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926
927 | class RedCorr(object):
"""
Reddening correction
RC = RedCorr()
"""
##
# @todo Manage error in extinction
# @todo print extinction laws with references
def __init__(self, E_BV=0., R_V=3.1, law='No correction', cHbeta=None,
UserFunction=None):
"""
Reddening correction tool.
Parameters:
E_BV [float]: differential extinction between bands B and V
R_V = AV/E_BV. Default value is 3.1
law [str]: one of the defined laws (available with RedCorr.getLaws())
cHbeta: logarithmic extinction at Hbeta (prevalence on E_BV)
UserFunction X(wave, param): A user-defined function that accept 2 parameters: wavelength(s) in Angstrom
and an optional parameter and return X(lambda) = A(lambda)/E_BV = R.A(lambda)/AV.
The correction is: 10**(0.4*E_bv*X)
**Usage:**
RC = RedCorr(E_BV = 1.)
RC.plot(laws = 'all')
def my_X(wave, params = [5000., 1., 2., 3.]):
\"""
Description of the user defined law
\"""
return params[1] * (wave/params[0]) + params[2] * (wave/params[0])**-1 + params[3] * (wave/params[0])**-2
RC.UserFunction = my_X
RC.UserParams = [6000., 0., 0., 1.]
RC.getCorr(5007)
"""
self.log_ = pn.log_
self.calling = 'RedCorr'
self._laws_dict = {} # dictionary pointing to a reddening function depending on the key
self._laws_dict['No correction'] = self._zeros
self._laws_dict['CCM89'] = self._CCM89
self._laws_dict['CCM89 Bal07'] = self._CCM89_Bal07
self._laws_dict['CCM89 oD94'] = self._CCM89_oD94
self._laws_dict['S79 H83 CCM89'] = self._S79_H83_CCM89
#self._laws_dict['GCC 09'] = self._GCC09
self._laws_dict['K76'] = self._K76
self._laws_dict['SM79 Gal'] = self._SM79_Gal
self._laws_dict['G03 LMC'] = self._G03_LMC
self._laws_dict['MCC99 FM90 LMC'] = self._MCC99_FM90_LMC
self._laws_dict['F99-like'] = self._F99_like
#self._laws_dict['F99-like IDL'] = self._F99_like_IDL
self._laws_dict['F99'] = self._F99
self._laws_dict['F88 F99 LMC'] = self._FM88_F99_LMC
self.UserFunction = UserFunction
self.UserParams = None
self.FitzParams = None
self._given = None
self.law = law
self.R_V = R_V
if cHbeta is not None:
self._given = 'cHbeta'
self.cHbeta = cHbeta
else:
self._given = 'E_BV'
self.E_BV = E_BV
def cHbetaFromEbv(self, ebv):
"""
Return cHbeta from E(BV)
Parameter:
ebv: E(B-V)
**Usage:**
(1-f_lambda).cHbeta = 0.4.EBV.X_lambda applied to lambda = 4861, with f_beta = 0.:
cHbeta = 0.4 . EBV . X_beta
"""
Xbeta = self.X(pn.CST.HBETA)
return 0.4 * ebv * Xbeta
#return np.asarray((-0.61 + (0.61 ** 2 + 4 * 0.024 * ebv) ** 0.5) / (2 * 0.024))
def EbvFromCHbeta(self, cHbeta):
"""
Return E(B-V) from cHbeta
Parameter:
cHbeta: -
Using:
(1-f_lambda).cHbeta = 0.4.EBV.X_lambda applied to lambda = 4861,
with f_beta = 0.:
cHbeta = 0.4 . EBV . X_beta
"""
Xbeta = self.X(pn.CST.HBETA)
if Xbeta != 0.:
return cHbeta * 2.5 / Xbeta
else:
return np.zeros_like(cHbeta)
#return np.asarray(0.61 * cHbeta + 0.024 * cHbeta ** 2.)
