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Discovered in 1995 at the Caltech Submillimeter Observatory (CSO), thevibrationally-excited water maser line at 658 GHz (455 micron) is seen inoxygen-rich giant and supergiant stars. Because this maser can be so strong (upto thousands of Janskys), it was very helpful during the commissioning phase ofthe highest frequency band (620-700 GHz) of the Submillimeter Array (SMA)interferometer. From late 2002 to early 2006, brief attempts were made tosearch for emission from additional sources beyond the original CSO survey.These efforts have expanded the source count from 10 to 16. The maser emissionappears to be quite compact spatially, as expected from theoreticalconsiderations; thus these objects can potentially be used as atmospheric phasecalibrators. Many of these objects also exhibit maser emission in thevibrationally-excited SiO maser at 215 GHz. Because both maser lines likelyoriginate from a similar physical region, these objects can be used to testtechniques of phase transfer calibration between millimeter and submillimeterbands. The 658 GHz masers will be important beacons to assess the performanceof the Atacama Large Millimeter Array (ALMA) in this challenging high-frequencyband.

658 GHz Vibrationally-Excited Water Masers with the Submillimeter Array