We observe ten known 22GHz H2O maser galaxies during February 19–22, 2011 using the 21 m Tamna telescope of the Korean VLBI Network and a new wide-band digital spectrometer. Simultaneously we searched for 43GHz SiO v = 1, 2, J = 1–0 maser emission. We detect H2O maser emission towards five sources (M 33, NGC 1052, NGC 1068, NGC 4258, M 82), with non-detections towards the remaining sources (UGC 3193, UGC 3789, Antennae H2O-West, M 51, NGC 6323) likely due to sensitivity. Our 22GHz spectra are consistent with earlier findings. Our simultaneous 43GHz SiO maser search produced non-detections, yielding – for the first time – upper limits on the 43GHz SiO maser emission in these sources at a 3  sensitivity level of 0.018K–0.033K (0.24 Jy–0.44 Jy) in a 1.75 km s−1 velocity resolution. Our findings suggest that any 43GHz SiO masers in these sources (some having starburst-associated H2O kilomasers) must be faint compared to the 22GHz H2O maser emission.

Abstract
1. INTRODUCTION
2. SOURCE SELECTION AND OBSERVATIONS
3. OBSERVATIONAL RESULTS AND DISCUSSION
    3.1. Comments on Three Individual Sources
    3.2. Operation and Performance ofWide-Band DigitalSpectrometer
4. SUMMARY
REFERENCES

• Se-Hyung Cho(Radio Astronomy Division, Korea Astronomy and Space Science Institute) Corresponding author
• Dong-Hwan Yoon(Radio Astronomy Division, Korea Astronomy and Space Science Institute)
• Jaeheon Kim(Radio Astronomy Division, Korea Astronomy and Space Science Institute)
• Do-Young Byun(Radio Astronomy Division, Korea Astronomy and Space Science Institute)
• Jan Wagner(Radio Astronomy Division, Korea Astronomy and Space Science Institute)