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We report the PACS-100um/160um detections of a sample of 42 GALEX-selectedand FIR-detected Lyman break galaxies (LBGs) at z ~ 1 located in the COSMOSfield and analyze their ultra-violet (UV) to far-infrared (FIR) properties. Thedetection of these LBGs in the FIR indicates that they have a dust content highenough so that its emission can be directly detected. According to a spectralenergy distribution (SED) fitting with stellar population templates to theirUV-to-near-IR observed photometry, PACS-detected LBGs tend to be bigger, moremassive, dustier, redder in the UV continuum, and UV-brighter thanPACS-undetected LBGs. PACS-detected LBGs at z ~ 1 are mostly disk-like galaxiesand are located over the green-valley and red sequence of the color-magnitudediagram of galaxies at their redshift. By using their UV and IR emission, wefind that PACS-detected LBGs tend to be less dusty and have slightly highertotal star-formation rates (SFRs) than other PACS-detected UV-selected galaxieswithin their same redshift range. As a consequence of the selection effect dueto the depth of the FIR observations employed, all our PACS-detected LBGs areLIRGs. However, none of them are in the ULIRG regime, where the FIRobservations are complete. The finding of ULIRGs-LBGs at higher redshiftssuggests an evolution of the FIR emission of LBGs with cosmic time. In anIRX-$\beta$ diagram, PACS-detected LBGs at z ~ 1 tend to be located around therelation for local starburst similarly to other UV-selected PACS-detectedgalaxies at their same redshift. Consequently, the dust-correction factorsobtained with their UV continuum slope allow to determine their total SFR,unlike at higher redshifts. However, the dust attenuation derived from UV toNIR SED fitting overestimates the total SFR for most of our PACS-detected LBGsin age-dependent way: the overestimation factor is higher in younger galaxies.

Lyman break and UV-selected galaxies at z ~ 1: II. PACS-100um/160um FIR detections