VLBI Imaging of the 86 GHz SiO Maser Emission in the Circumstellar Envelope of VX Sagittarii

Details VLBI Imaging of the 86 GHz SiO Maser Emission in the Circumstellar Envelope of VX Sagittarii VLBI Imaging of the 86 GHz SiO Maser Emission in the Circumstellar Envelope of VX Sagittarii

Feb 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...494..400d&link_type=abstract

Astrophysical Journal v.494, p.400

Astronomy and Astrophysics

Astronomy

25

Stars: Circumstellar Matter, Masers, Radio Lines: Stars, Stars: Individual Constellation Name: Vx Sagittarii

Scientific paper

We have observed and imaged the SiO maser source in the late-type star VX Sgr with a single VLBI baseline at 3.5 mm wavelength. Phase-referenced channel maps with a beamwidth of ~0.4 mas show multiple components over a LSR velocity range of -1 to 24 km s-1, and many of the maser features display velocity widths smaller than 1 km s-1. The maser spots in this 86 GHz transition (v = 1, J = 2 --> 1) are arranged in an irregular ring-shaped configuration of diameter ~30 mas, echoing the structures found in the J = 1 --> 0 transition at 43 GHz around several Mira variables and VX Sgr itself. Unlike previous observations of SiO masers, in VX Sgr we detect a clear, systematic velocity gradient of ~0.6 km s-1 AU-1 among the strongest complex of masers on the southernmost portion of the ring structure. This velocity gradient can be interpreted as a rigid rotation of the circumstellar envelope with v sin i ~ 13 km s-1. Maser emission is not detected on long (5000 km) baselines, which places a 0.1 mas lower limit on the size of strong maser spots.

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