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