Protoplanetary disks in the Orion Nebula Cluster: FUV radiation effects

Many stars are formed within stellar clusters, and for that reason, their disks evolve being affected by the radiation of neighbor stars. The study of cases like those, where the protoplanetary disk is not isolated and is embedded in regions with external factors that can change their chemical evolution, are important because they would constrain the protoplanetary disk evolution, and thus the planet formation. The aim of this research is to analyze the effects of external FUV radiation on disk chemistry. We present ALMA Band 6 observations of CO isotopologues, HCN, DCN, H2CO, C2H, and C3H2 at 0.12 angular resolution toward a survey of four protoplanetary disks located in the Orion Nebula Cluster, where the radiation field is dominated by the massive and young O-type star, ?¹ Ori. This analysis is possible because the sources are located at different distances from the star, receiving different amounts of FUV radiation, so we can quantify this effect. An additional feature of these disks is that the sources are still embedded in the parent molecular cloud, then the molecular line emission is more difficult to detect.