def lines(elem,asIndex=False):
"""
NAME:
lines
PURPOSE:
return the location of peaks in the window weight ('lines') for a given element
INPUT:
elem - element
asIndx= (False) if yes, return the indices into an apStar-like wavelengthh grid rather than the wavelengths directly
OUTPUT:
wavelengths of peaks in \AA
HISTORY:
2015-03-11 - Written - Bovy (IAS)
"""
# Load the window
win= read(elem,apStarWavegrid=True)
import apogee.spec.plot as splot
wavs= splot.apStarWavegrid()
# Find peaks
indx= (numpy.roll(win,1) < win)*(numpy.roll(win,-1) < win)\
*(win > 0.1)
if asIndex:
return indx
else:
return wavs[indx]
def dummy(dx=1./3.,sparse=False):
"""
NAME:
dummy
PURPOSE:
return a 'dummy' LSF that is a delta function
INPUT:
dx= (1/3) spacing between LSF centers in the apStar grid
sparse= (False) if True, return a sparse representation that can be passed to apogee.spec.lsf.convolve for easy convolution
OUTPUT:
LSF(x|pixel center);
pixel centers are apStarWavegrid if dx=1, and denser 1/integer versions if dx=1/integer
HISTORY:
2015-03-23 - Written - Bovy (IAS)
"""
# Are the x unit pixels or a fraction 1/hires thereof?
hires= int(round(1./dx))
# Setup output
wav= apStarWavegrid()
l10wav= numpy.log10(wav)
dowav= l10wav[1]-l10wav[0]
# Hi-res wavelength for output
hireswav= 10.**numpy.arange(l10wav[0],l10wav[-1]+dowav/hires,dowav/hires)
out= numpy.ones((len(hireswav),1))
if sparse: out= sparsify(out)
return out
def binaryModelGen(locationID, apogeeID, params, visit, ipf=None, ipg=None, plot=True): ''' Interpolates the spectra of the individual stars in the binary using some initial parameters and their velocity difference. :param locationID: The location ID of the binary. :param apogeeID: The apogee ID of the binary. :param params: The paramters to test against the observed data. format: [ [Teff1, ...], [logg1, ...], [metals1, ...], [am1, ...], [nm1, ...], [cm1, ...]] :param visit: The visit to test against. :param ip: The interpolator instance that keeps running ferre. Should be faster to keep using this instead. (default=None) :param plot: If true plots each component in the binary in 'plots/model_gen' (default=True) :returns: The binary model flux and the maximum value from the cross correlation function between the modeled totalFlux and the continuum-normalized spectrum. (totalFlux, max) ''' # Generate models (flux1, flux2) if (np.logical_and(ipf == None, ipg == None)): # todo: put in condition for both gk and f libraries mspecs = ferre.interpolate(params[0], params[1], params[2], params[3], params[4], params[5]) else: if (params[0][0] > 6000.): mspec1 = ipf(params[0][0], params[1][0], params[2][0], params[3][0], params[4][0], params[5][0]) else: mspec1 = ipg(params[0][0], params[1][0], params[2][0], params[3][0], params[4][0], params[5][0]) if (params[0][1] > 6000.): mspec2 = ipf(params[0][1], params[1][1], params[2][1], params[3][1], params[4][1], params[5][1]) else: mspec2 = ipg(params[0][1], params[1][1], params[2][1], params[3][1], params[4][1], params[5][1]) mspecs = [ mspec1, mspec2 ] for mspec in mspecs: mspec[np.isnan(mspec)] = 0. # Calculate deltaV RVs = getRVs(locationID, apogeeID, visit) # Generate the wavelength grid restLambda = splot.apStarWavegrid() # Calculates wavelength grid for the second star with a doppler shift shiftLambda = [restLambda * (1. + rv / (const.c / 1000.)) for rv in RVs] # The fluxes of both stars shiftedFlux = np.array([np.interp(restLambda, shiftLambda[i], mspecs[i]) for i in range(len(shiftLambda))]) # The combined flux of the stars in the modeled binary (params[7][1] defined as flux ratio) totalFlux = (shiftedFlux[0] + (shiftedFlux[1] * params[6][1])) / 2.0 # Make the plots if (plot == True): BinPlot.plotDeltaVCheck(locationID, apogeeID, visit, [[ restLambda, mspecs[0], 'blue', 'rest model specA' ], [ restLambda, mspecs[1], 'green', 'rest model specB' ], [ restLambda, shiftedFlux[0], 'orange', 'shift model specA' ], [ restLambda, shiftedFlux[1], 'purple', 'shift model specB' ]], [params[0][0], params[0][1]], 'Binary Model Gen - Prelim. Proc.', folder='model_gen'); return totalFlux
def eval(x, fiber='combo', sparse=False):
"""
NAME:
eval
PURPOSE:
evaluate the LSF for a given fiber
INPUT:
x - Array of X values for which to compute the LSF, in pixel offset relative to pixel centers; the LSF is calculated at the x offsets for each pixel center; x need to be 1/integer equally-spaced pixel offsets
fiber= ('combo') fiber number or 'combo' for an average LSF (uses the same one-based indexing as the APOGEE fibers [i.e., fibers range from 1 to 300])
sparse= (False) if True, return a sparse representation that can be passed to apogee.spec.lsf.convolve for easy convolution
OUTPUT:
LSF(x|pixel center);
pixel centers are apStarWavegrid if dx=1, and denser 1/integer versions if dx=1/integer
HISTORY:
2015-03-12 - Written based on Jon H's code (based on David N's code) - Bovy (IAS)
"""
# Parse fiber input
if isinstance(fiber, str) and fiber.lower() == 'combo':
fiber = [50, 100, 150, 200, 250, 300]
elif isinstance(fiber, int):
fiber = [fiber]
elif not isinstance(fiber, list) and isinstance(fiber[0], int):
raise ValueError(
'fiber input to apogee.spec.lsf.eval not understood ...')
# Are the x unit pixels or a fraction 1/hires thereof?
hires = int(round(1. / (x[1] - x[0])))
# Setup output
wav = apStarWavegrid()
l10wav = numpy.log10(wav)
dowav = l10wav[1] - l10wav[0]
# Hi-res wavelength for output
hireswav = 10.**numpy.arange(l10wav[0], l10wav[-1] + dowav / hires,
dowav / hires)
out = numpy.zeros((len(hireswav), len(x)))
for chip in ['a', 'b', 'c']:
# Get pixel array for this chip, use fiber[0] for consistency if >1 fib
pix = wave2pix(hireswav, chip, fiber[0])
dx = numpy.roll(
pix,
-hires,
) - pix
dx[-1] = dx[-1 - hires]
dx[-2] = dx[-2 - hires]
dx[-3] = dx[-3 - hires]
xs= numpy.tile(x,(len(hireswav),1))\
*numpy.tile(dx,(len(x),1)).T # nwav,nx
gd = True ^ numpy.isnan(pix)
# Read LSF file for this chip
lsfpars = apread.apLSF(chip, ext=0)
# Loop through the fibers
for fib in fiber:
out[gd] += raw(xs[gd], pix[gd], lsfpars[:, 300 - fib])
out[out < 0.] = 0.
out /= numpy.tile(numpy.sum(out, axis=1), (len(x), 1)).T
if sparse: out = sparsify(out)
return out
def eval(x,fiber='combo',sparse=False):
"""
NAME:
eval
PURPOSE:
evaluate the LSF for a given fiber
INPUT:
x - Array of X values for which to compute the LSF, in pixel offset relative to pixel centers; the LSF is calculated at the x offsets for each pixel center; x need to be 1/integer equally-spaced pixel offsets
fiber= ('combo') fiber number or 'combo' for an average LSF (uses the same one-based indexing as the APOGEE fibers [i.e., fibers range from 1 to 300])
sparse= (False) if True, return a sparse representation that can be passed to apogee.spec.lsf.convolve for easy convolution
OUTPUT:
LSF(x|pixel center);
pixel centers are apStarWavegrid if dx=1, and denser 1/integer versions if dx=1/integer
HISTORY:
2015-03-12 - Written based on Jon H's code (based on David N's code) - Bovy (IAS)
"""
# Parse fiber input
if isinstance(fiber,str) and fiber.lower() == 'combo':
fiber= [50,100,150,200,250,300]
elif isinstance(fiber,int):
fiber= [fiber]
elif not isinstance(fiber,list) and isinstance(fiber[0],int):
raise ValueError('fiber input to apogee.spec.lsf.eval not understood ...')
# Are the x unit pixels or a fraction 1/hires thereof?
hires= int(round(1./(x[1]-x[0])))
# Setup output
wav= apStarWavegrid()
l10wav= numpy.log10(wav)
dowav= l10wav[1]-l10wav[0]
# Hi-res wavelength for output
hireswav= 10.**numpy.arange(l10wav[0],l10wav[-1]+dowav/hires,dowav/hires)
out= numpy.zeros((len(hireswav),len(x)))
for chip in ['a','b','c']:
# Get pixel array for this chip, use fiber[0] for consistency if >1 fib
pix= wave2pix(hireswav,chip,fiber[0])
dx= numpy.roll(pix,-hires,)-pix
dx[-1]= dx[-1-hires]
dx[-2]= dx[-2-hires]
dx[-3]= dx[-3-hires]
xs= numpy.tile(x,(len(hireswav),1))\
*numpy.tile(dx,(len(x),1)).T # nwav,nx
gd= True-numpy.isnan(pix)
# Read LSF file for this chip
lsfpars= apread.apLSF(chip,ext=0)
# Loop through the fibers
for fib in fiber:
out[gd]+= raw(xs[gd],pix[gd],lsfpars[:,300-fib])
out[out<0.]= 0.
out/= numpy.tile(numpy.sum(out,axis=1),(len(x),1)).T
if sparse: out= sparsify(out)
return out
def equishwidth(elem,spec,specerr,refspec=None):
"""
NAME:
equishwidth
PURPOSE:
return an equivalent-width-ish quantity for a given element:
equishwidth = \sum_lam \Delta lam_center of window x (refspec-spec)/refspec x window/specerr^2 / \sum_lam window/specerr^2
or if refspec == 0:
equishwidth = \sum_lam \Delta lam_center of window x (1-spec) x window/specerr^2 / \sum_lam window/specerr^2
INPUT:
elem - element to consider
spec - spectrum on apStarWavegrid (nwave)
specerr - error on the spectrum on apStarWavegrid (nwave)
refspec= reference spectrum (assumed to be zero if absent)
OUTPUT:
equivalent-ish-width
HISTORY:
2015-02-11 - Written - Bovy (IAS@KITP)
"""
if refspec is None:
refspec= numpy.zeros_like(spec)
# Read windows
win= read(elem,apStarWavegrid=True)
startindxs, endindxs= waveregions(elem,asIndex=True,pad=0)
import apogee.spec.plot as splot
lams= splot.apStarWavegrid()
startlams= lams[startindxs]
endlams= lams[endindxs]
outval= 0.
norm= 0.
for (startindx,endindx,startlam,endlam) \
in zip(startindxs,endindxs,startlams,endlams):
norm+= numpy.sum(win[startindx:endindx]\
/specerr[startindx:endindx]**2.)
if not numpy.all(refspec == 0.):
outval+= (endlam-startlam)/(endindx-startindx)\
*numpy.sum(win[startindx:endindx]/specerr[startindx:endindx]**2.\
*(1.-spec[startindx:endindx]/refspec[startindx:endindx]))
else:
outval+= (endlam-startlam)/(endindx-startindx)\
*numpy.sum(win[startindx:endindx]/specerr[startindx:endindx]**2.\
*(1.-spec[startindx:endindx]))
outval/= norm
return outval
def equishwidth(elem,spec,specerr,refspec=None):
"""
NAME:
equishwidth
PURPOSE:
return an equivalent-width-ish quantity for a given element:
equishwidth = \sum_lam \Delta lam_center of window x (refspec-spec)/refspec x window/specerr^2 / \sum_lam window/specerr^2
or if refspec == 0:
equishwidth = \sum_lam \Delta lam_center of window x (1-spec) x window/specerr^2 / \sum_lam window/specerr^2
INPUT:
elem - element to consider
spec - spectrum on apStarWavegrid (nwave)
specerr - error on the spectrum on apStarWavegrid (nwave)
refspec= reference spectrum (assumed to be zero if absent)
OUTPUT:
equivalent-ish-width
HISTORY:
2015-02-11 - Written - Bovy (IAS@KITP)
"""
if refspec is None:
refspec= numpy.zeros_like(spec)
# Read windows
win= read(elem,apStarWavegrid=True)
startindxs, endindxs= waveregions(elem,asIndex=True,pad=0)
import apogee.spec.plot as splot
lams= splot.apStarWavegrid()
startlams= lams[startindxs]
endlams= lams[endindxs]
outval= 0.
