def get_computed_models(X, Xerr):
param_range = np.arange(1, 6)
n_iter = 10**3
xdgmm = XDGMM(n_iter=n_iter)
bic, optimal_n_comp, lowest_bic = xdgmm.bic_test(X, Xerr, param_range)
aic, optimal_n_aic_comp, lowest_aic = xdgmm.aic_test(X, Xerr, param_range)
print("optimal bic {}".format(optimal_n_comp))
print("optimal aic {}".format(optimal_n_aic_comp))
return bic, aic, optimal_n_comp
class Empiricist(object):
"""
Worker object that can fit supernova and host galaxy parameters
given noisy inputs using an XDGMM model, and then predict new
supernovae based on this model and a set of new host galaxies.
Parameters
----------
model_file: string (optional)
Name of text file containing model being used (default=None).
fit_method: string (optional)
Name of XD fitting method to use (default='astroML'). Must be
either 'astroML' or 'Bovy'.
Notes
-----
The class can be initialized with a model or one can be loaded or
fit to data.
"""
def __init__(self, model_file=None, fit_method='astroML'):
self.XDGMM = XDGMM(n_components=7, method=fit_method)
self.fit_method = fit_method
if model_file is not None:
self.read_model(model_file)
def get_SN(self, X, Xerr=None, n_SN=1):
"""
Conditions the XDGMM model based on the data in X and returns
SN parameters sampled from the conditioned model.
Parameters
----------
X: array_like, shape = (n_samples, n_features)
Input data. First 3 entries (SN parameters) should be NaN.
Xerr: array_like, shape = (n_samples, n_features), optional
Error on input data. SN errors should be 0.0. If None,
errors are not used for the conditioning.
n_SN: int (optional)
Number of SNe to sample (default = 1).
Returns
-------
SN_data: array_like, shape = (n_SN, 3)
Sample of SN data taken from the conditioned model.
Notes
-----
Assumes that the first three parameters used when fitting
the model are the SN parameters.
"""
if self.model_file is None:
raise StandardError("Model parameters not set.")
if Xerr is None: cond_XDGMM = self.XDGMM.condition(X)
else: cond_XDGMM = self.XDGMM.condition(X, Xerr)
return np.atleast_2d(cond_XDGMM.sample(n_SN))
def fit_model(self, X, Xerr, filename='empiriciSN_model.fit',
n_components=6):
"""
Fits the XD model to data.
Parameters
----------
X: array_like, shape = (n_samples, n_features)
Input data.
Xerr: array_like, shape = (n_samples, n_features, n_features)
Error on input data.
filename: string (optional)
Filename for model fit to be saved to (default =
'empiriciSN_model.fit').
n_components: float (optional)
Number of Gaussian components to use (default = 6)
Notes
-----
The specified method and n_components Gaussian components will
be used (typical BIC-optimized numbers of components for ~100s
of training datapoints are 6 or 7).
The fit will be saved in the file with name defined by the
filename variable.
"""
self.XDGMM.n_components = n_components
self.XDGMM = self.XDGMM.fit(X, Xerr)
self.XDGMM.save_model(filename)
self.model_file = filename
return
def fit_from_files(self, filelist, filename='empiriciSN_model.fit',
n_components=7):
"""
Fits the XD model to data contained in the files provided.
Parameters
----------
filelist: array_like
Array of strings containing names of files containing data
to fit.
filename: string (optional)
Filename for model fit (default = 'empiriciSN_model.fit').
n_components: float (optional)
Number of Gaussian components to use (default = 7)
method: string (optional)
XD fitting method to use (default = 'astroML')
Notes
-----
The model is fitted using the data contained in the files
named in the `filelist` variable. This assumes that the data
files are in the same format as those provided with this code
and that only redshift, distance from host nucleus, host colors,
and local host surface brightness are being used for the fit.
"""
X, Xerr = self.get_data(filelist)
self.fit_model(X, Xerr, filename=filename,
n_components=n_components)
return
def read_model(self, filename):
"""
Reads the parameters of a model from a file.
Parameters
----------
filename: string
Name of the file to read from.