def getLaws(self):
"""
Return the dictionary keys for the extinction laws
"""
return self._laws_dict.keys()
def printLaws(self):
"""
Print out the extinction laws
"""
for law in self._laws_dict.keys():
try:
doc = self._laws_dict[law].__doc__
except:
doc = ''
print("'{0}': {1}".format(law, doc))
def _get_e_bv(self):
return self.__E_BV
def _get_r_v(self):
return self.__R_V
def _get_law(self):
return self.__law
def _get_cHbeta(self):
return self.__cHbeta
def _get_AV(self):
return self.__AV
def _get_uf(self):
return self.__user_function
def _set_e_bv(self, value):
self.__E_BV = np.asarray(value)
self.__cHbeta = self.cHbetaFromEbv(self.__E_BV)
self.__AV = self.__E_BV * self.R_V
self._given = 'E_BV'
def _set_cHbeta(self, value):
self.__cHbeta = np.asarray(value)
self.__E_BV = self.EbvFromCHbeta(self.__cHbeta)
self.__AV = self.__E_BV * self.R_V
self._given = 'cHbeta'
def _set_AV(self, value):
self.__AV = np.asarray(value)
self.__E_BV = self.__AV / self.R_V
self.__cHbeta = self.cHbetaFromEbv(self.__E_BV)
self._given = 'AV'
def _set_r_v(self, value):
self.__R_V = np.asarray(value)
def _set_law(self, value):
if value not in self._laws_dict.keys():
self.log_.error('Unknown extinction law reference: {0}'.format(value), calling=self.calling)
self.__law = None
self.X = None
else:
self.__law = value
self.X = self._laws_dict[self.law]
if self._given == 'E_BV':
self.E_BV = self.E_BV
elif self._given == 'cHbeta':
self.cHbeta = self.cHbeta
elif self._given == 'AV':
self.AV = self.AV
def _set_uf(self, value):
self.__user_function = value
if value is None:
if 'user' in self._laws_dict:
del self._laws_dict['user']
else:
def _uf2(wave):
#This transform the user function with 2 parameters in a function of one single parameter
return np.asarray(self.__user_function(wave, self.UserParams))
_uf2.__doc__ = self.__user_function.__doc__
self._laws_dict['user'] = _uf2
E_BV = property(_get_e_bv, _set_e_bv, None, None)
R_V = property(_get_r_v, _set_r_v, None, None)
law = property(_get_law, _set_law, None, None)
cHbeta = property(_get_cHbeta, _set_cHbeta, None, None)
AV = property(_get_AV, _set_AV, None, None)
UserFunction = property(_get_uf, _set_uf, None, None)
def getCorr(self, wave, rel_wave=None):
"""
Return the extinction correction as:
correction = 10**(0.4 * EBV * Xx) = 10**(A_lambda / 2.5)
Parameters:
wave: wavelength (Angstrom)
rel_wave: wavelength (Angstrom) for a relative correction
**Usage:**
RC.getCorr(5007)
RC.getCorr(5007, 4861)
"""
if self.law is None:
self.log_.warn('No extinction law defined.', calling=self.calling)
return None
if self._laws_dict[self.law] is None:
self.log_.warn('No user defined extinction law.', calling=self.calling)
return None
else:
if rel_wave is None:
rel_corr = 1.
else:
rel_corr = self.getCorr(rel_wave)
X = self.X(wave)
return np.squeeze(10. ** (0.4 * np.outer(X, self.E_BV).reshape(X.shape + self.E_BV.shape))) / rel_corr
def getCorrHb(self, wave):
"""
Return the extinction correction normalized to the correction at 4861AA.
Parameter:
wave: wavelength (Angstrom)
"""
return self.getCorr(wave, np.ones_like(wave) * pn.CST.HBETA)
def getErrCorr(self, wave, err_E_BV, rel_wave=None):
"""
Return the error on the correction for a given wavelength, given the error on E(B-V)
Parameters:
wave: wavelength(s)
err_E_BV: error on E(B-V)
rel_wave: reference wavelength for the normalization (optional)
"""
if rel_wave is None:
rel_X = 0.
else:
rel_X = self.X(rel_wave)
return np.log(10) * abs(self.X(wave) - rel_X) * 0.4 * err_E_BV * self.E_BV
def getErrCorrHb(self, wave, err_E_BV):
"""
Return the the error on the correction relative to Hbeta for a given wavelength,
given the error on E(B-V)
Parameters:
wave: wavelength(s)
err_E_BV: error on E(B-V)
"""
return self.getErrCorr(self, wave, err_E_BV, rel_wave=pn.CST.HBETA)
def setCorr(self, obs_over_theo, wave1, wave2):
"""
Determination of the correction using the ratio of two observed line intensities
relative to the theoretical value.
Parameters:
obs_over_theo: ration of the observed ratio over the theoretical ratio
wave1: wavelengths at which the line rations are taken.
wave2: wavelengths at which the line rations are taken.
**Usage:**
rc.setCorr(6.5/2.85, 6563., 4861.)
