def get_photometry(ID=None,extra_fields=['_r','_RAJ2000','_DEJ2000'],**kwargs):
"""
Download all available photometry from a star to a record array.
For extra kwargs, see L{_get_URI} and L{mast2phot}
"""
to_units = kwargs.pop('to_units','erg/s/cm2/AA')
master_ = kwargs.get('master',None)
master = None
#-- retrieve all measurements
for source in cat_info.sections():
if source=='galex':
results,units,comms = galex(ID=ID,**kwargs)
else:
results,units,comms = search(source,ID=ID,**kwargs)
if results is not None:
master = mast2phot(source,results,units,master,extra_fields=extra_fields)
#-- convert the measurement to a common unit.
if to_units and master is not None:
#-- prepare columns to extend to basic master
dtypes = [('cwave','f8'),('cmeas','f8'),('e_cmeas','f8'),('cunit','a50')]
cols = [[],[],[],[]]
#-- forget about 'nan' errors for the moment
no_errors = np.isnan(master['e_meas'])
master['e_meas'][no_errors] = 0.
#-- extend basic master
zp = filters.get_info(master['photband'])
for i in range(len(master)):
try:
value,e_value = conversions.convert(master['unit'][i],to_units,master['meas'][i],master['e_meas'][i],photband=master['photband'][i])
except ValueError: # calibrations not available
value,e_value = np.nan,np.nan
except AssertionError: # postive flux and errors!
value,e_value = np.nan,np.nan
try:
eff_wave = filters.eff_wave(master['photband'][i])
except IOError:
eff_wave = np.nan
cols[0].append(eff_wave)
cols[1].append(value)
cols[2].append(e_value)
cols[3].append(to_units)
master = numpy_ext.recarr_addcols(master,cols,dtypes)
#-- reset errors
master['e_meas'][no_errors] = np.nan
master['e_cmeas'][no_errors] = np.nan
if master_ is not None and master is not None:
master = numpy_ext.recarr_addrows(master_,master.tolist())
elif master_ is not None:
master = master_
#-- and return the results
return master
def redden(flux,
wave=None,
photbands=None,
ebv=0.,
rtype='flux',
law='cardelli1989',
**kwargs):
"""
Redden flux or magnitudes
The reddening parameters C{ebv} means E(B-V).
If it is negative, we B{deredden}.
If you give the keyword C{wave}, it is assumed that you want to (de)redden
a B{model}, i.e. a spectral energy distribution.
If you give the keyword C{photbands}, it is assumed that you want to (de)redden
B{photometry}, i.e. integrated fluxes.
@param flux: fluxes to (de)redden (magnitudes if C{rtype='mag'})
@type flux: ndarray (floats)
@param wave: wavelengths matching the fluxes (or give C{photbands})
@type wave: ndarray (floats)
@param photbands: photometry bands matching the fluxes (or give C{wave})
@type photbands: ndarray of str
@param ebv: reddening parameter E(B-V)
@type ebv: float
@param rtype: type of dereddening (magnituds or fluxes)
@type rtype: str ('flux' or 'mag')
@return: (de)reddened flux/magnitude
@rtype: ndarray (floats)
"""
if photbands is not None:
wave = filters.get_info(photbands)['eff_wave']
old_settings = np.seterr(all='ignore')
wave, reddeningMagnitude = get_law(law, wave=wave, **kwargs)
if rtype == 'flux':
# In this case flux means really flux
flux_reddened = flux / 10**(reddeningMagnitude * ebv / 2.5)
np.seterr(**old_settings)
return flux_reddened
elif rtype == 'mag':
# In this case flux means actually a magnitude
magnitude = flux
magnitude_reddened = magnitude + reddeningMagnitude * ebv
np.seterr(**old_settings)
return magnitude_reddened
def get_photometry(ID=None, extra_fields=[], **kwargs):
"""
Download all available photometry from a star to a record array.
Extra fields will not be useful probably.
For extra kwargs, see L{_get_URI} and L{gcpd2phot}
"""
to_units = kwargs.pop('to_units', 'erg/s/cm2/AA')
master_ = kwargs.get('master', None)
master = None
#-- retrieve all measurements
for source in cat_info.sections():
results, units, comms = search(source, ID=ID, **kwargs)
if results is not None:
master = gcpd2phot(source,
results,
units,
master,
extra_fields=extra_fields)
#-- convert the measurement to a common unit.
if to_units and master is not None:
#-- prepare columns to extend to basic master
dtypes = [('cwave', 'f8'), ('cmeas', 'f8'), ('e_cmeas', 'f8'),
('cunit', 'U50')]
cols = [[], [], [], []]
#-- forget about 'nan' errors for the moment
no_errors = np.isnan(master['e_meas'])
master['e_meas'][no_errors] = 0.