Notes
-----
Model parameters are stored in the self.XDGMM model object.
The model filename is stored self.model_file.
"""
self.XDGMM.read_model(filename)
self.model_file = filename
return
def component_test(self, X, Xerr, component_range, no_err=False):
"""
Test the performance of the model for a range of numbers of
Gaussian components.
Parameters
----------
X: array_like, shape = (n_samples, n_features)
Input data.
Xerr: array_like, shape = (n_samples, n_features, n_features)
Error on input data.
component_range: array_like
Range of n_components to test.
no_err: bool (optional)
Flag for whether to calculate the BIC with the errors
included or not. (default = False)
Returns
-------
bics: array_like, shape = (len(param_range),)
BIC for each value of n_components
optimal_n_comp: float
Number of components with lowest BIC score
lowest_bic: float
Lowest BIC from the scores computed.
Notes
-----
Uses the XDGMM.bic_test method to compute the BIC score for
each n_components in the component_range array.
"""
bics, optimal_n_comp, lowest_bic = \
self.XDGMM.bic_test(X, Xerr, component_range, no_err)
return bics, optimal_n_comp, lowest_bic
def get_logR(self,cond_indices, R_index, X, Xerr=None):
"""
Uses a subset of parameters in the given data to condition the
model and return a sample value for log(R/Re).
Parameters
----------
cond_indices: array_like
Array of indices indicating which parameters to use to
condition the model. Cannot contain [0, 1, 2] since these
are SN parameters.
R_index: int
Index of log(R/Re) in the list of parameters that were used
to fit the model.
X: array_like, shape = (n < n_features,)
Input data.
Xerr: array_like, shape = (X.shape,) (optional)
Error on input data. If none, no error used to condition.
Returns
-------
logR: float
Sample value of log(R/Re) taken from the conditioned model.
Notes
-----
The fit_params array specifies a list of indices to use to
condition the model. The model will be conditioned and then
a radius will be drawn from the conditioned model.
This is so that the radius can then be used to calculate local
surface brightness to fully condition the model to sample
likely SN parameters.
This does not make assumptions about what parameters are being
used in the model, but does assume that the model has been
fit already and that the first three parameters in the data
that were used to fit the model are the SN parameters.
"""
if self.model_file is None:
raise StandardError("Model parameters not set.")
if 0 in cond_indices or 1 in cond_indices or 2 in cond_indices:
raise ValueError("Cannot condition model on SN parameters.")
if R_index in cond_indices:
raise ValueError("Cannot condition model on log(R/Re).")
cond_data = np.array([])
if Xerr is not None: cond_err = np.array([])
R_cond_idx = R_index
n_features = self.XDGMM.mu.shape[1]
j = 0
for i in range(n_features):
if i in cond_indices:
cond_data = np.append(cond_data,X[j])
if Xerr is not None: cond_err = np.append(cond_err, Xerr[j])
j += 1
if i < R_index: R_cond_idx -= 1
else:
cond_data = np.append(cond_data,np.nan)
if Xerr is not None: cond_err = np.append(cond_err, 0.0)
if Xerr is not None:
cond_XDGMM = self.XDGMM.condition(cond_data, cond_err)
else: cond_XDGMM = self.XDGMM.condition(cond_data)
sample = cond_XDGMM.sample()
logR = sample[0][R_cond_idx]
return logR
def get_local_SB(self, SB_params, R ):
"""
Uses magnitudes, a surface brightness (SB) profile, and
a SN location to fit local surface brightnesses at the location
of the SN.
Parameters
----------
SB_params: array_like, shape = (21,)
Array of parameters needed for the SB fit. First entry
should be a sersic index of 1 or 4, indicating whether to
use an exponential or de Vaucouleurs profile. Following this
should be sets of
(magnitude, mag_unc, effective radius, rad_unc) data for
each of the 5 ugriz filters, giving a total array length of
21. These data are assumed to be known by the user.
R: float
Separation from host nucleus in units of log(R/Re).
It is assumed that the Re used here is the r-band Re, as is
output by the get_logR function.