"""
COR = RedCorr(E_BV= -2.5, R_V=self.R_V, law=self.law, UserFunction=self.UserFunction)
f1 = np.log10(COR.getCorr(wave1))
f2 = np.log10(COR.getCorr(wave2))
if f1 != f2:
with np.errstate(invalid='ignore'):
self.E_BV = 2.5 * np.log10(obs_over_theo) / (f1 - f2)
else:
self.E_BV = 0.
del COR
def plot(self, w_inf=1000., w_sup=10000., laws=None, ax=None, **kwargs):
"""
Plot extinction laws
Parameters:
w_inf [float]: lower limit of plot
w_sup [float]: upper limit of plot
laws [list of strings]: list of extinction law labels. If set to 'all', all the laws are plotted
ax : an axis object. If None, onr is created
**kwargs: arguments to plot
"""
if ax is None:
f, ax = plt.subplots()
colors = ['r', 'g', 'b', 'y', 'm', 'c']
styles = ['-', '--', '-:', ':']
if not pn.config.INSTALLED['plt']:
pn.log_.error('matplotlib.pyplot not available for plotting', calling=self.calling)
old_E_BV = self.E_BV
old_law = self.law
self.E_BV = 2.5
w = np.linspace(w_inf, w_sup, 1000)
if laws is None:
laws = self.law
elif laws == 'all':
laws = self.getLaws()
if type(laws) is str:
laws = [laws]
try:
# Python 3 returns laws as a set, no sorting then
laws.sort()
except:
pass
for i, law in enumerate(laws):
self.law = law
corr = self.getCorrHb(w)
if corr is not None:
ax.plot(w, np.log10(corr), label=law, c=colors[i % 6], linestyle=styles[i // 6], **kwargs)
ax.legend()
ax.set_xlabel('Wavelength (A)')
ax.set_ylabel('X')
self.law = old_law
self.E_BV = old_E_BV
def _CCM89(self, wave):
"""
Cardelli, Clayton & Mathis 1989, ApJ 345, 245
http://adsabs.harvard.edu/abs/1989ApJ...345..245C
Parameters:
wave: wavelength (Angstrom)
**Comments:**
Depends on R_V, default value being 3.1
Scope: Applicable to both dense and diffuse ISM
Range: UV through IR
"""
x = 1e4 / np.asarray([wave]) # inv microns
a = np.zeros_like(x)
b = np.zeros_like(x)
tt = (x > 0.3) & (x <= 1.1)
a[tt] = 0.574 * x[tt] ** 1.61
b[tt] = -0.527 * x[tt] ** 1.61
tt = (x > 1.1) & (x <= 3.3)
yg = x[tt] - 1.82
a[tt] = (1. + 0.17699 * yg - 0.50447 * yg ** 2. - 0.02427 * yg ** 3. + 0.72085 * yg ** 4. +
0.01979 * yg ** 5. - 0.7753 * yg ** 6. + 0.32999 * yg ** 7.)
b[tt] = (0. + 1.41338 * yg + 2.28305 * yg ** 2. + 1.07233 * yg ** 3. - 5.38434 * yg ** 4. -
0.622510 * yg ** 5. + 5.3026 * yg ** 6. - 2.09002 * yg ** 7.)
tt = (x > 3.3) & (x <= 5.9)
a[tt] = 1.752 - 0.316 * x[tt] - 0.104 / ((x[tt] - 4.67) ** 2. + 0.341)
b[tt] = -3.090 + 1.825 * x[tt] + 1.206 / ((x[tt] - 4.62) ** 2 + 0.263)
tt = (x > 5.9) & (x <= 8.0)
a[tt] = (1.752 - 0.316 * x[tt] - 0.104 / ((x[tt] - 4.67) ** 2. + 0.341) -
0.04473 * (x[tt] - 5.9) ** 2. - 0.009779 * (x[tt] - 5.9) ** 3.)
b[tt] = (-3.090 + 1.825 * x[tt] + 1.206 / ((x[tt] - 4.62) ** 2. + 0.263) +
0.2130 * (x[tt] - 5.9) ** 2. + 0.1207 * (x[tt] - 5.9) ** 3.)
tt = (x > 8.0) & (x < 10.0)
a[tt] = (-1.073 - 0.628 * (x[tt] - 8) + 0.137 * (x[tt] - 8) ** 2. -
0.070 * (x[tt] - 8) ** 3.)
b[tt] = (13.670 + 4.257 * (x[tt] - 8) - 0.420 * (x[tt] - 8) ** 2. +
0.374 * (x[tt] - 8) ** 3.)
