Abstract
The emission lines emitted from gaseous nebulae carry valuable information about the physical conditions and chemical abundances of ionized gases in these objects, as well as the interstellar extinction. "proEQUIB" is a library containing several application programming interface (API) functions developed in the Interactive Data Language (IDL), which can be used for plasma diagnostics and abundance analysis of nebular spectra. This IDL library can also be used by the GNU Data Language (GDL), which is a free and open-source IDL compiler. This package includes several API functions to determine physical conditions and chemical abundances from collisionally excited lines (CEL) and recombination lines (RL), derive interstellar extinctions from Balmer lines, and deredden the observed fluxes. This IDL library heavily relies on the IDL Astronomy User's library and the IDL "AtomNeb" library. The API functions of this IDL library can easily be utilized for spatially-resolved studies of ionized gaseous nebulae observed using integral field spectroscopy.
Highlights
ProEQUIB is a library including several application programming interface (API) functions developed in the Interactive Data Language (IDL), which can be used to determine temperatures, densities, and chemical abundances from emission lines of ionized nebulae
This IDL library can be used by the GNU Data Language (GDL) (Arabas, Schellens, Coulais, Gales, & Messmer (2010); Coulais et al (2010)), which is a free and open-source alternative IDL compiler
The API functions for the collisionally excited lines (CEL) analysis were developed in the IDL programming language based on the algorithm of the FORTRAN program EQUIB (Howarth & Adams (1981); Howarth et al (2016)), which calculates atomic level populations and line emissivities in statistical equilibrium in multi-level atoms for the given physical conditions
Summary
ProEQUIB is a library including several application programming interface (API) functions developed in the Interactive Data Language (IDL), which can be used to determine temperatures, densities, and chemical abundances from emission lines of ionized nebulae. The emission lines emitted from gaseous nebulae carry valuable information about the physical conditions and chemical abundances of ionized gases in these objects, as well as the interstellar reddening. We determine the electron temperature, the electron density, and the ionic abundances from the dereddened fluxes of collisionally excited lines (CEL) and recombination lines (RL) identified in nebular spectra (see e.g. Danehkar, Parker, & Ercolano (2013); Danehkar, Todt, Ercolano, & Kniazev (2014); Danehkar, Parker, & Steffen (2016); Danehkar (2018a)).
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