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Nevertheless, several questions remain about the origin and evolution of these galaxies. In addition, the overall distribution of dust content, stellar population ages, and sizes have been determined at different cosmic epochs (Ferguson et al. These studies have made significant strides in characterizing various global statistics of the high-redshift galaxy population, including their UV luminosity function, stellar mass function, and clustering properties (e.g., Steidel et al. These systems are not expected in our sample: their presence implies that the frequency of such sources among our luminous z ≃ 3.7 LBGs may be an order of magnitude higher than in lower-redshift and lower-luminosity samples.ĭeep multi-wavelength space- and ground-based imaging surveys have enabled the identification and study of large numbers of high-redshift galaxies (e.g., Steidel et al. The latter may be a sign of a final stage of major merger, or clumpy disk formation. Finally, two galaxies each show two distinct sets of interstellar absorption features. In addition, we have discovered that five galaxies in the sample belong to a massive overdensity at z = 3.78.

Analyses of the composite spectra suggest that the UV luminous LBGs at z ≃ 3.7 may have a higher covering fraction of absorbing gas, and may be older (or have had more prolonged star formation histories) than their lower-redshift and lower-luminosity counterparts. The composite spectra are very similar to those of lower-redshift and lower-luminosity Lyman break galaxy (LBG) samples, but with some subtle differences.

We also stack the individual spectra to construct composite spectra of the absorption-line-only and Lyα-emitting subsets of the UV luminous galaxies at z ≃ 3.7. The luminosity- and mass-dependent outflow strengths suggest that the efficiency of feedback and enrichment of the surrounding medium depend on these galaxy parameters. We find tentative evidence that this measure of the outflow velocity increases with UV luminosity and/or stellar mass. Galaxies exhibiting both interstellar absorption and Lyα emission lines show a significant offset between the two features, with a relative velocity of 200–1150 km s −1. We find strong evidence of large-scale outflows, transporting the neutral/ionized gas in the interstellar medium away from the galaxy.

We present Keck DEIMOS spectroscopic observations of the most UV-luminous star-forming galaxies at redshifts 3.2 3 L*) exhibit strong Lyα emission.

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