Xx = self.R_V * a + b
return np.squeeze(Xx)
def _CCM89_Bal07(self, wave):
"""
Galactic extinction law based on Cardelli et al 1989, modified by Blagrave et al 2007
for 3.3 < x < 8 (1250 < lambda < 3030)
Blagrave et al 2007, ApJ, 655, 299
http://adsabs.harvard.edu/abs/2007ApJ...655..299B
Cardelli, Clayton & Mathis 1989, ApJ 345, 245
http://adsabs.harvard.edu/abs/1989ApJ...345..245C
Parameters:
wave: wavelength (Angstrom)
**Comments:**
Same as CCM89 for x<3.3 and x>8
Revised values for 3.3<x<8
Based on observation of Orion stars
Depends on R_V, default value being 3.1
Range: UV through IR
"""
x = 1e4 / np.asarray([wave]) # inv microns
a = np.zeros_like(x)
b = np.zeros_like(x)
tt = (x > 0.3) & (x <= 1.1)
a[tt] = 0.574 * x[tt] ** 1.61
b[tt] = -0.527 * x[tt] ** 1.61
tt = (x > 1.1) & (x <= 3.3)
yg = x[tt] - 1.82
a[tt] = (1. + 0.17699 * yg - 0.50447 * yg ** 2. - 0.02427 * yg ** 3. + 0.72085 * yg ** 4. +
0.01979 * yg ** 5. - 0.7753 * yg ** 6. + 0.32999 * yg ** 7.)
b[tt] = (0. + 1.41338 * yg + 2.28305 * yg ** 2. + 1.07233 * yg ** 3. - 5.38434 * yg ** 4. -
0.622510 * yg ** 5. + 5.3026 * yg ** 6. - 2.09002 * yg ** 7.)
tt = (x > 3.3) & (x <= 5.9)
a[tt] = 1.752 - 0.316 * x[tt] - 0.104 / ((x[tt] - 4.67) ** 2. + 0.341)
b[tt] = -2.9 + 1.825 * x[tt] + 0.93 / ((x[tt] - 4.65) ** 2 + 0.263)
tt = (x > 5.9) & (x <= 8.0)
a[tt] = (1.752 - 0.316 * x[tt] - 0.104 / ((x[tt] - 4.67) ** 2. + 0.341) -
0.04473 * (x[tt] - 5.9) ** 2. - 0.009779 * (x[tt] - 5.9) ** 3.)
b[tt] = (-2.9 + 1.825 * x[tt] + 0.93 / ((x[tt] - 4.65) ** 2 + 0.263) +
0.2130 * (x[tt] - 5.9) ** 2. + 0.1207 * (x[tt] - 5.9) ** 3.)
tt = (x > 8.0) & (x < 10.0)
a[tt] = (-1.073 - 0.628 * (x[tt] - 8) + 0.137 * (x[tt] - 8) ** 2. -
0.070 * (x[tt] - 8) ** 3.)
b[tt] = (13.670 + 4.257 * (x[tt] - 8) - 0.420 * (x[tt] - 8) ** 2. +
0.374 * (x[tt] - 8) ** 3.)
Xx = self.R_V * a + b
return np.squeeze(Xx)
def _CCM89_oD94(self, wave):
"""
Galactic extinction law based on Cardelli et al 1989, modified by O'Donnell 1994
for 1.1 < x < 3.3 (9100 < lambda < 3030)
O'Donnell 1994, ApJ, 422, 1580
http://adsabs.harvard.edu/abs/1994ApJ...422..158O
Cardelli, Clayton & Mathis 1989, ApJ 345, 245
http://adsabs.harvard.edu/abs/1989ApJ...345..245C
Parameters:
wave: wavelength (Angstrom)
**Comments:**
Same as CCM89 for x<1.1 and x>3.3
Revised values for 1.1<x<3.3
Produces lower correction in the near UV at low R_V
Scope: Galactic
Range: UV through IR
"""
x = 1e4 / np.asarray([wave]) # inv microns
a = np.zeros_like(x)
b = np.zeros_like(x)
tt = (x > 0.3) & (x <= 1.1)
a[tt] = 0.574 * x[tt] ** 1.61
b[tt] = -0.527 * x[tt] ** 1.61
tt = (x > 1.1) & (x <= 3.3)
yg = x[tt] - 1.82
a[tt] = (1. + 0.104 * yg - 0.609 * yg ** 2. + 0.701 * yg ** 3. + 1.137 * yg ** 4. -
1.718 * yg ** 5. - 0.827 * yg ** 6. + 1.647 * yg ** 7. - 0.505 * yg ** 8.)
