A SUBMILLIMETER ARRAY SURVEY OF PROTOPLANETARY DISKS IN THE ORION NEBULA CLUSTER

Abstract

We present the full results of our 3-year long Submillimeter Array survey of protoplanetary disks in the Orion Nebula Cluster. We imaged 23 fields at 880 microns and 2 fields at 1330 microns, covering an area of ~6.5 arcmin^2 and containing 67 disks. We detected 42 disks with fluxes between 6-135 mJy and at rms noise levels between 0.6 to 5.3 mJy/beam. Thermal dust emission above any free-free component was measured in 40 of the 42 detections, and the inferred disk masses range from 0.003-0.07 Msolar. We find that disks located within 0.3 pc of theta^1 Ori C have a truncated mass distribution, while disks located beyond 0.3 pc have masses more comparable to those found in low-mass star forming regions. The disk mass distribution in Orion has a distance dependence, with a derived relationship max(M_(disk)) = 0.046Msolar(d/0.3pc)^0.33 for the maximum disk masses. We found evidence of grain growth in disk 197-427, the only disk detected at both 880 microns and 1330 microns with the SMA. Despite the rapid erosion of the outer parts of the Orion disks by photoevaporation, the potential for planet formation remains high in this massive star forming region, with approximately 18% of the surveyed disks having masses greater than or equal to 0.01 Msolar within 60 AU.