学术文献库

The Ly$α$ emission line is one of the main observables of galaxies at high redshift, but its output depends strongly on the neutral gas distribution and kinematics around the star-forming regions where UV photons are produced. We present observations of Ly$α$ and 21-cm HI emission at comparable scales with the goal to qualitatively investigate how the neutral interstellar medium (ISM) properties impact Ly$α$ transfer in galaxies. We have observed 21-cm HI at the highest angular resolution possible (~ 3" beam) with the VLA in two local galaxies from the Lyman Alpha Reference Sample. We contrast this data with HST Ly$α$ imaging and spectroscopy, and MUSE and PMAS ionized gas observations. In LARS08, high intensity Ly$α$ emission is co-spatial with high column density HI where dust content is the lowest. The Ly$α$ line is strongly redshifted, consistent with velocity redistribution which allows Ly$α$ escape from high column density neutral medium with low dust content. In eLARS01, high intensity Ly$α$ emission is located in regions of low column density HI, below the HI data sensitivity limit ($<2\times10^{20}\,$cm$^{-2}$). The perturbed ISM distribution with low column density gas in front of the Ly$α$ emission region plays an important role in the escape. In both galaxies, the faint Ly$α$ emission ($\sim 1\times10^{-16}$erg.s$^{-1}$cm$^{-2}$arcsec$^{-2}$) traces intermediate H$α$ emission regions where HI is found, regardless of the dust content. Dust seems to modulate, but not prevent, the formation of a faint Ly$α$ halo. This study suggests the existence of scaling relations between dust, H$α$, HI, and Ly$α$ emission in galaxies.