pyequib.main package

pyequib main module

This module contains functions for Plasma Diagnostics and Abundance Analysis

pyequib.calc_abund_c_ii_rl(temperature=None, density=None, wavelength=None, line_flux=None, c_ii_rc_data=None, h_i_aeff_data=None)[source]

This function determines the ionic abundance from the observed flux intensity for the given wavelength of C II recombination line by using the recombination coefficients from from Davey et al. (2000) 2000A&AS..142…85D.

Returns

type=double. This function returns the ionic abundanc.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

wavelengthin, required, type=float

Line Wavelength in Angstrom

line_fluxin, required, type=float

line flux intensity

c_ii_rc_datain, required, type=array/object

C II recombination coefficients

h_i_aeff_datain, required, type=array/object

H I recombination coefficients

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_all_file= os.path.join(base_dir,data_rc_dir, 'rc_collection.fits')
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>> atom='h'
>>> ion='ii' # H I
>>> h_i_rc_data=atomneb.read_aeff_sh95(atom_rc_sh95_file, atom, ion)
>>> h_i_aeff_data=h_i_rc_data['aeff'][0]
>>> atom='c'
>>> ion='iii' # C II
>>> c_ii_rc_data=atomneb.read_aeff_collection(atom_rc_all_file, atom, ion)
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> c_ii_6151_flux = 0.028
>>> wavelength=6151.43
>>> abund_c_ii=pyequib.calc_abund_c_ii_rl(temperature=temperature, density=density,
>>>                               wavelength=wavelength, line_flux=c_ii_6151_flux,
>>>                               c_ii_rc_data=c_ii_rc_data, h_i_aeff_data=h_i_aeff_data)
>>> print('N(C^2+)/N(H+):', abund_c_ii)
   N(C^2+)/N(H+):    0.00063404650
Categories

Abundance Analysis, Recombination Lines

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on recombination coefficients for C II lines from Davey et al. 2000A&AS..142…85D.

Adopted from MOCASSIN, Ercolano et al. 2005MNRAS.362.1038E.

02/2003, Yong Zhang, added to MOCASSIN.

10/05/2013, A. Danehkar, Translated to IDL code.

15/04/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Made a new function calc_emiss_c_ii_rl()

for calculating line emissivities and separated it from calc_abund_c_ii_rl().

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_abund_c_iii_rl(temperature=None, density=None, wavelength=None, line_flux=None, c_iii_rc_data=None, h_i_aeff_data=None)[source]

This function determines the ionic abundance from the observed flux intensity for the given wavelength of C III recombination line by using the recombination coefficients from Pequignot et al. 1991A&A…251..680P.

Returns

type=double. This function returns the ionic abundanc.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

wavelengthin, required, type=float

Line Wavelength in Angstrom

line_fluxin, required, type=float

line flux intensity

c_iii_rc_datain, required, type=array/object

C III recombination coefficients

h_i_aeff_datain, required, type=array/object

H I recombination coefficients

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_ppb91_file=os.path.join(base_dir,data_rc_dir, 'rc_PPB91.fits')
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>> atom='h'
>>> ion='ii' # H I
>>> h_i_rc_data=atomneb.read_aeff_sh95(atom_rc_sh95_file, atom, ion)
>>> h_i_aeff_data=h_i_rc_data['aeff'][0]
>>> atom='c'
>>> ion='iv' # C III
>>> c_iii_rc_data=atomneb.read_aeff_ppb91(atom_rc_ppb91_file, atom, ion)
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> c_iii_4647_flux = 0.107
>>> wavelength=4647.42
>>> abund_c_iii=pyequib.calc_abund_c_iii_rl(temperature=temperature, density=density,
>>>                                 wavelength=wavelength, line_flux=c_iii_4647_flux,
>>>                                 c_iii_rc_data=c_iii_rc_data, h_i_aeff_data=h_i_aeff_data)
>>> print('N(C^3+)/N(H+):', abund_c_iii)
   N(C^3+)/N(H+):    0.00017502840
Categories

Abundance Analysis, Recombination Lines

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on effective radiative recombination coefficients for C III lines from Pequignot, Petitjean, Boisson, C. 1991A&A…251..680P.

18/05/2013, A. Danehkar, Translated to IDL code.

06/04/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Made a new function calc_emiss_c_iii_rl()

for calculating line emissivities and separated it from calc_abund_c_iii_rl().

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_abund_he_i_rl(temperature=None, density=None, linenum=None, line_flux=None, he_i_aeff_data=None, h_i_aeff_data=None)[source]

This function determines the ionic abundance from the observed flux intensity for the given wavelength of He I recombination line by using the recombination coefficients from Porter et al. 2012MNRAS.425L..28P.

Returns

type=double. This function returns the ionic abundanc.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

linenumin, required, type=int

Line Number for Wavelength

Wavelength=4120.84:linenum=7,

Wavelength=4387.93: linenum=8,

Wavelength=4437.55: linenum=9,

Wavelength=4471.50: linenum=10,

Wavelength=4921.93: linenum=12,

Wavelength=5015.68: linenum=13,

Wavelength=5047.74: linenum=14,

Wavelength=5875.66: linenum=15,

Wavelength=6678.16: linenum=16,

Wavelength=7065.25: linenum=17,

Wavelength=7281.35: linenum=18.

line_fluxin, required, type=float

line flux intensity

he_i_aeff_datain, required, type=array/object

He I recombination coefficients

h_i_aeff_datain, required, type=array/object

H I recombination coefficients

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_he_i_file= os.path.join(base_dir,data_rc_dir, 'rc_he_ii_PFSD12.fits')
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>> atom='h'
>>> ion='ii' # H I
>>> h_i_rc_data=atomneb.read_aeff_sh95(atom_rc_sh95_file, atom, ion)
>>> h_i_aeff_data=h_i_rc_data['aeff'][0]
>>> atom='he'
>>> ion='ii' # He I
>>> he_i_rc_data=atomneb.read_aeff_he_i_pfsd12(atom_rc_he_i_file, atom, ion)
>>> he_i_aeff_data=he_i_rc_data['aeff'][0]
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> he_i_4471_flux= 2.104
>>> linenum=10# 4471.50
>>> abund_he_i=pyequib.calc_abund_he_i_rl(temperature=temperature, density=density,
>>>                                  linenum=linenum, line_flux=he_i_4471_flux,
>>>                                  he_i_aeff_data=he_i_aeff_data, h_i_aeff_data=h_i_aeff_data)
>>> print('N(He^+)/N(H^+):', abund_he_i)
   N(He^+)/N(H^+):     0.040848393
Categories

Abundance Analysis, Recombination Lines

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on improved He I emissivities in the case B from Porter et al. 2012MNRAS.425L..28P

15/12/2013, A. Danehkar, IDL code written.

20/03/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Made a new function calc_emiss_he_i_rl()

for calculating line emissivities and separated it from calc_abund_he_i_rl().

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_abund_he_ii_rl(temperature=None, density=None, line_flux=None, he_ii_aeff_data=None, h_i_aeff_data=None)[source]

This function determines the ionic abundance from the observed flux intensity for the He II recombination line 4686 A by using the helium emissivities from Storey & Hummer, 1995MNRAS.272…41S.

Returns

type=double. This function returns the ionic abundanc.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

line_fluxin, required, type=float

line flux intensity

he_ii_aeff_datain, required, type=array/object

He II recombination coefficients

h_i_aeff_datain, required, type=array/object

H I recombination coefficients

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_he_i_file= os.path.join(base_dir,data_rc_dir, 'rc_he_ii_PFSD12.fits')
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>> atom='h'
>>> ion='ii' # H I
>>> h_i_rc_data=atomneb.read_aeff_sh95(atom_rc_sh95_file, atom, ion)
>>> h_i_aeff_data=h_i_rc_data['aeff'][0]
>>> atom='he'
>>> ion='iii' # He II
>>> he_ii_rc_data=atomneb.read_aeff_sh95(atom_rc_sh95_file, atom, ion)
>>> he_ii_aeff_data=he_ii_rc_data['aeff'][0]
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> he_ii_4686_flux = 135.833
>>> abund_he_ii=pyequib.calc_abund_he_ii_rl(temperature=temperature, density=density,
>>>                                 line_flux=he_ii_4686_flux,
>>>                                 he_ii_aeff_data=he_ii_aeff_data, h_i_aeff_data=h_i_aeff_data)
>>> print('N(He^2+)/N(H^+):', abund_he_ii)
   N(He^2+)/N(H^+):      0.11228817
Categories

Abundance Analysis, Recombination Lines

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on He II emissivities from Storey & Hummer, 1995MNRAS.272…41S.

15/12/2013, A. Danehkar, IDL code written.

02/04/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Made a new function calc_emiss_he_ii_rl()

for calculating line emissivities and separated it from calc_abund_he_ii_rl().

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_abund_n_ii_rl(temperature=None, density=None, wavelength=None, line_flux=None, n_ii_rc_br=None, n_ii_rc_data=None, h_i_aeff_data=None)[source]

This function determines the ionic abundance from the observed flux intensity for the given wavelength of N II recombination line by using the recombination coefficients from Escalante & Victor 1990ApJS…73..513E.

Returns

type=double. This function returns the ionic abundanc.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

wavelengthin, required, type=float

Line Wavelength in Angstrom

line_fluxin, required, type=float

line flux intensity

n_ii_rc_brin, required, type=array/object

N II branching ratios (Br)

n_ii_rc_datain, required, type=array/object

N II recombination coefficients

h_i_aeff_datain, required, type=array/object

H I recombination coefficients

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_all_file= os.path.join(base_dir,data_rc_dir, 'rc_collection.fits')
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>> atom='h'
>>> ion='ii' # H I
>>> h_i_rc_data=atomneb.read_aeff_sh95(atom_rc_sh95_file, atom, ion)
>>> h_i_aeff_data=h_i_rc_data['aeff'][0]
>>> atom='n'
>>> ion='iii' # N II
>>> n_ii_rc_data=atomneb.read_aeff_collection(atom_rc_all_file, atom, ion)
>>> n_ii_rc_data_br=atomneb.read_aeff_collection(atom_rc_all_file, atom, ion, br=True)
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> n_ii_4442_flux = 0.017
>>> wavelength=4442.02
>>> abund_n_ii=pyequib.calc_abund_n_ii_rl(temperature=temperature, density=density,
>>>                               wavelength=wavelength, line_flux=n_ii_4442_flux,
>>>                               n_ii_rc_br=n_ii_rc_data_br, n_ii_rc_data=n_ii_rc_data,
>>>                               h_i_aeff_data=h_i_aeff_data)
>>> print('N(N^2+)/N(H+):', abund_n_ii)
   N(N^2+)/N(H+):   0.00069297541
Categories

Abundance Analysis, Recombination Lines

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on Effective recombination coefficients for N II lines from Escalante & Victor 1990ApJS…73..513E.