#-- extend basic master
try:
zp = filters.get_info(master['photband'])
except:
print(master['photband'])
raise
for i in range(len(master)):
to_units_ = to_units + ''
try:
value, e_value = conversions.convert(
master['unit'][i],
to_units,
master['meas'][i],
master['e_meas'][i],
photband=master['photband'][i])
except ValueError: # calibrations not available
# if it is a magnitude color, try converting it to a flux ratio
if 'mag' in master['unit'][i]:
try:
value, e_value = conversions.convert(
'mag_color',
'flux_ratio',
master['meas'][i],
master['e_meas'][i],
photband=master['photband'][i])
to_units_ = 'flux_ratio'
except ValueError:
value, e_value = np.nan, np.nan
# else, we are powerless...
else:
value, e_value = np.nan, np.nan
try:
eff_wave = filters.eff_wave(master['photband'][i])
except IOError:
eff_wave = np.nan
cols[0].append(eff_wave)
cols[1].append(value)
cols[2].append(e_value)
cols[3].append(to_units_)
master = numpy_ext.recarr_addcols(master, cols, dtypes)
#-- reset errors
master['e_meas'][no_errors] = np.nan
master['e_cmeas'][no_errors] = np.nan
#-- if a master is given as a keyword, and data is found in this module,
# append the two
if master_ is not None and master is not None:
master = numpy_ext.recarr_addrows(master_, master.tolist())
elif master is None:
master = master_
#-- and return the results
return master
def get_photometry(ID=None,extra_fields=['dist','ra','dec'],**kwargs):
"""
Download all available photometry from a star to a record array.
For extra kwargs, see L{_get_URI} and L{gator2phot}
Example usage:
>>> import pylab
>>> import vizier
>>> name = 'kr cam'
>>> master = vizier.get_photometry(name,to_units='erg/s/cm2/AA',extra_fields=[])
>>> master = get_photometry(name,to_units='erg/s/cm2/AA',extra_fields=[],master=master)
>>> p = pylab.figure()
>>> wise = np.array(['WISE' in photband and True or False for photband in master['photband']])
>>> p = pylab.errorbar(master['cwave'],master['cmeas'],yerr=master['e_cmeas'],fmt='ko')
>>> p = pylab.errorbar(master['cwave'][wise],master['cmeas'][wise],yerr=master['e_cmeas'][wise],fmt='ro',ms=8)
>>> p = pylab.gca().set_xscale('log')
>>> p = pylab.gca().set_yscale('log')
>>> p = pylab.show()
Other examples:
>>> master = get_photometry(ra=71.239527,dec=-70.589427,to_units='erg/s/cm2/AA',extra_fields=[],radius=1.)
>>> master = get_photometry(ID='J044458.39-703522.6',to_units='W/m2',extra_fields=[],radius=1.)
"""
kwargs['ID'] = ID
to_units = kwargs.pop('to_units','erg/s/cm2/AA')
master_ = kwargs.get('master',None)
master = None
#-- retrieve all measurements
for source in cat_info.sections():
results,units,comms = search(source,**kwargs)
if results is not None:
master = gator2phot(source,results,units,master,extra_fields=extra_fields)
#-- convert the measurement to a common unit.
if to_units and master is not None:
#-- prepare columns to extend to basic master
dtypes = [('cwave','f8'),('cmeas','f8'),('e_cmeas','f8'),('cunit','a50')]
cols = [[],[],[],[]]
#-- forget about 'nan' errors for the moment
no_errors = np.isnan(master['e_meas'])
master['e_meas'][no_errors] = 0.
