The circumestellar disk of the B0 protostar powering the HH 80-81 radio jet

Abstract

We present subarcsecond angular resolution observations carried out with the Submillimeter Array (SMA) at 880 $\mu$m centered at the B0-type protostar GGD27~MM1, the driving source of the parsec scale HH 80-81 jet. We constrain its polarized continuum emission to be $\lesssim 0.8\%$ at this wavelength. Its submm spectrum is dominated by sulfur-bearing species tracing a rotating disk--like structure (SO and SO${}_2$ isotopologues mainly), but also shows HCN-bearing and CH${}_3$OH lines, which trace the disk and the outflow cavity walls excavated by the HH 80-81 jet. The presence of many sulfurated lines could indicate the presence of shocked gas at the disk's centrifugal barrier or that MM1 is a hot core at an evolved stage. The resolved SO${}_2$ emission traces very well the disk kinematics and we fit the SMA observations using a thin-disk Keplerian model, which gives the inclination (47${}^{\circ }$), the inner ($\lesssim 170$ AU) and outer ($\sim 950-1300$~AU) radii and the disk's rotation velocity (3.4 km s${}^{-1}$ at a putative radius of 1700 AU). We roughly estimate a protostellar dynamical mass of 4-18\msun. MM2 and WMC cores show, comparatively, an almost empty spectra suggesting that they are associated with extended emission detected in previous low-angular resolution observations, and therefore indicating youth (MM2) or the presence of a less massive object (WMC).

arXiv comment11 pages, 8 figures. Accepted for publication in the Astrophysical Journal

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