Adopted from MIDAS Rnii script written by X.W.Liu.

Revised based on scripts by Yong Zhang added to MOCASSIN, 02/2003

Ercolano et al. 2005MNRAS.362.1038E.

10/05/2013, A. Danehkar, Translated to IDL code.

25/04/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Made a new function calc_emiss_n_ii_rl()

for calculating line emissivities and separated it from calc_abund_n_ii_rl().

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_abund_n_iii_rl(temperature=None, density=None, wavelength=None, line_flux=None, n_iii_rc_data=None, h_i_aeff_data=None)[source]

This function determines the ionic abundance from the observed flux intensity for the given wavelength of N III recombination line by using the recombination coefficients from Pequignot et al. 1991A&A…251..680P.

Returns

type=double. This function returns the ionic abundanc.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

wavelengthin, required, type=float

Line Wavelength in Angstrom

line_fluxin, required, type=float

line flux intensity

n_iii_rc_datain, required, type=array/object

N III recombination coefficients

h_i_aeff_datain, required, type=array/object

H I recombination coefficients

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_ppb91_file=os.path.join(base_dir,data_rc_dir, 'rc_PPB91.fits')
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>> atom='h'
>>> ion='ii' # H I
>>> h_i_rc_data=atomneb.read_aeff_sh95(atom_rc_sh95_file, atom, ion)
>>> h_i_aeff_data=h_i_rc_data['aeff'][0]
>>> atom='n'
>>> ion='iv' # N III
>>> n_iii_rc_data=atomneb.read_aeff_ppb91(atom_rc_ppb91_file, atom, ion)
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> n_iii_4641_flux = 0.245
>>> wavelength=4640.64
>>> abund_n_iii=pyequib.calc_abund_n_iii_rl(temperature=temperature, density=density,
>>>                                 wavelength=wavelength, line_flux=n_iii_4641_flux,
>>>                                 n_iii_rc_data=n_iii_rc_data, h_i_aeff_data=h_i_aeff_data)
>>> print('N(N^3+)/N(H+):', abund_n_iii)
   N(N^3+)/N(H+):    6.3366175e-05
Categories

Abundance Analysis, Recombination Lines

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on effective radiative recombination coefficients for N III lines from Pequignot, Petitjean, Boisson, C. 1991A&A…251..680P.

10/05/2013, A. Danehkar, IDL code written.

20/04/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Made a new function calc_emiss_n_iii_rl()

for calculating line emissivities and separated it from calc_abund_n_iii_rl().

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_abund_ne_ii_rl(temperature=None, density=None, wavelength=None, line_flux=None, ne_ii_rc_data=None, h_i_aeff_data=None)[source]

This function determines the ionic abundance from the observed flux intensity for the given wavelength of Ne II recombination line by using the recombination coefficients from Kisielius et al. (1998) & Storey (unpublished).

Returns

type=double. This function returns the ionic abundanc.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

wavelengthin, required, type=float

Line Wavelength in Angstrom

line_fluxin, required, type=float

line flux intensity

ne_ii_rc_datain, required, type=array/object

Ne II recombination coefficients

h_i_aeff_datain, required, type=array/object

H I recombination coefficients

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_all_file= os.path.join(base_dir,data_rc_dir, 'rc_collection.fits')
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>> atom='h'
>>> ion='ii' # H I
>>> h_i_rc_data=atomneb.read_aeff_sh95(atom_rc_sh95_file, atom, ion)
>>> h_i_aeff_data=h_i_rc_data['aeff'][0]
>>> atom='ne'
>>> ion='iii' # Ne II
>>> ne_ii_rc_data=atomneb.read_aeff_collection(atom_rc_all_file, atom, ion)
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> ne_ii_3777_flux = 0.056
>>> wavelength=3777.14
>>> abund_ne_ii=pyequib.calc_abund_ne_ii_rl(temperature=temperature, density=density,
>>>                                 wavelength=wavelength, line_flux=ne_ii_3777_flux,
>>>                                 ne_ii_rc_data=ne_ii_rc_data, h_i_aeff_data=h_i_aeff_data)
>>> print('N(Ne^2+)/N(H+):', abund_ne_ii)
   N(Ne^2+)/N(H+):    0.00043376850
Categories

Abundance Analysis, Recombination Lines

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on effective radiative recombination coefficients for Ne II lines from Kisielius et al. 1998A&AS..133..257K & Storey (unpublished).

Adopted from MOCASSIN, Ercolano et al. 2005MNRAS.362.1038E.

02/2003, Yong Zhang, scripts added to MOCASSIN.

14/05/2013, A. Danehkar, Translated to IDL code.

10/04/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Made a new function calc_emiss_ne_ii_rl()

for calculating line emissivities and separated it from calc_abund_ne_ii_rl().

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_abund_o_ii_rl(temperature=None, density=None, wavelength=None, line_flux=None, o_ii_rc_br=None, o_ii_rc_data=None, h_i_aeff_data=None)[source]

This function determines the ionic abundance from the observed flux intensity for the given wavelength of O II recombination line by using the recombination coefficients from Storey 1994A&A…282..999S and Liu et al. 1995MNRAS.272..369L.

Returns

type=double. This function returns the ionic abundanc.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

wavelengthin, required, type=float

Line Wavelength in Angstrom

line_fluxin, required, type=float

line flux intensity

o_ii_rc_brin, required, type=array/object

O II branching ratios (Br)

o_ii_rc_datain, required, type=array/object

O II recombination coefficients

h_i_aeff_datain, required, type=array/object

H I recombination coefficients

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_all_file= os.path.join(base_dir,data_rc_dir, 'rc_collection.fits')
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>> atom='h'
>>> ion='ii' # H I
>>> h_i_rc_data=atomneb.read_aeff_sh95(atom_rc_sh95_file, atom, ion)
>>> h_i_aeff_data=h_i_rc_data['aeff'][0]
>>> atom='o'
>>> ion='iii' # O II
>>> o_ii_rc_data=atomneb.read_aeff_collection(atom_rc_all_file, atom, ion)
>>> o_ii_rc_data_br=atomneb.read_aeff_collection(atom_rc_all_file, atom, ion, br=True)
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> o_ii_4614_flux = 0.009
>>> wavelength=4613.68
>>> abund_o_ii=pyequib.calc_abund_o_ii_rl(temperature=temperature, density=density,
>>>                               wavelength=wavelength, line_flux=o_ii_4614_flux,
>>>                               o_ii_rc_br=o_ii_rc_data_br, o_ii_rc_data=o_ii_rc_data,
>>>                               h_i_aeff_data=h_i_aeff_data)
>>> print('N(O^2+)/N(H+):', abund_o_ii)
   N(O^2+)/N(H+):    0.0018886330
Categories

Abundance Analysis, Recombination Lines

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on recombination coefficients for O II lines from Storey 1994A&A…282..999S and Liu et al. 1995MNRAS.272..369L.

Adopted from MIDAS script Roii.prg written by X.W.Liu.

Revised based on scripts by Yong Zhang added to MOCASSIN, 02/2003

Ercolano et al. 2005MNRAS.362.1038E.

10/05/2013, A. Danehkar, Translated to IDL code.

25/04/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Made a new function calc_emiss_o_ii_rl()

for calculating line emissivities and separated it from calc_abund_o_ii_rl().

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_abundance(temperature=None, density=None, line_flux=None, atomic_levels=None, elj_data=None, omij_data=None, aij_data=None, h_i_aeff_data=None)[source]

This function determines the ionic abundance from the observed flux intensity for specified ion with level(s) by solving atomic level populations and line emissivities in statistical equilibrium for given electron density and temperature.

Returns

type=double. This function returns the ionic abundanc.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

line_fluxin, required, type=float

line flux intensity

atomic_levelsin, required, type=string

level(s) e.g ‘1,2/’, ‘1,2,1,3/’

elj_datain, required, type=array/object

energy levels (Ej) data

omij_datain, required, type=array/object

collision strengths (omega_ij) data

aij_datain, required, type=array/object

transition probabilities (Aij) data

h_i_aeff_datain, required, type=array/object

H I recombination coefficients

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_dir = os.path.join('atomic-data', 'chianti70')
>>> atom_elj_file = os.path.join(base_dir,data_dir, 'AtomElj.fits')
>>> atom_omij_file = os.path.join(base_dir,data_dir, 'AtomOmij.fits')
>>> atom_aij_file = os.path.join(base_dir,data_dir, 'AtomAij.fits')
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>> atom='o'
>>> ion='iii'
>>> o_iii_elj=atomneb.read_elj(atom_elj_file, atom, ion, level_num=5) # read Energy Levels (Ej)
>>> o_iii_omij=atomneb.read_omij(atom_omij_file, atom, ion) # read Collision Strengths (Omegaij)
>>> o_iii_aij=atomneb.read_aij(atom_aij_file, atom, ion) # read Transition Probabilities (Aij)
>>> atom='h'
>>> ion='ii' # H I
>>> hi_rc_data=atomneb.read_aeff_sh95(atom_rc_sh95_file, atom, ion)
>>> h_i_aeff_data=hi_rc_data['aeff'][0]
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> atomic_levels='3,4/'
>>> iobs5007=np.float64(1200.0)
>>> abb5007=np.float64(0.0)
>>> abb5007=pyequib.calc_abundance(temperature=temperature, density=density,
>>>                        line_flux=iobs5007, atomic_levels=atomic_levels,
>>>                        elj_data=o_iii_elj, omij_data=o_iii_omij,
>>>                        aij_data=o_iii_aij, h_i_aeff_data=hi_rc_data['aeff'][0])
>>> print('N(O^2+)/N(H+):', abb5007)
   N(O^2+)/N(H+):   0.00041256231
Categories

Abundance Analysis, Collisionally Excited Lines

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

15/09/2013, A. Danehkar, Translated from FORTRAN to IDL code.

20/10/2016, A. Danehkar, Replaced str2int with strnumber.

20/10/2016, A. Danehkar, Replaced CFY, SPLMAT, and CFD with

IDL function INTERPOL( /SPLINE).

20/10/2016, A. Danehkar, Replaced LUSLV with IDL LAPACK function

LA_LINEAR_EQUATION.

15/11/2016, A. Danehkar, Replaced LA_LINEAR_EQUATION (not work in GDL)

with IDL function LUDC & LUSOL.

