We present results on a search for 86.243 GHz SiO (J = 2 -- 1, v = 1) maser emission toward 67 OH/IR stars located near the Galactic Centre. We detected 32 spectral peaks, of which 28 correspond to SiO maser lines arising from the envelopes of these OH/IR stars. In OH/IR stars, we obtained an SiO maser detection rate of about 40%. We serendipitously detected two other lines from OH/IR stars at 86.18 GHz, which could be due to a CCS-molecule transition at 86.181 GHz or probably to an highly excited OH molecular transition at 86.178 GHz. The detection rate of 86 GHz maser emission is found to be about 60% for sources with The Midcourse Space Experiment (MSX) A - E 2.5 mag. This supports the hypothesis by Messineo et al. (2002) that the SiO masers are primarily found in relatively thinner circumstellar material.

中文翻译：

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银河系中心 OH/IR 星中的 86 GHz SiO 脉泽

我们展示了对位于银河中心附近的 67 颗 OH/IR 恒星的 86.243 GHz SiO (J = 2 -- 1, v = 1) 脉泽发射的搜索结果。我们检测到 32 个光谱峰，其中 28 个对应于这些 OH/IR 恒星包层产生的 SiO 脉泽线。在 OH/IR 恒星中，我们获得了大约 40% 的 SiO 脉泽探测率。我们偶然在 86.18 GHz 处检测到来自 OH/IR 恒星的另外两条谱线，这可能是由于 86.181 GHz 处的 CCS 分子跃迁或可能是由于 86.178 GHz 处的高度激发的 OH 分子跃迁所致。中途空间实验 (MSX) A - E 2.5 mag 发现 86 GHz 脉泽发射的检测率约为 60%。这支持了 Messineo 等人的假设。(2002) 认为 SiO 脉泽主要存在于相对较薄的星周物质中。