VLBA imaging of the 3mm SiO maser emission in the disk-wind from the massive protostellar system Orion Source I

TL;DR

This paper presents high-resolution VLBA images of 3mm SiO masers in Orion Source I, revealing their spatial distribution, velocity structure, and relation to the disk-wind, providing insights into the physical conditions and dynamics of the massive protostellar system.

Contribution

First high-resolution imaging of 3mm SiO masers in Orion Source I, linking their spatial and velocity structure to the disk-wind and protostellar rotation.

Findings

3mm masers form an X-shaped structure around Source I.

Spatial offset between 3mm and 7mm masers suggests different physical conditions.

Masers trace a wide-angle outflow with Keplerian rotation.

Abstract

We present the first images of the 28SiO v=1, J=2-1 maser emission around the closest known massive young stellar object Orion Source I observed at 86 GHz (3mm) with the VLBA. These images have high spatial (~0.3 mas) and spectral (~0.054 km/s) resolutions. We find that the 3mm masers lie in an X-shaped locus consisting of four arms, with blue-shifted emission in the south and east arms and red-shifted emission in the north and west arms. Comparisons with previous images of the 28SiO v=1,2, J=1-0 transitions at 7mm (observed in 2001-2002) show that the bulk of the J=2-1 transition emission follows the streamlines of the J=1-0 emission and exhibits an overall velocity gradient consistent with the gradient at 7mm. While there is spatial overlap between the 3mm and 7mm transitions, the 3mm emission, on average, lies at larger projected distances from Source I (~44 AU compared with ~35 AU for 7mm). The spatial overlap between the v=1, J=1-0 and J=2-1 transitions is suggestive of a range of temperatures and densities where physical conditions are favorable for both transitions of a same vibrational state. However, the observed spatial offset between the bulk of emission at 3mm and 7mm possibly indicates different ranges of temperatures and densities for optimal excitation of the masers. We discuss different maser pumping models that may explain the observed offset. We interpret the 3mm and 7mm masers as being part of a single wide-angle outflow arising from the surface of an edge-on disk rotating about a northeast-southwest axis, with a continuous velocity gradient indicative of differential rotation consistent with a Keplerian profile in a high-mass proto-binary.