  Lyman break galaxies (LBGs) represent one of the kinds of star-forming
galaxies that are found in the high-redshift universe. The detection of LBGs in
the FIR domain can provide very important clues on their dust attenuation and
total SFR, allowing a more detailed study than those performed so far. In this
work we explore the FIR emission of a sample of 16 LBGs at z ~ 3 in the
GOODS-North and GOODS-South fields that are individually detected in PACS-100um
or PACS-160um. These detections demonstrate the possibility of measuring the
dust emission of LBGs at high redshift. We find that PACS-detected LBGs at z ~
3 are highly obscured galaxies which belong to the Ultra luminous IR galaxies
or Hyper luminous IR galaxies class. Their total SFR cannot be recovered with
the dust attenuation factors obtained from their UV continuum slope or their
SED-derived dust attenuation employing Bruzual & Charlot (2003) templates. Both
methods underestimate the results for most of the galaxies. Comparing with a
sample of PACS-detected LBGs at z ~ 1 we find evidences that the FIR emission
of LBGs might have changed with redshift in the sense that the dustiest LBGs
found at z ~ 3 have more prominent FIR emission, are dustier for a given UV
slope, and have higher SFR for a given stellar mass than the dustiest LBGs
found at z ~ 1.