norm= 0.
for (startindx,endindx,startlam,endlam) \
in zip(startindxs,endindxs,startlams,endlams):
norm+= numpy.sum(win[startindx:endindx]\
/specerr[startindx:endindx]**2.)
if not numpy.all(refspec == 0.):
outval+= (endlam-startlam)/(endindx-startindx)\
*numpy.sum(win[startindx:endindx]/specerr[startindx:endindx]**2.\
*(1.-spec[startindx:endindx]/refspec[startindx:endindx]))
else:
outval+= (endlam-startlam)/(endindx-startindx)\
*numpy.sum(win[startindx:endindx]/specerr[startindx:endindx]**2.\
*(1.-spec[startindx:endindx]))
outval/= norm
return outval
def measure_apogee(allStar, linelist_obj, output_fits=False, *args, **kwargs):
if isinstance(linelist_obj, str):
linelist_obj = linelist.Linelist(linelist_obj)
loc_ids, apogee_ids = make_speclist(allStar)
lams = splot.apStarWavegrid()
ews = np.empty([np.shape(allStar)[0], np.shape(linelist_obj.labels)[0]])
errs = np.empty([np.shape(allStar)[0], np.shape(linelist_obj.labels)[0]])
try:
dr = int(_DEFAULT_DR)
except ValueError:
dr = 16
if dr <= 13:
lockey = 'LOCATION_ID'
else:
lockey = 'FIELD'
for i in tqdm(range(len(apogee_ids))):
try:
try:
loc, id = str(allStar[lockey][i],
'utf-8'), str(allStar['APOGEE_ID'][i], 'utf-8')
except (UnicodeDecodeError, AttributeError, TypeError):
if isinstance(allStar[lockey][i], str):
loc, id = allStar[lockey][i], allStar['APOGEE_ID'][i]
else:
raise IOError(
'Input allStar file seems to be incorrectly formatted, please check that the FIELD and APOGEE_ID fields are readable, and read in as either bytes or string'
)
scope = allStar['TELESCOPE'][i]
specs, hdr = apread.aspcapStar(loc, id, ext=1, telescope=scope)
errspec, hdr = apread.aspcapStar(loc, id, ext=2, telescope=scope)
spec = np.dstack([lams, specs, errspec])[0]
out = equivalentwidths.measurelinelist(spec,
linelist_obj,
error=True,
*args,
**kwargs)
ews[i], errs[i] = out[0], out[1]
except IOError:
print(
'Spectrum missing from SAS? Check that your RESULTS_VERS is set correctly.'
)
ews[i], errs[i] = np.ones(np.shape(
linelist_obj.labels)[0]) * np.nan, np.ones(
np.shape(linelist_obj.labels)[0]) * np.nan
return ews, errs
def lines(elem):
"""
NAME:
lines
PURPOSE:
return the location of peaks in the window weight ('lines') for a given element
INPUT:
elem - element
OUTPUT:
wavelengths of peaks in \AA
HISTORY:
2015-03-11 - Written - Bovy (IAS)
"""
# Load the window
win= read(elem,apStarWavegrid=True)
import apogee.spec.plot as splot
wavs= splot.apStarWavegrid()
# Find peaks
indx= (numpy.roll(win,1) < win)*(numpy.roll(win,-1) < win)\
*(win > 0.1)
return wavs[indx]
def vmacro(x, vmacro=6., sparse=False, norm=True):
"""
NAME:
vmacro
PURPOSE:
compute the proper macroturbulence kernel
INPUT:
x - Array of X values for which to compute the macroturbulence kernel, in pixel offset relative to pixel centers; the kernel is calculated at the x offsets for each pixel center; x need to be 1/integer equally-spaced pixel offsets
vmacro= (6.) macroturbulence in km/s (FWHM)
sparse= (False) if True, return a sparse representation that can be passed to apogee.spec.lsf.convolve for easy convolution
norm= (True) if False, don't normalize to sum to 1 (useful to check whether the kernel actually integrates to 1)
OUTPUT:
LSF-like array of the macroturbulence
HISTORY:
2015-03-23 - Written - Bovy (IAS)
"""
from apogee.spec.lsf import sparsify
# Convert vmacro to Gaussian sigma / c
sigvm = vmacro / 3. / 10.**5. / 2. / numpy.sqrt(2. * numpy.log(2.))
# Are the x unit pixels or a fraction 1/hires thereof?
hires = int(1. / (x[1] - x[0]))
# Setup output
wav = apStarWavegrid()
l10wav = numpy.log10(wav)
dowav = l10wav[1] - l10wav[0]
# Hi-res wavelength for output
hireswav = 10.**numpy.arange(l10wav[0], l10wav[-1] + dowav / hires,
dowav / hires)
# Calculate kernel
lam = numpy.tile(hireswav, (len(x), 1)).T
dlam= 10.**(numpy.tile(numpy.log10(hireswav),(len(x),1)).T\
+numpy.tile(x,(len(hireswav),1))*dowav)/lam-1.
u = numpy.fabs(dlam / sigvm)
out= 2./numpy.sqrt(numpy.pi)*u\
*(numpy.exp(-u**2.)/u-numpy.sqrt(numpy.pi)*special.erfc(u))
out[dlam == 0.] = 2. / numpy.sqrt(numpy.pi)
out *= (1. + dlam) * numpy.log(10.) / sigvm
if norm: out /= numpy.tile(numpy.sum(out, axis=1), (len(x), 1)).T
if sparse: out = sparsify(out)
return out
def vmacro(x,vmacro=6.,sparse=False,norm=True):
"""
NAME:
vmacro
PURPOSE:
compute the proper macroturbulence kernel
INPUT:
x - Array of X values for which to compute the macroturbulence kernel, in pixel offset relative to pixel centers; the kernel is calculated at the x offsets for each pixel center; x need to be 1/integer equally-spaced pixel offsets
vmacro= (6.) macroturbulence in km/s (FWHM)
sparse= (False) if True, return a sparse representation that can be passed to apogee.spec.lsf.convolve for easy convolution
norm= (True) if False, don't normalize to sum to 1 (useful to check whether the kernel actually integrates to 1)
OUTPUT:
LSF-like array of the macroturbulence
HISTORY:
2015-03-23 - Written - Bovy (IAS)
"""
from apogee.spec.lsf import sparsify
# Convert vmacro to Gaussian sigma / c
sigvm= vmacro/3./10.**5./2./numpy.sqrt(2.*numpy.log(2.))
# Are the x unit pixels or a fraction 1/hires thereof?
hires= int(1./(x[1]-x[0]))
# Setup output
wav= apStarWavegrid()
l10wav= numpy.log10(wav)
dowav= l10wav[1]-l10wav[0]
# Hi-res wavelength for output
hireswav= 10.**numpy.arange(l10wav[0],l10wav[-1]+dowav/hires,dowav/hires)
# Calculate kernel
lam= numpy.tile(hireswav,(len(x),1)).T
dlam= 10.**(numpy.tile(numpy.log10(hireswav),(len(x),1)).T\
+numpy.tile(x,(len(hireswav),1))*dowav)/lam-1.
u= numpy.fabs(dlam/sigvm)
out= 2./numpy.sqrt(numpy.pi)*u\
*(numpy.exp(-u**2.)/u-numpy.sqrt(numpy.pi)*special.erfc(u))
out[dlam == 0.]= 2./numpy.sqrt(numpy.pi)
out*= (1.+dlam)*numpy.log(10.)/sigvm
if norm: out/= numpy.tile(numpy.sum(out,axis=1),(len(x),1)).T
if sparse: out= sparsify(out)
return out
def shiftFlux(spec, vel): ''' Shifts flux provided. May want to allow user to pass restLambda in so we don't generate it again... :param spec: The spectrum to shift :param vel: The velocity to shift by :return: The shifted spectrum ''' # Generate the wavelength grid restLambda = splot.apStarWavegrid() if (len(spec.shape) > 1): # Calculates wavelength grid for the second star with a doppler shift shiftLambda = [restLambda * (1. + v / (const.c / 1000.)) for v in vel] # The fluxes of both stars shiftedFlux = [np.interp(restLambda, shiftLambda[i], spec[i]) for i in range(len(shiftLambda))] else: # Calculates wavelength grid for the second star with a doppler shift shiftLambda = restLambda * (1. + vel / (const.c / 1000.)) # The fluxes of both stars shiftedFlux = np.interp(restLambda, shiftLambda, spec) return shiftedFlux
def windows(*args,**kwargs):
"""
NAME:
windows
PURPOSE:
Generate model APOGEE spectra using Turbospectrum in selected wavelength windows (but the whole APOGEE spectral range is returned): this is a general routine that generates the non-continuum-normalized spectrum, convolves with the LSF and macrotubulence, and optionally continuum normalizes the output; use 'turbosynth' for a direct interface to Turbospectrum
INPUT ARGUMENTS:
Windows specification: Provide one of
(1) Element string: the APOGEE windows for this element will be loaded
(2) startindxs, endindxs= start and end indexes of the windows on the apStar wavelength grid
(3) startlams, endlams= start and end wavelengths in \AA
lists with abundance differences wrt the atmosphere (they don't all have to have the same length, missing ones are filled in with zeros):
[Atomic number1,diff1_1,diff1_2,diff1_3,...,diff1_N]
[Atomic number2,diff2_1,diff2_2,diff2_3,...,diff2_N]
...
[Atomic numberM,diffM_1,diffM_2,diffM_3,...,diffM_N]
INPUT KEYWORDS:
BASELINE: you can specify the baseline spectrum and the continuous opacity to not always re-compute it
baseline= baseline c-normalized spectrum on Turbospectrum wavelength grid (obtained from turbosynth)
mwav= Turbospectrum wavelength grid (obtained from turbosynth)
cflux= continuum flux from Turbospectrum
modelopac= (None)
(a) if set to an existing filename: assume babsma_lu has already been run and use this continuous opacity in bsyn_lu
(b) if set to a non-existing filename: store the continuous opacity in this file
Typically, you can obtain these three keywords by doing (kwargs are the keywords you provide to this function as well, and includes modelopac='SOME FILENAME')
>>> baseline= turbosynth(**kwargs)
>>> mwav= baseline[0]
>>> cflux= baseline[2]/baseline[1]
>>> baseline= baseline[1]
LSF:
lsf= ('all') LSF to convolve with; output of apogee.spec.lsf.eval; sparsify for efficiency; if 'all' or 'combo' a pre-computed version will be downloaded from the web
Either:
xlsf= (None) pixel offset grid on which the LSF is computed (see apogee.spec.lsf.eval); unnecessary if lsf=='all' or 'combo'
dxlsf= (None) spacing of pixel offsets
vmacro= (6.) macroturbulence to apply
CONTINUUM:
cont= ('aspcap') continuum-normalization to apply:
None: no continuum normalization
'true': Use the true continuum
'aspcap': Use the continuum normalization method of ASPCAP DR12
'cannon': Normalize using continuum pixels derived from the Cannon
SYNTHESIS:
air= (True) if True, perform the synthesis in air wavelengths (output is still in vacuum); set to False at your own risk, as Turbospectrum expects the linelist in air wavelengths!)
