The proEQUIB library is a collection of Interactive Data Language (IDL)/GNU Data Language (GDL) programs developed to perform plasma diagnostics and abundance analysis using emission line fluxes measured in ionzed nebulae. It uses the AtomNeb IDL library to read collision strengths and transition probabilities for collisionally excited lines (CEL), and recombination coefficients for recombination lines (RL). This IDL package can be used to determine interstellar extinctions, electron temperatures, electron densities, and ionic abundances from the measured fluxes of emission lines. It mainly contains the follwing API functions written purely in IDL/GDL:
- API functions for collisionally excited lines (CEL) have been developed based on the algorithm of the FORTRAN program EQUIB originally written in FORTRAN by Howarth & Adams (1981), extended and customized by other people (R. Clegg, D. Ruffle, X.-W. Liu, C. Pritchet, B. Ercolano & R. Wesson). The program EQUIB calculates atomic level populations and line emissivities in statistical equilibrium in multi-level atoms for different physical conditions of the stratification layers where the chemical elements are ionized. Using the IDL/GDL implementation of the program EQUIB, electron temperatures, electron densities, and ionic abundances are determined from the measured fluxes of collisionally excited lines.
- API functions for recombination lines (RL) have been developed based on the algorithm of the recombination scripts by X. W. Liu and Y. Zhang from output_mod.f90 included in the FORTRAN program MOCASSIN. These API functiosn are used to determine ionic abundances from recombination lines for some heavy element ions.
- API functions for reddening and extinctions have been developed according to the methods of the reddening law functions from STSDAS IRAF Package, which are used to obtain interstellar extinctions and deredden measured fluxes based on different reddening laws.
This package requires the following packages:
- The IDL Astronomy User's Library
- The AtomNeb IDL Library
- IDL MCMC Hammer library (currently not used!)
To get this package with all the dependent packages, you can simply use
gitcommand as follows:git clone --recursive https://github.com/equib/proEQUIB.git
- To install the proEQUIB library in the Interactive Data Language (IDL), you need to add the path of this package directory to your IDL path. For more information about the path management in IDL, read the tips for customizing IDL program path provided by Harris Geospatial Solutions or the IDL library installation note by David Fanning in the Coyote IDL Library.
- This package requires IDL version 7.1 or later.
You can install the GNU Data Language (GDL) if you do not have it on your machine:
- Linux (Fedora):
sudo dnf install gdl
- Linux (Ubuntu):
sudo apt-get install gnudatalanguage
- OS X:
brew install gnudatalanguage
- Windows: You can use the GNU Data Language for Win32 (Unofficial Version) or you can compile the GitHub source using Visual Studio 2015 as shown in appveyor.yml.
To install the proEQUIB library in GDL, you need to add the path of this package directory to your
.gdl_startupfile in your home directory:!PATH=!PATH + ':/home/proEQUIB/pro/' !PATH=!PATH + ':/home/proEQUIB/externals/misc/' !PATH=!PATH + ':/home/proEQUIB/externals/astron/pro/' !PATH=!PATH + ':/home/proEQUIB/externals/atomneb/pro/'
You may also need to set
GDL_STARTUPif you have not done in.bashrc(bash):export GDL_STARTUP=~/.gdl_startup
or in
.tcshrc(cshrc):setenv GDL_STARTUP ~/.gdl_startup
This package requires GDL version 0.9.8 or later.
The Documentation of the IDL functions provides in detail in the API Documentation (equib.github.io/proEQUIB/doc).