b[tt] = (0. + 1.952 * yg + 2.908 * yg ** 2. - 3.989 * yg ** 3. - 7.985 * yg ** 4. +
11.102 * yg ** 5. + 5.491 * yg ** 6. - 10.805 * yg ** 7. + 3.347 * yg ** 8.)
tt = (x > 3.3) & (x <= 5.9)
a[tt] = 1.752 - 0.316 * x[tt] - 0.104 / ((x[tt] - 4.67) ** 2. + 0.341)
b[tt] = -3.090 + 1.825 * x[tt] + 1.206 / ((x[tt] - 4.62) ** 2 + 0.263)
tt = (x > 5.9) & (x <= 8.0)
a[tt] = (1.752 - 0.316 * x[tt] - 0.104 / ((x[tt] - 4.67) ** 2. + 0.341) -
0.04473 * (x[tt] - 5.9) ** 2. - 0.009779 * (x[tt] - 5.9) ** 3.)
b[tt] = (-3.090 + 1.825 * x[tt] + 1.206 / ((x[tt] - 4.62) ** 2. + 0.263) +
0.2130 * (x[tt] - 5.9) ** 2. + 0.1207 * (x[tt] - 5.9) ** 3.)
tt = (x > 8.0) & (x < 10.0)
a[tt] = (-1.073 - 0.628 * (x[tt] - 8) + 0.137 * (x[tt] - 8) ** 2. -
0.070 * (x[tt] - 8) ** 3.)
b[tt] = (13.670 + 4.257 * (x[tt] - 8) - 0.420 * (x[tt] - 8) ** 2. +
0.374 * (x[tt] - 8) ** 3.)
Xx = self.R_V * a + b
return np.squeeze(Xx)
def _S79_H83_CCM89(self, wave):
"""
Galactic extinction law (0-33000 A range):
- In the UV, from Seaton 1979
- In the opt/NIR (3600-9100) Howarth 1983
- In the FIR (9100-33000) Cardelly et al 1989
Seaton 1979, MNRAS, 187, 73) and
http://adsabs.harvard.edu/abs/1979MNRAS.187P..73S
Howarth 1983, MNRAS, 203, 301) Galactic law
http://adsabs.harvard.edu/abs/1983MNRAS.204.1091H
Cardelli, Clayton and Mathis 1989, ApJ, 345, 245
http://adsabs.harvard.edu/abs/1989ApJ...345..245C
Parameters:
wave: wavelength (Angstrom)
Scope: Galactic
Range: UV through IR
"""
x = 1e4 / np.asarray([wave]) # inv microns
Xx = np.zeros_like(x)
# Cardelli, Clayton & Mathis 1989 33000-9000
tt = (x > 0.3) & (x <= 1.1)
Xx[tt] = self.R_V * (0.574 * x[tt] ** 1.61) - 0.527 * x[tt] ** 1.61
# Howarth 1983, Galactic 9000-5000
tt = (x > 1.1) & (x <= 1.83)
Xx[tt] = (self.R_V - 3.1) + ((1.86 - 0.48 * x[tt]) * x[tt] - 0.1) * x[tt]
# Howarth 1983, Galactic 5000-3600
tt = (x > 1.83) & (x <= 2.75)
Xx[tt] = self.R_V + 2.56 * (x[tt] - 1.83) - 0.993 * ((x[tt] - 1.83) ** 2)
# Seaton 1979, Galactic
tt = (x > 2.75) & (x <= 3.65)
Xx[tt] = (self.R_V - 3.2) + 1.56 + 1.048 * x[tt] + 1.01 / (((x[tt] - 4.6) ** 2) + 0.280)
# Seaton 1979, Galactic
tt = (x > 3.65) & (x <= 7.14)
Xx[tt] = (self.R_V - 3.2) + 2.29 + 0.848 * x[tt] + 1.01 / (((x[tt] - 4.6) ** 2) + 0.280)
# Seaton 1979, Galactic
tt = (x > 7.14)
Xx[tt] = (self.R_V - 3.2) + 16.17 - 3.20 * x[tt] + 0.2975 * x[tt] ** 2
return np.squeeze(Xx)
# Removed from the code because it is most probably wrong
#def _GCC09(self, wave):
"""
Gordon, Cartledge & Clayton 2009, ApJ, 705, 1320
http://adsabs.harvard.edu/abs/2009ApJ...705.1320G
Comments:
Extinction function R.A(wave)/A(V)
R_V dependent
WARNING: This law seems buggy in the 2200AA region.
