def filter_mag(filterfile, filterzero, syn_spec, syn_err=None, wrange=None):
'''
######################################################
# Input #
# -------------------------------------------------- #
# filterfile: file containing filter function #
# filterzero: flux [Jy] corresponding to mag=0 #
# syn_spec: synphot spectrum object of source #
# wrange: (start,end) observed wavelength range #
# -------------------------------------------------- #
# Output #
# -------------------------------------------------- #
# mag: magnitude of source in filter system. #
######################################################
'''
from synphot import SpectralElement, Observation, Empirical1D, SourceSpectrum
import astropy.units as u
#Load ascii filter function
if filterfile.split('/')[-1][:6] == 'Bessel':
filt = SpectralElement.from_file(filterfile, wave_unit='nm')
else:
filt = SpectralElement.from_file(filterfile, wave_unit='AA')
if wrange is None:
fwave = filt.waveset
swave = syn_spec.waveset
wrange = (max(fwave[0],swave[0]),min(fwave[-1],swave[-1]))
waves = np.linspace(wrange[0], wrange[-1], 10000)
#Synthetic observation
obs = Observation(syn_spec, filt, force='extrap')
flux = obs.effstim(flux_unit='jy', waverange=wrange).value
#flux = obs.effstim(flux_unit='jy', wavelengths=waves).value
#Calibrate magnitude with zero point
mag = -2.512*np.log10(flux/filterzero)
#Synthetic observation of error spectrum
if syn_err is not None:
#square filter and error spectrum
filt2 = SpectralElement(Empirical1D, points=fwave,
lookup_table=np.square(filt(fwave)))
pseudo_flux = np.square(syn_err(swave,flux_unit='jy')).value
syn_err2 = SourceSpectrum(Empirical1D, points=swave,
lookup_table=pseudo_flux)
#sum errors in quadrature
obs = Observation(syn_err2, filt2, force='extrap')
#flux_err = np.sqrt(obs.effstim(waverange=wrange).value)
flux_err = np.sqrt(obs.effstim(wavelengths=waves).value)
#convert to magnitude error
mag_err = (2.5/np.log(10))*(flux_err/flux)
return mag, mag_err
else:
return mag
def filter_flux(filterfile, syn_spec, syn_err=None, wrange=None):
'''
######################################################
# Input #
# -------------------------------------------------- #
# filterfile: file containing filter function #
# syn_spec: synphot spectrum object of source #
# wrange: (start,end) observed wavelength range #
# -------------------------------------------------- #
# Output #
# -------------------------------------------------- #
# flux: flux of source in filter system. #
######################################################
'''
from synphot import SpectralElement, Observation, Empirical1D, SourceSpectrum
import astropy.units as u
#Load ascii filter function
if filterfile.split('/')[-1][:6] == 'Bessel':
filt = SpectralElement.from_file(filterfile, wave_unit='nm')
else:
filt = SpectralElement.from_file(filterfile, wave_unit='AA')
if wrange is None:
fwave = filt.waveset
swave = syn_spec.waveset
wrange = (max(fwave[0],swave[0]),min(fwave[-1],swave[-1]))
wlengths = fwave[np.logical_and(fwave>wrange[0], fwave<wrange[1])]
else:
fwave = filt.waveset
wlengths = fwave[np.logical_and(fwave>wrange[0]*u.AA, fwave<wrange[1]*u.AA)]
#Synthetic observation
obs = Observation(syn_spec, filt, force='extrap')
flux = obs.effstim(flux_unit='jy', waverange=wrange).value
#flux = obs.effstim(flux_unit='jy', wavelengths=wlengths).value
#Synthetic observation of error spectrum
if syn_err is not None:
#square filter and error spectrum
filt2 = SpectralElement(Empirical1D, points=fwave,
lookup_table=np.square(filt(fwave)))
pseudo_flux = np.square(syn_err(swave,flux_unit='jy')).value
syn_err2 = SourceSpectrum(Empirical1D, points=swave,
lookup_table=pseudo_flux)
#sum errors in quadrature
obs = Observation(syn_err2, filt2, force='extrap')
flux_err = np.sqrt(obs.effstim(waverange=wrange).value)
return flux, flux_err
else:
return flux
def get_phot(waves, exts, bands):
"""
Compute the extinction in the requested bands
Parameters
----------
waves : numpy.ndarray
The wavelengths
exts : numpy.ndarray
The extinction values at wavelengths "waves"
bands: list of strings
Bands requested
Outputs
-------
band extinctions : numpy array
Calculated band extinctions
"""
# create a SourceSpectrum object from the extinction curve
spectrum = SourceSpectrum(
Empirical1D,
points=waves * 1e4,
lookup_table=exts,
)
# path for band response curves
band_path = (
"/Users/mdecleir/measure_extinction/measure_extinction/data/Band_RespCurves/"
)
# dictionary linking the bands to their response curves
bandnames = {
"J": "2MASSJ",
"H": "2MASSH",
"K": "2MASSKs",
"IRAC1": "IRAC1",
"IRAC2": "IRAC2",
"WISE1": "WISE1",
"WISE2": "WISE2",
"L": "AAOL",
"M": "AAOM",
}
# compute the extinction value in each band
band_ext = np.zeros(len(bands))
for k, band in enumerate(bands):
# create the bandpass (as a SpectralElement object)
bp = SpectralElement.from_file(
"%s%s.dat" %
(band_path,
bandnames[band])) # assumes wavelengths are in Angstrom!!
