[en] We explore the relationship between the spectral shape of the Lyα emission and the UV morphology of the host galaxy using a sample of 304 Lyα-emitting BVi-dropouts at 3 < z < 7 in the Great Observatories Origins Deep Survey and Cosmic Evolution Survey fields. Using our extensive reservoir of high-quality Keck DEIMOS spectra combined with Hubble Space Telescope WFC3 data, we measure the Lyα line asymmetries for individual galaxies and compare them to axial ratios measured from observed J- and H-band (restframe UV) images. We find that the Lyα skewness exhibits a large scatter at small elongation (a/b < 2), and this scatter decreases as the axial ratio increases. Comparison of this trend to radiative transfer models and various results from the literature suggests that these high-redshift Lyα emitters are not likely to be intrinsically round and symmetric disks, but they probably host galactic outflows traced by Lyα emitting clouds. The ionizing sources are centrally located, and the optical depth is a good indicator of the absorption and scattering events on the escape path of Lyα photons from the source. Our results find no evidence of evolution in Lyα asymmetry or axial ratio with look-back time

[en] Luminous (LIRGs; log (L_IR/L_☉) = 11.00-11.99) and ultraluminous infrared galaxies (ULIRGs; log (L_IR/L_☉) = 12.00-12.99) are the most extreme star-forming galaxies in the universe. The local (U)LIRGs provide a unique opportunity to study their multi-wavelength properties in detail for comparison with their more numerous counterparts at high redshifts. We present common large aperture photometry at radio through X-ray wavelengths and spectral energy distributions (SEDs) for a sample of 53 nearby (z < 0.083) LIRGs and 11 ULIRGs spanning log (L_IR/L_☉) = 11.14-12.57 from the flux-limited (f_60μm > 5.24 Jy) Great Observatories All-sky LIRG Survey. The SEDs for all objects are similar in that they show a broad, thermal stellar peak (∼0.3-2 μm), and a dominant FIR (∼40-200 μm) thermal dust peak, where νL_ν(60 μm)/νL_ν(V) increases from ∼2 to 30 with increasing L_IR. When normalized at IRAS 60 μm, the largest range in the luminosity ratio, R(λ) ≡ log[νL_ν(λ)/νL_ν(60 μm)], observed over the full sample is seen in the hard X-rays (HX = 2-10 keV), where ΔR_HX = 3.73 (R-bar_HX= -3.10). A small range is found in the radio (1.4 GHz), ΔR_1.4GHz = 1.75, where the mean ratio is largest, (R-bar_1.4GHz= -5.81). Total infrared luminosities, L_IR(8-1000 μm), dust temperatures, and dust masses were computed from fitting thermal dust emission modified blackbodies to the mid-infrared (MIR) through submillimeter SEDs. The new results reflect an overall ∼0.02 dex lower luminosity than the original IRAS values. Total stellar masses were computed by fitting stellar population synthesis models to the observed near-infrared (NIR) through ultraviolet (UV) SEDs. Mean stellar masses are found to be log (M_*/M_☉) = 10.79 ± 0.40. Star formation rates have been determined from the infrared (SFR_IR ∼ 45 M_☉ yr^–1) and from the monochromatic UV luminosities (SFR_UV ∼ 1.3 M_☉ yr^–1), respectively. Multi-wavelength active galactic nucleus (AGN) indicators have be used to select putative AGNs: About 60% of the ULIRGs would have been classified as an AGN by at least one of the selection criteria.