The Search for New Mira Stars Through H2O Maser Emission

Details The Search for New Mira Stars Through H2O Maser Emission The Search for New Mira Stars Through H2O Maser Emission

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...19915505l&link_type=abstract

American Astronomical Society, 199th AAS Meeting, #155.05; Bulletin of the American Astronomical Society, Vol. 34, p.562

Astronomy and Astrophysics

Astronomy

Scientific paper

It is known that Mira stars at the late stages of evolution, when they actively loose mass and create optically thick gas/dust envelopes, become detectable sources of maser emission in the microwave lines of OH, H2O, and SiO. Considering masing in the 1.35cm H2O line as a distnguishing feature of old Miras, we used the MIT Haystack 37m radio telescope for confirmation of preliminary Mira classification ascribed recently to several stars based on their optical variability. Published infrared characteristics of the stars were used to narrow the list of probable H2O emittors. After 1-4 hours of integration, none of the candidate stars showed signs of H2O emission exceeding the noise level of +/-.4 Jy, within the bandwidth of 17.8 MHz (240 km/s). We discuss the implications of this result. This project was supported by the NSF/REU grant AST-9820555 and the Nantucket Maria Mitchell Association.

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