Returns
-------
SBs: array_list, shape = (5,)
Local surface brightness at the location of the SN for each
of the 5 ugriz filters. Units = mag/arcsec^2
SB_errs: array_like, shape = (5,)
Uncertainties on the local surface brightnesses.
"""
if SB_params[0]!=1 and SB_params[0]!=4:
raise ValueError("Sersic index must be 1 or 4")
sep = (10**R) * SB_params[11] # separation in arcsec
SBs = np.array([])
SB_errs = np.array([])
for j in range(5):
halfmag = SB_params[j*4+1] + 0.75257
magerr = SB_params[j*4+2]
Re = SB_params[j*4+3]
Re_err = SB_params[j*4+4]
r = sep/Re
Ie = halfmag + 2.5 * np.log10(np.pi*Re**2)
Re2_unc = 2 * Re * Re_err * np.pi
log_unc = 2.5 * Re2_unc/(np.log10(np.pi*Re**2) * np.log(10))
Ie_unc = np.sqrt(magerr**2 + log_unc**2)
if SB_params[0] == 1:
Io = Ie-1.824
Io_unc = Ie_unc
sb = Io*np.exp(-1.68*(r))
exp_unc = np.exp(-1.68*(r))*1.68*sep*Re_err/(Re**2)
sb_unc = sb * np.sqrt((Io_unc/Io)**2 +
(exp_unc/np.exp(-1.68*(r)))**2)
if np.isnan(sb_unc): sb_unc = 0.0
if sb_unc < 0: sb_unc = sb_unc*-1.0
SBs = np.append(SBs,sb)
SB_errs = np.append(SB_errs,sb_unc)
if SB_params[0] == 4:
Io = Ie-8.328
Io_unc = Ie_unc
sb = Io*np.exp(-7.67*((r)**0.25))
exp_unc = np.exp(-7.67*((r)**0.25))*7.67*sep \
*Re_err/(4*Re**(1.25))
sb_unc = sb*np.sqrt((Io_unc/Io)**2+(exp_unc \
/np.exp(-7.67*((r)**0.25))))
if np.isnan(sb_unc): sb_unc = 0.0
if sb_unc < 0: sb_unc = sb_unc*-1.0
SBs = np.append(SBs,sb)
SB_errs = np.append(SB_errs,sb_unc)
return SBs, SB_errs
def set_fit_method(self, fit_method):
"""
Sets the XD fitting method to use.
Parameters
----------
fit_method: string
Name of fitting method to use. Must be either 'astroML' or
'Bovy'.
Notes
-----
Changes the fitting method of self.XDGMM to the one specified
in `fit_method`.
"""
if fit_method == 'astroML':
n_iter = 100
elif fit_method == 'Bovy':
n_iter = 10**9
else:
raise ValueError("Method must be either 'astroML' or 'Bovy'")
self.XDGMM.method = fit_method
self.XDGMM.n_iter = n_iter
self.fit_method = fit_method
return
def get_data(self, filelist):
"""
Parses SN and host data from a list of data files.
Parameters
----------
filelist: array_like
Array of strings containing names of files containing data
to fit.
Returns
-------
X: array_like, shape = (n_samples, n_features)
Output data. Contains SALT2 SN parameters, host redshift,
log(R/Re), host colors, and host brightnesses at the
locations of the SN in each filter.
Xerr: array_like, shape = (n_samples, n_features, n_features)
Error on output data.
Notes
-----
Reads in each data file and returns an array of data and a
matrix of errors, which can be used to fit the XDGMM model.
Currently reads the SALT2 SN parameters, host redshift,
log(R/Re), host magnitudes, and host surface brightnesses
at the location of the SN.
This method needs further modularizing, to enable the worker
to calculate host surface brightnesses separately (in a static method).