19/11/2016, A. Danehkar, Replaced INTERPOL (not accurate) with

SPL_INIT & SPL_INTERP.

20/11/2016, A. Danehkar, Made a new function calc_populations()

for solving atomic level populations and separated it from calc_abundance(), calc_density() and calc_temperature().

21/11/2016, A. Danehkar, Made a new function calc_emissivity()

for calculating line emissivities and separated it from calc_abundance().

10/03/2017, A. Danehkar, Integration with AtomNeb, now uses atomic data

input elj_data, omij_data, aij_data.

12/06/2017, A. Danehkar, Cleaning the function, and remove unused varibales

from calc_abundance().

03/10/2020, A. Danehkar, Transferred from IDL to Python.

FORTRAN HISTORY:

03/05/1981, I.D.Howarth, Version 1.

05/05/1981, I.D.Howarth, Minibug fixed!

07/05/1981, I.D.Howarth, Now takes collision rates or strengths.

03/08/1981, S.Adams, Interpolates collision strengths.

07/08/1981, S.Adams, Input method changed.

19/11/1984, R.E.S.Clegg, SA files entombed in scratch disk. Logical

filenames given to SA’s data files.

08/1995, D.P.Ruffle, Changed input file format. Increased matrices.

02/1996, X.W.Liu, Tidy up. SUBROUTINES SPLMAT, HGEN, CFY and CFD

modified such that matrix sizes (i.e. maximum of Te and maximum no of levels) can now be cha by modifying the parameters NDIM1, NDIM2 and N in the Main program. EASY! Now takes collision rates as well. All variables are declared explicitly Generate two extra files (ionpop.lis and ionra of plain stream format for plotting.

06/1996, C.J.Pritchet, Changed input data format for cases IBIG=1,2.

Fixed readin bug for IBIG=2 case. Now reads reformatted upsilons (easier to see and the 0 0 0 data end is excluded for these c The A values have a different format for IBIG=.

2006, B.Ercolano, Converted to F90.

2009, R.Wesson, Misc updates and improvements.

Converted to F90. Version written only for calculating ionic abundances. Takes arguments from the command line.

pyequib.calc_crit_density(temperature=None, elj_data=None, omij_data=None, aij_data=None, level_num=None, irats=None)[source]

This function calculates critical densities in statistical equilibrium for given electron temperature.

Returns

type=array/object. This function returns the critical densities.

Keywords
temperaturein, required, type=float

electron temperature

elj_datain, required, type=array/object

energy levels (Ej) data

omij_datain, required, type=array/object

collision strengths (omega_ij) data

aij_datain, required, type=array/object

transition probabilities (Aij) data

level_numin, type=int

Number of levels

iratsin, type=int

Else Coll. rates = tabulated values * 10 ** irats

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_dir = os.path.join('atomic-data', 'chianti70')
>>> atom_elj_file = os.path.join(base_dir,data_dir, 'AtomElj.fits')
>>> atom_omij_file = os.path.join(base_dir,data_dir, 'AtomOmij.fits')
>>> atom_aij_file = os.path.join(base_dir,data_dir, 'AtomAij.fits')
>>> atom='s'
>>> ion='ii'
>>> s_ii_elj=atomneb.read_elj(atom_elj_file, atom, ion, level_num=5) # read Energy Levels (Ej)
>>> s_ii_omij=atomneb.read_omij(atom_omij_file, atom, ion) # read Collision Strengths (Omegaij)
>>> s_ii_aij=atomneb.read_aij(atom_aij_file, atom, ion) # read Transition Probabilities (Aij)        >>> temperature=np.float64(10000.0)
>>> n_crit=pyequib.calc_crit_density(temperature=temperature,
>>>                          elj_data=s_ii_elj, omij_data=s_ii_omij,
>>>                          aij_data=s_ii_aij)
>>> print('Critical Densities:', n_crit)
   Critical Densities:       0.0000000       5007.8396       1732.8414       1072685.0       2220758.1
Categories

Plasma Diagnostics, Abundance Analysis, Collisionally Excited Lines

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

15/09/2013, A. Danehkar, Translated from FORTRAN to IDL code.

20/10/2016, A. Danehkar, Replaced str2int with strnumber.

20/10/2016, A. Danehkar, Replaced CFY, SPLMAT, and CFD with

IDL function INTERPOL( /SPLINE).

20/10/2016, A. Danehkar, Replaced LUSLV with IDL LAPACK function

LA_LINEAR_EQUATION.

15/11/2016, A. Danehkar, Replaced LA_LINEAR_EQUATION (not work in GDL)

with IDL function LUDC & LUSOL.

19/11/2016, A. Danehkar, Replaced INTERPOL (not accurate) with

SPL_INIT & SPL_INTERP.

20/11/2016, A. Danehkar, Made a new function calc_populations()

for solving atomic level populations and separated it from calc_abundance(), calc_density() and calc_temperature().

10/03/2017, A. Danehkar, Integration with AtomNeb, now uses atomic data

input elj_data, omij_data, aij_data.

12/06/2017, A. Danehkar, Cleaning the function, and remove unused varibales

from calc_populations().

27/02/2019, A. Danehkar, Simplify the calc_populations() routine

for external usage.

01/03/2019, A. Danehkar, Create the calc_crit_density() routine

from the calc_populations() routine.

04/03/2019, A. Danehkar, Use the get_omij_temp() routine.

03/10/2020, A. Danehkar, Transferred from IDL to Python.

FORTRAN HISTORY:

03/05/1981, I.D.Howarth, Version 1.

05/05/1981, I.D.Howarth, Minibug fixed!

07/05/1981, I.D.Howarth, Now takes collision rates or strengths.

03/08/1981, S.Adams, Interpolates collision strengths.

07/08/1981, S.Adams, Input method changed.

19/11/1984, R.E.S.Clegg, SA files entombed in scratch disk. Logical

filenames given to SA’s data files.

08/1995, D.P.Ruffle, Changed input file format. Increased matrices.

02/1996, X.W.Liu, Tidy up. SUBROUTINES SPLMAT, HGEN, CFY and CFD

modified such that matrix sizes (i.e. maximum of Te and maximum no of levels) can now be cha by modifying the parameters NDIM1, NDIM2 and N in the Main program. EASY! Now takes collision rates as well. All variables are declared explicitly Generate two extra files (ionpop.lis and ionra of plain stream format for plotting.

06/1996, C.J.Pritchet, Changed input data format for cases IBIG=1,2.

Fixed readin bug for IBIG=2 case. Now reads reformatted upsilons (easier to see and the 0 0 0 data end is excluded for these c The A values have a different format for IBIG=.

2006, B.Ercolano, Converted to F90.

2009, R.Wesson, Misc updates and improvements.

Converted to F90. Version written only for calculating ionic abundances. Takes arguments from the command line.

pyequib.calc_density(line_flux_ratio=None, temperature=None, upper_levels=None, lower_levels=None, elj_data=None, omij_data=None, aij_data=None, low_density=None, high_density=None, num_density=None, min_temperature=None)[source]

This function determines electron density from given flux intensity ratio for specified ion with upper level(s) lower level(s) by solving atomic level populations and line emissivities in statistical equilibrium for given electron temperature.

Returns

type=double. This function returns the electron density.

Keywords
line_flux_ratioin, required, type=float

flux intensity ratio

temperaturein, required, type=float

electron temperature

upper_levelsin, required, type=string

upper atomic level(s) e.g ‘1,2/’, ‘1,2,1,3/’

lower_levelsin, required, type=string

lower atomic level(s) e.g ‘1,2/’, ‘1,2,1,3/’

elj_datain, required, type=array/object

energy levels (Ej) data

omij_datain, required, type=array/object

collision strengths (omega_ij) data

aij_datain, required, type=array/object

transition probabilities (Aij) data

low_densityin, optional, type=float

lower density range

high_densityin, optional, type=float

upper density range

num_densityin, optional, type=integer

number of the iteration step

min_temperaturein, optional, type=float

minimum temperature

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_dir = os.path.join('atomic-data', 'chianti70')
>>> atom_elj_file = os.path.join(base_dir,data_dir, 'AtomElj.fits')
>>> atom_omij_file = os.path.join(base_dir,data_dir, 'AtomOmij.fits')
>>> atom_aij_file = os.path.join(base_dir,data_dir, 'AtomAij.fits')
>>> atom='s'
>>> ion='ii'
>>> s_ii_elj=atomneb.read_elj(atom_elj_file, atom, ion, level_num=5) # read Energy Levels (Ej)
>>> s_ii_omij=atomneb.read_omij(atom_omij_file, atom, ion) # read Collision Strengths (Omegaij)
>>> s_ii_aij=atomneb.read_aij(atom_aij_file, atom, ion) # read Transition Probabilities (Aij)        >>> upper_levels='1,2/'
>>> lower_levels='1,3/'
>>> temperature=np.float64(7000.0)#
>>> line_flux_ratio=np.float64(1.506)#
>>> density=pyequib.calc_density(line_flux_ratio=line_flux_ratio, temperature=temperature,
>>>                      upper_levels=upper_levels, lower_levels=lower_levels,
>>>                      elj_data=s_ii_elj, omij_data=s_ii_omij,
>>>                      aij_data=s_ii_aij)
>>> print("Electron Density:", density)
   Electron Density:       2312.6395
Categories

Plasma Diagnostics, Collisionally Excited Lines

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

15/09/2013, A. Danehkar, Translated from FORTRAN to IDL code.

20/10/2016, A. Danehkar, Replaced str2int with strnumber.

20/10/2016, A. Danehkar, Replaced CFY, SPLMAT, and CFD with

IDL function INTERPOL( /SPLINE).

20/10/2016, A. Danehkar, Replaced LUSLV with IDL LAPACK function

LA_LINEAR_EQUATION.

15/11/2016, A. Danehkar, Replaced LA_LINEAR_EQUATION (not work in GDL)

with IDL function LUDC & LUSOL.

19/11/2016, A. Danehkar, Replaced INTERPOL (not accurate) with

SPL_INIT & SPL_INTERP.

20/11/2016, A. Danehkar, Made a new function calc_populations()

for solving atomic level populations and separated it from calc_abundance(), calc_density() and calc_temperature().

10/03/2017, A. Danehkar, Integration with AtomNeb, now uses atomic data

input elj_data, omij_data, aij_data.

12/06/2017, A. Danehkar, Cleaning the function, and remove unused varibales

from calc_density().

27/02/2019, A. Danehkar, Fix a bug in the atomic level assumption, and

use the simplified calc_populations() routine.

04/03/2019, A. Danehkar, Use the get_omij_temp() routine.

