Circumstellar environments of oxygen-rich stars are among the strongest SiO maser emitters. Physical processes such as collisions, infrared pumping, and overlaps favor the inversion of level population and produce maser emission at different vibrational states. Despite numerous observational and theoretical efforts, we still do not have a unified picture including all of the physical processes involved in 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 isotopologs. 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 a by-product, we report detections of 27 thermal rotational lines from other molecules, including isotopologs of SiS, H₂S, SO, SO₂, and NaCl.

富氧恒星的星周环境是最强的 SiO 脉泽发射体之一。碰撞、红外泵浦和重叠等物理过程有利于能级布居的反转，并在不同振动状态下产生脉泽发射。尽管进行了大量的观测和理论工作，我们仍然没有一个统一的图景，包括 SiO 脉泽发射所涉及的所有物理过程。这项工作的目的是提供大量富氧恒星样本的均匀数据。我们对 67 颗直径 7 到 1 毫米的富氧恒星进行了调查，它们的旋转跃迁从J = 1 → 0 到J = 5 → 4，三种主要 SiO 同位素中的振动数v从 0 到 6。我们使用了 Robledo 的 34 m NASA 天线之一和 IRAM 30 m 射电望远镜。报告了对v = 6 线的首次尝试性检测，以及对新微波激射线的检测。最高振动水平似乎仅限于小体积，大概靠近恒星。在几乎一半的样本中， J = 1 → 0, v = 2 线通量大于相应的v = 1，这可以证实对脉动周期的预测依赖性。该数据库在应考虑大多数物理因素、时间依赖性和质量损失率的模型中可能有用。作为副产品，我们报告检测到来自其他分子的 27 条热旋转线，包括 SiS、H ₂ S、SO、SO ₂和 NaCl 的同位素。