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Circumstellar environments of oxygen-rich stars are among the strongest SiOmaser emitters. Physical processes such as collisions, infrared pumping andoverlaps favors the inversion of level population and produce maser emission atdifferent vibrational states. Despite numerous observational and theoreticalefforts, we still do not have an unified picture including all the physicalprocesses involved in the SiO maser emission. The aim of this work is toprovide homogeneous data in a large sample of oxygen-rich stars. We present asurvey of 67 oxygen-rich stars from 7 to 1 mm, in their rotational transitionsfrom J=1-0 to J=5-4, for vibrational numbers v from 0 to 6 in the three mainSiO isotopologues. We have used one of the 34 m NASA antennas at Robledo andthe IRAM 30 m radio telescope. The first tentative detection of a v=6 line isreported, as well as the detection of new maser lines. The highest vibrationallevels seem confined to small volumes, presumably close to the stars. TheJ=1-0, v=2 line flux is greater than the corresponding v=1 in almost half ofthe sample, which may confirm a predicted dependence on the pulsation cycle.This database is potentially useful in models which should consider most of thephysical agents, time dependency, and mass-loss rates. As by-product, we reportdetections of 27 thermal rotational lines from other molecules, includingisotopologues of SiS, H2S, SO, SO2, and NaCl.

SiO, 29SiO, and 30SiO emission from 67 oxygen-rich stars. A survey of 61 maser lines from 7 to 1 mm