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We make use of deep 1.2mm-continuum observations (12.7microJy/beam RMS) of a1 arcmin^2 region in the Hubble Ultra Deep Field to probe dust-enshrouded starformation from 330 Lyman-break galaxies spanning the redshift range z=2-10 (to~2-3 Msol/yr at 1sigma over the entire range). Given the depth and area ofASPECS, we would expect to tentatively detect 35 galaxies extrapolating theMeurer z~0 IRX-beta relation to z>~2 (assuming T_d~35 K). However, only 6tentative detections are found at z>~2 in ASPECS, with just three at >3sigma.Subdividing z=2-10 galaxies according to stellar mass, UV luminosity, andUV-continuum slope and stacking the results, we only find a significantdetection in the most massive (>10^9.75 Msol) subsample, with an infraredexcess (IRX=L_{IR}/L_{UV}) consistent with previous z~2 results. However, theinfrared excess we measure from our large selection of sub-L* (<10^9.75 Msol)galaxies is 0.11(-0.42)(+0.32) and 0.14(-0.14)(+0.15) at z=2-3 and z=4-10,respectively, lying below even an SMC IRX-beta relation (95% confidence). Theseresults demonstrate the relevance of stellar mass for predicting the IRluminosity of z>~2 galaxies. We furthermore find that the evolution of theIRX-stellar mass relationship depends on the evolution of the dust temperature.If the dust temperature increases monotonically with redshift (as (1+z)^0.32)such that T_d~44-50 K at z>=4, current results are suggestive of littleevolution in this relationship to z~6. We use these results to revisit recentestimates of the z>~3 SFR density. One less obvious implication is ininterpreting the high Halpha EWs seen in z~5 galaxies: our results imply thatstar-forming galaxies produce Lyman-continuum photons at twice the efficiency(per unit UV luminosity) as implied in conventional models. Star-forminggalaxies can then reionize the Universe, even if the escape fraction is <10%.

astrophysical journal/the astrophysical journal

ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: The Infrared  Excess of UV-selected z=2-10 galaxies as a function of UV-continuum Slope and  Stellar Mass