The infrared emission of ultraviolet-selected galaxies from z = 0 to z = 1

Aims. We want to study the IR (>8 μm) emission of galaxies selected on the basis of their rest-frame UV light in a very homogeneous way (wavelength and luminosity) from z = 0 to z = 1. We compare their UV and IR rest-frame emission to study the evolution in dust attenuation with z as well as to check if a UV selection is capable of tracking all star formation. This UV selection will also be compared to a sample of Lyman break galaxies selected at z ≃ 1. Methods. We select galaxies in UV (1500-1800 A) rest-frame at z = 0, z = 0.6-0.8, z = 0.8-1.2, and with as Lyman break galaxies at z = 0.9-1.3, the samples are compiled to sample the same range of luminosity at any redshift. The UV rest-frame data come from GALEX for z 0 sources. The evolution in the IR and UV luminosities with z is analysed for individual galaxies as well as in terms of luminosity functions. Results. The L I R/Lu v ratio is used to measure dust attenuation. This ratio does not seem to evolve significantly with z for the bulk of our sample galaxies, but some trends are found for both galaxies with a strong dust attenuation and UV luminous sources: galaxies with L IR/ L uv > 10 are more frequent at z > 0 than at z = 0, and the largest values of L IR /L UV are found for UV faint objects; in contrast, the most luminous galaxies of our samples (L UV > 2 x 10 10 L ⊙ ), detected at z = 1, exhibit a lower dust attenuation than fainter ones. The value of L IR /L UV increases with the K rest-frame luminosity of the galaxies at all redshifts considered and shows a residual anticorrelation with L u v. The most massive and UV luminous galaxies exhibit quite high specific star formation rates. Lyman break galaxies exhibit systematically lower dust attenuation than UV-selected galaxies of same luminosity, but similar specific star formation rates. The analysis of the UV + IR luminosity functions leads to the conclusion that up to z = 1, most of the star formation activity of UV-selected galaxies is emitted in IR. Although we are able to infer information about all the star formation from our UV selection at z = 0.7, at z = 1 we miss a large fraction of galaxies more luminous than ≃10 11 L ⊙ . The effect is found to be larger for Lyman break galaxies.

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