Scope:
UV
"""
"""
x = 1e4 / np.asarray([wave]) # inv microns
Xx = np.zeros_like(x)
tt = (x > 0.3) & (x <= 1.1)
Xx[tt] = (self.R_V * 0.574 - 0.527) * x[tt] ** 1.61
tt = (x > 1.1) & (x <= 3.3)
y = x[tt] - 1.82
a = 1 + y * (0.17699 + y * (-0.50447 + y * (-0.02427 + y * (0.72085 + \
y * (0.01979 + y * (-0.77530 + y * 0.32999))))))
b = y * (1.41338 + y * (2.28305 + y * (1.07233 + y * (-5.38434 + \
y * (-0.62251 + y * (5.30260 - y * 2.09002))))))
Xx[tt] = self.R_V * a + b
##
# @bug The coefficients are obviously not correct;
tt = (x > 3.3) & (x <= 5.9)
a = 1.896 - 0.372 * x[tt] - 0.0108 / ((x[tt] - 4.57) ** 2 + 0.0422)
b = -3.503 + 2.057 * x[tt] + 0.7180 / ((x[tt] - 4.59) ** 2 + 0.0530)
Xx[tt] = self.R_V * a + b
tt = (x > 5.9) & (x <= 11.0)
a = 1.896 - 0.372 * x[tt] - 0.0108 / ((x[tt] - 4.57) ** 2 + 0.0422)
b = -3.503 + 2.057 * x[tt] + 0.7180 / ((x[tt] - 4.59) ** 2 + 0.0530)
y = x[tt] - 5.9
a += -(0.110 + 0.0099 * y) * y ** 2
b += (0.537 + 0.0530 * y) * y ** 2
Xx[tt] = self.R_V * a + b
return np.squeeze(Xx)
"""
def _K76(self, wave):
"""
Kaler 1976, ApJS, 31, 517
http://adsabs.harvard.edu/abs/1976ApJS...31..517K
Comments:
This function returns the correction relative to Hbeta (f_lambda) and not
the extinction law (X(1/lambda)).
It cannot be used for absolute correction.
Range: 3000 to >20000
"""
w = np.asarray([wave]) # inv microns
if self.E_BV == 0.:
return np.ones_like(w)
f_tab = np.loadtxt(ROOT_DIR + '/extinction/Gal_Kaler.txt')
f = np.interp(w, f_tab[:, 0], f_tab[:, 1])
return np.squeeze(f * self.cHbeta / 0.4 / self.E_BV)
def _SM79_Gal(self, wave):
"""
Galactic extinction law
Savage & Mathis 1979, ARA&A, 17, 73
http://adsabs.harvard.edu/abs/1979ARA%26A..17...73S
Comments:
Average of several extinction laws
R_V=3.1
Scope: Galactic
Range: UV through IR
"""
x = 1e4 / np.asarray([wave]) # inv microns
X_tab = np.loadtxt(ROOT_DIR + '/extinction/Gal_SM79.txt')
Xx = np.interp(x, X_tab[:, 0], X_tab[:, 1])
return np.squeeze(Xx)
def _G03_LMC(self, wave):
"""
Extinction curve for the LMC
Gordon et al. (2003, ApJ, 594,279)
http://adsabs.harvard.edu/abs/2003ApJ...594..279G
Comments:
Average curve for the LMC
R_V = 3.41
Scope: LMC
Range: 1200 through fIR
"""
x = 1e4 / np.asarray([wave]) # inv microns
X_tab = np.loadtxt(ROOT_DIR + '/extinction/LMC_Gordon.txt')
Xx = self.R_V * np.interp(x, X_tab[:, 0], X_tab[:, 1])
return np.squeeze(Xx)
def _F99_like(self, wave):
"""
In the UV, it returns the Fitzpatrick & Massa 1990 law.
In the opt/IR, it returns the Fitzpatrick & Massa 1990 law.
Fitzpatrick 1999, PASP, 11, 63
http://adsabs.harvard.edu/abs/1999PASP..111...63F
Fitzpatrick & Massa 1990, ApJS, 72, 163
http://adsabs.harvard.edu/abs/1990ApJS...72..163F
Comments:
The FM90 depends on 6 parameters which must be set by the user and are stored in RedCorr.FitzParams.
For the predefined set of parameters defined in FM99, use instead the F99 law.
