Lyman "bump" galaxies - I. Spectral energy distribution of galaxies with an escape of nebular Lyman continuum

TL;DR

This paper investigates the spectral energy distribution of galaxies with nebular Lyman continuum escape, revealing a characteristic Lyman 'bump' feature that can help identify young, metal-poor stellar populations and assess their role in cosmic reionization.

Contribution

It introduces the concept of a Lyman 'bump' caused by nebular LyC escape and explores how this feature can be used to detect specific stellar populations and understand their impact on reionization.

Findings

The Lyman 'bump' appears just below the Lyman limit due to nebular LyC escape.

The bump's strength depends on nebular temperature, escape fractions, and stellar properties.

Nebular LyC escape increases total LyC photon escape but has limited impact on reionization energy.

Abstract

It is essential to know galactic emissivity and spectrum of Lyman continuum (LyC) in order to understand the cosmic reionization. Here we consider an escape of nebular LyC from galaxies and examine the consequent spectral energy distribution. It is usually assumed that hydrogen nebular LyC mostly produced by bound-free transitions is consumed within photo-ionized nebulae (so-called "on-the-spot" approximation). However, an escape of the continuum should be taken into account if stellar LyC escapes from galaxies through "matter-bounded" nebulae. We show that the escaping hydrogen bound-free LyC makes a strong bump just below the Lyman limit. Such a galaxy would be observed as a Lyman "bump" galaxy. This bump results from the radiation energy re-distribution of stellar LyC by nebulae. The strength of the bump depends on electron temperature in nebulae, escape fraction of stellar and nebular LyC, hardness of stellar LyC (i.e. metallicity, initial mass function, age and star formation history), and IGM attenuation. We can use the bump to find very young ($\sim1$ Myr), massive ($\sim100$ $M_\odot$), and extremely metal-poor (or metal-free) stellar populations at $z<4$. Because of the bump, 900 \AA-to-1500 \AA luminosity density ratio (per Hz) becomes maximum (2--3 times larger than the stellar intrinsic ratio) when about 40% of the stellar LyC is absorbed by nebulae. The total number of escaping LyC photons increases due to the escape of nebular LyC but does not exceed the stellar intrinsic one. The radiation energy re-distribution by nebulae reduces the mean energy of escaping LyC only by $\approx10$% relative to that of stellar LyC. Therefore, the effect of the escape of nebular LyC on the reionization process may be small.