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We present results of far-infrared photometric observations with HerschelPACS of a sample of Upper Scorpius stars, with a detection rate of previouslyknown disk-bearing K and M stars at 70, 100, and 160 micron of 71%, 56%, and50%, respectively. We fit power-law disk models to the spectral energydistributions of K & M stars with infrared excesses, and have found that whilemany disks extend in to the sublimation radius, the dust has settled to lowerscale heights than in disks of the less evolved Taurus-Auriga population, andhave much reduced dust masses. We also conducted Herschel PACS observations forfar-infrared line emission and JCMT observations for millimeter CO lines. AmongB and A stars, 0 of 5 debris disk hosts exhibit gas line emission, and among Kand M stars, only 2 of 14 dusty disk hosts are detected. The OI 63 micron andCII 157 micron lines are detected toward [PZ99] J160421.7-213028 and [PBB2002]J161420.3-190648, which were found in millimeter photometry to host two of themost massive dust disks remaining in the region. Comparison of the OI lineemission and 63 micron continuum to that of Taurus sources suggests theemission in the former source is dominated by the disk, while in the otherthere is a significant contribution from a jet. The low dust masses found bydisk modeling and low number of gas line detections suggest that few stars inUpper Scorpius retain sufficient quantities of material for giant planetformation. By the age of Upper Scorpius, giant planet formation is essentiallycomplete.

A Herschel PACS survey of the dust and gas in Upper Scorpius disks