PyNeb: a new tool for analyzing emission lines. I. Code description and validation of results

Abstract

Analysis of emission lines in gaseous nebulae yields direct measures of physical conditions and chemical abundances and is the cornerstone of nebular astrophysics. Although the physical problem is conceptually simple, its practical complexity can be overwhelming since the amount of data to be analyzed steadily increases; furthermore, results depend crucially on the input atomic data, whose determination also improves each year. To address these challenges we created PyNeb, an innovative code for analyzing emission lines. PyNeb computes physical conditions and ionic and elemental abundances, and produces both theoretical and observational diagnostic plots. It is designed to be portable, modular, and largely customizable in aspects such as the atomic data used, the format of the observational data to be analyzed, and the graphical output. It gives full access to the intermediate quantities of the calculation, making it possible to write scripts tailored to the specific type of analysis one wants to carry out. In the case of collisionally excited lines, PyNeb works by solving the equilibrium equations for an n-level atom; in the case of recombination lines, it works by interpolation in emissivity tables. The code offers a choice of extinction laws and ionization correction factors, which can be complemented by user-provided recipes. It is entirely written in the python programming language and uses standard python libraries. It is fully vectorized, making it apt for analyzing huge amounts of data. The code is stable and has been benchmarked against IRAF/NEBULAR. It is public, fully documented, and has already been satisfactorily used in a number of published papers.

17 pages, 12 figures. Accepted for publication in Astronomy & Astrophysics. Typos and reference list corrected in this version

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• Resolving dust and Lyα emission in a lensed galaxy at the epoch of reionization with JWST/CANUCS
• Carbon Abundances in Compact Galactic Planetary Nebulae: An Ultraviolet spectroscopic study with the Space Telescope Imaging Spectrograph (STIS)
• The ionization structure and chemical history in isolated H ii regions of dwarf galaxies with VIMOS/IFU II. The Leo A galaxy
• GA-NIFS: AGN activity in a Lyα emitter within a triple-AGN system anchored by a passive galaxy at z=3
• Fast, dust-poor outflows in the local candidate dual AGN MCG-03-34-64 observed with VLT/ERIS
• The Nature of Jets in Double-Peaked Emission Line AGN in the KISSR Sample
• Quokka-based understanding of outflows (QED) -- IV. Limitations of H$\alpha$ as an outflow diagnostic
• Andromeda's tenuous veil: A likely Milky Way nebula projected toward M31
• QSOFEED: Investigating warm molecular, low- and high-ionization atomic gas in six type-2 quasars with GTC/EMIR
• The accretion-ejection connection in the asymmetric Th 28 jet revealed by MUSE-NFM
• Is the nitrogen-rich source PN K4-47 a true planetary nebula?
• Implication of a galaxy-scale negative feedback by one of the most powerful multi-phase outflows in a hyper-luminous infrared galaxy at the intermediate redshift
• Beyond the [OIII]$\lambda$4363 auroral line: [NeIII]$\lambda$3868 as a direct tracer of electron temperature
• Dissecting NGC 3132: Tracing the mass-loss history of the southern ring planetary nebula
• UV bright red-sequence galaxies: a comparative study between UV upturn and UV weak systems
• The relationship between warm and hot gas-phase metallicity in massive elliptical galaxies and the influence of AGN feedback
• SDSS-IV MaNGA: Data-Model Discrepancy in Temperature-sensitive Line Ratios for Star-forming Galaxies