Protoplanetary disks around young stellar and substellar objects in the \({\sigma }\) Orionis cluster

Understanding the evolution and dissipation of protoplanetary disks are crucial in star and planet formation studies. We report the protoplanetary disk population in the nearby young \(\sigma \) Orionis cluster (\(d\sim 408\) pc; \(\textrm{age}\sim 1.8\) Myr) and analyse the disk properties, such as dependence on stellar mass and disk evolution. We utilize the comprehensive census of 170 spectroscopic members of the region refined using astrometry from Gaia DR3 for a wide mass range of \(\sim \)19–0.004 \(M_\odot \). Using the near-infrared (2MASS) and mid-infrared (WISE) photometries, we classify the sources based on the spectral index, into class I, class II, flat spectrum and class III young stellar objects. The frequency of sources hosting a disk with stellar mass <2 \(M_\odot \) in this region is \(41\pm 7\)%, which is consistent with the disk fraction estimated in previous studies. We see that there is no significant dependence of disk fraction on stellar mass among T Tauri stars (<2 \(M_\odot \)), but we propose rapid disk depletion around higher mass stars (>2 \(M_\odot \)). Furthermore, we found the lowest mass of a disk-bearing object to be \(\sim \)20 \(M_{\textrm{Jup}}\) and the pronounced disk-fraction among the brown dwarf population hints at the formation scenario that brown dwarfs form similar to low-mass stars.