24/05/2019, A. Danehkar, Add the optional density range.

03/10/2020, A. Danehkar, Transferred from IDL to Python.

FORTRAN HISTORY:

03/05/1981, I.D.Howarth, Version 1.

05/05/1981, I.D.Howarth, Minibug fixed!

07/05/1981, I.D.Howarth, Now takes collision rates or strengths.

03/08/1981, S.Adams, Interpolates collision strengths.

07/08/1981, S.Adams, Input method changed.

19/11/1984, R.E.S.Clegg, SA files entombed in scratch disk. Logical

filenames given to SA’s data files.

08/1995, D.P.Ruffle, Changed input file format. Increased matrices.

02/1996, X.W.Liu, Tidy up. SUBROUTINES SPLMAT, HGEN, CFY and CFD

modified such that matrix sizes (i.e. maximum of Te and maximum no of levels) can now be cha by modifying the parameters NDIM1, NDIM2 and N in the Main program. EASY! Now takes collision rates as well. All variables are declared explicitly Generate two extra files (ionpop.lis and ionra of plain stream format for plotting.

06/1996, C.J.Pritchet, Changed input data format for cases IBIG=1,2.

Fixed readin bug for IBIG=2 case. Now reads reformatted upsilons (easier to see and the 0 0 0 data end is excluded for these c The A values have a different format for IBIG=.

2006, B.Ercolano, Converted to F90.

2009, R.Wesson, Misc updates and improvements.

Converted to F90. Version written only for calculating ionic abundances. Takes arguments from the command line.

pyequib.calc_emiss_c_ii_rl(temperature=None, density=None, wavelength=None, c_ii_rc_data=None)[source]

This function calculates the emissivity for the given wavelength of C II recombination line by using the recombination coefficients from from Davey et al. (2000) 2000A&AS..142…85D.

Returns

type=double. This function returns the line emissivity.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

wavelengthin, required, type=float

Line Wavelength in Angstrom

c_ii_rc_datain, required, type=array/object

C II recombination coefficients

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_all_file= os.path.join(base_dir,data_rc_dir, 'rc_collection.fits')
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>>
>>> atom='c'
>>> ion='iii' # C II
>>> c_ii_rc_data=atomneb.read_aeff_collection(atom_rc_all_file, atom, ion)
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> wavelength=6151.43
>>> emiss_c_ii=pyequib.calc_emiss_c_ii_rl(temperature=temperature, density=density,
>>>                               wavelength=wavelength,
>>>                               c_ii_rc_data=c_ii_rc_data)
>>> print('Emissivity:', emiss_c_ii)
   Emissivity:   5.4719511e-26
Categories

Abundance Analysis, Recombination Lines, Emissivity

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on recombination coefficients for C II lines from Davey et al. 2000A&AS..142…85D.

Adopted from MOCASSIN, Ercolano et al. 2005MNRAS.362.1038E.

02/2003, Yong Zhang, added to MOCASSIN.

10/05/2013, A. Danehkar, Translated to IDL code.

15/04/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Made a new function calc_emiss_c_ii_rl()

for calculating line emissivities and separated it from calc_abund_c_ii_rl().

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_emiss_c_iii_rl(temperature=None, density=None, wavelength=None, c_iii_rc_data=None)[source]

This function calculates the emissivity for the given wavelength of C III recombination line by using the recombination coefficients from Pequignot et al. 1991A&A…251..680P.

Returns

type=double. This function returns the line emissivity.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

wavelengthin, required, type=float

Line Wavelength in Angstrom

c_iii_rc_datain, required, type=array/object

C III recombination coefficients

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_ppb91_file=os.path.join(base_dir,data_rc_dir, 'rc_PPB91.fits')
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>>
>>> atom='c'
>>> ion='iv' # C III
>>> c_iii_rc_data=atomneb.read_aeff_ppb91(atom_rc_ppb91_file, atom, ion)
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> wavelength=4647.42
>>> emiss_c_iii=pyequib.calc_emiss_c_iii_rl(temperature=temperature, density=density,
>>>                                 wavelength=wavelength,
>>>                                 c_iii_rc_data=c_iii_rc_data)
>>> print('Emissivity:', emiss_c_iii)
   Emissivity:   7.5749632e-25
Categories

Abundance Analysis, Recombination Lines, Emissivity

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on effective radiative recombination coefficients for C III lines from Pequignot, Petitjean, Boisson, C. 1991A&A…251..680P.

18/05/2013, A. Danehkar, Translated to IDL code.

06/04/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Made a new function calc_emiss_c_iii_rl()

for calculating line emissivities and separated it from calc_abund_c_iii_rl().

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_emiss_h_alpha(temperature=None, density=None, h_i_aeff_data=None)[source]

This function calculates the emissivity for H_alpha 6563A Emis(HAlpha)= 4pi j(HAlpha 6563 A)/Np Ne) for the given temperature and density by using the hydrogn emissivities from Storey & Hummer, 1995MNRAS.272…41S.

Private

Returns

type=double. This function returns the H alpha emissivity 4pi j(HAlpha 6563)/Np Ne).

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

h_i_aeff_datain, required, type=array/object

H I recombination coefficients

Categories

Abundance Analysis, Recombination Lines, Emissivity

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on H I emissivities from Storey & Hummer, 1995MNRAS.272…41S.

25/08/2012, A. Danehkar, IDL code written.

11/03/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Change from logarithmic to linear

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_emiss_h_beta(temperature=None, density=None, h_i_aeff_data=None)[source]

This function calculates the emissivity for H_beta 4861A Emis(Hbeta)= 4pi j(HBeta 4861 A)/Np Ne) for the given temperature and density by using the hydrogn emissivities from Storey & Hummer, 1995MNRAS.272…41S.

Private

Returns

type=double. This function returns the H beta emissivity 4pi j(HBeta 4861)/Np Ne).

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

h_i_aeff_datain, required, type=array/object

H I recombination coefficients

Categories

Abundance Analysis, Recombination Lines, Emissivity

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on H I emissivities from Storey & Hummer, 1995MNRAS.272…41S.

25/08/2012, A. Danehkar, IDL code written.

11/03/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Change from logarithmic to linear

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_emiss_h_i(temperature=None, density=None, h_i_aeff_data=None, low_level=None, high_level=None)[source]

This function calculates the emissivity for H I Emis(Hbeta)= 4pi j(H I)/Np Ne) for the given temperature and density by using the hydrogn emissivities from Storey & Hummer, 1995MNRAS.272…41S.

Private

Returns

type=double. This function returns the H I emissivity 4pi j(H I)/Np Ne).

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

h_i_aeff_datain, required, type=array/object

H I recombination coefficients

low_levelin, required, type=int

low level

high_levelin, required, type=int

high level

Categories

Abundance Analysis, Recombination Lines, Emissivity

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on H I emissivities from Storey & Hummer, 1995MNRAS.272…41S.

25/08/2012, A. Danehkar, IDL code written.

11/03/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Change from logarithmic to linear

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_emiss_he_i_rl(temperature=None, density=None, linenum=None, he_i_aeff_data=None)[source]

This function calculates the emissivity for the given wavelength of He I recombination line by using the recombination coefficients from Porter et al. 2012MNRAS.425L..28P.

Returns

type=double. This function returns the line emissivity.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

linenumin, required, type=int

Line Number for Wavelength

Wavelength=4120.84:linenum=7,

Wavelength=4387.93: linenum=8,

Wavelength=4437.55: linenum=9,

Wavelength=4471.50: linenum=10,

Wavelength=4921.93: linenum=12,

Wavelength=5015.68: linenum=13,

Wavelength=5047.74: linenum=14,

Wavelength=5875.66: linenum=15,

Wavelength=6678.16: linenum=16,

Wavelength=7065.25: linenum=17,

Wavelength=7281.35: linenum=18.

line_fluxin, required, type=float

line flux intensity

he_i_aeff_datain, required, type=array/object

He I recombination coefficients

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_he_i_file= filepath('rc_he_ii_PFSD12.fits', root_dir=base_dir, subdir=data_rc_dir )
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>>
>>> atom='he'
>>> ion='ii' # He I
>>> he_i_rc_data=atomneb.read_aeff_he_i_pfsd12(atom_rc_he_i_file, atom, ion)
>>> he_i_aeff_data=he_i_rc_data['aeff'][0]
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> linenum=10# 4471.50
>>> emiss_he_i=pyequib.calc_emiss_he_i_rl(temperature=temperature, density=density,
>>>                                linenum=linenum,
>>>                                he_i_aeff_data=he_i_aeff_data)
>>> print('Emissivity:', emiss_he_i)
   Emissivity:   6.3822830e-26
Categories

Abundance Analysis, Recombination Lines, Emissivity

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on improved He I emissivities in the case B from Porter et al. 2012MNRAS.425L..28P

15/12/2013, A. Danehkar, IDL code written.

20/03/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Made a new function calc_emiss_he_i_rl()

for calculating line emissivities and separated it from calc_abund_he_i_rl().

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_emiss_he_ii_rl(temperature=None, density=None, he_ii_aeff_data=None)[source]

This functioncalculates the emissivity for the He II recombination line 4686 A by using the helium emissivities from Storey & Hummer, 1995MNRAS.272…41S.

Returns

type=double. This function returns the line emissivity.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

he_ii_aeff_datain, required, type=array/object

He II recombination coefficients

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_he_i_file= os.path.join(base_dir,data_rc_dir, 'rc_he_ii_PFSD12.fits')
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>>
>>> atom='he'
>>> ion='iii' # He II
>>> he_ii_rc_data=atomneb.read_aeff_sh95(atom_rc_sh95_file, atom, ion)
>>> he_ii_aeff_data=he_ii_rc_data['aeff'][0]
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> he_ii_4686_flux = 135.833
>>> emiss_he_ii=pyequib.calc_emiss_he_ii_rl(temperature=temperature, density=density,
>>>                                 he_ii_aeff_data=he_ii_aeff_data)
>>> print('Emissivity:', emiss_he_ii)
   Emissivity:   1.4989134e-24
Categories

Abundance Analysis, Recombination Lines, Emissivity

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on He II emissivities from Storey & Hummer, 1995MNRAS.272…41S.

15/12/2013, A. Danehkar, IDL code written.

02/04/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Change from logarithmic to linear

10/07/2019, A. Danehkar, Made a new function calc_emiss_he_ii_rl()

for calculating line emissivities and separated it from calc_abund_he_ii_rl().

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_emiss_n_ii_rl(temperature=None, density=None, wavelength=None, n_ii_rc_br=None, n_ii_rc_data=None)[source]

This function calculates the emissivity for the given wavelength of N II recombination line by using the recombination coefficients from Escalante & Victor 1990ApJS…73..513E.