"""
x0 = np.array([])
x0_err = np.array([])
x1 = np.array([])
x1_err = np.array([])
c = np.array([])
c_err = np.array([])
z = np.array([])
z_err = np.array([])
logr = np.array([])
logr_err = np.array([])
umag = np.array([])
umag_err = np.array([])
gmag = np.array([])
gmag_err = np.array([])
rmag = np.array([])
rmag_err = np.array([])
imag = np.array([])
imag_err = np.array([])
zmag = np.array([])
zmag_err = np.array([])
SB_u = np.array([])
SB_u_err = np.array([])
SB_g = np.array([])
SB_g_err = np.array([])
SB_r = np.array([])
SB_r_err = np.array([])
SB_i = np.array([])
SB_i_err = np.array([])
SB_z = np.array([])
SB_z_err = np.array([])
for filename in filelist:
infile = open(filename,'r')
inlines = infile.readlines()
infile.close()
for line1 in inlines:
if line1[0]=='#': continue
line = line1.split(',')
if line[33]=='nan' or line[39]=='nan' or line[45]=='nan'\
or line[51]=='nan' or line[57]=='nan': continue
# SN params
x0 = np.append(x0,float(line[7])) #x0
x0_err = np.append(x0_err,float(line[8]))
x1 = np.append(x1,float(line[9])) # x1
x1_err = np.append(x1_err,float(line[10]))
c = np.append(c,float(line[11])) # c
c_err = np.append(c_err,float(line[12]))
# Host params
z = np.append(z,float(line[4]))
z_err = np.append(z_err,0.0)
logr = np.append(logr,np.log10(float(line[15])/float(line[42]))) # r
logr_err = np.append(logr_err,float(line[43])/(float(line[42])*np.log(10)))
umag = np.append(umag,float(line[18])) # u_mag
umag_err = np.append(umag_err,float(line[19]))
gmag = np.append(gmag,float(line[20])) # g_mag
gmag_err = np.append(gmag_err,float(line[21]))
rmag = np.append(rmag,float(line[22])) # r_mag
rmag_err = np.append(rmag_err,float(line[23]))
imag = np.append(imag,float(line[24])) # i_mag
imag_err = np.append(imag_err,float(line[25]))
zmag = np.append(zmag,float(line[26])) # z_mag
zmag_err = np.append(zmag_err,float(line[27]))
SB_u = np.append(SB_u,float(line[32])) # SB_u
SB_u_err = np.append(SB_u_err,float(line[33]))
SB_g = np.append(SB_g,float(line[38])) # SB_g
SB_g_err = np.append(SB_g_err,float(line[39]))
SB_r = np.append(SB_r,float(line[44])) # SB_r
SB_r_err = np.append(SB_r_err,float(line[45]))
SB_i = np.append(SB_i,float(line[50])) # SB_i
SB_i_err = np.append(SB_i_err,float(line[52]))
SB_z = np.append(SB_z,float(line[56])) # SB_z
SB_z_err = np.append(SB_z_err,float(line[57]))
ug = umag-gmag
ug_err = np.sqrt(umag_err**2+gmag_err**2)
ur = umag-rmag
ur_err = np.sqrt(umag_err**2+rmag_err**2)
ui = umag-imag
ui_err = np.sqrt(umag_err**2+imag_err**2)
uz = umag-zmag
uz_err = np.sqrt(umag_err**2+zmag_err**2)
gr = gmag-rmag
gr_err = np.sqrt(gmag_err**2+rmag_err**2)
gi = gmag-imag
gi_err = np.sqrt(gmag_err**2+imag_err**2)
gz = gmag-zmag
gz_err = np.sqrt(gmag_err**2+zmag_err**2)
ri = rmag-imag
ri_err = np.sqrt(rmag_err**2+imag_err**2)
rz = rmag-zmag
rz_err = np.sqrt(rmag_err**2+zmag_err**2)
iz = imag-zmag
iz_err = np.sqrt(imag_err**2+zmag_err**2)
X = np.vstack([x0,x1,c,z,logr,ug,ur,ui,uz,gr,gi,gz,ri,rz,iz,SB_u,
SB_g,SB_r,SB_i,SB_z]).T
Xerr = np.zeros(X.shape + X.shape[-1:])
diag = np.arange(X.shape[-1])
Xerr[:, diag, diag] = np.vstack([x0_err**2,x1_err**2,c_err**2,
z_err**2,logr_err**2,ug_err**2,
ur_err**2,ui_err**2,uz_err**2,
gr_err**2,gi_err**2,gz_err**2,
ri_err**2,rz_err**2,iz_err**2,
SB_u_err**2,SB_g_err**2,
SB_r_err**2,SB_i_err**2,
SB_z_err**2]).T
return X, Xerr
class Empiricist(object):
"""
Worker object that can fit supernova and host galaxy parameters
given noisy inputs using an XDGMM model, and then predict new
supernovae based on this model and a set of new host galaxies.
