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.
-
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.
-
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.
-
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_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 helium 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_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.
-
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.
-
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.
-
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.