Returns

type=double. This function returns the line emissivity.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

wavelengthin, required, type=float

Line Wavelength in Angstrom

n_ii_rc_brin, required, type=array/object

N II branching ratios (Br)

n_ii_rc_datain, required, type=array/object

N II recombination coefficients

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_all_file= os.path.join(base_dir,data_rc_dir, 'rc_collection.fits')
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>> atom='h'
>>> ion='ii' # H I
>>> h_i_rc_data=atomneb.read_aeff_sh95(atom_rc_sh95_file, atom, ion)
>>> h_i_aeff_data=h_i_rc_data['aeff'][0]
>>> atom='n'
>>> ion='iii' # N II
>>> n_ii_rc_data=atomneb.read_aeff_collection(atom_rc_all_file, atom, ion)
>>> n_ii_rc_data_br=atomneb.read_aeff_collection(atom_rc_all_file, atom, ion, br=True)
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> wavelength=4442.02
>>> emiss_n_ii=pyequib.calc_emiss_n_ii_rl(temperature=temperature, density=density,
>>>                               wavelength=wavelength,
>>>                               n_ii_rc_br=n_ii_rc_data_br, n_ii_rc_data=n_ii_rc_data,
>>>                               h_i_aeff_data=h_i_aeff_data)
>>> print('Emissivity:', emiss_n_ii)
   Emissivity:   3.0397397e-26
Categories

Abundance Analysis, Recombination Lines, Emissivity

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on Effective recombination coefficients for N II lines from Escalante & Victor 1990ApJS…73..513E.

Adopted from MIDAS Rnii script written by X.W.Liu.

Revised based on scripts by Yong Zhang added to MOCASSIN, 02/2003

Ercolano et al. 2005MNRAS.362.1038E.

10/05/2013, A. Danehkar, Translated to IDL code.

25/04/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Made a new function calc_emiss_n_ii_rl()

for calculating line emissivities and separated it from calc_abund_n_ii_rl().

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_emiss_n_iii_rl(temperature=None, density=None, wavelength=None, n_iii_rc_data=None)[source]

This function calculates the emissivity for the given wavelength of N III recombination line by using the recombination coefficients from Pequignot et al. 1991A&A…251..680P.

Returns

type=double. This function returns the line emissivity.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

wavelengthin, required, type=float

Line Wavelength in Angstrom

n_iii_rc_datain, required, type=array/object

N III recombination coefficients

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_ppb91_file=os.path.join(base_dir,data_rc_dir, 'rc_PPB91.fits')
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>>
>>> atom='n'
>>> ion='iv' # N III
>>> n_iii_rc_data=atomneb.read_aeff_ppb91(atom_rc_ppb91_file, atom, ion)
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> wavelength=4640.64
>>> emiss_n_iii=pyequib.calc_abund_n_iii_rl(temperature=temperature, density=density,
>>>                                 wavelength=wavelength,
>>>                                 n_iii_rc_data=n_iii_rc_data)
>>> print('Emissivity:', emiss_n_iii)
   Emissivity:   4.7908644e-24
Categories

Abundance Analysis, Recombination Lines, Emissivity

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on effective radiative recombination coefficients for N III lines from Pequignot, Petitjean, Boisson, C. 1991A&A…251..680P.

10/05/2013, A. Danehkar, IDL code written.

20/04/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Made a new function calc_emiss_n_iii_rl()

for calculating line emissivities and separated it from calc_abund_n_iii_rl().

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_emiss_ne_ii_rl(temperature=None, density=None, wavelength=None, ne_ii_rc_data=None)[source]

This function calculates the emissivity for the given wavelength of Ne II recombination line by using the recombination coefficients from Kisielius et al. (1998) & Storey (unpublished).

Returns

type=double. This function returns the line emissivity.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

wavelengthin, required, type=float

Line Wavelength in Angstrom

ne_ii_rc_datain, required, type=array/object

Ne II recombination coefficients

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_all_file= os.path.join(base_dir,data_rc_dir, 'rc_collection.fits')
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>>
>>> atom='ne'
>>> ion='iii' # Ne II
>>> ne_ii_rc_data=atomneb.read_aeff_collection(atom_rc_all_file, atom, ion)
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> wavelength=3777.14
>>> emiss_ne_ii=pyequib.calc_emiss_ne_ii_rl(temperature=temperature, density=density,
>>>                                 wavelength=wavelength,
>>>                                 ne_ii_rc_data=ne_ii_rc_data, h_i_aeff_data=h_i_aeff_data)
>>> print('Emissivity:', emiss_ne_ii)
   Emissivity:   1.5996881e-25
Categories

Abundance Analysis, Recombination Lines, Emissivity

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on effective radiative recombination coefficients for Ne II lines from Kisielius et al. 1998A&AS..133..257K & Storey (unpublished).

Adopted from MOCASSIN, Ercolano et al. 2005MNRAS.362.1038E.

02/2003, Yong Zhang, scripts added to MOCASSIN.

14/05/2013, A. Danehkar, Translated to IDL code.

10/04/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Made a new function calc_emiss_ne_ii_rl()

for calculating line emissivities and separated it from calc_abund_ne_ii_rl().

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_emiss_o_ii_rl(temperature=None, density=None, wavelength=None, o_ii_rc_br=None, o_ii_rc_data=None)[source]

This function calculates the emissivity for the given wavelength of O II recombination line by using the recombination coefficients from Storey 1994A&A…282..999S and Liu et al. 1995MNRAS.272..369L.

Returns

type=double. This function returns the line emissivity.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

wavelengthin, required, type=float

Line Wavelength in Angstrom

o_ii_rc_brin, required, type=array/object

O II branching ratios (Br)

o_ii_rc_datain, required, type=array/object

O II recombination coefficients

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_all_file= os.path.join(base_dir,data_rc_dir, 'rc_collection.fits')
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>>
>>> atom='o'
>>> ion='iii' # O II
>>> o_ii_rc_data=atomneb.read_aeff_collection(atom_rc_all_file, atom, ion)
>>> o_ii_rc_data_br=atomneb.read_aeff_collection(atom_rc_all_file, atom, ion, br=True)
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> wavelength=4613.68
>>> emiss_o_ii=pyequib.calc_emiss_o_ii_rl(temperature=temperature, density=density,
>>>                               wavelength=wavelength,
>>>                               o_ii_rc_br=o_ii_rc_data_br, o_ii_rc_data=o_ii_rc_data,
>>>                               h_i_aeff_data=h_i_aeff_data)
>>> print('Emissivity:', emiss_o_ii)
   Emissivity:   5.9047319e-27
Categories

Abundance Analysis, Recombination Lines, Emissivity

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on recombination coefficients for O II lines from Storey 1994A&A…282..999S and Liu et al. 1995MNRAS.272..369L.

Adopted from MIDAS script Roii.prg written by X.W.Liu.

Revised based on scripts by Yong Zhang added to MOCASSIN, 02/2003

Ercolano et al. 2005MNRAS.362.1038E.

10/05/2013, A. Danehkar, Translated to IDL code.

25/04/2017, A. Danehkar, Integration with AtomNeb.

10/07/2019, A. Danehkar, Made a new function calc_emiss_o_ii_rl()

for calculating line emissivities and separated it from calc_abund_o_ii_rl().

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.calc_emissivity(temperature=None, density=None, atomic_levels=None, elj_data=None, omij_data=None, aij_data=None)[source]

This function calculates line emissivities for specified ion with level(s) by solving atomic level populations and in statistical equilibrium for given electron density and temperature.

Returns

type=double. This function returns the line emissivity.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

atomic_levelsIn, required, type=string

level(s) e.g ‘1,2/’, ‘1,2,1,3/’

elj_datain, required, type=array/object

energy levels (Ej) data

omij_datain, required, type=array/object

collision strengths (omega_ij) data

aij_datain, required, type=array/object

transition probabilities (Aij) data

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_dir = os.path.join('atomic-data', 'chianti70')
>>> atom_elj_file = os.path.join(base_dir,data_dir, 'AtomElj.fits')
>>> atom_omij_file = os.path.join(base_dir,data_dir, 'AtomOmij.fits')
>>> atom_aij_file = os.path.join(base_dir,data_dir, 'AtomAij.fits')
>>> atom='o'
>>> ion='iii'
>>> o_iii_elj=atomneb.read_elj(atom_elj_file, atom, ion, level_num=5) # read Energy Levels (Ej)
>>> o_iii_omij=atomneb.read_omij(atom_omij_file, atom, ion) # read Collision Strengths (Omegaij)
>>> o_iii_aij=atomneb.read_aij(atom_aij_file, atom, ion) # read Transition Probabilities (Aij)
>>> temperature=np.float64(10000.0)
>>> density=np.float64(5000.0)
>>> atomic_levels='3,4/'
>>> emiss5007=np.float64(0.0)
>>> emiss5007=pyequib.calc_emissivity(temperature=temperature, density=density,
>>>                           atomic_levels=atomic_levels,
>>>                           elj_data=o_iii_elj, omij_data=o_iii_omij,
>>>                           aij_data=o_iii_aij
>>> print('Emissivity(O III 5007):', emiss5007)
   Emissivity(O III 5007):   3.6041012e-21
Categories

Abundance Analysis, Collisionally Excited Lines, Emissivity

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

15/09/2013, A. Danehkar, Translated from FORTRAN to IDL code.

20/10/2016, A. Danehkar, Replaced str2int with strnumber.

20/10/2016, A. Danehkar, Replaced CFY, SPLMAT, and CFD with

IDL function INTERPOL( /SPLINE).

20/10/2016, A. Danehkar, Replaced LUSLV with IDL LAPACK function

LA_LINEAR_EQUATION.

15/11/2016, A. Danehkar, Replaced LA_LINEAR_EQUATION (not work in GDL)

with IDL function LUDC & LUSOL.

19/11/2016, A. Danehkar, Replaced INTERPOL (not accurate) with

SPL_INIT & SPL_INTERP.

20/11/2016, A. Danehkar, Made a new function calc_populations()

for solving atomic level populations and separated it from calc_abundance(), calc_density() and calc_temperature().

21/11/2016, A. Danehkar, Made a new function calc_emissivity()

for calculating line emissivities and separated it from calc_abundance().

10/03/2017, A. Danehkar, Integration with AtomNeb, now uses atomic data

input elj_data, omij_data, aij_data.

12/06/2017, A. Danehkar, Cleaning the function, and remove unused varibales

from calc_emissivity().