Hlinelist= (None) Hydrogen linelists to use; can be set to the path of a linelist file or to the name of an APOGEE linelist; if None, then we first search for the Hlinedata.vac in the APOGEE linelist directory (if air=False) or we use the internal Turbospectrum Hlinelist (if air=True)
linelist= (None) molecular and atomic linelists to use; can be set to the path of a linelist file or to the name of an APOGEE linelist, or lists of such files; if a single filename is given, the code will first search for files with extensions '.atoms', '.molec' or that start with 'turboatoms.' and 'turbomolec.'
wmin, wmax, dw= (15000.000, 17000.000, 0.10000000, 7.0000000) spectral synthesis limits, step, and width of calculation (see MOOG)
costheta= (1.) cosine of the viewing angle
MODEL ATMOSPHERE PARAMETERS:
Specify one of the following:
(a) modelatm= (None) model-atmosphere instance
(b) parameters of a KURUCZ model atmosphere:
(1) teff= (4500) Teff
logg= (2.5) logg
metals= (0.) metallicity
cm= (0.) carbon-enhancement
am= (0.) alpha-enhancement
(2) fparam= standard ASPCAP output format
lib= ('kurucz_filled') model atmosphere library
vmicro= (2.) microturbulence (only used if the MOOG-formatted atmosphere is not found) (can also be part of fparam)
MISCELLANEOUS:
dr= return the path corresponding to this data release
raw= (False) if True, return the raw turbosynth output
OUTPUT:
spectra (nspec,nwave)
(wavelengths,cont-norm. spectrum, spectrum (nwave)) if raw == True
HISTORY:
2015-04-17 - Written - Bovy (IAS)
"""
# Pop some kwargs
baseline= kwargs.pop('baseline',None)
mwav= kwargs.pop('mwav',None)
cflux= kwargs.pop('cflux',None)
raw= kwargs.pop('raw',False)
# Check that we have the LSF and store the relevant keywords
lsf= kwargs.pop('lsf','all')
if isinstance(lsf,str):
xlsf, lsf= aplsf._load_precomp(dr=kwargs.get('dr',None),fiber=lsf)
dxlsf= None
else:
xlsf= kwargs.pop('xlsf',None)
dxlsf= kwargs.pop('dxlsf',None)
if xlsf is None and dxlsf is None: raise ValueError('xlsf= or dxlsf= input needs to be given if the LSF is given as an array')
vmacro= kwargs.pop('vmacro',6.)
# Parse continuum-normalization keywords
cont= kwargs.pop('cont','aspcap')
# Parse the wavelength regions
apWave= apStarWavegrid()
if isinstance(args[0],str): #element string given
si,ei= apwindow.waveregions(args[0],pad=3,asIndex=True)
args= args[1:]
else:
if isinstance(args[0][0],int): # assume index
si,ei= args[0], args[1]
else: # assume wavelengths in \AA
sl,el= args[0], args[1]
# Convert to index
si, ei= [], []
for s,e in zip(sl,el):
# Find closest index into apWave
si.append(numpy.argmin(numpy.fabs(s-apWave)))
ei.append(numpy.argmin(numpy.fabs(e-apWave)))
args= args[2:]
# Setup the model atmosphere
modelatm= kwargs.pop('modelatm',None)
# Parse fparam, if present
fparam= kwargs.pop('fparam',None)
if not fparam is None:
kwargs['teff']= fparam[0,paramIndx('TEFF')]
kwargs['logg']= fparam[0,paramIndx('LOGG')]
kwargs['metals']= fparam[0,paramIndx('METALS')]
kwargs['am']= fparam[0,paramIndx('ALPHA')]
kwargs['cm']= fparam[0,paramIndx('C')]
kwargs['vmicro']= 10.**fparam[0,paramIndx('LOG10VDOP')]
# Need to pass a model atmosphere instance to turbosynth (needs to be made
# more efficient, because now turbosynth always write the atmosphere
if modelatm is None: # Setup a model atmosphere
modelatm= atlas9.Atlas9Atmosphere(teff=kwargs.get('teff',4500.),
logg=kwargs.get('logg',2.5),
metals=kwargs.get('metals',0.),
am=kwargs.get('am',0.),
cm=kwargs.get('cm',0.),
dr=kwargs.get('dr',None))
if isinstance(modelatm,str) and os.path.exists(modelatm):
raise ValueError('modelatm= input is an existing filename, but you need to give an Atmosphere object instead')
elif isinstance(modelatm,str):
raise ValueError('modelatm= input needs to be an Atmosphere instance')
# Check temperature
if modelatm._teff > 7000.:
warnings.warn('Turbospectrum does not include all necessary physics to model stars hotter than about 7000 K; proceed with caution',RuntimeWarning)
kwargs['modelatm']= modelatm
try:
rmModelopac= False
if not 'modelopac' in kwargs:
rmModelopac= True
kwargs['modelopac']= tempfile.mktemp('mopac')
# Make sure opacity is first calculated over the full wav. range
kwargs['babsma_wmin']= 15000.
kwargs['babsma_wmax']= 17000.
elif 'modelopac' in kwargs and not isinstance(kwargs['modelopac'],str):
raise ValueError('modelopac needs to be set to a filename')
# Run synth for the whole wavelength range as a baseline
if baseline is None or mwav is None or cflux is None:
baseline= turbosynth(**kwargs)
mwav= baseline[0]
cflux= baseline[2]/baseline[1]
baseline= baseline[1]
elif isinstance(baseline,tuple): #probably accidentally gave the entire output of turbosynth
mwav= baseline[0]
cflux= baseline[2]/baseline[1]
baseline= baseline[1]
# Convert the apStarWavegrid windows to turboWavegrid regions
sm,em= [], []
for start,end in zip(si,ei):
if kwargs.get('air',True):
sm.append(numpy.argmin(numpy.fabs(vac2air(apWave[start])-mwav)))
em.append(numpy.argmin(numpy.fabs(vac2air(apWave[end])-mwav)))
else:
sm.append(numpy.argmin(numpy.fabs(apWave[start]-mwav)))
em.append(numpy.argmin(numpy.fabs(apWave[end]-mwav)))
# Run Turbospectrum synth for all abundances and all windows
if len(args) == 0: #special case that there are *no* differences
args= ([26,0.],)
nsynths= numpy.array([len(args[ii])-1 for ii in range(len(args))])
nsynth= numpy.amax(nsynths) #Take the longest abundance list
out= numpy.tile(baseline,(nsynth,1))
# Run all windows
for start, end in zip(sm,em):
kwargs['wmin']= mwav[start]
kwargs['wmax']= mwav[end]+0.001
for ii in range(nsynth):
newargs= ()
for jj in range(len(args)):
tab= [args[jj][0]]
if len(args[jj]) > ii+1:
tab.append(args[jj][ii+1])
newargs= newargs+(tab,)
tmpOut= turbosynth(*newargs,**kwargs)
if numpy.isnan(tmpOut[1][-1]):
# NaN returned for reasons that I don't understand
out[ii,start:end]= tmpOut[1][:-1]
else:
out[ii,start:end+1]= tmpOut[1]
except: raise
finally:
if rmModelopac and os.path.exists(kwargs['modelopac']):
os.remove(kwargs['modelopac'])
kwargs.pop('modelopac')
# Now multiply each continuum-normalized spectrum with the continuum
out*= numpy.tile(cflux,(nsynth,1))
if raw: return (mwav,out/numpy.tile(cflux,(nsynth,1)),out)
# If the synthesis was done in air, convert wavelength array
if kwargs.get('air',True):
mwav= numpy.array([air2vac(w) for w in list(mwav)])
# Now convolve with the LSF
out= aplsf.convolve(mwav,out,
lsf=lsf,xlsf=xlsf,dxlsf=dxlsf,vmacro=vmacro)
# Now continuum-normalize
if cont.lower() == 'true':
# Get the true continuum on the apStar wavelength grid
apWave= apStarWavegrid()
baseline= numpy.polynomial.Polynomial.fit(mwav,cflux,4)
ip= interpolate.InterpolatedUnivariateSpline(mwav,
cflux/baseline(mwav),
k=3)
cflux= baseline(apWave)*ip(apWave)
# Divide it out
out/= numpy.tile(cflux,(nsynth,1))
elif not cont is None:
cflux= apcont.fit(out,numpy.ones_like(out),type=cont)
out[cflux > 0.]/= cflux[cflux > 0.]
out[cflux <= 0.]= numpy.nan
return out
def convolve(wav,spec,
lsf=None,xlsf=None,dxlsf=None,fiber='combo',
vmacro=6.):
"""
NAME:
convolve
PURPOSE:
convolve with the APOGEE LSF and resample to APOGEE's apStar wavelength grid
INPUT:
wav - wavelength array (linear in wavelength in \AA)
spec - spectrum on wav wavelength grid [nspec,nwave]
lsf= (None) pre-calculated LSF array from apogee.spec.lsf.eval
Either:
xlsf= (None) 1/integer equally-spaced pixel offsets at which the lsf=lsf input is calculated
dxlsf= (None) spacing of pixel offsets
fiber= if lsf is None, the LSF is calculated for this fiber
vmacro= (6.) Gaussian macroturbulence smoothing to apply as well (FWHM or a [sparse] matrix like lsf on the same x grid; can be computed with apogee.modelspec.vmacro)
OUTPUT:
spectrum on apStar wavelength grid
HISTORY:
2015-03-14 - Written - Bovy (IAS)
"""
# Parse LSF input
if lsf is None:
xlsf= numpy.linspace(-7.,7.,43)
lsf= eval(xlsf,fiber=fiber)
if not isinstance(lsf,sparse.dia_matrix):
lsf= sparsify(lsf)
if dxlsf is None:
dx= xlsf[1]-xlsf[0]
else:
dx= dxlsf
hires= int(round(1./dx))
l10wav= numpy.log10(apStarWavegrid())
dowav= l10wav[1]-l10wav[0]
tmpwav= 10.**numpy.arange(l10wav[0],l10wav[-1]+dowav/hires,dowav/hires)
tmp= numpy.empty(len(l10wav)*hires)
# Setup vmacro
if not vmacro is None and isinstance(vmacro,float):
sigvm= vmacro/3./10.**5./numpy.log(10.)*hires/dowav\
/2./numpy.sqrt(2.*numpy.log(2.))
# Interpolate the input spectrum, starting from a polynomial baseline
if len(spec.shape) == 1: spec= numpy.reshape(spec,(1,len(spec)))
nspec= spec.shape[0]
tmp= numpy.empty((nspec,len(tmpwav)))
for ii in range(nspec):
baseline= numpy.polynomial.Polynomial.fit(wav,spec[ii],4)
ip= interpolate.InterpolatedUnivariateSpline(wav,
spec[ii]/baseline(wav),
k=3)
tmp[ii]= baseline(tmpwav)*ip(tmpwav)
# Add macroturbulence
if not vmacro is None and isinstance(vmacro,float):
tmp= ndimage.gaussian_filter1d(tmp,sigvm,mode='constant',axis=1)
elif not vmacro is None:
# Use sparse representations to quickly calculate the convolution
tmp= sparse.csr_matrix(tmp)
if isinstance(vmacro,numpy.ndarray):
vmacro= sparsify(vmacro)
tmp= vmacro.dot(tmp.T).T
if not isinstance(lsf,sparse.csr_matrix):
# Use sparse representations to quickly calculate the convolution
tmp= sparse.csr_matrix(tmp)
return lsf.dot(tmp.T).T.toarray()[:,::hires]
def deconvolve(spec,specerr,
lsf=None,eps=2500.,smooth=None):
"""
NAME:
deconvolve
PURPOSE:
deconvolve the LSF
INPUT:
spec - spectrum (nwave)
specerr - spectrum uncertainty array (nwave)
lsf= (None) LSF to deconvolve, needs to be specified in non-sparse format
eps= (2500.) smoothness parameter
smooth= (None) if set to a resolution, smooth with a FWHM resolution of 'smooth' and return the spectrum on the apStar wavelength grid
OUTPUT:
high-resolution deconvolved spectrum or smoothed deconvolved spectrum on apStar wavelength grid is smooth= is set
HISTORY:
2015-04-24 - Written - Bovy (IAS)
"""
# Parse LSF input
if lsf is None:
raise ValueError("lsf= keyword with LSF in non-sparse format required for apogee.spec.lsf.deconvolve")
if isinstance(lsf,sparse.dia_matrix):
raise ValueError("lsf= keyword with LSF needs to be in non-sparse format")
lsf[numpy.isnan(lsf)]= 0.
# How much higher resolution is the LSF than the data?
hires= int(round(lsf.shape[0]/8575.))
