A Herschel View of Protoplanetary Disks in the σ Ori Cluster

We present new Herschel observations using the Photodetector Array Camera and Spectrometer of 32 T Tauri stars in the young (∼3 Myr) σ Ori cluster. Most of our objects are K and M stars with large excesses at 24 μm. We used irradiated accretion disk models of D’Alessio et al. to compare their spectral energy distributions with our observational data. We arrive at the following six conclusions. (I) The observed disks are consistent with irradiated accretion disk systems. (II) Most of our objects (60%) can be explained by significant dust depletion from the upper disk layers. (III) Similarly, 61% of our objects can be modeled with large disk sizes (R _d ≥ 100 au). (IV) The masses of our disks range between 0.03 and 39 M _Jup, where 35% of our objects have disk masses less than 1 M _Jup. Although these are lower limits, high-mass (>0.05 {M}_⊙ ) disks, which are present in, e.g., Taurus, are missing. (v) By assuming a uniform distribution of objects around the brightest stars at the center of the cluster, we found that 80% of our disks are exposed to external FUV radiation of 300≤slant {G}₀≤slant 1000, which can be strong enough to photoevaporate the outer edges of the closer disks. (VI) Within 0.6 pc from σ Ori we found forbidden emission lines of [N II] in the spectrum of one of our large disks (SO662), but no emission in any of our small ones. This suggests that this object may be an example of a photoevaporating disk.