Parameters
----------
model_file: string (optional)
Name of text file containing model being used (default=None).
fit_method: string (optional)
Name of XD fitting method to use (default='astroML'). Must be
either 'astroML' or 'Bovy'.
Notes
-----
The class can be initialized with a model or one can be loaded or
fit to data.
"""
def __init__(self, model_file=None, fit_method='astroML'):
self.XDGMM = XDGMM(n_components=7, method=fit_method)
self.fit_method = fit_method
if model_file is not None:
self.read_model(model_file)
def get_SN(self, X, Xerr=None, n_SN=1):
"""
Conditions the XDGMM model based on the data in X and returns
SN parameters sampled from the conditioned model.
Parameters
----------
X: array_like, shape = (n_samples, n_features)
Input data. First 3 entries (SN parameters) should be NaN.
Xerr: array_like, shape = (n_samples, n_features), optional
Error on input data. SN errors should be 0.0. If None,
errors are not used for the conditioning.
n_SN: int (optional)
Number of SNe to sample (default = 1).
Returns
-------
SN_data: array_like, shape = (n_SN, 3)
Sample of SN data taken from the conditioned model.
Notes
-----
Assumes that the first three parameters used when fitting
the model are the SN parameters.
"""
if self.model_file is None:
raise StandardError("Model parameters not set.")
if Xerr is None: cond_XDGMM = self.XDGMM.condition(X)
else: cond_XDGMM = self.XDGMM.condition(X, Xerr)
return np.atleast_2d(cond_XDGMM.sample(n_SN))
def fit_model(self,
X,
Xerr,
filename='empiriciSN_model.fit',
n_components=6):
"""
Fits the XD model to data.
Parameters
----------
X: array_like, shape = (n_samples, n_features)
Input data.
Xerr: array_like, shape = (n_samples, n_features, n_features)
Error on input data.
filename: string (optional)
Filename for model fit to be saved to (default =
'empiriciSN_model.fit').
n_components: float (optional)
Number of Gaussian components to use (default = 6)
Notes
-----
The specified method and n_components Gaussian components will
be used (typical BIC-optimized numbers of components for ~100s
of training datapoints are 6 or 7).
The fit will be saved in the file with name defined by the
filename variable.
"""
self.XDGMM.n_components = n_components
self.XDGMM = self.XDGMM.fit(X, Xerr)
self.XDGMM.save_model(filename)
self.model_file = filename
return
def fit_from_files(self,
filelist,
filename='empiriciSN_model.fit',
n_components=7):
"""
Fits the XD model to data contained in the files provided.
Parameters
----------
filelist: array_like
Array of strings containing names of files containing data
to fit.
filename: string (optional)
Filename for model fit (default = 'empiriciSN_model.fit').
n_components: float (optional)
Number of Gaussian components to use (default = 7)
method: string (optional)
XD fitting method to use (default = 'astroML')
Notes
-----
The model is fitted using the data contained in the files
named in the `filelist` variable. This assumes that the data
files are in the same format as those provided with this code
and that only redshift, distance from host nucleus, host colors,
and local host surface brightness are being used for the fit.
"""
X, Xerr = self.get_data(filelist)
self.fit_model(X, Xerr, filename=filename, n_components=n_components)
return
def read_model(self, filename):
"""
Reads the parameters of a model from a file.
Parameters
----------
filename: string
Name of the file to read from.
Notes
-----
Model parameters are stored in the self.XDGMM model object.
The model filename is stored self.model_file.
"""
self.XDGMM.read_model(filename)
self.model_file = filename
return
def component_test(self, X, Xerr, component_range, no_err=False):
"""
Test the performance of the model for a range of numbers of
Gaussian components.