#-- extend basic master
zp = filters.get_info(master['photband'])
for i in range(len(master)):
try:
value,e_value = conversions.convert(master['unit'][i],to_units,master['meas'][i],master['e_meas'][i],photband=master['photband'][i])
except ValueError: # calibrations not available
value,e_value = np.nan,np.nan
except AssertionError: # the error or flux must be positive number
value,e_value = np.nan,np.nan
try:
eff_wave = filters.eff_wave(master['photband'][i])
except IOError:
eff_wave = np.nan
cols[0].append(eff_wave)
cols[1].append(value)
cols[2].append(e_value)
cols[3].append(to_units)
master = numpy_ext.recarr_addcols(master,cols,dtypes)
#-- reset errors
master['e_meas'][no_errors] = np.nan
master['e_cmeas'][no_errors] = np.nan
if master_ is not None and master is not None:
master = numpy_ext.recarr_addrows(master_,master.tolist())
elif master_ is not None:
master = master_
#-- and return the results
return master
def get_photometry(ID=None,extra_fields=['dist','ra','dec'],**kwargs):
"""
Download all available photometry from a star to a record array.
For extra kwargs, see L{_get_URI} and L{gator2phot}
Example usage:
>>> import pylab
>>> import vizier
>>> name = 'kr cam'
>>> master = vizier.get_photometry(name,to_units='erg/s/cm2/AA',extra_fields=[])
>>> master = get_photometry(name,to_units='erg/s/cm2/AA',extra_fields=[],master=master)
>>> p = pylab.figure()
>>> wise = np.array(['WISE' in photband and True or False for photband in master['photband']])
>>> p = pylab.errorbar(master['cwave'],master['cmeas'],yerr=master['e_cmeas'],fmt='ko')
>>> p = pylab.errorbar(master['cwave'][wise],master['cmeas'][wise],yerr=master['e_cmeas'][wise],fmt='ro',ms=8)
>>> p = pylab.gca().set_xscale('log')
>>> p = pylab.gca().set_yscale('log')
>>> p = pylab.show()
Other examples:
>>> master = get_photometry(ra=71.239527,dec=-70.589427,to_units='erg/s/cm2/AA',extra_fields=[],radius=1.)
>>> master = get_photometry(ID='J044458.39-703522.6',to_units='W/m2',extra_fields=[],radius=1.)
"""
kwargs['ID'] = ID
to_units = kwargs.pop('to_units','erg/s/cm2/AA')
master_ = kwargs.get('master',None)
master = None
#-- retrieve all measurements
for source in cat_info.sections():
results,units,comms = search(source,**kwargs)
if results is not None:
master = gator2phot(source,results,units,master,extra_fields=extra_fields)
#-- convert the measurement to a common unit.
if to_units and master is not None:
#-- prepare columns to extend to basic master
dtypes = [('cwave','f8'),('cmeas','f8'),('e_cmeas','f8'),('cunit','U50')]
cols = [[],[],[],[]]
#-- forget about 'nan' errors for the moment
no_errors = np.isnan(master['e_meas'])
master['e_meas'][no_errors] = 0.
#-- extend basic master
zp = filters.get_info(master['photband'])
for i in range(len(master)):
try:
value,e_value = conversions.convert(master['unit'][i],to_units,master['meas'][i],master['e_meas'][i],photband=master['photband'][i])
except ValueError: # calibrations not available
value,e_value = np.nan,np.nan
except AssertionError: # the error or flux must be positive number
value,e_value = np.nan,np.nan
try:
eff_wave = filters.eff_wave(master['photband'][i])
except IOError:
eff_wave = np.nan
cols[0].append(eff_wave)
cols[1].append(value)
cols[2].append(e_value)
cols[3].append(to_units)
master = numpy_ext.recarr_addcols(master,cols,dtypes)
#-- reset errors
master['e_meas'][no_errors] = np.nan
master['e_cmeas'][no_errors] = np.nan
if master_ is not None and master is not None:
master = numpy_ext.recarr_addrows(master_,master.tolist())
elif master_ is not None:
master = master_
#-- and return the results
return master
def get_law(name, norm='E(B-V)', wave_units='AA', photbands=None, **kwargs):
"""
Retrieve an interstellar reddening law.
Parameter C{name} must be the function name of one of the laws defined in
this module.
By default, the law will be interpolated on a grid from 100 angstrom to
10 micron in steps of 10 angstrom. This can be adjusted with the parameter
C{wave} (array), which B{must} be in angstrom. You can change the units
ouf the returned wavelength array via C{wave_units}.
By default, the curve is normalised with respect to E(B-V) (you get
A(l)/E(B-V)). You can set the C{norm} keyword to Av if you want A(l)/Av.
Remember that
A(V) = Rv * E(B-V)
The parameter C{Rv} is by default 3.1, other reasonable values lie between
2.0 and 5.1
Extra accepted keywords depend on the type of reddening law used.
