Abstract
The results of a VLBI observation between Kashima 34 m and Nobeyama 45 m are presented. Water maser at 22.235 GHz and SiO masers at 43 GHz in some late type stars are mapped almost simultaneously. Data reduction is still on the way, then we report mainly for the blocking model of H 2 O maser.
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CITATION STYLE
APA
Takaba, H., Iwata, T., Miyoshi, M., Ukita, N., Kameno, S., & Matumoto, K. (1994). VLBI Observations of H 2 O and SiO Masers in Late Type Stars. International Astronomical Union Colloquium, 140, 62–63. https://doi.org/10.1017/s0252921100019138
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