From November 26, 2018 13:15 until November 26, 2018 13:45
At Seminar Room
In our current understanding of the reionization era, the sources responsible for the transition of the universe from a neutral state to an ionized state are likely faint, low mass, star-forming galaxies. One way to study this type of population is to study the Luminosity Function (LF) of galaxies selected from their Ly-a emission. However, the current studies and their conclusions are limited by the lower luminosity that can be reached in the surveys.
In order to reach lower luminosities and to set more reliable constraints on the contribution of the Lyman-alpha emitters (LAE) population to reionization, we are working in lensing clusters. To the cost of a significant increase in complexity and a lower volume of universe explored, we are able to select a large population of LAE (~160) that are typically 10 times fainter than in blank field surveys, providing more constraints on the shape of the faint end of the luminosity function. This population is selected by MUSE, a large field of view integral field unit placed at one of the VLTs, ideal to work on the galaxy luminosity function. It allows to select a large population LAEs in a wide redshift range (2.9 < z < 7), without any prior photometric selection and with a better understanding of the selection effects.
During this presentation, I will present the new methods we developed to compute, as rigorously as possible, the LF of LAEs behind lensing clusters, the results obtained and the possible implications for reionization.