27/06/2019, A. Danehkar, Use the simplified calc_populations() routine.

03/10/2020, A. Danehkar, Transferred from IDL to Python.

FORTRAN HISTORY:

03/05/1981, I.D.Howarth, Version 1.

05/05/1981, I.D.Howarth, Minibug fixed!

07/05/1981, I.D.Howarth, Now takes collision rates or strengths.

03/08/1981, S.Adams, Interpolates collision strengths.

07/08/1981, S.Adams, Input method changed.

19/11/1984, R.E.S.Clegg, SA files entombed in scratch disk. Logical

filenames given to SA’s data files.

08/1995, D.P.Ruffle, Changed input file format. Increased matrices.

02/1996, X.W.Liu, Tidy up. SUBROUTINES SPLMAT, HGEN, CFY and CFD

modified such that matrix sizes (i.e. maximum of Te and maximum no of levels) can now be cha by modifying the parameters NDIM1, NDIM2 and N in the Main program. EASY! Now takes collision rates as well. All variables are declared explicitly Generate two extra files (ionpop.lis and ionra of plain stream format for plotting.

06/1996, C.J.Pritchet, Changed input data format for cases IBIG=1,2.

Fixed readin bug for IBIG=2 case. Now reads reformatted upsilons (easier to see and the 0 0 0 data end is excluded for these c The A values have a different format for IBIG=.

2006, B.Ercolano, Converted to F90.

2009, R.Wesson, Misc updates and improvements.

Converted to F90. Version written only for calculating ionic abundances. Takes arguments from the command line.

pyequib.calc_populations(temperature=None, density=None, elj_data=None, omij_data=None, aij_data=None, eff_omij=None, level_num=None, irats=None)[source]

This function solves atomic level populations in statistical equilibrium for given electron temperature and density.

Returns

type=array/object. This function returns the atomic level populations.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

elj_datain, required, type=array/object

energy levels (Ej) data

omij_datain, required, type=array/object

collision strengths (omega_ij) data

aij_datain, required, type=array/object

transition probabilities (Aij) data

eff_Omijin, type=array/object

effective collision strengths (Omij_T) at given temperature

level_numin, type=int

Number of levels

iratsin, type=int

Else Coll. rates = tabulated values * 10 ** irats

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_dir = os.path.join('atomic-data', 'chianti70')
>>> atom_elj_file = os.path.join(base_dir,data_dir, 'AtomElj.fits')
>>> atom_omij_file = os.path.join(base_dir,data_dir, 'AtomOmij.fits')
>>> atom_aij_file = os.path.join(base_dir,data_dir, 'AtomAij.fits')
>>> atom='s'
>>> ion='ii'
>>> s_ii_elj=atomneb.read_elj(atom_elj_file, atom, ion, level_num=5) # read Energy Levels (Ej)
>>> s_ii_omij=atomneb.read_omij(atom_omij_file, atom, ion) # read Collision Strengths (Omegaij)
>>> s_ii_aij=atomneb.read_aij(atom_aij_file, atom, ion) # read Transition Probabilities (Aij)        >>> density = np.float64(1000)
>>> temperature=np.float64(10000.0)#
>>> nlj=pyequib.calc_populations(temperature=temperature, density=density,
>>>                      elj_data=s_ii_elj, omij_data=s_ii_omij,
>>>                      aij_data=s_ii_aij)
>>> print('Atomic Level Populations:', nlj)
   Atomic Level Populations:    0.96992832    0.0070036315     0.023062261   2.6593671e-06   3.1277019e-06
Categories

Plasma Diagnostics, Abundance Analysis, Collisionally Excited Lines

Dirs
./

Subroutines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

15/09/2013, A. Danehkar, Translated from FORTRAN to IDL code.

20/10/2016, A. Danehkar, Replaced str2int with strnumber.

20/10/2016, A. Danehkar, Replaced CFY, SPLMAT, and CFD with

IDL function INTERPOL( /SPLINE).

20/10/2016, A. Danehkar, Replaced LUSLV with IDL LAPACK function

LA_LINEAR_EQUATION.

15/11/2016, A. Danehkar, Replaced LA_LINEAR_EQUATION (not work in GDL)

with IDL function LUDC & LUSOL.

19/11/2016, A. Danehkar, Replaced INTERPOL (not accurate) with

SPL_INIT & SPL_INTERP.

20/11/2016, A. Danehkar, Made a new function calc_populations()

for solving atomic level populations and separated it from calc_abundance(), calc_density() and calc_temperature().

10/03/2017, A. Danehkar, Integration with AtomNeb, now uses atomic data

input elj_data, omij_data, aij_data.

12/06/2017, A. Danehkar, Cleaning the function, and remove unused varibales

from calc_populations().

27/02/2019, A. Danehkar, Simplify the calc_populations() routine

for external usage.

04/03/2019, A. Danehkar, Use the get_omij_temp() routine.

03/10/2020, A. Danehkar, Transferred from IDL to Python.

FORTRAN HISTORY:

03/05/1981, I.D.Howarth, Version 1.

05/05/1981, I.D.Howarth, Minibug fixed!

07/05/1981, I.D.Howarth, Now takes collision rates or strengths.

03/08/1981, S.Adams, Interpolates collision strengths.

07/08/1981, S.Adams, Input method changed.

19/11/1984, R.E.S.Clegg, SA files entombed in scratch disk. Logical

filenames given to SA’s data files.

08/1995, D.P.Ruffle, Changed input file format. Increased matrices.

02/1996, X.W.Liu, Tidy up. SUBROUTINES SPLMAT, HGEN, CFY and CFD

modified such that matrix sizes (i.e. maximum of Te and maximum no of levels) can now be cha by modifying the parameters NDIM1, NDIM2 and N in the Main program. EASY! Now takes collision rates as well. All variables are declared explicitly Generate two extra files (ionpop.lis and ionra of plain stream format for plotting.

06/1996, C.J.Pritchet, Changed input data format for cases IBIG=1,2.

Fixed readin bug for IBIG=2 case. Now reads reformatted upsilons (easier to see and the 0 0 0 data end is excluded for these c The A values have a different format for IBIG=.

2006, B.Ercolano, Converted to F90.

2009, R.Wesson, Misc updates and improvements.

Converted to F90. Version written only for calculating ionic abundances. Takes arguments from the command line.

pyequib.calc_temperature(line_flux_ratio=None, density=None, upper_levels=None, lower_levels=None, elj_data=None, omij_data=None, aij_data=None, low_temperature=None, high_temperature=None, num_temperature=None, min_density=None)[source]

This function determines electron temperature from given flux intensity ratio for specified ion with upper level(s) lower level(s) by solving atomic level populations and line emissivities in statistical equilibrium for given electron density.

Returns

type=double. This function returns the electron temperature.

Keywords
line_flux_ratioin, required, type=float

flux intensity ratio

densityin, required, type=float

electron density

upper_levelsin, required, type=string,

upper atomic level(s) e.g ‘1,2/’, ‘1,2,1,3/’

lower_levelsin, required, type=string

lower atomic level(s) e.g ‘1,2/’, ‘1,2,1,3/’

elj_datain, required, type=array/object

energy levels (Ej) data

omij_datain, required, type=array/object

collision strengths (omega_ij) data

aij_datain, required, type=array/object

transition probabilities (Aij) data

low_temperaturein, optional, type=float

lower temperature range

high_temperaturein, optional, type=float

upper temperature range

num_temperaturein, optional, type=integer

number of the iteration step

min_densityin, optional, type=float

lower density range

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_dir = os.path.join('atomic-data', 'chianti70')
>>> atom_elj_file = os.path.join(base_dir,data_dir, 'AtomElj.fits')
>>> atom_omij_file = os.path.join(base_dir,data_dir, 'AtomOmij.fits')
>>> atom_aij_file = os.path.join(base_dir,data_dir, 'AtomAij.fits')
>>> atom='s'
>>> ion='ii'
>>> s_ii_elj=atomneb.read_elj(atom_elj_file, atom, ion, level_num=5) # read Energy Levels (Ej)
>>> s_ii_omij=atomneb.read_omij(atom_omij_file, atom, ion) # read Collision Strengths (Omegaij)
>>> s_ii_aij=atomneb.read_aij(atom_aij_file, atom, ion) # read Transition Probabilities (Aij)
>>> upper_levels='1,2,1,3/'
>>> lower_levels='1,5/'
>>> density = np.float64(2550)
>>> line_flux_ratio=np.float64(10.753)
>>> temperature=pyequib.calc_temperature(line_flux_ratio=line_flux_ratio, density=density,
>>>                              upper_levels=upper_levels, lower_levels=lower_levels,
>>>                              elj_data=s_ii_elj, omij_data=s_ii_omij,
>>>                              aij_data=s_ii_aij)
>>> print("Electron Temperature:", temperature)
   Electron Temperature:       7920.2865
Categories

Plasma Diagnostics, Collisionally Excited Lines

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

15/09/2013, A. Danehkar, Translated from FORTRAN to IDL code.

20/10/2016, A. Danehkar, Replaced str2int with strnumber.

20/10/2016, A. Danehkar, Replaced CFY, SPLMAT, and CFD with

IDL function INTERPOL( /SPLINE).

20/10/2016, A. Danehkar, Replaced LUSLV with IDL LAPACK function

LA_LINEAR_EQUATION.

15/11/2016, A. Danehkar, Replaced LA_LINEAR_EQUATION (not work in GDL)

with IDL function LUDC & LUSOL.

19/11/2016, A. Danehkar, Replaced INTERPOL (not accurate) with

SPL_INIT & SPL_INTERP.

20/11/2016, A. Danehkar, Made a new function calc_populations()

for solving atomic level populations and separated it from calc_abundance(), calc_density() and calc_temperature().

10/03/2017, A. Danehkar, Integration with AtomNeb, now uses atomic data

input elj_data, omij_data, aij_data.

12/06/2017, A. Danehkar, Cleaning the function, and remove unused varibales

from calc_temperature().

27/02/2019, A. Danehkar, Fix a bug in the atomic level assumption, and

use the simplified calc_populations() routine.

04/03/2019, A. Danehkar, Use the get_omij_temp() routine.

24/05/2019, A. Danehkar, Add the optional temperature range.

03/10/2020, A. Danehkar, Transferred from IDL to Python.

FORTRAN HISTORY:

03/05/1981, I.D.Howarth, Version 1.

05/05/1981, I.D.Howarth, Minibug fixed!

07/05/1981, I.D.Howarth, Now takes collision rates or strengths.

03/08/1981, S.Adams, Interpolates collision strengths.

07/08/1981, S.Adams, Input method changed.