Example usage:
>>> wave = np.r_[1e3:1e5:10]
>>> wave,mag = get_law('cardelli1989',wave=wave,Rv=3.1)
@param name: name of the interstellar law
@type name: str, one of the functions defined here
@param norm: type of normalisation of the curve
@type norm: str (one of E(B-V), Av)
@param wave_units: wavelength units
@type wave_units: str (interpretable for units.conversions.convert)
@param photbands: list of photometric passbands
@type photbands: list of strings
@keyword wave: wavelength array to interpolate the law on
@type wave: ndarray
@return: wavelength, reddening magnitude
@rtype: (ndarray,ndarray)
"""
#-- get the inputs
wave_ = kwargs.pop('wave', None)
Rv = kwargs.setdefault('Rv', 3.1)
#-- get the curve
wave, mag = globals()[name.lower()](**kwargs)
wave_orig, mag_orig = wave.copy(), mag.copy()
#-- interpolate on user defined grid
if wave_ is not None:
if wave_units != 'AA':
wave_ = conversions.convert(wave_units, 'AA', wave_)
mag = np.interp(wave_, wave, mag, right=0)
wave = wave_
#-- pick right normalisation: convert to A(lambda)/Av if needed
if norm.lower() == 'e(b-v)':
mag *= Rv
else:
#-- we allow ak and av as shortcuts for normalisation in JOHNSON K and
# V bands
if norm.lower() == 'ak':
norm = 'JOHNSON.K'
elif norm.lower() == 'av':
norm = 'JOHNSON.V'
norm_reddening = model.synthetic_flux(wave_orig, mag_orig, [norm])[0]
logger.info('Normalisation via %s: Av/%s = %.6g' %
(norm, norm, 1. / norm_reddening))
mag /= norm_reddening
#-- maybe we want the curve in photometric filters
if photbands is not None:
mag = model.synthetic_flux(wave, mag, photbands)
wave = filters.get_info(photbands)['eff_wave']
#-- set the units of the wavelengths
if wave_units != 'AA' and photbands is not None:
wave = conversions.convert('AA', wave_units, wave)
return wave, mag
def get_photometry(ID=None,extra_fields=[],**kwargs):
"""
Download all available photometry from a star to a record array.
Extra fields will not be useful probably.
For extra kwargs, see L{_get_URI} and L{gcpd2phot}
"""
to_units = kwargs.pop('to_units','erg/s/cm2/AA')
master_ = kwargs.get('master',None)
master = None
#-- retrieve all measurements
for source in cat_info.sections():
results,units,comms = search(source,ID=ID,**kwargs)
if results is not None:
master = gcpd2phot(source,results,units,master,extra_fields=extra_fields)
#-- convert the measurement to a common unit.
if to_units and master is not None:
#-- prepare columns to extend to basic master
dtypes = [('cwave','f8'),('cmeas','f8'),('e_cmeas','f8'),('cunit','a50')]
cols = [[],[],[],[]]
#-- forget about 'nan' errors for the moment
no_errors = np.isnan(master['e_meas'])
master['e_meas'][no_errors] = 0.
#-- extend basic master
try:
zp = filters.get_info(master['photband'])
except:
print master['photband']
raise
for i in range(len(master)):
to_units_ = to_units+''
try:
value,e_value = conversions.convert(master['unit'][i],to_units,master['meas'][i],master['e_meas'][i],photband=master['photband'][i])
except ValueError: # calibrations not available
# if it is a magnitude color, try converting it to a flux ratio
if 'mag' in master['unit'][i]:
try:
value,e_value = conversions.convert('mag_color','flux_ratio',master['meas'][i],master['e_meas'][i],photband=master['photband'][i])
to_units_ = 'flux_ratio'
except ValueError:
value,e_value = np.nan,np.nan
# else, we are powerless...
else:
value,e_value = np.nan,np.nan
try:
eff_wave = filters.eff_wave(master['photband'][i])
except IOError:
eff_wave = np.nan
cols[0].append(eff_wave)
cols[1].append(value)
cols[2].append(e_value)
cols[3].append(to_units_)
master = numpy_ext.recarr_addcols(master,cols,dtypes)
#-- reset errors
master['e_meas'][no_errors] = np.nan
master['e_cmeas'][no_errors] = np.nan
#-- if a master is given as a keyword, and data is found in this module,
# append the two
if master_ is not None and master is not None:
master = numpy_ext.recarr_addrows(master_,master.tolist())
elif master is None:
master = master_
#-- and return the results
return master
