A Semi-Analytical Line Transfer (SALT) model to interpret the spectra of galaxy outflows

TL;DR

The paper introduces SALT, a semi-analytical model for interpreting galaxy outflow spectra, accurately reproducing observed line profiles and accounting for complex scattering and observational effects.

Contribution

SALT provides a simplified yet accurate approach to modeling galaxy outflow line profiles, including multiple scatterings and aperture effects, improving interpretation over previous models.

Findings

SALT reproduces main features of complex transfer code profiles.

Resonant scattering fills in absorption profiles, affecting gas property estimates.

Fluorescent emission lines indicate the importance of emission filling effects.

Abstract

We present a Semi-Analytical Line Transfer model, SALT, to study the absorption and re-emission line profiles from expanding galactic envelopes. The envelopes are described as a superposition of shells with density and velocity varying with the distance from the center. We adopt the Sobolev approximation to describe the interaction between the photons escaping from each shell and the remaining of the envelope. We include the effect of multiple scatterings within each shell, properly accounting for the atomic structure of the scattering ions. We also account for the effect of a finite circular aperture on actual observations. For equal geometries and density distributions, our models reproduce the main features of the profiles generated with more complicated transfer codes. Also, our SALT line profiles nicely reproduce the typical asymmetric resonant absorption line profiles observed in star-forming/starburst galaxies whereas these absorption profiles cannot be reproduced with thin shells moving at a fixed outflow velocity. We show that scattered resonant emission fills in the resonant absorption profiles, with a strength that is different for each transition. Observationally, the effect of resonant filling depends on both the outflow geometry and the size of the outflow relative to the spectroscopic aperture. Neglecting these effects will lead to incorrect values of gas covering fraction and column density. When a fluorescent channel is available, the resonant profiles alone cannot be used to infer the presence of scattered re-emission. Conversely, the presence of emission lines of fluorescent transitions reveals that emission filling cannot be neglected.