R_V must be provided, as the law depends on it. The dependence with R_V follows Table 4 in the F99 paper
Range: UV through IR
"""
def fit_UV(x):
Xx = c1 + c2 * x
Xx += c3 * x ** 2 / ((x ** 2 - x0 ** 2) ** 2 + (x * gamma) ** 2)
tt2 = (x > 5.9)
if tt2 is not False:
Xx[tt2] += c4 * (0.5392 * (x[tt2] - 5.9) ** 2 + 0.05644 * (x[tt2] - 5.9) ** 3)
Xx += self.R_V
return Xx
x = 1e4 / np.asarray([wave]) # inv microns
Xx = np.zeros_like(x)
if self.FitzParams is None:
pn.log_.warn('Fitzpatrick law requires FitzParams', calling=self.calling)
return None
x0 = self.FitzParams[0]
gamma = self.FitzParams[1]
c1 = self.FitzParams[2]
c2 = self.FitzParams[3]
c3 = self.FitzParams[4]
c4 = self.FitzParams[5]
# UV from the 1988 paper:
xcutuv = 10000.0 / 2700.0
tt = (x >= xcutuv)
Xx[tt] = fit_UV(x[tt])
l2x = lambda l: 1e4 / l
x_opir = np.array([0, l2x(26500.0), l2x(12200.0), l2x(6000.0), l2x(5470.0), l2x(4670.0), l2x(4110.0),
l2x(2700.), l2x(2600.)])
norm = self.R_V / 3.1
# Opt and IR from the 1999 paper
y_opir = np.array([0., 0.265 * norm, 0.829 * norm, -0.426 + 1.0044 * self.R_V,
- 0.050 + 1.0016 * self.R_V , 0.701 + 1.0016 * self.R_V,
1.208 + 1.0032 * self.R_V - 0.00033 * self.R_V ** 2, fit_UV(l2x(2700.)), fit_UV(l2x(2600.))])
tt = x < xcutuv
if tt.sum() > 0:
tck = interpolate.splrep(x_opir, y_opir)
Xx[tt] = interpolate.splev(x[tt], tck, der=0)
return np.squeeze(Xx)
# Commented out because it duplicates _F99_like
# def _F99_like_IDL(self, wave):
"""
Same as F99_like, but with a different function in the opt/IR fitting, based on an IDL program
provided by F99. The results should be identical.
In the UV, it returns the Fitzpatrick & Massa 1990 law.
In the opt/IR, it returns the Fitzpatrick 1990 law.
Fitzpatrick 1999, PASP, 11, 63
http://adsabs.harvard.edu/abs/1999PASP..111...63F
Fitzpatrick & Massa 1990, ApJS, 72, 163
http://adsabs.harvard.edu/abs/1990ApJS...72..163F
Comments:
The FM90 depends on 6 parameters which must be set by the user and are stored in RedCorr.FitzParams.
For the predefined set of parameters defined in FM99, use instead the F_99 method.
R_V must be provided, as the law depends on it. The dependence with R_V follows Table 4 in the F99 paper
Scope:
Range: UV through IR
"""
"""
def fit_UV(x):
Xx = c1 + c2 * x
Xx += c3 * x ** 2 / ((x ** 2 - x0 ** 2) ** 2 + (x * gamma) ** 2)
tt2 = (x > 5.9)
if tt2 is not False:
Xx[tt2] += c4 * (0.5392 * (x[tt2] - 5.9) ** 2 + 0.05644 * (x[tt2] - 5.9) ** 3)
Xx += self.R_V
return Xx
x = 1e4 / np.asarray([wave]) # inv microns
Xx = np.zeros_like(x)
if self.FitzParams is None:
pn.log_.error('Fitzpatrick law requires FitzParams to be set', calling=self.calling)
return None
x0 = self.FitzParams[0]
gamma = self.FitzParams[1]
c1 = self.FitzParams[2]
c2 = self.FitzParams[3]
c3 = self.FitzParams[4]
c4 = self.FitzParams[5]
xcutuv = 10000.0 / 2700.0
tt = (x >= xcutuv)
Xx[tt] = fit_UV(x[tt])
l2x = lambda l: 1e4 / l
x_opir = np.array([0, l2x(26500.0), l2x(12200.0), l2x(6000.0), l2x(5470.0), l2x(4670.0), l2x(4110.0),
l2x(2700.), l2x(2600.)])
