Lyman alpha emission from the first galaxies: Implications of UV backgrounds and the formation of molecules

Abstract

The Lyman alpha line is a robust tracer of high redshift galaxies. We present estimates of Lyman alpha emission from a protogalactic halo illuminated by UV background radiation fields with various intensities. For this purpose, we performed cosmological hydrodynamics simulations with the adaptive mesh refinement code FLASH, including a detailed network for primordial chemistry,comprising the formation of primordial molecules, a multi-level model for the hydrogen atom as well as the photo-ionization and photo-dissociation processes in a UV background. We find that the presence of a background radiation field J_21 excites the emission of Lyman alpha photons, increasing the Lyman alpha luminosity up to two orders of magnitude. For a halo of \sim 10^10 M_sun, we find that a maximum flux of 5 \times 10^-15 erg cm^-2 s^-1 is obtained for J21 \times f_esc = 0.1, where f_esc is the escape fraction of the ionizing radiation. Depending on the environmental conditions, the flux may vary by three orders of magnitude. For J_21 \times f_esc > 0.1 the Lyman alpha luminosity decreases as the atomic hydrogen abundance becomes rather small. The fluxes derived here can be probed using Subaru and the upcoming James Webb Space Telescope. The emission of Lyman alpha photons is extended and comes from the envelope of the halo rather than its core. In the center of the halo, line trapping becomes effective above columns of 10^22 cm^-2 and suppresses the emission of Lyman alpha. In addition, cooling by primordial molecules may decrease the gas temperature in the central region, which further reduces Lyman alpha emission. In the central core, H_2 is photo-dissociated for a background flux of J_21 \geq 1000. For weaker radiation fields, i.e. J_21 < 0.1, H_2 and HD cooling are particularly strong in the center of the halo, leading to gas temperatures as low as \sim 100 K.