Program: GS-2021B-Q-125

The young stellar object [BHB2007]-01, is located near the dark molecular cloud Barnard 59 (the pit of the Pipe Nebula), at a distance of 163 pc from the Sun. Two recent investigations, one based on ALMA data and the other one on NIR VLT/NACO images, have revealed the presence of a companion object with a mass in the range 4-70 Mjup. This system appears to be an interesting case where both a star and a giant planet are growing in tandem. Although both investigations agree with relation to the companion object, they provide contradictory values for the mass of the central host star. While a Keplerian model fit to the CO emission from the disk (ALMA) provides for the embedded protostar a mass of 2.23 +/- 0.04 solar masses, the NIR data (VLT/NACO) suggest a value in the range 0.65-0.85 solar mass. A speculative solution for this disagreement could be that the central star is in reality an unresolved binary, each star with almost 1 solar mass. In order to investigate this mass discrepancy we propose to obtain high-resolution NIR spectra of the central source of [BHB2007]-01. These data will also be used to better characterize the central source.