19/11/1984, R.E.S.Clegg, SA files entombed in scratch disk. Logical

filenames given to SA’s data files.

08/1995, D.P.Ruffle, Changed input file format. Increased matrices.

02/1996, X.W.Liu, Tidy up. SUBROUTINES SPLMAT, HGEN, CFY and CFD

modified such that matrix sizes (i.e. maximum of Te and maximum no of levels) can now be cha by modifying the parameters NDIM1, NDIM2 and N in the Main program. EASY! Now takes collision rates as well. All variables are declared explicitly Generate two extra files (ionpop.lis and ionra of plain stream format for plotting.

06/1996, C.J.Pritchet, Changed input data format for cases IBIG=1,2.

Fixed readin bug for IBIG=2 case. Now reads reformatted upsilons (easier to see and the 0 0 0 data end is excluded for these c The A values have a different format for IBIG=.

2006, B.Ercolano, Converted to F90.

2009, R.Wesson, Misc updates and improvements.

Converted to F90. Version written only for calculating ionic abundances. Takes arguments from the command line.

pyequib.deredden_flux(wavelength, flux, m_ext, ext_law=None, rv=None, fmlaw=None)[source]

This function dereddens absolute flux intensity based on the reddening law.

Returns

type=double. This function returns the deredden flux intensity.

Params
wavelengthin, required, type=float/array

Wavelength in Angstrom

fluxin, required, type=float,

absolute flux intensity

m_extin, required, type=float,

logarithmic extinction

Keywords
ext_lawin, optional, type=string, default=’GAL’

the extinction law:

‘GAL’ for Howarth Galactic.

‘GAL2’ for Savage and Mathis.

‘CCM’ for CCM galactic.

‘JBK’ for Whitford, Seaton, Kaler.

‘FM’ for Fitxpatrick.

‘SMC’ for Prevot SMC.

‘LMC’ for Howarth LMC.

rvin, optional, type=float, default=3.1

the optical total-to-selective extinction ratio, RV = A(V)/E(B-V).

fmlawin, optional, type=string, default=’GAL’

the fmlaw keyword is used only in the redlaw_fm function:

‘GAL’ for the default fit parameters for the R-dependent

Galactic extinction curve from Fitzpatrick & Massa (Fitzpatrick, 1999, PASP, 111, 63).

‘LMC2’ for the fit parameters are those determined for

reddening the LMC2 field (inc. 30 Dor) from Misselt et al. (1999, ApJ, 515, 128).

‘AVGLMC’ for the fit parameters are those determined for

reddening in the general Large Magellanic Cloud (LMC) field by Misselt et al. (1999, ApJ, 515, 128).

Examples

For example:

>>> import pyequib
>>> wavelength=6563.0
>>> ext_law='GAL'
>>> r_v=3.1
>>> m_ext=1.0
>>> flux=1.0
>>> flux_deredden=pyequib.deredden_flux(wavelength, flux, m_ext, ext_law=ext_law, rv=r_v) # deredden absolute flux intensity
>>> print('dereddened flux(6563):', flux_deredden)
   dereddened flux(6563):       4.7847785
Categories

Interstellar Extinction

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

31/08/2012, A. Danehkar, IDL code.

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.deredden_relflux(wavelength, relflux, m_ext, ext_law=None, rv=None, fmlaw=None)[source]

This function dereddens flux intensity relative to Hb=100, based on the reddening law.

Returns

type=double. This function returns the deredden flux intensity relative to Hb=100.

Params
wavelengthin, required, type=float/array

Wavelength in Angstrom

relfluxin, required, type=float,

flux intensity relative to Hb=100

m_extin, required, type=float,

logarithmic extinction

Keywords
ext_lawin, optional, type=string, default=’GAL’

the extinction law:

‘GAL’ for Howarth Galactic.

‘GAL2’ for Savage and Mathis.

‘CCM’ for CCM galactic.

‘JBK’ for Whitford, Seaton, Kaler.

‘FM’ for Fitxpatrick.

‘SMC’ for Prevot SMC.

‘LMC’ for Howarth LMC.

rvin, optional, type=float, default=3.1

the optical total-to-selective extinction ratio, RV = A(V)/E(B-V).

fmlawin, optional, type=string, default=’GAL’

the fmlaw keyword is used only in the redlaw_fm function:

‘GAL’ for the default fit parameters for the R-dependent

Galactic extinction curve from Fitzpatrick & Massa (Fitzpatrick, 1999, PASP, 111, 63).

‘LMC2’ for the fit parameters are those determined for

reddening the LMC2 field (inc. 30 Dor) from Misselt et al. (1999, ApJ, 515, 128).

‘AVGLMC’ for the fit parameters are those determined for

reddening in the general Large Magellanic Cloud (LMC) field by Misselt et al. (1999, ApJ, 515, 128).

Examples

For example:

>>> import pyequib
>>> wavelength=6563.0
>>> ext_law='GAL'
>>> r_v=3.1
>>> m_ext=1.0
>>> flux=1.0
>>> flux_deredden=pyequib.deredden_relflux(wavelength, flux, m_ext, ext_law=ext_law, rv=r_v) # deredden absolute flux intensity
>>> print('dereddened relative flux(6563):', flux_deredden)
   dereddened relative flux(6563):       0.47847785
Categories

Interstellar Extinction

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

31/08/2012, A. Danehkar, IDL code.

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.get_omij_temp(temperature=None, omij_data=None, elj_data=None, level_num=None, irats=None)[source]

This function derives the effective collision strengths (Omij_T) from the collision strengths (omega_ij) data for the given temperature.

Returns

type=array/object. This function returns the effective collision strengths (Omij_T).

Keywords
temperaturein, required, type=float

electron temperature

omij_datain, required, type=array/object

collision strengths (omega_ij) data

level_numin, type=int

Number of levels

iratsin, type=int

Else Coll. rates = tabulated values * 10 ** irats

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_dir = os.path.join('atomic-data', 'chianti70')
>>> atom_elj_file = os.path.join(base_dir,data_dir, 'AtomElj.fits')
>>> atom_omij_file = os.path.join(base_dir,data_dir, 'AtomOmij.fits')
>>> atom_aij_file = os.path.join(base_dir,data_dir, 'AtomAij.fits')
>>> atom='s'
>>> ion='ii'
>>> s_ii_elj=atomneb.read_elj(atom_elj_file, atom, ion, level_num=5) # read Energy Levels (Ej)
>>> s_ii_omij=atomneb.read_omij(atom_omij_file, atom, ion) # read Collision Strengths (Omegaij)
>>> s_ii_aij=atomneb.read_aij(atom_aij_file, atom, ion) # read Transition Probabilities (Aij)        >>> temperature=np.float64(10000.0)#
>>> omij_t=pyequib.get_omij_temp(temperature=temperature, omij_data=s_ii_omij)
>>> print('Effective Collision Strengths: ')
>>> print(omij_t)
   Effective Collision Strengths:
   0.0000000       0.0000000       0.0000000       0.0000000       0.0000000
   2.7800000       0.0000000       0.0000000       0.0000000       0.0000000
   4.1600000       7.4600000       0.0000000       0.0000000       0.0000000
   1.1700000       1.8000000       2.2000000       0.0000000       0.0000000
   2.3500000       3.0000000       4.9900000       2.7100000       0.0000000
Categories

Plasma Diagnostics, Abundance Analysis, Collisionally Excited Lines

Dirs
./

Subroutines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

04/03/2019, A. Danehkar, create the get_omij_temp() routine.

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.print_ionic(temperature=None, density=None, elj_data=None, omij_data=None, aij_data=None, h_i_aeff_data=None, printemissivity=None, printpopulations=None, printcritdensity=None)[source]

This function prints the atom’s transitions information, atomic level populations, critical densities, and emissivities for given temperature and density.

Keywords
temperaturein, required, type=float

electron temperature

densityin, required, type=float

electron density

elj_datain, required, type=array/object

energy levels (Ej) data

omij_datain, required, type=array/object

collision strengths (omega_ij) data

aij_datain, required, type=array/object

transition probabilities (Aij) data

h_i_aeff_datain, type=array/object

H I recombination coefficients

printEmissivityin, type=boolean

Set for printing Emissivities

printPopulationsin, type=boolean

Set for printing Populations

printCritDensityin, type=boolean

Set for printing Critical Densities

Examples

For example:

>>> import pyequib
>>> import atomneb
>>> import os
>>> base_dir = '../externals/atomneb/'
>>> data_dir = os.path.join('atomic-data', 'chianti70')
>>> atom_elj_file = os.path.join(base_dir,data_dir, 'AtomElj.fits')
>>> atom_omij_file = os.path.join(base_dir,data_dir, 'AtomOmij.fits')
>>> atom_aij_file = os.path.join(base_dir,data_dir, 'AtomAij.fits')
>>> data_rc_dir = os.path.join('atomic-data-rc')
>>> atom_rc_sh95_file= os.path.join(base_dir,data_rc_dir, 'rc_SH95.fits')
>>> atom='o'
>>> ion='iii'
>>> o_iii_elj=atomneb.read_elj(atom_elj_file, atom, ion, level_num=5) # read Energy Levels (Ej)
>>> o_iii_omij=atomneb.read_omij(atom_omij_file, atom, ion) # read Collision Strengths (Omegaij)
>>> o_iii_aij=atomneb.read_aij(atom_aij_file, atom, ion) # read Transition Probabilities (Aij)
>>> atom='h'
>>> ion='ii' # H I
>>> hi_rc_data=atomneb.read_aeff_sh95(atom_rc_sh95_file, atom, ion)
>>> temperature=np.float64(10000.0)#
>>> density = np.float64(1000.)
>>> pyequib.print_ionic, temperature=temperature, density=density,
>>>              elj_data=o_iii_elj, omij_data=o_iii_omij,
>>>              aij_data=o_iii_aij, h_i_aeff_data=hi_rc_data['aeff'][0]
   Temperature =   10000.0 K
   Density =    1000.0 cm-3

   Level    Populations   Critical Densities
   Level 1:   3.063E-01   0.000E+00
   Level 2:   4.896E-01   4.908E+02
   Level 3:   2.041E-01   3.419E+03
   Level 4:   4.427E-05   6.853E+05
   Level 5:   2.985E-09   2.547E+07

    2.597E-05
        88.34um
       (2-->1)
    2.859E-22

    0.000E+00   9.632E-05
        32.66um      51.81um
       (3-->1)     (3-->2)
    0.000E+00   7.536E-22

    2.322E-06   6.791E-03   2.046E-02
      4932.60A    4960.29A    5008.24A
       (4-->1)     (4-->2)     (4-->3)
    4.140E-25   1.204E-21   3.593E-21

    0.000E+00   2.255E-01   6.998E-04   1.685E+00
      2315.58A    2321.67A    2332.12A    4364.45A
       (5-->1)     (5-->2)     (5-->3)     (5-->4)
    0.000E+00   5.759E-24   1.779E-26   2.289E-23

   H-beta emissivity: 1.237E-25 N(H+) Ne  [erg/s]
Categories

Plasma Diagnostics, Abundance Analysis, Collisionally Excited Lines

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

04/03/2019, A. Danehkar, create the print_ionic() routine.