norm = self.R_V / 3.1
# Opt and IR computed with the IDL program provided by Fitzpatrick 1999:
y_opir = np.array([0.0, 0.26469 * norm, 0.82925 * norm, poly(self.R_V, [-4.22809e-01, 1.00270, 2.13572e-04]),
poly(self.R_V, [-5.13540e-02, 1.00216, -7.35778e-05]),
poly(self.R_V, [ 7.00127e-01, 1.00184, -3.32598e-05]),
poly(self.R_V, [ 1.19456, 1.01707, -5.46959e-03, 7.97809e-04, -4.45636e-05]),
fit_UV(l2x(2700.)), fit_UV(l2x(2600.))])
tt = x < xcutuv
if tt.sum() > 0:
tck = interpolate.splrep(x_opir, y_opir)
Xx[tt] = interpolate.splev(x[tt], tck, der=0)
return np.squeeze(Xx)
"""
def _MCC99_FM90_LMC(self, wave):
"""
In the UV, this method returns the extinction curve proposed for the LMC
by Misselt et al 1999 based on the 1990 variant of the Fitzpatrick & Massa law
In the opt/IR, it returns the Fitzpatrick & Massa 1990 law.
Misselt, Clayton & Gordon 1999 , ApJ, 515, 128
http://adsabs.harvard.edu/abs/1999ApJ...515..128M
Fitzpatrick & Massa 1990, ApJS, 72, 163
http://adsabs.harvard.edu/abs/1990ApJS...72..163F
Comments:
The Fitzpatrick & Massa 1990 law in the UV depends on 6 parameters, stored in RedCorr.FitzParams.
The method sets RedCorr.FitzParams to the values of set in the Fitzpatrick 1999 paper,
which includes an explicit dependence on R_V.
R_V must be provided, as the law depends on its value.
We refer to FM90 and not to the original FM88 because the value of a constant in F(lambda) slightly changed (0.0564 -> 0.05644)
The value of another constant of F(lambda) appears to change from FM90 to MCC99, but it is probably a typo (0.5392 -> 0.5329)
Scope: LMC
"""
x0 = 4.596
gamma = 0.91
c1 = -1.28
c2 = 1.11
c3 = 2.73
c4 = 0.64
self.FitzParams = [x0, gamma, c1, c2, c3, c4]
return self._F99_like(wave)
def _F99(self, wave):
"""
This method returns the R-dependent IR-through-UV extinction curve proposed by Fitzpatrick 1999.
Fitzpatrick 1999, PASP, 11, 63
http://adsabs.harvard.edu/abs/1999PASP..111...63F
based on:
Fitzpatrick & Massa 1990, ApJS, 72, 163
http://adsabs.harvard.edu/abs/1990ApJS...72..163F
Comments:
The Fitzpatrick & Massa 1990 law in the UV depends on 6 parameters, stored in RedCorr.FitzParams.
The method sets RedCorr.FitzParams to the values of set in the Fitzpatrick 1999 paper,
which includes an explicit dependence on R_V.
R_V must be provided, as the law depends on its value.
Range: UV through IR
"""
x0 = 4.596
gamma = 0.99
c3 = 3.23
c4 = 0.41
c2 = -0.824 + 4.717 / self.R_V # 0.7 if RV=3.1
c1 = 2.030 - 3.007 * c2 # -0.0677 if RV = 3.1
self.FitzParams = [x0, gamma, c1, c2, c3, c4]
return self._F99_like(wave)
def _FM88_F99_LMC(self, wave):
"""
This method returns:
- in the UV, the average LMC extinction curve derived by Fitzpatrick & Massa 1988
- in the opt/IR, the R-dependent extinction curve proposed by Fitzpatrick 1999.
Fitzpatrick 1999, PASP, 11, 63
http://adsabs.harvard.edu/abs/1999PASP..111...63F
Fitzpatrick & Massa 1988, ApJ, 328, 734
http://adsabs.harvard.edu/abs/1988ApJ...328..734F
Comments:
The Fitzpatrick and Massa law in the UV depends on 6 parameters, stored in RedCorr.FitzParams and
here set to the LMC values derived in FM88
R_V must be provided, as the law depends on it
Scope: LMC
Range: UV through IR
"""
x0 = 4.608
gamma = 0.994
c1 = -0.687
c2 = 0.891
c3 = 2.55
c4 = 0.504
self.FitzParams = [x0, gamma, c1, c2, c3, c4]
return self._F99_like(wave)
def _zeros(self, wave):
"""
No correction, return 0.0
"""
return np.zeros_like(wave)
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