High Mass Star Formation Studied through IRDCs

One of the open questions in stellar astrophysics is the formation of massive young stars. Two models best explain how massive protostars grow: the turbulent core and the competitive accretion models. However, the fast timescale of these objects and the distance of the massive protostar formation regions make it difficult to find them and get observational constraints that favor one or another model. In this context, the Infra-Red Dark Clouds (IRDC) are crucial sources for understanding the process. The IRDCs are composed of many cores of dust condensations and low-temperature dense gas, named dark because they appear as dark compared to the galactic Infrared background emission. We have explored the ALMA archive by searching for molecular emissions in clumps of the IRDCs. We found molecular emission in some of those clumps, indicating the existence of a protostar. We also discussed the existence of outflows.