# Setup output
out= numpy.zeros(lsf.shape[0])
# Loop through the detectors and analyze each one separately
for sindx, eindx in zip([140,3450,6250],[3370,6200,8450]):
# Get the LSF for this detector
slsf= sparsify(lsf[hires*sindx:hires*eindx])
# Parse the spectrum and its error for this detector, normalize
tspec= numpy.ones((eindx-sindx)*hires)
tinvspecerr= numpy.zeros((eindx-sindx)*hires)
norm= numpy.nanmean(spec[sindx:eindx])
tspec[::hires]= spec[sindx:eindx]/norm
tinvspecerr[::hires]= norm/specerr[sindx:eindx]
# Deal with NaNs
tinvspecerr[numpy.isnan(tspec)]= 0.
tspec[numpy.isnan(tspec)]= 1.
# Set up the necessary sparse matrices
Cinv= sparse.diags([tinvspecerr**2.],[0])
CinvL= Cinv.dot(slsf)
LTCinvL= (slsf.T).dot(CinvL)
# P smoothness matrix
diags1= -numpy.ones(slsf.shape[1])
diags1[-1]= 0.
diags2= numpy.ones(slsf.shape[1]-1)
P= sparse.diags([diags1,diags2],[0,1])
A= LTCinvL+eps*(P.T).dot(P)
# b
Cinvs= Cinv.dot(tspec)
b= (slsf.T).dot(Cinvs)
tmp= scipy.sparse.linalg.bicg(A,b)
if tmp[1] == 0:
tmp= tmp[0]
else:
raise RuntimeError("Deconvolution did not converge")
out[sindx*hires:eindx*hires]= tmp*norm
if not smooth is None:
wav= apStarWavegrid()
l10wav= numpy.log10(wav)
dowav= l10wav[1]-l10wav[0]
sigvm= hires/dowav/smooth/numpy.log(10.)\
/2./numpy.sqrt(2.*numpy.log(2.))
out= ndimage.gaussian_filter1d(out,sigvm,mode='constant')[::hires]
return out
def waveregions(elem,asIndex=False,pad=0,dr=None):
"""
NAME:
waveregions
PURPOSE:
return the wavelength regions corresponding to different elements
INPUT:
elem - element
asIndx= (False) if yes, return the indices into an apStar-like wavelength grid rather than the wavelengths directly
pad= (0) pad on each side by this many log10 wavelengths in 6e-6 (changes how windows are combined)
dr= read the window corresponding to this data release
OUTPUT:
(startlams,endlams) or (startindxs, endindxs)
BUGS:
range that comes out of asIndex=True is (or can be) different from that of asIndex=False
HISTORY:
2015-01-26 - Written - Bovy (IAS@KITP)
"""
# Load the window
win= read(elem,apStarWavegrid=True,dr=dr)
# Calculate number of contiguous regions, assume this is not at the edge
mask= ((win > 0.)*(True-numpy.isnan(win))).astype('int')
dmaskp= numpy.roll(mask,-1)-mask
dmaskn= numpy.roll(mask,1)-mask
# Calculate the distance between adjacent windows and combine them if close
import apogee.spec.plot as splot
l10wavs= numpy.log10(splot.apStarWavegrid())
indices= numpy.arange(len(l10wavs))
if asIndex:
startindxs= indices[dmaskp == 1.]
endindxs= indices[dmaskn == 1.]
startl10lams= l10wavs[dmaskp == 1.]
endl10lams= l10wavs[dmaskn == 1.]
if pad > 0:
if asIndex:
startindxs= [si-pad for si in startindxs]
endindxs= [ei+pad for ei in endindxs]
startl10lams-= pad*splot._DLOG10LAMBDA
endl10lams+= pad*splot._DLOG10LAMBDA
# Check that each window is at least _MINWIDTH wide
width= 10.**endl10lams-10.**startl10lams
for ii in range(len(startl10lams)):
if width[ii] < _MINWIDTH:
if asIndex: # Approximate
dindx= int(numpy.ceil((_MINWIDTH-width[ii])/2.\
/(10.**startl10lams[ii]\
+10.**endl10lams[ii])/2.\
/numpy.log(10.)/splot._DLOG10LAMBDA))
startindxs[ii]-= dindx
endindxs[ii]+= dindx
startl10lams[ii]= numpy.log10(10.**startl10lams[ii]\
-(_MINWIDTH-width[ii])/2.)
endl10lams[ii]= numpy.log10(10.**endl10lams[ii]\
+(_MINWIDTH-width[ii])/2.)
diff= numpy.roll(startl10lams,-1)-endl10lams
if asIndex:
newStartindxs, newEndindxs= [startindxs[0]], [endindxs[0]]
newStartl10lams, newEndl10lams= [startl10lams[0]], [endl10lams[0]]
winIndx= 0
for ii in range(len(startl10lams)-1):
if diff[ii] < 10.*splot._DLOG10LAMBDA:
if asIndex:
newEndindxs[winIndx]= endindxs[ii+1]
newEndl10lams[winIndx]= endl10lams[ii+1]
else:
if asIndex:
newStartindxs.append(startindxs[ii+1])
newEndindxs.append(endindxs[ii+1])
newStartl10lams.append(startl10lams[ii+1])
newEndl10lams.append(endl10lams[ii+1])
winIndx+= 1
if asIndex:
return (newStartindxs,newEndindxs)
else:
return (10.**numpy.array(newStartl10lams),
10.**numpy.array(newEndl10lams))
def waveregions(elem,asIndex=False,pad=0,dr=None):
"""
NAME:
waveregions
PURPOSE:
return the wavelength regions corresponding to different elements
INPUT:
elem - element
asIndx= (False) if yes, return the indices into an apStar-like wavelength grid rather than the wavelengths directly
pad= (0) pad on each side by this many log10 wavelengths in 6e-6 (changes how windows are combined)
dr= read the window corresponding to this data release
OUTPUT:
(startlams,endlams) or (startindxs, endindxs)
BUGS:
range that comes out of asIndex=True is (or can be) different from that of asIndex=False
HISTORY:
2015-01-26 - Written - Bovy (IAS@KITP)
"""
# Load the window
win= read(elem,apStarWavegrid=True,dr=dr)
# Calculate number of contiguous regions, assume this is not at the edge
mask= ((win > 0.)*(True-numpy.isnan(win))).astype('int')
dmaskp= numpy.roll(mask,-1)-mask
dmaskn= numpy.roll(mask,1)-mask
# Calculate the distance between adjacent windows and combine them if close
import apogee.spec.plot as splot
l10wavs= numpy.log10(splot.apStarWavegrid())
indices= numpy.arange(len(l10wavs))
if asIndex:
startindxs= indices[dmaskp == 1.]
endindxs= indices[dmaskn == 1.]
startl10lams= l10wavs[dmaskp == 1.]
endl10lams= l10wavs[dmaskn == 1.]
if pad > 0:
if asIndex:
startindxs= [si-pad for si in startindxs]
endindxs= [ei+pad for ei in endindxs]
startl10lams-= pad*splot._DLOG10LAMBDA
endl10lams+= pad*splot._DLOG10LAMBDA
# Check that each window is at least _MINWIDTH wide
width= 10.**endl10lams-10.**startl10lams
for ii in range(len(startl10lams)):
if width[ii] < _MINWIDTH:
if asIndex: # Approximate
dindx= int(numpy.ceil((_MINWIDTH-width[ii])/2.\
/(10.**startl10lams[ii]\
+10.**endl10lams[ii])/2.\
/numpy.log(10.)/splot._DLOG10LAMBDA))
startindxs[ii]-= dindx
endindxs[ii]+= dindx
startl10lams[ii]= numpy.log10(10.**startl10lams[ii]\
-(_MINWIDTH-width[ii])/2.)
endl10lams[ii]= numpy.log10(10.**endl10lams[ii]\
+(_MINWIDTH-width[ii])/2.)
diff= numpy.roll(startl10lams,-1)-endl10lams
if asIndex:
newStartindxs, newEndindxs= [startindxs[0]], [endindxs[0]]
newStartl10lams, newEndl10lams= [startl10lams[0]], [endl10lams[0]]
winIndx= 0
for ii in range(len(startl10lams)-1):
if diff[ii] < 10.*splot._DLOG10LAMBDA:
if asIndex:
newEndindxs[winIndx]= endindxs[ii+1]
newEndl10lams[winIndx]= endl10lams[ii+1]
else:
if asIndex:
newStartindxs.append(startindxs[ii+1])
newEndindxs.append(endindxs[ii+1])
newStartl10lams.append(startl10lams[ii+1])
newEndl10lams.append(endl10lams[ii+1])
winIndx+= 1
if asIndex:
return (newStartindxs,newEndindxs)
else:
return (10.**numpy.array(newStartl10lams),
10.**numpy.array(newEndl10lams))
def windows(*args,**kwargs):
"""
NAME:
windows
PURPOSE:
Generate model APOGEE spectra using MOOG in selected wavelength windows (but the whole APOGEE spectral range is returned): this is a general routine that generates the non-continuum-normalized spectrum, convolves with the LSF and macrotubulence, and optionally continuum normalizes the output; use 'moogsynth' for a direct interface to MOOG
INPUT ARGUMENTS:
Windows specification: Provide one of
(1) Element string: the APOGEE windows for this element will be loaded
(2) startindxs, endindxs= start and end indexes of the windows on the apStar wavelength grid
(3) startlams, endlams= start and end wavelengths in \AA
lists with abundance differences wrt the atmosphere (they don't all have to have the same length, missing ones are filled in with zeros):
[Atomic number1,diff1_1,diff1_2,diff1_3,...,diff1_N]
[Atomic number2,diff2_1,diff2_2,diff2_3,...,diff2_N]
...
[Atomic numberM,diffM_1,diffM_2,diffM_3,...,diffM_N]
INPUT KEYWORDS:
BASELINE: you can specify the baseline spectrum to not always re-compute it
baseline= baseline c-normalized spectrum on MOOG wavelength grid (obtained from moogsynth)
mwav= MOOG wavelength grid (obtained from moogsynth)
cflux= continuum flux from MOOG
Typically, you can obtain these three keywords by doing (kwargs are the keywords you provide to this function as well)
>>> baseline= moogsynth(**kwargs)[1]
>>> mwav, cflux= moogsynth(doflux=True,**kwargs)
LSF:
lsf= ('all') LSF to convolve with; output of apogee.spec.lsf.eval; sparsify for efficiency; if 'all' or 'combo' a pre-computed version will be downloaded from the web
Either:
xlsf= (None) pixel offset grid on which the LSF is computed (see apogee.spec.lsf.eval); unnecessary if lsf=='all' or 'combo'
dxlsf= (None) spacing of pixel offsets
vmacro= (6.) macroturbulence to apply
CONTINUUM:
cont= ('aspcap') continuum-normalization to apply:
None: no continuum normalization
'true': Use the true continuum
'aspcap': Use the continuum normalization method of ASPCAP DR12
'cannon': Normalize using continuum pixels derived from the Cannon
SYNTHESIS:
linelist= (None) linelist to use; if this is None, the code looks for a weed-out version of the linelist appropriate for the given model atmosphere
run_weedout= (False) if True, run MOOG weedout on the linelist first
wmin, wmax, dw, width= (15000.000, 17000.000, 0.10000000, 7.0000000) spectral synthesis limits *for the whole spectrum* (not just the windows), step, and width of calculation (see MOOG)
MODEL ATMOSPHERE PARAMETERS:
Specify one of the following:
(a) modelatm= (None) can be set to the filename of a model atmosphere or to a model-atmosphere instance (if filename, needs to end in .mod)
(b) parameters of a KURUCZ model atmosphere:
(1) teff= (4500) Teff
logg= (2.5) logg
metals= (0.) metallicity
cm= (0.) carbon-enhancement
am= (0.) alpha-enhancement
(2) fparam= standard ASPCAP output format (
lib= ('kurucz_filled') model atmosphere library
dr= (None) use model atmospheres from this data release
vmicro= (2.) microturbulence (only used if the MOOG-formatted atmosphere is not found) (can also be part of fparam)
MISCELLANEOUS:
dr= return the path corresponding to this data release
OUTPUT:
spectra (nspec,nwave)
HISTORY:
2015-03-18 - Written - Bovy (IAS)
"""
# Pop some kwargs
run_weedout= kwargs.pop('run_weedout',False)
baseline= kwargs.pop('baseline',None)
mwav= kwargs.pop('mwav',None)
cflux= kwargs.pop('cflux',None)
# Check that we have the LSF and store the relevant keywords
lsf= kwargs.pop('lsf','all')
if isinstance(lsf,str):
xlsf, lsf= aplsf._load_precomp(dr=kwargs.get('dr',None),fiber=lsf)
dxlsf= None
else:
xlsf= kwargs.pop('xlsf',None)
dxlsf= kwargs.pop('dxlsf',None)
if xlsf is None and dxlsf is None: raise ValueError('xlsf= or dxlsf= input needs to be given if the LSF is given as an array')
vmacro= kwargs.pop('vmacro',6.)
