The formation of stars has been subject to extensive studies in the past decades from molecular cloud to protoplanetary disk scales. It is still not fully understood how the surrounding material in a protostellar system, that often shows asymmetric structures with complex kinematic properties, is delivered onto the disk and how this may shape the properties of the protostar and disk. We...
The process of star and disk formation is known to involve interactions with the surrounding environment. Recent observations have revealed evidence of several young, embedded objects showing elongated, asymmetric infall. We refer to these features as streamers when they appear unconnected to the parental dense core. Such streamers can deliver substantial mass and angular momentum, potentially...
An open problem in planet formation theory is the growth of dust grains from centimetre to metre sizes. The streaming instability has been proposed as a mechanism to overcome barriers in dust grain growth; however, it is only triggered in regions of sufficiently high dust to gas ratio. We therefore require protoplanetary discs to contain substructures where dust grains can collide and...
Ophiuchus is one of the closest and youngest star-forming regions to our planet, making it a perfect laboratory to study star and planet formation. The Ophiuchus DIsk Survey Employing ALMA (ODISEA) originally targeted ~300 YSOs at different stages of evolution (from SED Class I to III) in Band-6 and at modest resolution. After several follow up programs, there are now observations on multiple...
