : bool, optional
Set to False to suppress plotting the final reduced spectrum to
the screen. Useful for running in quiet batch mode. (Default is
True)
"""
if (len(biaslist) > 0):
bias = pydis.biascombine(biaslist, trim=trim, silent=silent)
else:
bias = 0.0
if (len(biaslist) > 0) and (len(flatlist) > 0):
flat, fmask_out = pydis.flatcombine(flatlist,
bias,
trim=trim,
mode=flat_mode,
display=False,
flat_poly=flat_order,
response=flat_response)
else:
flat = 1.0
fmask_out = (1, )
if HeNeAr_prev is False:
prev = ''
else:
prev = HeNeAr_file + '.lines'
# do the HeNeAr mapping first, must apply to all science frames
if (len(HeNeAr_file) > 0):
wfit = pydis.HeNeAr_fit(HeNeAr_file,
trim=trim,
fmask=fmask_out,
interac=HeNeAr_interac,
previous=prev,
mode='poly',
display=display_HeNeAr,
tol=HeNeAr_tol,
fit_order=HeNeAr_order)
# read in the list of target spectra
# assumes specfile is a list of file names of object
specfile = np.array([np.loadtxt(speclist, dtype='string')]).flatten()
for i in range(len(specfile)):
spec = specfile[i]
if silent is False:
print("> Processing file " + spec + " [" + str(i) + "/" +
str(len(specfile)) + "]")
# raw, exptime, airmass, wapprox = pydis.OpenImg(spec, trim=trim)
img = pydis.OpenImg(spec, trim=trim)
raw = img.data
exptime = img.exptime
airmass = img.airmass
wapprox = img.wavelength
# remove bias and flat, divide by exptime
data = ((raw - bias) / flat) / exptime
if display is True:
plt.figure()
plt.imshow(np.log10(data),
origin='lower',
aspect='auto',
cmap=cm.Greys_r)
plt.title(spec + ' (flat and bias corrected)')
plt.show()
# with reduced data, trace the aperture
if (i == 0) or (trace1 is False):
trace = pydis.ap_trace(data,
fmask=fmask_out,
nsteps=ntracesteps,
recenter=trace_recenter,
interac=trace_interac)
# extract the spectrum, measure sky values along trace, get flux errors
ext_spec, sky, fluxerr = pydis.ap_extract(data,
trace,
apwidth=apwidth,
skysep=skysep,
skywidth=skywidth,
skydeg=skydeg,
coaddN=1)
xbins = np.arange(data.shape[1])
if display is True:
plt.figure()
plt.imshow(np.log10(data),
origin='lower',
aspect='auto',
cmap=cm.Greys_r)
plt.plot(xbins, trace, 'b', lw=1)
plt.plot(xbins, trace - apwidth, 'r', lw=1)
plt.plot(xbins, trace + apwidth, 'r', lw=1)
plt.plot(xbins, trace - apwidth - skysep, 'g', lw=1)
plt.plot(xbins, trace - apwidth - skysep - skywidth, 'g', lw=1)
plt.plot(xbins, trace + apwidth + skysep, 'g', lw=1)
plt.plot(xbins, trace + apwidth + skysep + skywidth, 'g', lw=1)
plt.title('(with trace, aperture, and sky regions)')
plt.show()
if (len(HeNeAr_file) > 0):
wfinal = pydis.mapwavelength(trace, wfit, mode='poly')
else:
# if no line lamp given, use approx from the img header
wfinal = wapprox
# plt.figure()
# plt.plot(wfinal,'r')
# plt.show()
# subtract local sky level, divide by exptime to get flux units
# (counts / sec)
flux_red = (ext_spec - sky)
# now correct the spectrum for airmass extinction
flux_red_x = pydis.AirmassCor(wfinal,
flux_red,
airmass,
airmass_file=airmass_file)
# now get flux std IF stdstar is defined
# !! assume first object in list is std star !!
if (len(stdstar) > 0) and (i == 0):
sens_flux = pydis.DefFluxCal(wfinal,
flux_red_x,
stdstar=stdstar,
mode=std_mode,
polydeg=std_order,
display=display_std)
sens_wave = wfinal
elif (len(stdstar) == 0) and (i == 0):
# if 1st obj not the std, then just make array of 1's to multiply thru
sens_flux = np.ones_like(flux_red_x)
sens_wave = wfinal
# final step in reduction, apply sensfunc
ffinal, efinal = pydis.ApplyFluxCal(wfinal, flux_red_x, fluxerr,
sens_wave, sens_flux)
if write_reduced is True:
pydis._WriteSpec(spec, wfinal, ffinal, efinal, trace)
now = datetime.datetime.now()
lout = open(spec + '.log', 'w')
lout.write('# This file contains the reduction parameters \n' +
'# used in autoreduce for ' + spec + '\n')
lout.write('DATE-REDUCED = ' + str(now) + '\n')
lout.write('HeNeAr_tol = ' + str(HeNeAr_tol) + '\n')
lout.write('HeNeAr_order = ' + str(HeNeAr_order) + '\n')
lout.write('trace1 = ' + str(trace1) + '\n')
lout.write('ntracesteps = ' + str(ntracesteps) + '\n')
lout.write('trim = ' + str(trim) + '\n')
lout.write('response = ' + str(flat_response) + '\n')
lout.write('apwidth = ' + str(apwidth) + '\n')
lout.write('skysep = ' + str(skysep) + '\n')
lout.write('skywidth = ' + str(skywidth) + '\n')
lout.write('skydeg = ' + str(skydeg) + '\n')
lout.write('stdstar = ' + str(stdstar) + '\n')
lout.write('airmass_file = ' + str(airmass_file) + '\n')
lout.close()
if display_final is True:
# the final figure to plot
plt.figure()
# plt.plot(wfinal, ffinal)
plt.errorbar(wfinal, ffinal, yerr=efinal)
plt.xlabel('Wavelength')
plt.ylabel('Flux')
plt.title(spec)
#plot within percentile limits
plt.ylim((np.percentile(ffinal, 2), np.percentile(ffinal, 98)))
plt.show()
return
#KingValdez170615
#Code to test out and run some pydis functions
# if pyDIS isn't in the currnet working directory, add to path
import sys
sys.path.append('/home/kvaldez/github/pydis/')
import numpy as np
# must import, of course
import pydis
# reduce and extract the data with the fancy autoreduce script
#wave, flux, err = pydis.autoreduce('objlist.r.txt', 'flatlist.r.txt', 'biaslist.r.txt',
#'HeNeAr.0005r.fits', stdstar='spec50cal/fiege34.dat')
dir = '/usr/netapp/physics/linux-lab/data/apo/UT170422/'
rbias_file = dir + 'rbias.txt'
bias = pydis.biascombine(rbias_file, trim=True)