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.redlaw(wavelength, ext_law=None, rv=None, fmlaw=None)[source]

This function determines the reddening law function of the line at the given wavelength for the used extinction law.

Returns

type=double/array. This function returns the reddening law function value for the given wavelength.

Params
wavelengthin, required, type=float/array

Wavelength in Angstrom

Keywords
ext_lawin, optional, type=string, default=’GAL’

the extinction law:

‘GAL’ for Howarth Galactic.

‘GAL2’ for Savage and Mathis.

‘CCM’ for CCM galactic.

‘JBK’ for Whitford, Seaton, Kaler.

‘FM’ for Fitxpatrick.

‘SMC’ for Prevot SMC.

‘LMC’ for Howarth LMC.

rvin, optional, type=float, default=3.1

the optical total-to-selective extinction ratio, RV = A(V)/E(B-V).

fmlawin, optional, type=string, default=’GAL’

the fmlaw keyword is used only in the redlaw_fm function:

‘GAL’ for the default fit parameters for the R-dependent

Galactic extinction curve from Fitzpatrick & Massa (Fitzpatrick, 1999, PASP, 111, 63).

‘LMC2’ for the fit parameters are those determined for

reddening the LMC2 field (inc. 30 Dor) from Misselt et al. (1999, ApJ, 515, 128).

‘AVGLMC’ for the fit parameters are those determined for

reddening in the general Large Magellanic Cloud (LMC) field by Misselt et al. (1999, ApJ, 515, 128).

Examples

For example:

>>> import pyequib
>>> wavelength=6563.0
>>> r_v=3.1
>>> fl=pyequib.redlaw(wavelength, rv=r_v)
>>> print('fl(6563)', fl)
   fl(6563)     -0.32013816
Categories

Interstellar Extinction

Dirs
./

Main routines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Originally from IRAF STSDAS SYNPHOT redlaw.x, ebmvxfunc.x

31/08/2012, A. Danehkar, Converted to IDL code.

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.redlaw_ccm(wavelength, rv=None)[source]

This function determines the reddening law function of Cardelli, Clayton & Mathis.

Returns

type=double/array. This function returns the reddening law function value for the given wavelength.

Params
wavelengthin, required, type=float/array

Wavelength in Angstrom

Keywords
RVin, optional, type=float, default=3.1

the optical total-to-selective extinction ratio, RV = A(V)/E(B-V).

Examples

For example:

>>> import pyequib
>>> wavelength=6563.0
>>> r_v=3.1
>>> fl=pyequib..redlaw_ccm(wavelength, rv=r_v)
>>> print('fl(6563)', fl)
   fl(6563)     -0.29756615
Categories

Interstellar Extinction

Dirs
./

Subroutines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on Formulae by Cardelli, Clayton & Mathis 1989, ApJ 345, 245-256. 1989ApJ…345..245C

Originally from IRAF STSDAS SYNPHOT redlaw.x

18/05/1993, R. A. Shaw, Initial IRAF implementation, based upon CCM module

in onedspec.deredden.

31/08/2012, A. Danehkar, Converted to IDL code.

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.redlaw_fm(wavelength, rv=None, fmlaw=None)[source]

This function determines the reddening law function by Fitzpatrick & Massa for the line at the given wavelength.

Returns

type=double/array. This function returns the reddening law function value for the given wavelength.

Params
wavelengthin, required, type=float/array

Wavelength in Angstrom

Keywords
RVin, optional, type=float, default=3.1

the optical total-to-selective extinction ratio, RV = A(V)/E(B-V).

fmlawin, optional, type=string, default=’GAL’

the fmlaw keyword is used only in the redlaw_fm function:

‘GAL’ for the default fit parameters for the R-dependent

Galactic extinction curve from Fitzpatrick & Massa (Fitzpatrick, 1999, PASP, 111, 63).

‘LMC2’ for the fit parameters are those determined for

reddening the LMC2 field (inc. 30 Dor) from Misselt et al. (1999, ApJ, 515, 128).

‘AVGLMC’ for the fit parameters are those determined for

reddening in the general Large Magellanic Cloud (LMC) field by Misselt et al. (1999, ApJ, 515, 128).

Examples

For example:

>>> import pyequib
>>> wavelength=6563.0
>>> r_v=3.1
>>> fl=pyequib.redlaw_fm(wavelength, rv=r_v)
>>> print('fl(6563)', fl)
   fl(6563)     -0.35054942
Categories

Interstellar Extinction

Dirs
./

Subroutines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on Formulae by Fitzpatrick 1999, PASP, 11, 63 1999PASP..111…63F, Fitzpatrick & Massa 1990, ApJS, 72, 163, 1990ApJS…72..163F

Adopted from NASA IDL Library & PyAstronomy.

30/12/2016, A. Danehkar, Revised in IDL code.

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.redlaw_gal(wavelength, rv=None)[source]

This function determines the reddening law function of the line at the given wavelength for Galactic Seaton1979+Howarth1983+CCM1983.

Returns

type=double/array. This function returns the reddening law function value(s) for the given wavelength(s).

Params
wavelengthin, required, type=float

Wavelength in Angstrom

Keywords
rvin, optional, type=float, default=3.1

the optical total-to-selective extinction ratio, RV = A(V)/E(B-V).

Examples

For example:

>>> import pyequib
>>> wavelength=6563.0
>>> r_v=3.1
>>> fl=pyequib.redlaw_gal(wavelength, rv=r_v)
>>> print('fl(6563)', fl)
   fl(6563)     -0.32013816
Categories

Interstellar Extinction

Dirs
./

Subroutines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on the UV Formulae from Seaton 1979, MNRAS, 187, 73 1979MNRAS.187P..73S, the opt/NIR from Howarth 1983, MNRAS, 203, 301 the FIR from Cardelli, Clayton and Mathis 1989, ApJ, 345, 245 1989ApJ…345..245C

Originally from IRAF STSDAS SYNPHOT ebmvxfunc.x, pyneb.extinction

31/08/2012, A. Danehkar, Converted to IDL code.

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.redlaw_gal2(wavelength)[source]

This function determines the reddening law function of the line at the given wavelength for Galactic Savage & Mathis 1979.

Returns

type=double/array. This function returns the reddening law function value(s) for the given wavelength(s).

Params
wavelengthin, required, type=float

Wavelength in Angstrom

Examples

For example:

>>> import pyequib
>>> wavelength=6563.0
>>> fl=pyequib.redlaw_gal2(wavelength)
>>> print('fl(6563)', fl)
   fl(6563)     -0.30925984
Categories

Interstellar Extinction

Dirs
./

Subroutines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on Savage & Mathis 1979, ARA&A, vol. 17, 73-111

Originally from IRAF STSDAS SYNPHOT ebmvxfunc.x

20/09/1994, R. A. Shaw, Initial IRAF implementation.

04/03/1995, R. A. Shaw, Return A(lambda)/A(V) instead.

31/08/2012, A. Danehkar, Converted to IDL code.

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.redlaw_jbk(wavelength)[source]

This function determines the reddening law function for Galactic Whitford1958 + Seaton1977 + Kaler1976.

Returns

type=double/array. This function returns the reddening law function value(s) for the given wavelength(s).

Params
wavelengthin, required, type=float

Wavelength in Angstrom

Examples

For example:

>>> import pyequib
>>> wavelength=6563.0
>>> fl=pyequib.redlaw_jbk(wavelength)
>>> print('fl(6563)', fl)
   fl(6563)     -0.33113684
Categories

Interstellar Extinction

Dirs
./

Subroutines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on Whitford (1958), extended to the UV by Seaton (1977), adapted by Kaler (1976).

Originally from IRAF STSDAS SYNPHOT redlaw.x

13/05/1993, R. A. Shaw, Initial IRAF implementation.

31/08/2012, A. Danehkar, Converted to IDL code.

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.redlaw_lmc(wavelength)[source]

This function determines the reddening law function of the line at the given wavelength for the Large Magellanic Cloud.

Returns

type=double/array. This function returns the reddening law function value(s) for the given wavelength(s).

Params
wavelengthin, required, type=float

Wavelength in Angstrom

Examples

For example:

>>> import pyequib
>>> wavelength=6563.0
>>> fl=pyequib.redlaw_lmc(wavelength)
>>> print('fl(6563)', fl)
   fl(6563)     -0.30871187
Categories

Interstellar Extinction

Dirs
./

Subroutines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on Formulae by Howarth 1983, MNRAS, 203, 301 1983MNRAS.203..301H

Originally from IRAF STSDAS SYNPHOT ebmvlfunc.x, redlaw.x

18/10/1994, R. A. Shaw, Initial IRAF implementation.

14/03/1995, R. A. Shaw, Return A(lambda)/A(V) instead.

31/08/2012, A. Danehkar, Converted to IDL code.

03/10/2020, A. Danehkar, Transferred from IDL to Python.

pyequib.redlaw_smc(wavelength)[source]

This function determines the reddening law function of the line at the given wavelength for Small Magellanic Cloud.

Returns

type=double/array. This function returns the reddening law function value(s) for the given wavelength(s).

Params
wavelengthin, required, type=float

Wavelength in Angstrom

Examples

For example:

>>> import pyequib
>>> wavelength=6563.0
>>> fl=pyequib.redlaw_smc(wavelength)
>>> print('fl(6563)', fl)
   fl(6563)     -0.22659261
Categories

Interstellar Extinction

Dirs
./

Subroutines

Author

Ashkbiz Danehkar

Copyright

This library is released under a GNU General Public License.

Version

0.3.0

History

Based on Prevot et al. (1984), A&A, 132, 389-392 1984A%26A…132..389P

Originally from IRAF STSDAS SYNPHOT redlaw.x, ebmvxfunc.x

20/09/1994, R. A. Shaw, Initial IRAF implementation.

04/03/1995, R. A. Shaw, Return A(lambda)/A(V) instead.

31/08/2012, A. Danehkar, Converted to IDL code.

03/10/2020, A. Danehkar, Transferred from IDL to Python.