def deredden(data, host_EBV=None, host_RV=None, MW_EBV=None, MW_RV=3.1,
*args, **kwargs):
"""Correct for extinction."""
if not _can_deredden:
return data
# Milky Way extinction
if MW_EBV is not None and MW_EBV != 0. and MW_RV is not None:
data[:, 1], _a, _b = unred(data[:, 0], data[:, 1], MW_EBV, R_V=MW_RV)
# Host extinction
if host_EBV is not None and host_EBV != 0. and host_RV is not None:
data[:, 1], _a, _b = unred(data[:, 0], data[:, 1], host_EBV, R_V=host_RV)
return data
def __call__(self, x):
m = num.array([
deredden.unred(x[i], x[i] * 0 + 1, -self.pars[0],
R_V=self.pars[1])[0] for i in range(x.shape[0])
])
#m *= self.pars[0]
return m
def R(self,
Rv=3.1,
wave=None,
flux=None,
z=0.0,
EBV=0.001,
redlaw='ccm',
strict_ccm=False):
'''For a given reddening law Rv (default 3.1), find the ratio of total
to selective absorption for this filter: R = A/E(B-V). You can
specify a specific spectrum by supplying a wave and flux and redshift
(default is defined by filters.reference_wave and
filters.refernce_flux at z=0). You can also specify E(B-V) (EBV) which can
change the value of R if the spectrum is significantly non-stellar. You
can specify redlaw='fm' if you prefer a Fitzpatric (1999) reddening
law.'''
global standards
if wave is None:
wave,flux = standards['Vega']['VegaB'].wave,\
standards['Vega']['VegaB'].resp
flux0 = self.response(wave, flux, z, photons=1)
if flux0 <= 0:
return (num.nan)
redf = unred(wave,
flux,
-EBV,
Rv,
z,
redlaw=redlaw,
strict_ccm=strict_ccm)[0]
fluxr = self.response(wave, redf, z, photons=1)
return (-2.5 * num.log10(fluxr / flux0) / EBV)
def preprocess(data,
z=None,
wave_range=None,
normalize=False,
scale=False,
E_BV=None):
'''
`data` formatted by:
data[: 0] -> wavelength
data[: 1] -> flux
data[: 2] -> flux_err
'''
# Get rid of NaN values
data = data[~np.isnan(data).any(axis=1)]
# Put wavelength in rest frame
data[:, 0] = deredshift(data[:, 0], z)
# Prune to wavelength range
if wave_range is not None:
data = prune(data, wave_range)
# Correct for MW reddening
if E_BV is not None:
data[:, 1], _, _0 = unred(data[:, 0], data[:, 1], E_BV, MW_RV)
if scale:
data = scale_flux(data)
elif normalize:
data = normalize_flux(data)
return data
def R(self, Rv=3.1, wave=None, flux=None, z=0.0, EBV=0.001, redlaw='ccm',
strict_ccm=False):
'''For a given reddening law Rv (default 3.1), find the ratio of total
to selective absorption for this filter: R = A/E(B-V). You can
specify a specific spectrum by supplying a wave and flux and redshift
(default is defined by filters.reference_wave and
filters.refernce_flux at z=0). You can also specify E(B-V) (EBV) which can
change the value of R if the spectrum is significantly non-stellar. You
can specify redlaw='fm' if you prefer a Fitzpatric (1999) reddening
law.'''
global standards
if wave is None:
wave,flux = standards['Vega']['VegaB'].wave,\
standards['Vega']['VegaB'].resp
flux0 = self.response(wave, flux, z, photons=1)
if flux0 <= 0:
return(num.nan)
redf = unred(wave, flux, -EBV, Rv, z, redlaw=redlaw,
strict_ccm=strict_ccm)[0]
fluxr = self.response(wave, redf, z, photons=1)
return(-2.5*num.log10(fluxr/flux0)/EBV)
def __call__(self, x):
m = num.array([deredden.unred(x[i], x[i]*0+1, -self.pars[0],
R_V=self.pars[1])[0] for i in range(x.shape[0])])
#m *= self.pars[0]
return m
