Dust properties of Lyman-break galaxies at

Context. Since the mid-1990s, the sample of Lyman-break galaxies (LBGs) has been growing thanks to the increasing sensitivities in the optical and in near-infrared telescopes for objects at z> 2.5. However, the dust properties of the LBGs are poorly known because the samples are small and/or biased against far-infrared (far-IR) or submillimeter (submm) observations. Aims. This work explores from a statistical point of view the far-IR and submm properties of a large sample of LBGs at z ~ 3 that cannot be individually detected from current far-IR observations. Methods. We select a sample of 22, 000 LBGs at 2.5 <z< 3.5 in the COSMOS field using the dropout technique. The large number of galaxies included in the sample allows us to split it into several bins as a function of UV luminosity (LFUV), UV continuum slope (βUV), and stellar mass (M∗) to better sample their variety. We stack in PACS (100 and 160 μm) images from PACS Evolution Probe survey (PEP), SPIRE (250, 350 and 500 μm) images from the Herschel Multi-tied Extragalactic Survey (HerMES) programs, and AzTEC (1.1 mm) images from the Atacama Submillimeter Telescope Experiment (ASTE). Our stacking procedure corrects the biases induced by galaxy clustering and incompleteness of our input catalogue in dense regions. Results. We obtain the full infrared spectral energy distributions (SED) of subsamples of LBGs and derive the mean IR luminosity as a function of LFUV, βUV, and M∗. The average IRX (or dust attenuation) is roughly constant over the LFUV range, with a mean of 7.9 (1.8 mag). However, it is correlated with βUV, AFUV = (3.15 ± 0.12) + (1.47 ± 0.14) βUV, and stellar mass, log (IRX) = (0.84 ± 0.11)log (M∗/ 1010.35) + 1.17 ± 0.05. We investigate using a statistically controlled stacking analysis as a function of (M∗, βUV), the dispersion of the IRX-βUV and IRX-M∗ plane. On the one hand, the dust attenuation shows a departure of up to 2.8 mag above the mean IRX-βUV relation when log (M∗ [ M⊙ ]) increases from 9.75 to 11.5 in the same βUV bin. This strongly suggests that M∗ plays an important role in shaping the IRX-βUV plane. On the other hand, the IRX-M∗ plane is less dispersed for variation in the βUV. However, the dust attenuation shows a departure of up to 1.3 mag above the mean IRX-M∗ relation, when βUV increases from −1.7 to 0.5 in the same M∗ bin. The low stellar mass LBGs (log (M∗ [ M⊙ ] ) −0.7), 15% of the total sample, present a high dust attenuation than the mean IRX-M∗, but they are still in agreement with the mean IRX-βUV relation. We suggest that we have to combine both the IRX-βUV and IRX-M∗ relations to obtain the best estimation of the dust attenuation from the UV and NIR properties of the galaxies (LFUV, βUV, M∗). Our results enable us to study the average relation between star formation rate (SFR) and stellar mass, and we show that our LBG sample lies on the main sequence of star formation at z ~ 3. we demonstrate that the SFR is underestimate for LBGs with high stellar mass, but it give a good estimation for LBGs with lower stellar mass when we calculate the SFR by correcting the LFUV using the IRX-βUV relation