On the Detectability of Lyman-alpha Emission in Star-forming Galaxies: The Role of Dust

TL;DR

This study investigates how dust and gas kinematics affect Lyman-alpha emission escape in star-forming galaxies, revealing low escape fractions and cautioning against simplistic interpretations of high-redshift observations.

Contribution

It provides a detailed analysis of Lyman-alpha escape mechanisms in nearby galaxies, emphasizing the roles of dust, gas kinematics, and ISM morphology, and proposes a new calibration for star formation rates based on Lyman-alpha.

Findings

Lyman-alpha escape fraction is mostly below 10%.

Gas kinematics, especially outflows, influence Lyman-alpha escape.

Simple dust correction underestimates star formation rates from Lyman-alpha.

Abstract

Lyman-alpha is now widely used to investigate the galaxy formation and evolution in the high redshift universe. However, without a rigorous understanding of the processes which regulate the Lya escape fraction, physical interpretations of high-z observations remain questionable. We examine six nearby star-forming galaxies to disentangle the role of the dust from other parameters such as gas kinematics, geometry and ISM morphology in the obscuration of Ly-alpha. Thereby we aim to understand the Ly-a escape physics and infer the implications for high-redshift studies. We use HST/ACS to produce continuum-subtracted Lya maps, and ground-based observations (ESO/NTT and NOT) to map the Halpha emission and the extinction E(B-V) in the gas phase derived from the Balmer decrement Halpha/Hbeta. When large outflows are present, the Lya emission appears not to correlate with the dust content, confirming the role of the HI kinematics in the escape of Lya photons. In the case of a dense, static HI covering, we observe a damped absorption with a declining relationship between Lya and E(B-V). We found that the Lya escape fraction does not exceed 10% in all our galaxies and is mostly about 3% or below. Finally, because of the radiative transfer complexity of the Lya line, star formation rate based on Lya luminosity is underestimated with respect to that derived from UV luminosity. The failure of simple dust correction to recover the intrinsic Lya/Ha ratio or the total star formation rate should prompt us to be more cautious when interpreting high-z observations and related properties, such as SFRs based on Lya alone. To this end we propose a more realistic calibration for SFR(Lya) which accounts for dust attenuation and resonant scattering effects via the Lya escape fraction.