ALMA survey of Lupus class III stars: Early planetesimal belt formation and rapid disk dispersal

Class III stars are those in star forming regions without large non-photospheric infrared emission, suggesting recent dispersal of their protoplanetary discs. We observed 30 class III stars in the 1-3 Myr Lupus region with ALMA at similar to 856 mu m, resulting in four detections that we attribute to circumstellar dust. Inferred dust masses are 0.036-0.093M(circle plus), similar to 1 order of magnitude lower than any previous measurements; one disc is resolved with radius similar to 80 au. Two class II sources in the field of view were also detected, and 11 other sources, consistent with sub-mm galaxy number counts. Stacking non-detections yields a marginal detection with mean dust mass similar to 0.0048M(circle plus). We searched for gas emission from the CO J = 3-2 line, and present its detection to NO Lup inferring a gas mass (4.9 +/- 1.1) x 10(-5) M-circle plus and gas-to-dust ratio 1.0 +/- 0.4. Combining our survey with class II sources shows a gap in the disc mass distribution from 0.09-2M(circle plus) for >0.7 M-circle plus Lupus stars, evidence of rapid dispersal of mm-sized dust from protoplanetary discs. The class III disc mass distribution is consistent with a population model of planetesimal belts that go on to replenish the debris discs seen around main sequence stars. This suggests that planetesimal belt formation does not require long-lived protoplanetary discs, i.e. planetesimals form within similar to 2 Myr. While all four class III discs are consistent with collisional replenishment, for two the gas and/or mid-IR emission could indicate primordial circumstellar material in the final stages of protoplanetary disc dispersal. Two class III stars without sub-mm detections exhibit hot emission that could arise from ongoing planet formation processes inside similar to 1 au.