Parameters
----------
X: array_like, shape = (n_samples, n_features)
Input data.
Xerr: array_like, shape = (n_samples, n_features, n_features)
Error on input data.
component_range: array_like
Range of n_components to test.
no_err: bool (optional)
Flag for whether to calculate the BIC with the errors
included or not. (default = False)
Returns
-------
bics: array_like, shape = (len(param_range),)
BIC for each value of n_components
optimal_n_comp: float
Number of components with lowest BIC score
lowest_bic: float
Lowest BIC from the scores computed.
Notes
-----
Uses the XDGMM.bic_test method to compute the BIC score for
each n_components in the component_range array.
"""
bics, optimal_n_comp, lowest_bic = \
self.XDGMM.bic_test(X, Xerr, component_range, no_err)
return bics, optimal_n_comp, lowest_bic
def get_logR(self, cond_indices, R_index, X, Xerr=None):
"""
Uses a subset of parameters in the given data to condition the
model and return a sample value for log(R/Re).
Parameters
----------
cond_indices: array_like
Array of indices indicating which parameters to use to
condition the model. Cannot contain [0, 1, 2] since these
are SN parameters.
R_index: int
Index of log(R/Re) in the list of parameters that were used
to fit the model.
X: array_like, shape = (n < n_features,)
Input data.
Xerr: array_like, shape = (X.shape,) (optional)
Error on input data. If none, no error used to condition.
Returns
-------
logR: float
Sample value of log(R/Re) taken from the conditioned model.
Notes
-----
The fit_params array specifies a list of indices to use to
condition the model. The model will be conditioned and then
a radius will be drawn from the conditioned model.
This is so that the radius can then be used to calculate local
surface brightness to fully condition the model to sample
likely SN parameters.
This does not make assumptions about what parameters are being
used in the model, but does assume that the model has been
fit already and that the first three parameters in the data
that were used to fit the model are the SN parameters.
"""
if self.model_file is None:
raise StandardError("Model parameters not set.")
if 0 in cond_indices or 1 in cond_indices or 2 in cond_indices:
raise ValueError("Cannot condition model on SN parameters.")
if R_index in cond_indices:
raise ValueError("Cannot condition model on log(R/Re).")
cond_data = np.array([])
if Xerr is not None: cond_err = np.array([])
R_cond_idx = R_index
n_features = self.XDGMM.mu.shape[1]
j = 0
for i in range(n_features):
if i in cond_indices:
cond_data = np.append(cond_data, X[j])
if Xerr is not None: cond_err = np.append(cond_err, Xerr[j])
j += 1
if i < R_index: R_cond_idx -= 1
else:
cond_data = np.append(cond_data, np.nan)
if Xerr is not None: cond_err = np.append(cond_err, 0.0)
if Xerr is not None:
cond_XDGMM = self.XDGMM.condition(cond_data, cond_err)
else:
cond_XDGMM = self.XDGMM.condition(cond_data)
sample = cond_XDGMM.sample()
logR = sample[0][R_cond_idx]
return logR
def get_local_SB(self, SB_params, R):
"""
Uses magnitudes, a surface brightness (SB) profile, and
a SN location to fit local surface brightnesses at the location
of the SN.
Parameters
----------
SB_params: array_like, shape = (21,)
Array of parameters needed for the SB fit. First entry
should be a sersic index of 1 or 4, indicating whether to
use an exponential or de Vaucouleurs profile. Following this
should be sets of
(magnitude, mag_unc, effective radius, rad_unc) data for
each of the 5 ugriz filters, giving a total array length of
21. These data are assumed to be known by the user.
R: float
Separation from host nucleus in units of log(R/Re).
It is assumed that the Re used here is the r-band Re, as is
output by the get_logR function.
Returns
-------
SBs: array_list, shape = (5,)
Local surface brightness at the location of the SN for each
of the 5 ugriz filters. Units = mag/arcsec^2
SB_errs: array_like, shape = (5,)
Uncertainties on the local surface brightnesses.
