Searching for candidate pre-brown dwarf with NIKA2
From molecular clouds to young stellar objects, every step in the evolution of young stars can be observed in the millimetric range. As part of the NIKA2 (Adam et al. 2018) Large Program GASTON (PI: Nicolas Peretto), we observed at 1.2mm and 2mm the Ophiuchus Molecular Cloud. The dual band capabilities of NIKA2 allow us to understand the properties of dust in star-forming regions, and their relationship with the objects they form, in this case, low-mass stars, under ten solar masses. In L1688, the main region of this cloud, Oph B-11, detected with interferometric observations, is a pre-brown dwarf i.e a prestellar core in the brown dwarf mass regime. Its final mass will not be important enough for the final star to burn hydrogen. The rationale for this part of the GASTON large program is to try to detect more of these kind of brown dwarf precursors to understand their environment and mechanisms of formation, with the unrivaled sensitivity of NIKA2. In this talk, I will explain the goals of the brown dwarf part of the GASTON Large Program and the scientific results already achieved with 10h on L1688 and L1689 each.