See Jupyter Notebooks: Notebooks.ipynb
Run Jupyter Notebooks on Binder:
There are three main object units:
Collision Unit has the API functions for plasma diagnostics and abundance analysis of collisionally excited lines. Here are some examples of using Collision Unit:
Temperature:
s2=obj_new('collision') s2->set,['s','ii'] upper_levels='1,2,1,3/' lower_levels='1,5/' density = double(2550) line_flux_ratio=double(10.753) temperature=s2->calc_temperature(line_flux_ratio=line_flux_ratio, density=density, $ upper_levels=upper_levels, lower_levels=lower_levels) print, "Electron Temperature:", temperature
which gives:
Electron Temperature: 7920.2865
Density:
s2=obj_new('collision') s2->set,['s','ii'] upper_levels='1,2/' lower_levels='1,3/' temperature=double(7000.0); line_flux_ratio=double(1.506); density=s2->calc_density(line_flux_ratio=line_flux_ratio, temperature=temperature, $ upper_levels=upper_levels, lower_levels=lower_levels) print, "Electron Density:", density
which gives:
Electron Density: 2312.6395
Ionic Abundance:
o3=obj_new('collision') o3->set,['o','iii'] levels5007='3,4/' temperature=double(10000.0) density=double(5000.0) iobs5007=double(1200.0) Abb5007=o3->calc_abundance(temperature=temperature, density=density, $ line_flux=iobs5007, atomic_levels=levels5007) print, 'N(O^2+)/N(H+):', Abb5007
which gives:
N(O^2+)/N(H+): 0.00041256231
Emissivity:
o3=obj_new('collision') o3->set,['o','iii'] levels5007='3,4/' temperature=double(10000.0) density=double(5000.0) iobs5007=double(1200.0) emis=o3->calc_emissivity(temperature=temperature, density=density, $ atomic_levels=levels5007) print, 'Emissivity(O III 5007):', emis
which gives:
Emissivity(O III 5007): 3.6041012e-21
Atomic Level Population:
s2=obj_new('collision') s2->set,['s','ii'] density = double(1000) temperature=double(10000.0); Nlj=s2->calc_populations(temperature=temperature, density=density) print, 'Populations:', Nlj
which prints:
Populations: 0.96992832 0.0070036315 0.023062261 2.6593671e-06 3.1277019e-06
Critical Density:
s2=obj_new('collision') s2->set,['s','ii'] temperature=double(10000.0) N_crit=s2->calc_crit_density(temperature=temperature) print, 'Critical Densities:', N_crit
which gives:
Critical Densities: 0.0000000 5007.8396 1732.8414 1072685.0 2220758.1
All Ionic Level Information:
o3=obj_new('collision') o3->set,['o','iii'] temperature=double(10000.0) density=double(5000.0) o3->print_ionic, temperature=temperature, density=density
which gives:
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]
Recombination Unit has the API functions for plasma diagnostics and abundance analysis of recombination lines. Here are some examples of using Recombination Unit:
He+ Ionic Abundance:
he1=obj_new('recombination') he1->set,['he','ii'] ; He I temperature=double(10000.0) density=double(5000.0) he_i_4471_flux= 2.104 linenum=10; 4471.50 Abund_he_i=he1->calc_abundance(temperature=temperature, density=density, $ linenum=linenum, line_flux=he_i_4471_flux) print, 'N(He^+)/N(H^+):', Abund_he_i
which gives:
N(He^+)/N(H^+): 0.040848393
He++ Ionic Abundance:
he2=obj_new('recombination') he2->set,['he','iii'] ; He II temperature=double(10000.0) density=double(5000.0) he_ii_4686_flux = 135.833 Abund_he_ii=he2->calc_abundance(temperature=temperature, density=density, $ line_flux=he_ii_4686_flux) print, 'N(He^2+)/N(H^+):', Abund_he_ii
which gives:
N(He^2+)/N(H^+): 0.11228817
C++ Ionic Abundance:
c2=obj_new('recombination') c2->set,['c','iii'] ; C II temperature=double(10000.0) density=double(5000.0) wavelength=6151.43 c_ii_6151_flux = 0.028 Abund_c_ii=c2->calc_abundance(temperature=temperature, density=density, $ wavelength=wavelength, line_flux=c_ii_6151_flux) print, 'N(C^2+)/N(H+):', Abund_c_ii
which gives:
N(C^2+)/N(H+): 0.00063404650
C3+ Ionic Abundance:
c3=obj_new('recombination') c3->set,['c','iv'] ; C III temperature=double(10000.0) density=double(5000.0) wavelength=4647.42 c_iii_4647_flux = 0.107 Abund_c_iii=c3->calc_abundance(temperature=temperature, density=density, $ wavelength=wavelength, line_flux=c_iii_4647_flux) print, 'N(C^3+)/N(H+):', Abund_c_iii
