Recent work suggests that many luminous blue variables (LBVs) and B[e] supergiants (sgB[e]) are isolated, implying that they may be products of massive binaries, kicked by partner supernovae. However, the evidence is somewhat complex and controversial. To test this scenario, we measure the proper-motion velocities for these objects in the LMC and SMC, using Gaia Data Release 3. Our LMC results show that the kinematics, luminosities, and IR properties point to LBVs and sgB[e] stars being distinct classes. We find that Class 1 LBVs, which have dusty nebulae, and sgB[e] stars both show velocity distributions comparable to that of SMC field OBe stars, which are known to have experienced SN kicks. The sgB[e] stars are faster, plausibly due to their lower average masses. However, Class 2 LBVs, which are luminous objects without dusty nebulae, show no signs of acceleration, therefore suggesting that they are single stars, pre-SN binaries, or perhaps binary mergers. The candidate LBV Class 3 stars, which are dominated by hot dust, are all confirmed sgB[e] stars; their luminosities and velocities show that they simply represent the most luminous and massive of the sgB[e] class. There are very few SMC objects, but the sgB[e] stars are faster than their LMC counterparts, which may be consistent with expectations that lower-metallicity binaries are tighter, causing faster ejections. We also examine the distinct class of dust-free, weak-lined sgB[e] stars, finding that the SMC objects have the fastest velocities of the entire sample.

中文翻译：

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对发光蓝色变星和 B[e] 超巨星的运动学见解


最近的研究表明，许多发光蓝色变星 （LBV） 和 B[e] 超巨星 （sgB[e]） 是孤立的，这意味着它们可能是由伙伴超新星踢出的大质量双星的产物。然而，证据有些复杂和有争议。为了测试这种情况，我们使用 Gaia Data Release 3 测量了 LMC 和 SMC 中这些物体的适当运动速度。我们的 LMC 结果表明，运动学、光度和 IR 特性表明 LBV 和 sgB[e] 星是不同的类别。我们发现，具有尘埃状星云的 1 类 LBV 和 sgB[e] 星都显示出与 SMC 场 OBe 星相当的速度分布，众所周知，SMC 场 OBe 星经历了 SN 踢。sgB[e] 星的速度更快，这似乎是由于它们的平均质量较低。然而，2 类 LBV 是没有尘埃星云的发光天体，没有加速的迹象，因此表明它们是单星、前 SN 双星，或者可能是双星合并。以热尘埃为主的候选LBV 3类恒星都是已确认的sgB[e]星;它们的光度和速度表明它们只是代表了 sgB[e] 类中最亮和最重的。SMC 天体很少，但 sgB[e] 星比它们的 LMC 对应星更快，这可能与预期一致，即低金属度双星更紧密，导致更快的抛射。我们还检查了不同类别的无尘、弱线 sgB[e] 恒星，发现 SMC 天体在整个样本中具有最快的速度。