Ly-alpha Emission-Line Galaxies at z = 3.1 in the Extended Chandra Deep Field South

TL;DR

This study presents a deep survey of Ly-alpha emission-line galaxies at z=3.1, analyzing their properties, luminosity function, and star formation rates, revealing insights into their internal extinction and evolutionary state.

Contribution

It provides the first comprehensive characterization of Ly-alpha emitters at z=3.1, including their equivalent width distribution, luminosity function, and star formation rate discrepancies.

Findings

Equivalent width distribution follows an exponential with scale length 76 Å.

Luminosity function has a faint-end slope of -1.49 and log L* of 42.64.

Ly-alpha derived star formation rates are about three times lower than UV continuum estimates.

Abstract

We describe the results of an extremely deep, 0.28 deg^2 survey for z = 3.1 Ly-alpha emission-line galaxies in the Extended Chandra Deep Field South. By using a narrow-band 5000 Anstrom filter and complementary broadband photometry from the MUSYC survey, we identify a statistically complete sample of 162 galaxies with monochromatic fluxes brighter than 1.5 x 10^-17 ergs cm^-2 s^-1 and observers frame equivalent widths greater than 80 Angstroms. We show that the equivalent width distribution of these objects follows an exponential with a rest-frame scale length of w_0 = 76 +/- 10 Angstroms. In addition, we show that in the emission line, the luminosity function of Ly-alpha galaxies has a faint-end power-law slope of alpha = -1.49 +/- 0.4, a bright-end cutoff of log L^* = 42.64 +/- 0.2, and a space density above our detection thresholds of 1.46 +/- 0.12 x 10^-3 h70^3 galaxies Mpc^-3. Finally, by comparing the emission-line and continuum properties of the LAEs, we show that the star-formation rates derived from Ly-alpha are ~3 times lower than those inferred from the rest-frame UV continuum. We use this offset to deduce the existence of a small amount of internal extinction within the host galaxies. This extinction, coupled with the lack of extremely-high equivalent width emitters, argues that these galaxies are not primordial Pop III objects, though they are young and relatively chemically unevolved.