Metallicities and kinematics of Lyman-alpha Galaxies at z=3.1

Details Metallicities and kinematics of Lyman-alpha Galaxies at z=3.1 Metallicities and kinematics of Lyman-alpha Galaxies at z=3.1

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010noao.prop..481r&link_type=abstract

NOAO Proposal ID #2010A-0481

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Scientific paper

We propose to measure the metallicities of z=3.1 Lyα emitting galaxies. Lyα emitters are the youngest class of high redshift galaxies, with typical ages of only 10^7 years and stellar masses of 10^7 - 10^9 Msun, even though their spatial clustering indicates halo masses of 10^11 Msun. By measuring the [OII], [OIII], and H(beta) line fluxes with NIRI, we will estimate metallicities for these galaxies for the first time ever. By doing so, we will (a) supply one of the missing pieces in understanding Lyα galaxies, whose stellar populations, masses of halos and ages have been constrained (b) pin down the low-mass end of the mass-metallicity relation at z=3, and (c) differentiate the kinematics of the resonantly scattered Lyα line from other nebular lines; e.g. [OII] and [OIII]. This will allow us to (d) distinguish scenarios where the Lyα escape is due to special kinematics from those where the galaxies are relatively dust- free. (e) We will cross-calibrate the star-formation rates derived from various emission lines. Finally, (f) we will determine the velocity offset between the resonantly scattered Lyα line and other lines. This is a critical parameter in determining how much of the blue wing of the Lyα line is absorbed by intergalactic gas. By establishing this quantity directly, we will lay a firm foundation for tests of reionization based on Lyα galaxy statistics at z > 6.

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