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We observed the 43 GHz v=1, 2, and 3 and 86 GHz v=1 SiO maser transitionsquasi-simultaneously for a Mira-variable-dominated sample of over 80 sourcesfrom the Bulge Asymmetries and Dynamical Evolution (BAaDE) project, using ATCA,and statistically compared the relative line strengths. On average, the 43 GHzv=1 line is brighter than the 86 GHz v=1 line by a factor of 1.36+/-0.15. As aresult, an 86 GHz v=1 observed sample can be observed to 85.9% of the distanceof a 43 GHz v=1 observed sample using the same sensitivity. We discuss whatimpact this may have on the BAaDE Galactic plane survey using the VLA and ALMA.Despite fewer v=3 detections, specific trends are discerned or strengthenedwhen the 43 GHz v=3 line is detected. In particular the 43 and 86 GHz v=1 linesare on average equal for sources with no detectable 43 GHz v=3 emission, butthe 43 GHz v=1 line strength is on average about twice as bright as the 86 GHzv=1 line for sources with detectable 43 GHz v=3 emission. Some weakcorrelations are found between line strengths and Midcourse Space Experimentflux densities and colors, which are tightened when considering only sourceswith detectable 43 GHz v=3 emission. We discuss these trends in the context ofa radiative pumping model to highlight how the 43 GHz v=3 line, when coupledwith the v=1 and v=2 lines, can further our understanding of variableconditions like density in the circumstellar envelopes.

Quasi-simultaneous 43 and 86 GHz SiO Maser Observations and Potential Bias in the BAaDE Survey Are Resolved