# Parse continuum-normalization keywords
cont= kwargs.pop('cont','aspcap')
# Parse the wavelength regions
apWave= apStarWavegrid()
if isinstance(args[0],str): #element string given
si,ei= apwindow.waveregions(args[0],pad=3,asIndex=True)
args= args[1:]
else:
if isinstance(args[0][0],int): # assume index
si,ei= args[0], args[1]
else: # assume wavelengths in \AA
sl,el= args[0], args[1]
# Convert to index
si, ei= [], []
for s,e in zip(sl,el):
# Find closest index into apWave
si.append(numpy.argmin(numpy.fabs(s-apWave)))
ei.append(numpy.argmin(numpy.fabs(e-apWave)))
args= args[2:]
# Setup the model atmosphere
modelatm= kwargs.pop('modelatm',None)
tmpModelAtmDir= False
# Parse fparam, if present
fparam= kwargs.pop('fparam',None)
if not fparam is None:
kwargs['teff']= fparam[0,paramIndx('TEFF')]
kwargs['logg']= fparam[0,paramIndx('LOGG')]
kwargs['metals']= fparam[0,paramIndx('METALS')]
kwargs['am']= fparam[0,paramIndx('ALPHA')]
kwargs['cm']= fparam[0,paramIndx('C')]
kwargs['vm']= 10.**fparam[0,paramIndx('LOG10VDOP')]
if modelatm is None: # Setup a model atmosphere
modelatm= atlas9.Atlas9Atmosphere(teff=kwargs.get('teff',4500.),
logg=kwargs.get('logg',2.5),
metals=kwargs.get('metals',0.),
am=kwargs.get('am',0.),
cm=kwargs.get('cm',0.),
dr=kwargs.get('dr',None))
if isinstance(modelatm,str) and os.path.exists(modelatm):
modelfilename= modelatm
elif isinstance(modelatm,str):
raise ValueError('modelatm= input is a non-existing filename')
else: # model atmosphere instance
# Need to write this instance to a file; we will run in a temp
# subdirectory of the current directory
tmpDir= tempfile.mkdtemp(dir=os.getcwd())
tmpModelAtmDir= True # need to remove this later
modelfilename= os.path.join(tmpDir,'modelatm.mod')
modelatm.writeto(modelfilename)
kwargs['modelatm']= modelfilename
try:
# Check whether a MOOG version of the model atmosphere exists
if not os.path.exists(modelfilename.replace('.mod','.org')):
# Convert to MOOG format
convert_modelAtmosphere(**kwargs)
# Run weedout on the linelist first if requested
if run_weedout:
linelistfilename= modelfilename.replace('.mod','.lines')
if not os.path.exists(linelistfilename):
weedout(**kwargs)
kwargs['linelist']= linelistfilename
# Run MOOG synth for the whole wavelength range as a baseline, also contin
if baseline is None:
baseline= moogsynth(**kwargs)[1]
elif isinstance(baseline,tuple): #probably accidentally gave wav as well
baseline= baseline[1]
if mwav is None or cflux is None:
mwav, cflux= moogsynth(doflux=True,**kwargs)
# Convert the apStarWavegrid windows to moogWavegrid regions
sm,em= [], []
for start,end in zip(si,ei):
sm.append(numpy.argmin(numpy.fabs(apWave[start]-mwav)))
em.append(numpy.argmin(numpy.fabs(apWave[end]-mwav)))
# Run MOOG synth for all abundances and all windows
if len(args) == 0: #special case that there are *no* differences
args= ([26,0.],)
nsynths= numpy.array([len(args[ii])-1 for ii in range(len(args))])
nsynth= numpy.amax(nsynths) #Take the longest abundance list
out= numpy.tile(baseline,(nsynth,1))
# Run all windows
for start, end in zip(sm,em):
kwargs['wmin']= mwav[start]
kwargs['wmax']= mwav[end]
# Check whether the number of syntheses is > 5 and run multiple
# MOOG instances if necessary, bc MOOG only does 5 at a time
ninstances= int(numpy.ceil(nsynth/5.))
for ii in range(ninstances):
newargs= ()
for jj in range(len(args)):
tab= [args[jj][0]]
if len(args[jj][5*ii+1:5*(ii+1)+1]) > 0:
tab.extend(args[jj][5*ii+1:5*(ii+1)+1])
newargs= newargs+(tab,)
out[5*ii:5*(ii+1),start:end+1]= moogsynth(*newargs,**kwargs)[1]
except: raise
finally:
if tmpModelAtmDir: # need to remove this temporary directory
os.remove(modelfilename)
moogmodelfilename= modelfilename.replace('.mod','.org')
if os.path.exists(moogmodelfilename):
os.remove(moogmodelfilename)
if run_weedout:
os.remove(modelfilename.replace('.mod','.lines'))
os.rmdir(tmpDir)
# Now multiply each continuum-normalized spectrum with the continuum
out*= numpy.tile(cflux,(nsynth,1))
# Now convolve with the LSF
out= aplsf.convolve(mwav,out,
lsf=lsf,xlsf=xlsf,dxlsf=dxlsf,vmacro=vmacro)
# Now continuum-normalize
if cont.lower() == 'true':
# Get the true continuum on the apStar wavelength grid
apWave= apStarWavegrid()
baseline= numpy.polynomial.Polynomial.fit(mwav,cflux,4)
ip= interpolate.InterpolatedUnivariateSpline(mwav,
cflux/baseline(mwav),
k=3)
cflux= baseline(apWave)*ip(apWave)
# Divide it out
out/= numpy.tile(cflux,(nsynth,1))
elif not cont is None:
cflux= apcont.fit(out,numpy.ones_like(out),type=cont)
out[cflux > 0.]/= cflux[cflux > 0.]
out[cflux <= 0.]= numpy.nan
return out
def synth(*args,**kwargs):
"""
NAME:
synth
PURPOSE:
Generate model APOGEE spectra using MOOG: this is a general routine that generates the non-continuum-normalized spectrum, convolves with the LSF and macrotubulence, and optionally continuum normalizes the output; use 'moogsynth' for a direct interface to MOOG
INPUT ARGUMENTS:
lists with abundances wrt the atmosphere (they don't all have to have the same length, missing ones are filled in with zeros):
[Atomic number1,diff1_1,diff1_2,diff1_3,...,diff1_N]
[Atomic number2,diff2_1,diff2_2,diff2_3,...,diff2_N]
...
[Atomic numberM,diffM_1,diffM_2,diffM_3,...,diffM_N]
INPUT KEYWORDS:
LSF:
lsf= ('all') LSF to convolve with; output of apogee.spec.lsf.eval; sparsify for efficiency; if 'all' or 'combo' a pre-computed version will be downloaded from the web
Either:
xlsf= (None) pixel offset grid on which the LSF is computed (see apogee.spec.lsf.eval); unnecessary if lsf=='all' or 'combo'
dxlsf= (None) spacing of pixel offsets
vmacro= (6.) macroturbulence to apply
CONTINUUM:
cont= ('aspcap') continuum-normalization to apply:
None: no continuum normalization
'true': Use the true continuum
'aspcap': Use the continuum normalization method of ASPCAP DR12
'cannon': Normalize using continuum pixels derived from the Cannon
SYNTHESIS:
linelist= (None) linelist to use; can be set to the path of a linelist file or to the name of an APOGEE linelist
run_weedout= (False) if True, run MOOG weedout on the linelist first
wmin, wmax, dw, width= (15000.000, 17000.000, 0.10000000, 7.0000000) spectral synthesis limits, step, and width of calculation (see MOOG)
lib= ('kurucz_filled') spectral library
MODEL ATMOSPHERE PARAMETERS:
Specify one of the following:
(a) modelatm= (None) can be set to the filename of a model atmosphere or to a model-atmosphere instance (if filename, needs to end in .mod)
(b) parameters of a KURUCZ model atmosphere:
(1) teff= (4500) Teff
logg= (2.5) logg
metals= (0.) metallicity
cm= (0.) carbon-enhancement
am= (0.) alpha-enhancement
(2) fparam= standard ASPCAP output format
lib= ('kurucz_filled') model atmosphere library
dr= (None) use model atmospheres from this data release
vmicro= (2.) microturbulence (only used if the MOOG-formatted atmosphere is not found) (can also be part of fparam)
MISCELLANEOUS:
dr= return the path corresponding to this data release
OUTPUT:
spectra (nspec,nwave)
HISTORY:
2015-03-15 - Written - Bovy (IAS)
"""
run_weedout= kwargs.pop('run_weedout',False)
# Check that we have the LSF and store the relevant keywords
lsf= kwargs.pop('lsf','all')
if isinstance(lsf,str):
xlsf, lsf= aplsf._load_precomp(dr=kwargs.get('dr',None),fiber=lsf)
dxlsf= None
else:
xlsf= kwargs.pop('xlsf',None)
dxlsf= kwargs.pop('dxlsf',None)
if xlsf is None and dxlsf is None: raise ValueError('xlsf= or dxlsf= input needs to be given if the LSF is given as an array')
vmacro= kwargs.pop('vmacro',6.)
# Parse continuum-normalization keywords
cont= kwargs.pop('cont','aspcap')
# Setup the model atmosphere
modelatm= kwargs.pop('modelatm',None)
tmpModelAtmDir= False
# Parse fparam, if present
fparam= kwargs.pop('fparam',None)
if not fparam is None:
kwargs['teff']= fparam[paramIndx('TEFF')]
kwargs['logg']= fparam[paramIndx('LOGG')]
kwargs['metals']= fparam[paramIndx('METALS')]
kwargs['am']= fparam[paramIndx('ALPHA')]
kwargs['cm']= fparam[paramIndx('C')]
kwargs['vm']= 10.**fparam[paramIndx('LOG10VDOP')]
if modelatm is None: # Setup a model atmosphere
modelatm= atlas9.Atlas9Atmosphere(teff=kwargs.get('teff',4500.),
logg=kwargs.get('logg',2.5),
metals=kwargs.get('metals',0.),
am=kwargs.get('am',0.),
cm=kwargs.get('cm',0.),
dr=kwargs.get('dr',None))
if isinstance(modelatm,str) and os.path.exists(modelatm):
modelfilename= modelatm
elif isinstance(modelatm,str):
raise ValueError('modelatm= input is a non-existing filename')
else: # model atmosphere instance
# Need to write this instance to a file; we will run in a temp
# subdirectory of the current directory
tmpDir= tempfile.mkdtemp(dir=os.getcwd())
tmpModelAtmDir= True # need to remove this later
modelfilename= os.path.join(tmpDir,'modelatm.mod')
modelatm.writeto(modelfilename)
kwargs['modelatm']= modelfilename
try:
# Check whether a MOOG version of the model atmosphere exists
if not os.path.exists(modelfilename.replace('.mod','.org')):
# Convert to MOOG format
convert_modelAtmosphere(**kwargs)
# Run weedout on the linelist first if requested
if run_weedout:
linelistfilename= modelfilename.replace('.mod','.lines')
if not os.path.exists(linelistfilename):
weedout(**kwargs)
kwargs['linelist']= linelistfilename
# Run MOOG synth for all abundances
if len(args) == 0: #special case that there are *no* differences
args= ([26,0.],)
nsynths= numpy.array([len(args[ii])-1 for ii in range(len(args))])
nsynth= numpy.amax(nsynths) #Take the longest abundance list
nmoogwav= int((kwargs.get('wmax',_WMAX_DEFAULT)\
-kwargs.get('wmin',_WMIN_DEFAULT))\
/kwargs.get('dw',_DW_DEFAULT)+1)
out= numpy.empty((nsynth,nmoogwav))
# Check whether the number of syntheses is > 5 and run multiple
# MOOG instances if necessary, bc MOOG only does 5 at a time
ninstances= int(numpy.ceil(nsynth/5.))