# integrate the extinction curve over the bandpass, only if the bandpass fully overlaps with the extinction curve (this actually excludes WISE2)
if bp.check_overlap(spectrum) == "full":
obs = Observation(spectrum, bp)
band_ext[k] = obs.effstim().value
else:
band_ext[k] = np.nan
return band_ext
def calculate_values(detector, filt, mjd, aper):
# parameters can be removed from obsmode as needed
obsmode = 'wfc3,{},{},mjd#{},aper#{}'.format(detector, filt, mjd, aper)
bp = stsyn.band(obsmode)
# STMag
photflam = bp.unit_response(stsyn.conf.area) # inverse sensitivity in flam
stmag = -21.1 - 2.5 * log10(photflam.value)
# Pivot Wavelength and bandwidth
photplam = bp.pivot() # pivot wavelength in angstroms
bandwidth = bp.photbw() # bandwidth in angstroms
# ABMag
abmag = stmag - 5 * log10(photplam.value) + 18.6921
# Vegamag
#for some reason stsyn.Vega doesn't load so we redefine it
stsyn.Vega = SourceSpectrum.from_vega()
obs = Observation(
stsyn.Vega, bp, binset=bp.binset
) # synthetic observation of vega in bandpass using vega spectrum
vegamag = -obs.effstim(flux_unit='obmag', area=stsyn.conf.area)
return obsmode, photplam.value, bandwidth.value, photflam.value, stmag, abmag, vegamag.value
def _observe_through_filter(bp, B, unit):
if not synphot:
raise AstropyWarning('synphot is required for bandpass filtering.')
obs = Observation(B, bp)
wave = obs.effective_wavelength()
fluxd = obs.effstim(unit)
return wave, fluxd
def get_phot(spec, bands):
"""
Compute the fluxes in the requested bands.
Parameters
----------
spec : SpecData object
the spectrum
bands: list of strings
bands requested
Outputs
-------
band fluxes : numpy array
calculated band fluxes
"""
# create a SourceSpectrum object from the spectrum, excluding the bad regions
spectrum = SourceSpectrum(
Empirical1D,
points=spec.waves.to(u.Angstrom)[spec.npts != 0],
lookup_table=spec.fluxes[spec.npts != 0],
)
# path for band response curves
band_path = pkg_resources.resource_filename("measure_extinction",
"data/Band_RespCurves/")
# dictionary linking the bands to their response curves
bandnames = {
"J": "2MASSJ",
"H": "2MASSH",
"K": "2MASSKs",
"IRAC1": "IRAC1",
"IRAC2": "IRAC2",
"WISE1": "WISE1",
"WISE2": "WISE2",
"L": "AAOL",
"M": "AAOM",
}
# define the units of the output fluxes
funit = u.erg / (u.s * u.cm * u.cm * u.Angstrom)
# compute the flux in each band
fluxes = np.zeros(len(bands))
for k, band in enumerate(bands):
# create the bandpass (as a SpectralElement object)
bp = SpectralElement.from_file(
"%s%s.dat" %
(band_path,
bandnames[band])) # assumes wavelengths are in Angstrom!!
