Description
Among the different observational techniques used to select high-redshift galaxies, the hydrogen recombination line Lyman-alpha (Ly{alpha}) is of particular interest because it gives access to the measurement of cosmological quantities such as the star formation rate (SFR) of distant galaxy populations. However, interpreting this line and calibrating such observables are still subject to serious uncertainties. In this context, it important to understand the mechanisms responsible for the attenuation of Ly{alpha} emission, and under what conditions the Ly{alpha} emission line can be used as a reliable star formation diagnostic tool. We used a sample of 24 Ly{alpha} emitters at z~0.3 with an optical spectroscopic follow-up to calculate the Ly{alpha} escape fraction and its dependence upon different physical properties. We also examined the reliability of Ly{alpha} as a SFR indicator. We combined these observations with a compilation of Ly{alpha} emitters selected at z=0-0.3 from the literature to assemble a larger sample.
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