which gives:
N(C^3+)/N(H+): 0.00017502840
N++ Ionic Abundance:
n2=obj_new('recombination') n2->set,['n','iii'] ; N II wavelength=4442.02 n_ii_4442_flux = 0.017 Abund_n_ii=n2->calc_abundance(temperature=temperature, density=density, $ wavelength=wavelength, line_flux=n_ii_4442_flux) print, 'N(N^2+)/N(H+):', Abund_n_ii
which gives:
N(N^2+)/N(H+): 0.00069297541
N3+ Ionic Abundance:
n3=obj_new('recombination') n3->set,['n','iv'] ; N III wavelength=4640.64 n_iii_4641_flux = 0.245 Abund_n_iii=n3->calc_abundance(temperature=temperature, density=density, $ wavelength=wavelength, line_flux=n_iii_4641_flux) print, 'N(N^3+)/N(H+):', Abund_n_iii
which gives:
N(N^3+)/N(H+): 6.3366175e-05
O++ Ionic Abundance:
o2=obj_new('recombination') o2->set,['o','iii'] ; O II wavelength=4613.68 o_ii_4614_flux = 0.009 Abund_o_ii=o2->calc_abundance(temperature=temperature, density=density, $ wavelength=wavelength, line_flux=o_ii_4614_flux) print, 'N(O^2+)/N(H+):', Abund_o_ii
which gives:
N(O^2+)/N(H+): 0.0018886330
Ne++ Ionic Abundance:
ne2=obj_new('recombination') ne2->set,['ne','iii'] ; Ne II wavelength=3777.14 ne_ii_3777_flux = 0.056 Abund_ne_ii=ne2->calc_abundance(temperature=temperature, density=density, $ wavelength=wavelength, line_flux=ne_ii_3777_flux) print, 'N(Ne^2+)/N(H+):', Abund_ne_ii
which gives:
N(Ne^2+)/N(H+): 0.00043376850
He I Emissivity:
he1=obj_new('recombination') he1->set,['he','ii'] ; He I temperature=double(10000.0) density=double(5000.0) linenum=10; 4471.50 emiss_he_i=he1->calc_emissivity(temperature=temperature, density=density, $ linenum=linenum) print, 'He I Emissivity:', emiss_he_i
which gives:
He I Emissivity: 6.3822830e-26
He II Emissivity:
he2=obj_new('recombination') he2->set,['he','iii'] ; He II temperature=double(10000.0) density=double(5000.0) emiss_he_ii=he2->calc_emissivity(temperature=temperature, density=density) print, 'He II Emissivity:', emiss_he_ii
which gives:
He II Emissivity: 1.4989134e-24
C II Emissivity:
c2=obj_new('recombination') c2->set,['c','iii'] ; C II temperature=double(10000.0) density=double(5000.0) wavelength=6151.43 emiss_c_ii=c2->calc_emissivity(temperature=temperature, density=density, $ wavelength=wavelength) print, 'C II Emissivity:', emiss_c_ii
which gives:
C II Emissivity: 5.4719511e-26
C III Emissivity:
c3=obj_new('recombination') c3->set,['c','iv'] ; C III temperature=double(10000.0) density=double(5000.0) wavelength=4647.42 emiss_c_iii=c3->calc_emissivity(temperature=temperature, density=density, $ wavelength=wavelength) print, 'C III Emissivity:', emiss_c_iii
which gives:
C III Emissivity: 7.5749632e-25
N II Emissivity:
n2=obj_new('recombination') n2->set,['n','iii'] ; N II wavelength=4442.02 emiss_n_ii=n2->calc_emissivity(temperature=temperature, density=density, $ wavelength=wavelength) print, 'N II Emissivity:', emiss_n_ii
which gives:
N II Emissivity: 3.0397397e-26
N III Emissivity:
n3=obj_new('recombination') n3->set,['n','iv'] ; N III wavelength=4640.64 emiss_n_iii=n3->calc_emissivity(temperature=temperature, density=density, $ wavelength=wavelength) print, 'N III Emissivity:', emiss_n_iii
which gives:
N III Emissivity: 4.7908644e-24
O II Emissivity:
o2=obj_new('recombination') o2->set,['o','iii'] ; O II wavelength=4613.68 emiss_o_ii=o2->calc_emissivity(temperature=temperature, density=density, $ wavelength=wavelength) print, 'O II Emissivity:', emiss_o_ii
which gives:
O II Emissivity: 5.9047319e-27
Ne II Emissivity:
ne2=obj_new('recombination') ne2->set,['ne','iii'] ; Ne II wavelength=3777.14 emiss_ne_ii=ne2->calc_emissivity(temperature=temperature, density=density, $ wavelength=wavelength) print, 'Ne II Emissivity:', emiss_ne_ii
which gives:
Ne II Emissivity: 1.5996881e-25
Reddening Unit has the API functions for estimating logarithmic extinctions at H-beta and dereddening observed fluxes based on reddening laws and extinctions. Here are some examples of using Reddening Unit:
Reddening Law Function:
