A decade of unchanged 1.3 CM VLBI structure of SGR A*

Details A decade of unchanged 1.3 CM VLBI structure of SGR A* A decade of unchanged 1.3 CM VLBI structure of SGR A*

Mar 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...343..801m&link_type=abstract

Astronomy and Astrophysics, v.343, p.801-805 (1999)

Astronomy and Astrophysics

Astrophysics

6

Galaxies: Jets, Galaxy: Center, Techniques: Interferometric

Scientific paper

We observed Sgr A* at 1.3 cm on 1992 November 8 with a 14 station VLBI array and, using data from 10 of these stations, obtained a high-dynamic range image with a beam of 3.35x1.7 milliarcseconds in position angle 14(deg) . The observed surface brightness distribution of Sgr A* is best modelled by an elliptically shaped gaussian component with parameter values: flux density 1.05+/- 0.10 Jy, major axis of FWHM 2.67+/- 0.15 milliarcseconds in position angle 79(deg) +/- 10(deg) , and axial ratio 0.61+/- 0.12, which are almost the same as the estimates of Alberdi {et al. } (1993). We found no evidence of changes in the source structure of Sgr A* among four sets of 1.3 cm VLBI observations spanning almost a decade. It seems reasonable to conclude that both the emission of Sgr A* itself and the surrounding medium acting as a refractive screen have reasonably constant relative orientation, emission rates and structures.

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