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S.S. Doeleman, R.B. Phillips, A.E.E. Rogers, J.M. Attridge, M.A. Titus, D.L. Smythe, R.J. Cappallo, T.A. Buretta, A.R. Whitney (MIT Haystack Observatory), T Krichbaum, D.A. Graham, W. Alef, A. Polatidis, U. Bach, A. Witzel, J.A. Zensus (MPIfR-Bonn), A. Greve, M. Grewing (IRAM), R. Freund (NRAO), P. Strittmatter, L. Ziurys, T. Wilson, H. Fagg (Steward Observatory)
In April 2002 an array of antennas operating at 129GHz successfully detected VLBI fringes on both continuum AGN and SiO spectral line sources. The 129GHz fringes on maser sources represent the highest frequency spectral line VLBI detections to date. The AGN 3C279 was detected on long baselines at both 129GHz (and at 147GHz) yielding fringe spacings of 50-56 micro arc seconds, an angular resolution record. The array consisted of the Kitt Peak 12m antenna and the Heinrich Hertz 10m Telescope (HHT), both operatedby the Arizona Radio Observatory, and the IRAM 30m dish on Pico Veleta (Spain).
At 129GHz, a number of evolved stars and several young stellar objects exhibit strong SiO maser emission in the v=1 J=3-2 transition. We present maps of the v=1 J=3-2 maser emission towards the hypergiant VYCMa and discuss the relation of the maser features to the optical asymmetric nebula surrounding the star.
Future high frequency VLBI using these telescopes will include continuum observations of the radio source at the Galactic Center, SgrA*, and higher frequency maser lines including HCN and methanol.
The author(s) of this abstract have provided an email address for comments about the abstract: dole@haystack.mit.edu
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Bulletin of the American Astronomical Society, 34, #4
© 2002. The American Astronomical Soceity.