for ii in range(ninstances):
newargs= ()
for jj in range(len(args)):
tab= [args[jj][0]]
if len(args[jj][5*ii+1:5*(ii+1)+1]) > 0:
tab.extend(args[jj][5*ii+1:5*(ii+1)+1])
newargs= newargs+(tab,)
out[5*ii:5*(ii+1)]= moogsynth(*newargs,**kwargs)[1]
# We'll grab the wavelength grid from the continuum below
# Now compute the continuum and multiply each c-norm spectrum with it
mwav, cflux= moogsynth(doflux=True,**kwargs)
except: raise
finally:
if tmpModelAtmDir: # need to remove this temporary directory
os.remove(modelfilename)
moogmodelfilename= modelfilename.replace('.mod','.org')
if os.path.exists(moogmodelfilename):
os.remove(moogmodelfilename)
if run_weedout:
os.remove(modelfilename.replace('.mod','.lines'))
os.rmdir(tmpDir)
out*= numpy.tile(cflux,(nsynth,1))
# Now convolve with the LSF
out= aplsf.convolve(mwav,out,
lsf=lsf,xlsf=xlsf,dxlsf=dxlsf,vmacro=vmacro)
# Now continuum-normalize
if cont.lower() == 'true':
# Get the true continuum on the apStar wavelength grid
apWave= apStarWavegrid()
baseline= numpy.polynomial.Polynomial.fit(mwav,cflux,4)
ip= interpolate.InterpolatedUnivariateSpline(mwav,
cflux/baseline(mwav),
k=3)
cflux= baseline(apWave)*ip(apWave)
# Divide it out
out/= numpy.tile(cflux,(nsynth,1))
elif not cont is None:
cflux= apcont.fit(out,numpy.ones_like(out),type=cont)
out[cflux > 0.]/= cflux[cflux > 0.]
out[cflux <= 0.]= numpy.nan
return out
def synth(*args, **kwargs):
"""
NAME:
synth
PURPOSE:
Generate model APOGEE spectra using MOOG: this is a general routine that generates the non-continuum-normalized spectrum, convolves with the LSF and macrotubulence, and optionally continuum normalizes the output; use 'moogsynth' for a direct interface to MOOG
INPUT ARGUMENTS:
lists with abundances wrt the atmosphere (they don't all have to have the same length, missing ones are filled in with zeros):
[Atomic number1,diff1_1,diff1_2,diff1_3,...,diff1_N]
[Atomic number2,diff2_1,diff2_2,diff2_3,...,diff2_N]
...
[Atomic numberM,diffM_1,diffM_2,diffM_3,...,diffM_N]
INPUT KEYWORDS:
LSF:
lsf= ('all') LSF to convolve with; output of apogee.spec.lsf.eval; sparsify for efficiency; if 'all' or 'combo' a pre-computed version will be downloaded from the web
Either:
xlsf= (None) pixel offset grid on which the LSF is computed (see apogee.spec.lsf.eval); unnecessary if lsf=='all' or 'combo'
dxlsf= (None) spacing of pixel offsets
vmacro= (6.) macroturbulence to apply
CONTINUUM:
cont= ('aspcap') continuum-normalization to apply:
None: no continuum normalization
'true': Use the true continuum
'aspcap': Use the continuum normalization method of ASPCAP DR12
'cannon': Normalize using continuum pixels derived from the Cannon
SYNTHESIS:
linelist= (None) linelist to use; can be set to the path of a linelist file or to the name of an APOGEE linelist
run_weedout= (False) if True, run MOOG weedout on the linelist first
wmin, wmax, dw, width= (15000.000, 17000.000, 0.10000000, 7.0000000) spectral synthesis limits, step, and width of calculation (see MOOG)
lib= ('kurucz_filled') spectral library
MODEL ATMOSPHERE PARAMETERS:
Specify one of the following:
(a) modelatm= (None) can be set to the filename of a model atmosphere or to a model-atmosphere instance (if filename, needs to end in .mod)
(b) parameters of a KURUCZ model atmosphere:
(1) teff= (4500) Teff
logg= (2.5) logg
metals= (0.) metallicity
cm= (0.) carbon-enhancement
am= (0.) alpha-enhancement
(2) fparam= standard ASPCAP output format
lib= ('kurucz_filled') model atmosphere library
dr= (None) use model atmospheres from this data release
vmicro= (2.) microturbulence (only used if the MOOG-formatted atmosphere is not found) (can also be part of fparam)
MISCELLANEOUS:
dr= return the path corresponding to this data release
OUTPUT:
spectra (nspec,nwave)
HISTORY:
2015-03-15 - Written - Bovy (IAS)
"""
run_weedout = kwargs.pop('run_weedout', False)
# Check that we have the LSF and store the relevant keywords
lsf = kwargs.pop('lsf', 'all')
if isinstance(lsf, str):
xlsf, lsf = aplsf._load_precomp(dr=kwargs.get('dr', None), fiber=lsf)
dxlsf = None
else:
xlsf = kwargs.pop('xlsf', None)
dxlsf = kwargs.pop('dxlsf', None)
if xlsf is None and dxlsf is None:
raise ValueError(
'xlsf= or dxlsf= input needs to be given if the LSF is given as an array'
)
vmacro = kwargs.pop('vmacro', 6.)
# Parse continuum-normalization keywords
cont = kwargs.pop('cont', 'aspcap')
# Setup the model atmosphere
modelatm = kwargs.pop('modelatm', None)
tmpModelAtmDir = False
# Parse fparam, if present
fparam = kwargs.pop('fparam', None)
if not fparam is None:
kwargs['teff'] = fparam[paramIndx('TEFF')]
kwargs['logg'] = fparam[paramIndx('LOGG')]
kwargs['metals'] = fparam[paramIndx('METALS')]
kwargs['am'] = fparam[paramIndx('ALPHA')]
kwargs['cm'] = fparam[paramIndx('C')]
kwargs['vm'] = 10.**fparam[paramIndx('LOG10VDOP')]
if modelatm is None: # Setup a model atmosphere
modelatm = atlas9.Atlas9Atmosphere(teff=kwargs.get('teff', 4500.),
logg=kwargs.get('logg', 2.5),
metals=kwargs.get('metals', 0.),
am=kwargs.get('am', 0.),
cm=kwargs.get('cm', 0.),
dr=kwargs.get('dr', None))
if isinstance(modelatm, str) and os.path.exists(modelatm):
modelfilename = modelatm
elif isinstance(modelatm, str):
raise ValueError('modelatm= input is a non-existing filename')
else: # model atmosphere instance
# Need to write this instance to a file; we will run in a temp
# subdirectory of the current directory
tmpDir = tempfile.mkdtemp(dir=os.getcwd())
tmpModelAtmDir = True # need to remove this later
modelfilename = os.path.join(tmpDir, 'modelatm.mod')
modelatm.writeto(modelfilename)
kwargs['modelatm'] = modelfilename
try:
# Check whether a MOOG version of the model atmosphere exists
if not os.path.exists(modelfilename.replace('.mod', '.org')):
# Convert to MOOG format
convert_modelAtmosphere(**kwargs)
# Run weedout on the linelist first if requested
if run_weedout:
linelistfilename = modelfilename.replace('.mod', '.lines')
if not os.path.exists(linelistfilename):
weedout(**kwargs)
kwargs['linelist'] = linelistfilename
# Run MOOG synth for all abundances
if len(args) == 0: #special case that there are *no* differences
args = ([26, 0.], )
nsynths = numpy.array([len(args[ii]) - 1 for ii in range(len(args))])
nsynth = numpy.amax(nsynths) #Take the longest abundance list
nmoogwav= int((kwargs.get('wmax',_WMAX_DEFAULT)\
-kwargs.get('wmin',_WMIN_DEFAULT))\
/kwargs.get('dw',_DW_DEFAULT)+1)
out = numpy.empty((nsynth, nmoogwav))
# Check whether the number of syntheses is > 5 and run multiple
# MOOG instances if necessary, bc MOOG only does 5 at a time
ninstances = int(numpy.ceil(nsynth / 5.))
for ii in range(ninstances):
newargs = ()
for jj in range(len(args)):
tab = [args[jj][0]]
if len(args[jj][5 * ii + 1:5 * (ii + 1) + 1]) > 0:
tab.extend(args[jj][5 * ii + 1:5 * (ii + 1) + 1])
newargs = newargs + (tab, )
out[5 * ii:5 * (ii + 1)] = moogsynth(*newargs, **kwargs)[1]
# We'll grab the wavelength grid from the continuum below
# Now compute the continuum and multiply each c-norm spectrum with it
mwav, cflux = moogsynth(doflux=True, **kwargs)
except:
raise
finally:
if tmpModelAtmDir: # need to remove this temporary directory
os.remove(modelfilename)
moogmodelfilename = modelfilename.replace('.mod', '.org')
if os.path.exists(moogmodelfilename):
os.remove(moogmodelfilename)
if run_weedout:
os.remove(modelfilename.replace('.mod', '.lines'))
os.rmdir(tmpDir)
out *= numpy.tile(cflux, (nsynth, 1))
# Now convolve with the LSF
out = aplsf.convolve(mwav,
out,
lsf=lsf,
xlsf=xlsf,
dxlsf=dxlsf,
vmacro=vmacro)
# Now continuum-normalize
if cont.lower() == 'true':
# Get the true continuum on the apStar wavelength grid
apWave = apStarWavegrid()
baseline = numpy.polynomial.Polynomial.fit(mwav, cflux, 4)
ip = interpolate.InterpolatedUnivariateSpline(mwav,
cflux / baseline(mwav),
k=3)
cflux = baseline(apWave) * ip(apWave)
# Divide it out
out /= numpy.tile(cflux, (nsynth, 1))
elif not cont is None:
cflux = apcont.fit(out, numpy.ones_like(out), type=cont)
out[cflux > 0.] /= cflux[cflux > 0.]
out[cflux <= 0.] = numpy.nan
return out
def windows(*args, **kwargs):
"""
NAME:
windows
PURPOSE:
Generate model APOGEE spectra using MOOG in selected wavelength windows (but the whole APOGEE spectral range is returned): this is a general routine that generates the non-continuum-normalized spectrum, convolves with the LSF and macrotubulence, and optionally continuum normalizes the output; use 'moogsynth' for a direct interface to MOOG
INPUT ARGUMENTS:
Windows specification: Provide one of
(1) Element string: the APOGEE windows for this element will be loaded
(2) startindxs, endindxs= start and end indexes of the windows on the apStar wavelength grid
(3) startlams, endlams= start and end wavelengths in \AA
lists with abundance differences wrt the atmosphere (they don't all have to have the same length, missing ones are filled in with zeros):
[Atomic number1,diff1_1,diff1_2,diff1_3,...,diff1_N]
[Atomic number2,diff2_1,diff2_2,diff2_3,...,diff2_N]
...