ext=obj_new('reddening') wavelength=6563.0 R_V=3.1 fl=ext->redlaw(wavelength, rv=R_V, ext_law='GAL') print, 'fl(6563):', fl
which gives:
fl(6563): -0.32013816
Galactic Reddening Law Function based on Seaton (1979), Howarth (1983), & CCM (1983):
ext=obj_new('reddening') wavelength=6563.0 R_V=3.1 fl=ext->redlaw_gal(wavelength, rv=R_V) print, 'fl(6563):', fl
which gives:
fl(6563): -0.32013816
Galactic Reddening Law Function based on Savage & Mathis (1979):
ext=obj_new('reddening') wavelength=6563.0 fl=ext->redlaw_gal2(wavelength) print, 'fl(6563):', fl
which gives:
fl(6563): -0.30925984
Reddening Law Function based on Cardelli, Clayton & Mathis (1989):
ext=obj_new('reddening') wavelength=6563.0 R_V=3.1 fl=ext->redlaw_ccm(wavelength, rv=R_V) print, 'fl(6563):', fl
which gives:
fl(6563): -0.29756615
Galactic Reddening Law Function based on Whitford (1958), Seaton (1977), & Kaler(1976):
ext=obj_new('reddening') wavelength=6563.0 fl=ext->redlaw_jbk(wavelength) print, 'fl(6563):', fl
which gives:
fl(6563): -0.33113684
Reddening Law Function based on Fitzpatrick & Massa (1990), Fitzpatrick (1999), Misselt (1999):
ext=obj_new('reddening') wavelength=6563.0 R_V=3.1 fmlaw='AVGLMC' fl=ext->redlaw_fm(wavelength, fmlaw=fmlaw, rv=R_V) print, 'fl(6563):', fl
which gives:
fl(6563): -0.35053032
Reddening Law Function for the Small Magellanic Cloud:
ext=obj_new('reddening') wavelength=6563.0 fl=ext->redlaw_smc(wavelength) print, 'fl(6563):', fl
which gives:
fl(6563): -0.22659261
Reddening Law Function for the Large Magellanic Cloud:
ext=obj_new('reddening') wavelength=6563.0 fl=ext->redlaw_lmc(wavelength) print, 'fl(6563):', fl
which gives:
fl(6563): -0.30871187
Dereddening Relative Flux:
ext=obj_new('reddening') wavelength=6563.0 m_ext=1.0 flux=1.0 ext_law='GAL' R_V=3.1 flux_deredden=ext->deredden_relflux(wavelength, flux, m_ext, ext_law=ext_law, rv=R_V) print, 'dereddened flux(6563)', flux_deredden
which gives:
dereddened flux(6563) 0.47847785
Dereddening Absolute Flux:
ext=obj_new('reddening') wavelength=6563.0 m_ext=1.0 flux=1.0 ext_law='GAL' R_V=3.1 flux_deredden=ext->deredden_flux(wavelength, flux, m_ext, ext_law=ext_law, rv=R_V) print, 'dereddened flux(6563)', flux_deredden
which gives:
dereddened flux(6563) 4.7847785
For more information on how to use the API functions from the proEQUIB libray, please read the API Documentation published on equib.github.io/proEQUIB.
- Danehkar, A. (2018). proEQUIB: IDL Library for Plasma Diagnostics and Abundance Analysis. J. Open Source Softw., 3, 899. doi:10.21105/joss.00899 ads:2018JOSS....3..899D.
- Danehkar, A. (2020). pyEQUIB Python Package, an addendum to proEQUIB: IDL Library for Plasma Diagnostics and Abundance Analysis. J. Open Source Softw., 5, 2798. doi:10.21105/joss.02798 ads:2020JOSS....5.2798D.
- Danehkar, A. (2018). Bi-Abundance Ionisation Structure of the Wolf-Rayet Planetary Nebula PB 8, PASA, 35, e005. doi:10.1017/pasa.2018.1 ads:2018PASA...35....5D.
- Danehkar, A. (2021). Physical and Chemical Properties of Wolf-Rayet Planetary Nebulae, ApJS, 257, 58. doi:10.3847/1538-4365/ac2310 ads:2021ApJS..257...58D.
Using the proEQUIB IDL library in a scholarly publication? Please cite these papers:
@article{Danehkar2018,
author = {{Danehkar}, Ashkbiz},
title = {proEQUIB: IDL Library for Plasma Diagnostics and Abundance Analysis},
journal = {Journal of Open Source Software},
volume = {3},
number = {32},
pages = {899},
year = {2018},
doi = {10.21105/joss.00899}
}and if you use the pyEQUIB Python package:
@article{Danehkar2020,
author = {{Danehkar}, Ashkbiz},
title = {pyEQUIB Python Package, an addendum to proEQUIB: IDL Library
for Plasma Diagnostics and Abundance Analysis},
journal = {Journal of Open Source Software},
volume = {5},
number = {55},
pages = {2798},
year = {2020},
doi = {10.21105/joss.02798}
}| Documentation | https://equib.github.io/proEQUIB/doc/ |
| Repository | https://github.com/equib/proEQUIB |
| Issues & Ideas | https://github.com/equib/proEQUIB/issues |
| DOI | 10.21105/joss.00899 |
| Archive | 10.5281/zenodo.1890336 |