"""
if SB_params[0] != 1 and SB_params[0] != 4:
raise ValueError("Sersic index must be 1 or 4")
sep = (10**R) * SB_params[11] # separation in arcsec
SBs = np.array([])
SB_errs = np.array([])
for j in range(5):
halfmag = SB_params[j * 4 + 1] + 0.75257
magerr = SB_params[j * 4 + 2]
Re = SB_params[j * 4 + 3]
Re_err = SB_params[j * 4 + 4]
r = sep / Re
Ie = halfmag + 2.5 * np.log10(np.pi * Re**2)
Re2_unc = 2 * Re * Re_err * np.pi
log_unc = 2.5 * Re2_unc / (np.log10(np.pi * Re**2) * np.log(10))
Ie_unc = np.sqrt(magerr**2 + log_unc**2)
if SB_params[0] == 1:
Io = Ie - 1.824
Io_unc = Ie_unc
sb = Io * np.exp(-1.68 * (r))
exp_unc = np.exp(-1.68 * (r)) * 1.68 * sep * Re_err / (Re**2)
sb_unc = sb * np.sqrt((Io_unc / Io)**2 +
(exp_unc / np.exp(-1.68 * (r)))**2)
if np.isnan(sb_unc): sb_unc = 0.0
if sb_unc < 0: sb_unc = sb_unc * -1.0
SBs = np.append(SBs, sb)
SB_errs = np.append(SB_errs, sb_unc)
if SB_params[0] == 4:
Io = Ie - 8.328
Io_unc = Ie_unc
sb = Io * np.exp(-7.67 * ((r)**0.25))
exp_unc = np.exp(-7.67*((r)**0.25))*7.67*sep \
*Re_err/(4*Re**(1.25))
sb_unc = sb*np.sqrt((Io_unc/Io)**2+(exp_unc \
/np.exp(-7.67*((r)**0.25))))
if np.isnan(sb_unc): sb_unc = 0.0
if sb_unc < 0: sb_unc = sb_unc * -1.0
SBs = np.append(SBs, sb)
SB_errs = np.append(SB_errs, sb_unc)
return SBs, SB_errs
def set_fit_method(self, fit_method):
"""
Sets the XD fitting method to use.
Parameters
----------
fit_method: string
Name of fitting method to use. Must be either 'astroML' or
'Bovy'.
Notes
-----
Changes the fitting method of self.XDGMM to the one specified
in `fit_method`.
"""
if fit_method == 'astroML':
n_iter = 100
elif fit_method == 'Bovy':
n_iter = 10**9
else:
raise ValueError("Method must be either 'astroML' or 'Bovy'")
self.XDGMM.method = fit_method
self.XDGMM.n_iter = n_iter
self.fit_method = fit_method
return
def get_data(self, filelist):
"""
Parses SN and host data from a list of data files.
Parameters
----------
filelist: array_like
Array of strings containing names of files containing data
to fit.
Returns
-------
X: array_like, shape = (n_samples, n_features)
Output data. Contains SALT2 SN parameters, host redshift,
log(R/Re), host colors, and host brightnesses at the
locations of the SN in each filter.
Xerr: array_like, shape = (n_samples, n_features, n_features)
Error on output data.
Notes
-----
Reads in each data file and returns an array of data and a
matrix of errors, which can be used to fit the XDGMM model.
Currently reads the SALT2 SN parameters, host redshift,
log(R/Re), host magnitudes, and host surface brightnesses
at the location of the SN.
This method needs further modularizing, to enable the worker
to calculate host surface brightnesses separately (in a static method).