[Atomic numberM,diffM_1,diffM_2,diffM_3,...,diffM_N]
INPUT KEYWORDS:
BASELINE: you can specify the baseline spectrum to not always re-compute it
baseline= baseline c-normalized spectrum on MOOG wavelength grid (obtained from moogsynth)
mwav= MOOG wavelength grid (obtained from moogsynth)
cflux= continuum flux from MOOG
Typically, you can obtain these three keywords by doing (kwargs are the keywords you provide to this function as well)
>>> baseline= moogsynth(**kwargs)[1]
>>> mwav, cflux= moogsynth(doflux=True,**kwargs)
LSF:
lsf= ('all') LSF to convolve with; output of apogee.spec.lsf.eval; sparsify for efficiency; if 'all' or 'combo' a pre-computed version will be downloaded from the web
Either:
xlsf= (None) pixel offset grid on which the LSF is computed (see apogee.spec.lsf.eval); unnecessary if lsf=='all' or 'combo'
dxlsf= (None) spacing of pixel offsets
vmacro= (6.) macroturbulence to apply
CONTINUUM:
cont= ('aspcap') continuum-normalization to apply:
None: no continuum normalization
'true': Use the true continuum
'aspcap': Use the continuum normalization method of ASPCAP DR12
'cannon': Normalize using continuum pixels derived from the Cannon
SYNTHESIS:
linelist= (None) linelist to use; if this is None, the code looks for a weed-out version of the linelist appropriate for the given model atmosphere
run_weedout= (False) if True, run MOOG weedout on the linelist first
wmin, wmax, dw, width= (15000.000, 17000.000, 0.10000000, 7.0000000) spectral synthesis limits *for the whole spectrum* (not just the windows), step, and width of calculation (see MOOG)
MODEL ATMOSPHERE PARAMETERS:
Specify one of the following:
(a) modelatm= (None) can be set to the filename of a model atmosphere or to a model-atmosphere instance (if filename, needs to end in .mod)
(b) parameters of a KURUCZ model atmosphere:
(1) teff= (4500) Teff
logg= (2.5) logg
metals= (0.) metallicity
cm= (0.) carbon-enhancement
am= (0.) alpha-enhancement
(2) fparam= standard ASPCAP output format (
lib= ('kurucz_filled') model atmosphere library
dr= (None) use model atmospheres from this data release
vmicro= (2.) microturbulence (only used if the MOOG-formatted atmosphere is not found) (can also be part of fparam)
MISCELLANEOUS:
dr= return the path corresponding to this data release
OUTPUT:
spectra (nspec,nwave)
HISTORY:
2015-03-18 - Written - Bovy (IAS)
"""
# Pop some kwargs
run_weedout = kwargs.pop('run_weedout', False)
baseline = kwargs.pop('baseline', None)
mwav = kwargs.pop('mwav', None)
cflux = kwargs.pop('cflux', None)
# Check that we have the LSF and store the relevant keywords
lsf = kwargs.pop('lsf', 'all')
if isinstance(lsf, str):
xlsf, lsf = aplsf._load_precomp(dr=kwargs.get('dr', None), fiber=lsf)
dxlsf = None
else:
xlsf = kwargs.pop('xlsf', None)
dxlsf = kwargs.pop('dxlsf', None)
if xlsf is None and dxlsf is None:
raise ValueError(
'xlsf= or dxlsf= input needs to be given if the LSF is given as an array'
)
vmacro = kwargs.pop('vmacro', 6.)
# Parse continuum-normalization keywords
cont = kwargs.pop('cont', 'aspcap')
# Parse the wavelength regions
apWave = apStarWavegrid()
if isinstance(args[0], str): #element string given
si, ei = apwindow.waveregions(args[0], pad=3, asIndex=True)
args = args[1:]
else:
if isinstance(args[0][0], int): # assume index
si, ei = args[0], args[1]
else: # assume wavelengths in \AA
sl, el = args[0], args[1]
# Convert to index
si, ei = [], []
for s, e in zip(sl, el):
# Find closest index into apWave
si.append(numpy.argmin(numpy.fabs(s - apWave)))
ei.append(numpy.argmin(numpy.fabs(e - apWave)))
args = args[2:]
# Setup the model atmosphere
modelatm = kwargs.pop('modelatm', None)
tmpModelAtmDir = False
# Parse fparam, if present
fparam = kwargs.pop('fparam', None)
if not fparam is None:
kwargs['teff'] = fparam[0, paramIndx('TEFF')]
kwargs['logg'] = fparam[0, paramIndx('LOGG')]
kwargs['metals'] = fparam[0, paramIndx('METALS')]
kwargs['am'] = fparam[0, paramIndx('ALPHA')]
kwargs['cm'] = fparam[0, paramIndx('C')]
kwargs['vm'] = 10.**fparam[0, paramIndx('LOG10VDOP')]
if modelatm is None: # Setup a model atmosphere
modelatm = atlas9.Atlas9Atmosphere(teff=kwargs.get('teff', 4500.),
logg=kwargs.get('logg', 2.5),
metals=kwargs.get('metals', 0.),
am=kwargs.get('am', 0.),
cm=kwargs.get('cm', 0.),
dr=kwargs.get('dr', None))
if isinstance(modelatm, str) and os.path.exists(modelatm):
modelfilename = modelatm
elif isinstance(modelatm, str):
raise ValueError('modelatm= input is a non-existing filename')
else: # model atmosphere instance
# Need to write this instance to a file; we will run in a temp
# subdirectory of the current directory
tmpDir = tempfile.mkdtemp(dir=os.getcwd())
tmpModelAtmDir = True # need to remove this later
modelfilename = os.path.join(tmpDir, 'modelatm.mod')
modelatm.writeto(modelfilename)
kwargs['modelatm'] = modelfilename
try:
# Check whether a MOOG version of the model atmosphere exists
if not os.path.exists(modelfilename.replace('.mod', '.org')):
# Convert to MOOG format
convert_modelAtmosphere(**kwargs)
# Run weedout on the linelist first if requested
if run_weedout:
linelistfilename = modelfilename.replace('.mod', '.lines')
if not os.path.exists(linelistfilename):
weedout(**kwargs)
kwargs['linelist'] = linelistfilename
# Run MOOG synth for the whole wavelength range as a baseline, also contin
if baseline is None:
baseline = moogsynth(**kwargs)[1]
elif isinstance(baseline,
tuple): #probably accidentally gave wav as well
baseline = baseline[1]
if mwav is None or cflux is None:
mwav, cflux = moogsynth(doflux=True, **kwargs)
# Convert the apStarWavegrid windows to moogWavegrid regions
sm, em = [], []
for start, end in zip(si, ei):
sm.append(numpy.argmin(numpy.fabs(apWave[start] - mwav)))
em.append(numpy.argmin(numpy.fabs(apWave[end] - mwav)))
# Run MOOG synth for all abundances and all windows
if len(args) == 0: #special case that there are *no* differences
args = ([26, 0.], )
nsynths = numpy.array([len(args[ii]) - 1 for ii in range(len(args))])
nsynth = numpy.amax(nsynths) #Take the longest abundance list
out = numpy.tile(baseline, (nsynth, 1))
# Run all windows
for start, end in zip(sm, em):
kwargs['wmin'] = mwav[start]
kwargs['wmax'] = mwav[end]
# Check whether the number of syntheses is > 5 and run multiple
# MOOG instances if necessary, bc MOOG only does 5 at a time
ninstances = int(numpy.ceil(nsynth / 5.))
for ii in range(ninstances):
newargs = ()
for jj in range(len(args)):
tab = [args[jj][0]]
if len(args[jj][5 * ii + 1:5 * (ii + 1) + 1]) > 0:
tab.extend(args[jj][5 * ii + 1:5 * (ii + 1) + 1])
newargs = newargs + (tab, )
out[5 * ii:5 * (ii + 1),
start:end + 1] = moogsynth(*newargs, **kwargs)[1]
except:
raise
finally:
if tmpModelAtmDir: # need to remove this temporary directory
os.remove(modelfilename)
moogmodelfilename = modelfilename.replace('.mod', '.org')
if os.path.exists(moogmodelfilename):
os.remove(moogmodelfilename)
if run_weedout:
os.remove(modelfilename.replace('.mod', '.lines'))
os.rmdir(tmpDir)
# Now multiply each continuum-normalized spectrum with the continuum
out *= numpy.tile(cflux, (nsynth, 1))
# Now convolve with the LSF
out = aplsf.convolve(mwav,
out,
lsf=lsf,
xlsf=xlsf,
dxlsf=dxlsf,
vmacro=vmacro)
# Now continuum-normalize
if cont.lower() == 'true':
# Get the true continuum on the apStar wavelength grid
apWave = apStarWavegrid()
baseline = numpy.polynomial.Polynomial.fit(mwav, cflux, 4)
ip = interpolate.InterpolatedUnivariateSpline(mwav,
cflux / baseline(mwav),
k=3)
cflux = baseline(apWave) * ip(apWave)
# Divide it out
out /= numpy.tile(cflux, (nsynth, 1))
elif not cont is None:
cflux = apcont.fit(out, numpy.ones_like(out), type=cont)
out[cflux > 0.] /= cflux[cflux > 0.]
out[cflux <= 0.] = numpy.nan
return out
if params[1][0] >= 5.0:
params[1][0] = params[1][2] = params[1][1] = 4.9
# Generate models (flux1, flux2)
mspecs = ferre.interpolate(params[0], params[1], params[2], params[3], params[4], params[5])
# for mspec in mspecs:
# mspec[np.where(np.isnan(mspec))] = 0.0
# prep obs spec
"""aspec= np.reshape(spec,(1,len(spec)))
aspecerr= np.reshape(specerr,(1,len(specerr)))
cont= spec / continuum.fit(aspec,aspecerr,type='aspcap')[0]"""
"""spec[np.where(np.isnan(spec))] = 0.0
cont = spec / max(spec)"""
# Generate the wavelength grid
restLambda = splot.apStarWavegrid()
ccfs = []
velocityShift = 0
for mspec in mspecs:
print(mspec.shape)
nan_vals = np.where(np.isnan(mspec))[0]
# nan_vals = np.where(spec == 0.0)[0]
chip_ranges = [
(nan_vals[i] + 1, nan_vals[i + 1])
for i in range(len(nan_vals) - 1)
if nan_vals[i + 1] != nan_vals[i] + 1
]
mspec[np.where(np.isnan(mspec))[0]] = 0.0
ycorr = np.array([])
def synth(*args,**kwargs):
"""
NAME:
synth
PURPOSE:
Generate model APOGEE spectra using Turbospectrum: this is a general routine that generates the non-continuum-normalized spectrum, convolves with the LSF and macrotubulence, and optionally continuum normalizes the output; use 'turbosynth' for a direct interface to Turbospectrum
INPUT ARGUMENTS:
lists with abundances differences wrt the atmosphere (they don't all have to have the same length, missing ones are filled in with zeros):
[Atomic number1,diff1_1,diff1_2,diff1_3,...,diff1_N]
[Atomic number2,diff2_1,diff2_2,diff2_3,...,diff2_N]
...
[Atomic numberM,diffM_1,diffM_2,diffM_3,...,diffM_N]
INPUT KEYWORDS:
LSF:
lsf= ('all') LSF to convolve with; output of apogee.spec.lsf.eval; sparsify for efficiency; if 'all' or 'combo' a pre-computed version will be downloaded from the web
Either:
xlsf= (None) pixel offset grid on which the LSF is computed (see apogee.spec.lsf.eval); unnecessary if lsf=='all' or 'combo'
dxlsf= (None) spacing of pixel offsets
vmacro= (6.) macroturbulence to apply
CONTINUUM:
cont= ('aspcap') continuum-normalization to apply:
None: no continuum normalization
'true': Use the true continuum
'aspcap': Use the continuum normalization method of ASPCAP DR12
'cannon': Normalize using continuum pixels derived from the Cannon
SYNTHESIS:
air= (True) if True, perform the synthesis in air wavelengths (output is still in vacuum); set to False at your own risk, as Turbospectrum expects the linelist in air wavelengths!)