# integrate the spectrum over the bandpass, only if the bandpass fully overlaps with the spectrum (this actually excludes WISE2)
if bp.check_overlap(spectrum) == "full":
obs = Observation(spectrum, bp)
fluxes[k] = obs.effstim(funit).value
else:
fluxes[k] = np.nan
return fluxes
def filter_vega_zp(filterfile, filterzero):
'''
######################################################
# Input #
# -------------------------------------------------- #
# filterfile: file containing filter function #
# filterzero: flux corresponding to mag=0 #
# -------------------------------------------------- #
# Output #
# -------------------------------------------------- #
# mag_0: magnitude of Vega in filter system. #
######################################################
'''
from synphot import SourceSpectrum, SpectralElement, Observation
#load Vega spectrum
spec = SourceSpectrum.from_vega()
#Load ascii filter function
if filterfile.split('/')[-1][:6] == 'Bessel':
filt = SpectralElement.from_file(filterfile, wave_unit='nm')
else:
filt = SpectralElement.from_file(filterfile, wave_unit='AA')
wave = filt.waveset
#Synthetic observation
obs = Observation(spec, filt)
flux = obs.effstim(flux_unit='jy', waverange=(wave[0],wave[-1]))
#Calibrate to zero point (zp)
mag_0 = -2.512*np.log10(flux/filterzero)
return mag_0
def kvega_to_f335abmag(self, kmag):
'''Convert K band vegamag to F335M ABmag'''
kmag = kmag * units.VEGAMAG
new_g2v = self.g2v.normalize(kmag,
band=self.kband,
area=self.telescope_area,
vegaspec=self.vega)
obs = Observation(new_g2v, self.bp, binset=self.wave_bins)
abmag = obs.effstim('ABmag', area=self.telescope_area)
return abmag
def f335abmag_to_kvega(self, abmag):
'''Convert F335M ABmag to K band vegamag'''
abmag = abmag * u.ABmag
new_g2v = self.g2v.normalize(abmag,
band=self.bp,
area=self.telescope_area,
vegaspec=self.vega)
obs = Observation(new_g2v, self.kband, binset=self.wave_bins)
kmag = obs.effstim('Vegamag',
area=self.telescope_area,
vegaspec=self.vega)
return kmag
def zero_mag_flux(filter_name, photometric_system, return_filter=False):
"""
Returns the zero magnitude photon flux for a filter
Acceptable filter names are those given in
``scopesim.effects.ter_curves_utils.FILTER_DEFAULTS`` or a string with an
appropriate name for a filter in the Spanish-VO filter-service. Such strings
must use the naming convention: observatory/instrument.filter. E.g:
``paranal/HAWKI.Ks``, or ``Gemini/GMOS-N.CaT``.
Parameters
----------
filter_name : str
Name of the filter - see above
photometric_system : str
["vega", "AB", "ST"] Name of the photometric system
return_filter : bool, optional
If True, also returns the filter curve object
Returns
-------
flux : float
[PHOTLAM]
filt : ``synphot.SpectralElement``
If ``return_filter`` is True
"""
filt = get_filter(filter_name)
spec = get_zero_mag_spectrum(photometric_system)
obs = Observation(spec, filt)
flux = obs.effstim(flux_unit=PHOTLAM)
if return_filter:
return flux, filt
else:
return flux
def synphot_calcs(self, bpfile):
"""
Calculate zeropoint for a given bandpass in several
photometric systems
Arguments:
----------
bpfile -- Text file containing the throuput table for
a single bandpass
Returns:
--------
Bandpass zeropoint value in Vega mags, AB mags, ST mags,
photflam, photfnu, and megajansky. Also returns pivot wavelength
"""
# Define wavelength list to use
#wave_bins = np.arange(0.5, 5, 0.1) * u.micron
# Use refactored synphot to calculate zeropoints
orig_bp = SpectralElement.from_file(bpfile)
# Now reduce the PCE curve by a factor equal to
# the gain, in order to get the output to translate
# from ADU/sec rather than e/sec
bp = orig_bp / self.gain
#bp.model.lookup_table = bp.model.lookup_table / self.gain
photflam = bp.unit_response(self.telescope_area)
photplam = bp.pivot()
st_zpt = -2.5 * np.log10(photflam.value) - 21.1
ab_zpt = (-2.5 * np.log10(photflam.value) - 21.1 -
5 * np.log10(photplam.value) + 18.6921)
#mjy_zpt = units.convert_flux(photplam,photflam, 'MJy')
mjy_zpt = photflam.to(u.MJy, u.spectral_density(photplam))
obs = Observation(self.vega, bp, binset=wave_bins)
vega_zpt = -obs.effstim(flux_unit='obmag', area=self.telescope_area)
photfnu = units.convert_flux(photplam, photflam, units.FNU)
return (vega_zpt.value, ab_zpt, st_zpt, photflam.value, photfnu.value,
mjy_zpt.value, photplam.value)