"""
x0 = np.array([])
x0_err = np.array([])
x1 = np.array([])
x1_err = np.array([])
c = np.array([])
c_err = np.array([])
z = np.array([])
z_err = np.array([])
logr = np.array([])
logr_err = np.array([])
umag = np.array([])
umag_err = np.array([])
gmag = np.array([])
gmag_err = np.array([])
rmag = np.array([])
rmag_err = np.array([])
imag = np.array([])
imag_err = np.array([])
zmag = np.array([])
zmag_err = np.array([])
SB_u = np.array([])
SB_u_err = np.array([])
SB_g = np.array([])
SB_g_err = np.array([])
SB_r = np.array([])
SB_r_err = np.array([])
SB_i = np.array([])
SB_i_err = np.array([])
SB_z = np.array([])
SB_z_err = np.array([])
for filename in filelist:
infile = open(filename, 'r')
inlines = infile.readlines()
infile.close()
for line1 in inlines:
if line1[0] == '#': continue
line = line1.split(',')
if line[33]=='nan' or line[39]=='nan' or line[45]=='nan'\
or line[51]=='nan' or line[57]=='nan':
continue
# SN params
x0 = np.append(x0, float(line[7])) #x0
x0_err = np.append(x0_err, float(line[8]))
x1 = np.append(x1, float(line[9])) # x1
x1_err = np.append(x1_err, float(line[10]))
c = np.append(c, float(line[11])) # c
c_err = np.append(c_err, float(line[12]))
# Host params
z = np.append(z, float(line[4]))
z_err = np.append(z_err, 0.0)
logr = np.append(logr,
np.log10(float(line[15]) /
float(line[42]))) # r
logr_err = np.append(
logr_err,
float(line[43]) / (float(line[42]) * np.log(10)))
umag = np.append(umag, float(line[18])) # u_mag
umag_err = np.append(umag_err, float(line[19]))
gmag = np.append(gmag, float(line[20])) # g_mag
gmag_err = np.append(gmag_err, float(line[21]))
rmag = np.append(rmag, float(line[22])) # r_mag
rmag_err = np.append(rmag_err, float(line[23]))
imag = np.append(imag, float(line[24])) # i_mag
imag_err = np.append(imag_err, float(line[25]))
zmag = np.append(zmag, float(line[26])) # z_mag
zmag_err = np.append(zmag_err, float(line[27]))
SB_u = np.append(SB_u, float(line[32])) # SB_u
SB_u_err = np.append(SB_u_err, float(line[33]))
SB_g = np.append(SB_g, float(line[38])) # SB_g
SB_g_err = np.append(SB_g_err, float(line[39]))
SB_r = np.append(SB_r, float(line[44])) # SB_r
SB_r_err = np.append(SB_r_err, float(line[45]))
SB_i = np.append(SB_i, float(line[50])) # SB_i
SB_i_err = np.append(SB_i_err, float(line[52]))
SB_z = np.append(SB_z, float(line[56])) # SB_z
SB_z_err = np.append(SB_z_err, float(line[57]))
ug = umag - gmag
ug_err = np.sqrt(umag_err**2 + gmag_err**2)
ur = umag - rmag
ur_err = np.sqrt(umag_err**2 + rmag_err**2)
ui = umag - imag
ui_err = np.sqrt(umag_err**2 + imag_err**2)
uz = umag - zmag
uz_err = np.sqrt(umag_err**2 + zmag_err**2)
gr = gmag - rmag
gr_err = np.sqrt(gmag_err**2 + rmag_err**2)
gi = gmag - imag
gi_err = np.sqrt(gmag_err**2 + imag_err**2)
gz = gmag - zmag
gz_err = np.sqrt(gmag_err**2 + zmag_err**2)
ri = rmag - imag
ri_err = np.sqrt(rmag_err**2 + imag_err**2)
rz = rmag - zmag
rz_err = np.sqrt(rmag_err**2 + zmag_err**2)
iz = imag - zmag
iz_err = np.sqrt(imag_err**2 + zmag_err**2)
X = np.vstack([
x0, x1, c, z, logr, ug, ur, ui, uz, gr, gi, gz, ri, rz, iz, SB_u,
SB_g, SB_r, SB_i, SB_z
]).T
Xerr = np.zeros(X.shape + X.shape[-1:])
diag = np.arange(X.shape[-1])
Xerr[:, diag, diag] = np.vstack([
x0_err**2, x1_err**2, c_err**2, z_err**2, logr_err**2, ug_err**2,
ur_err**2, ui_err**2, uz_err**2, gr_err**2, gi_err**2, gz_err**2,
ri_err**2, rz_err**2, iz_err**2, SB_u_err**2, SB_g_err**2,
SB_r_err**2, SB_i_err**2, SB_z_err**2
]).T
return X, Xerr