Hlinelist= (None) Hydrogen linelists to use; can be set to the path of a linelist file or to the name of an APOGEE linelist; if None, then we first search for the Hlinedata.vac in the APOGEE linelist directory (if air=False) or we use the internal Turbospectrum Hlinelist (if air=True)
linelist= (None) molecular and atomic linelists to use; can be set to the path of a linelist file or to the name of an APOGEE linelist, or lists of such files; if a single filename is given, the code will first search for files with extensions '.atoms', '.molec' or that start with 'turboatoms.' and 'turbomolec.'
wmin, wmax, dw= (15000.000, 17000.000, 0.10000000) spectral synthesis limits and step
costheta= (1.) cosine of the viewing angle
lib= ('kurucz_filled') spectral library
MODEL ATMOSPHERE PARAMETERS:
Specify one of the following:
(a) modelatm= (None) model-atmosphere instance
(b) parameters of a KURUCZ model atmosphere:
(1) teff= (4500) Teff
logg= (2.5) logg
metals= (0.) metallicity
cm= (0.) carbon-enhancement
am= (0.) alpha-enhancement
(2) fparam= standard ASPCAP output format
lib= ('kurucz_filled') model atmosphere library
vmicro= (2.) microturbulence (only used if the MOOG-formatted atmosphere is not found) (can also be part of fparam)
MISCELLANEOUS:
dr= return the path corresponding to this data release
OUTPUT:
spectra (nspec,nwave)
HISTORY:
2015-04-16 - Written - Bovy (IAS)
"""
# Check that we have the LSF and store the relevant keywords
lsf= kwargs.pop('lsf','all')
if isinstance(lsf,str):
xlsf, lsf= aplsf._load_precomp(dr=kwargs.get('dr',None),fiber=lsf)
dxlsf= None
else:
xlsf= kwargs.pop('xlsf',None)
dxlsf= kwargs.pop('dxlsf',None)
if xlsf is None and dxlsf is None: raise ValueError('xlsf= or dxlsf= input needs to be given if the LSF is given as an array')
vmacro= kwargs.pop('vmacro',6.)
# Parse continuum-normalization keywords
cont= kwargs.pop('cont','aspcap')
# Setup the model atmosphere
modelatm= kwargs.pop('modelatm',None)
# Parse fparam, if present
fparam= kwargs.pop('fparam',None)
if not fparam is None:
kwargs['teff']= fparam[paramIndx('TEFF')]
kwargs['logg']= fparam[paramIndx('LOGG')]
kwargs['metals']= fparam[paramIndx('METALS')]
kwargs['am']= fparam[paramIndx('ALPHA')]
kwargs['cm']= fparam[paramIndx('C')]
kwargs['vmicro']= 10.**fparam[paramIndx('LOG10VDOP')]
# Need to pass a model atmosphere instance to turbosynth (needs to be made
# more efficient, because now turbosynth always write the atmosphere
if modelatm is None: # Setup a model atmosphere
modelatm= atlas9.Atlas9Atmosphere(teff=kwargs.get('teff',4500.),
logg=kwargs.get('logg',2.5),
metals=kwargs.get('metals',0.),
am=kwargs.get('am',0.),
cm=kwargs.get('cm',0.),
dr=kwargs.get('dr',None))
if isinstance(modelatm,str) and os.path.exists(modelatm):
raise ValueError('modelatm= input is an existing filename, but you need to give an Atmosphere object instead')
elif isinstance(modelatm,str):
raise ValueError('modelatm= input needs to be an Atmosphere instance')
# Check temperature
if modelatm._teff > 7000.:
warnings.warn('Turbospectrum does not include all necessary physics to model stars hotter than about 7000 K; proceed with caution',RuntimeWarning)
kwargs['modelatm']= modelatm
try:
# Run turbosynth for all abundances
if len(args) == 0: #special case that there are *no* differences
args= ([26,0.],)
nsynths= numpy.array([len(args[ii])-1 for ii in range(len(args))])
nsynth= numpy.amax(nsynths) #Take the longest abundance list
nturbowav= int((kwargs.get('wmax',_WMAX_DEFAULT)\
-kwargs.get('wmin',_WMIN_DEFAULT))\
/kwargs.get('dw',_DW_DEFAULT)+1)
out= numpy.empty((nsynth,nturbowav))
for ii in range(nsynth):
newargs= ()
for jj in range(len(args)):
tab= [args[jj][0]]
if len(args[jj]) > ii+1:
tab.append(args[jj][ii+1])
newargs= newargs+(tab,)
tmpOut= turbosynth(*newargs,**kwargs)
out[ii]= tmpOut[2] # incl. continuum
# wavelength grid from final one
mwav= tmpOut[0]
except: raise
# If the synthesis was done in air, convert wavelength array
if kwargs.get('air',True):
mwav= numpy.array([air2vac(w) for w in list(mwav)])
# Now convolve with the LSF
out= aplsf.convolve(mwav,out,
lsf=lsf,xlsf=xlsf,dxlsf=dxlsf,vmacro=vmacro)
# Now continuum-normalize
if cont.lower() == 'true':
# Get the true continuum on the apStar wavelength grid
apWave= apStarWavegrid()
baseline= numpy.polynomial.Polynomial.fit(mwav,tmpOut[2]/tmpOut[1],4)
ip= interpolate.InterpolatedUnivariateSpline(mwav,
tmpOut[2]/tmpOut[1]\
/baseline(mwav),
k=3)
cflux= baseline(apWave)*ip(apWave)
# Divide it out
out/= numpy.tile(cflux,(nsynth,1))
elif not cont is None:
cflux= apcont.fit(out,numpy.ones_like(out),type=cont)
out[cflux > 0.]/= cflux[cflux > 0.]
out[cflux <= 0.]= numpy.nan
return out
def targetGrid(gridParam, minimizedVisitParams, plot=True):
'''
The grid tests against ranging effective temperatures for both stars and the flux ratio of the
secondary component. This is done by target.
:param gridParam: [in/out] The GridParam of the target
:param gridRes: [out] The visits that have the same paramters as the minimized chi2 visit
:param plot: [in] If true makes plots to see intermediate steps (default=True)
'''
locationID = gridParam.locationID
apogeeID = gridParam.apogeeID
badheader, header = apread.apStar(locationID, apogeeID, ext=0, header=True)
specs = apread.apStar(locationID, apogeeID, ext=1, header=False)
specerrs = apread.apStar(locationID, apogeeID, ext=2, header=False)
nvisits = header['NVISITS']
# chi2 = np.full((nvisits, nrangeTeffA, nrangeTeffB, nrangeFluxRatio), -1.)
#chi2 = np.full((nvisits, nrangeTeffA, nrangeTeffB, nrangeFluxRatio, nrangeRVA, nrangeRVB), -1.)
ipg = ferre.Interpolator(lib='GK')
ipf = ferre.Interpolator(lib='F')
# Create file to store all the chi2 values
path = 'lists/all_chi2/' + str(locationID) + '/'
if not os.path.exists(path):
os.makedirs(path)
fn = open(path + apogeeID + '.lis', 'w')
fn.write(gridParam.toStringHeader())
timer = Timer()
timeSum = 0.0
allChi2 = []
visitGridParamsBuffer = []
for visit in range(1, nvisits + 1):
timer.start()
if (nvisits != 1):
spec = specs[1+visit]
specerr = specerrs[1+visit]
else:
spec = specs
specerr = specerrs
if (len(minimizedVisitParams) == 0):
gridParam = GridParam(locationID, apogeeID)
gridParam.constructParams()
gridParam.getRVs(visit)
else:
gridParam = minimizedVisitParams[visit - 1]
visitGridParamsBuffer.append(gridParam)
# Prepare grid ranges
rangeTeffA = np.arange(gridParam.minTeffA, gridParam.maxTeffA, gridParam.teffStepA)
rangeTeffB = np.arange(gridParam.minTeffB, gridParam.maxTeffB, gridParam.teffStepB)
rangeFluxRatio = np.arange(gridParam.minFluxRatio, gridParam.maxFluxRatio, gridParam.fluxStep)
rangeRVA = np.arange(gridParam.minRVA, gridParam.maxRVA, gridParam.rvAStep)
rangeRVB = np.arange(gridParam.minRVB, gridParam.maxRVB, gridParam.rvBStep)
nrangeTeffA = len(rangeTeffA)
nrangeTeffB = len(rangeTeffB)
nrangeFluxRatio = len(rangeFluxRatio)
nrangeRVA =len(rangeRVA)
nrangeRVB =len(rangeRVB)
chi2 = np.full((nrangeTeffA, nrangeTeffB, nrangeFluxRatio, nrangeRVA, nrangeRVB), -1.)
print('Visit: ' + str(visit) ,'Grid dimensions: ' + str(chi2.shape))
# Prep Spectra
aspec= np.reshape(spec,(1, len(spec)))
aspecerr= np.reshape(specerr,(1, len(specerr)))
cont= spec / continuum.fit(aspec, aspecerr, type='aspcap')[0]
conterr = specerr / continuum.fit(aspec, aspecerr, type='aspcap')[0]
shiftedSpec = bm.shiftFlux(cont, header['VHELIO' + str(visit)])
# Run grid
for i in range(nrangeTeffA):
gridParam.modelParamA.teff = rangeTeffA[i]
componentA = bm.genComponent(gridParam.modelParamA, ipf, ipg)
for j in range(nrangeTeffB):
gridParam.modelParamB.teff = rangeTeffB[j]
componentB = bm.genComponent(gridParam.modelParamB, ipf, ipg)
for k in range(nrangeFluxRatio):
gridParam.modelParamB.fluxRatio = rangeFluxRatio[k]
componentBR = componentB * rangeFluxRatio[k]
for l in range(nrangeRVA):
gridParam.modelParamA.rv = rangeRVA[l]
componentAS = bm.shiftFlux(componentA, rangeRVA[l])
for m in range(nrangeRVB):
gridParam.modelParamB.rv = rangeRVB[m]
componentBS = bm.shiftFlux(componentBR, rangeRVB[m])
binaryFlux = bm.combineFlux(componentAS, componentBS)
chi2[i][j][k][l][m] = calcChi2(binaryFlux, shiftedSpec, conterr) / (len(binaryFlux) - 5.0)
gridParam.chi2 = chi2[i][j][k][l][m]
fn.write(gridParam.toString())
if (plot is True):
restLambda = splot.apStarWavegrid()
BinPlot.plotDeltaVCheck(locationID, apogeeID, visit,
[ [ restLambda, binaryFlux, 'blue', 'model' ],
[ restLambda, cont, 'orange', 'unshifted' ],
[ restLambda, shiftedSpec, 'green', 'shifted' ]],
[gridParam.modelParamA.teff,gridParam.modelParamB.teff, gridParam.modelParamB.fluxRatio],
'Delta V Shift', folder='grid_deltaVCheck')
timeSum+=timer.end()
allChi2.append(chi2)
fn.close()
print('Average visit time: ' + str(round(timeSum/nvisits, 2)) + str('s'))
# Get minized values for each visit
indices = None
for i in range(nvisits):
inds = getMinIndicies(allChi2[i])
rangeTeffA = np.arange(visitGridParamsBuffer[i].minTeffA, visitGridParamsBuffer[i].maxTeffA, visitGridParamsBuffer[i].teffStepA)
rangeTeffB = np.arange(visitGridParamsBuffer[i].minTeffB, visitGridParamsBuffer[i].maxTeffB, visitGridParamsBuffer[i].teffStepB)
rangeFluxRatio = np.arange(visitGridParamsBuffer[i].minFluxRatio, visitGridParamsBuffer[i].maxFluxRatio, visitGridParamsBuffer[i].fluxStep)
rangeRVA = np.arange(visitGridParamsBuffer[i].minRVA, visitGridParamsBuffer[i].maxRVA, visitGridParamsBuffer[i].rvAStep)
rangeRVB = np.arange(visitGridParamsBuffer[i].minRVB, visitGridParamsBuffer[i].maxRVB, visitGridParamsBuffer[i].rvBStep)
nrangeTeffA = len(rangeTeffA)
nrangeTeffB = len(rangeTeffB)
nrangeFluxRatio = len(rangeFluxRatio)
nrangeRVA =len(rangeRVA)
nrangeRVB =len(rangeRVB)
visitGridParamsBuffer[i].setParams(i + 1, rangeTeffA[inds[0]], rangeTeffB[inds[1]], rangeFluxRatio[inds[2]],
rangeRVA[inds[3]], rangeRVB[inds[4]], allChi2[i][inds[0]][inds[1]][inds[2]][inds[3]][inds[4]])
if (indices is None):
indices = [i + 1, inds, allChi2[i][inds[0]][inds[1]][inds[2]][inds[3]][inds[4]]]
if (allChi2[i][inds[0]][inds[1]][inds[2]][inds[3]][inds[4]] < indices[2]):
indices = [i + 1, inds, allChi2[i][inds[0]][inds[1]][inds[2]][inds[3]][inds[4]]]
inds = getMinIndicies(allChi2)
gridParam = visitGridParamsBuffer[inds[0]]
return gridParam, visitGridParamsBuffer