发表机构
Nagoya University; Gifu University; Institute for Advanced Study, Gifu University; National Astronomical Observatory of Japan, National Institutes of Natural Sciences; Institute for Advanced Research, Nagoya University; Western Sydney University（名古屋大学; 岐阜大学; 岐阜大学高等研究院; 日本国立天文台，国立自然科学研究所; 名古屋大学高等研究院; 西悉尼大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过ALMA观测发现大麦哲伦云的DEM L241/LMC P3存在微类星体驱动的冷分子CO喷流，为微类星体喷流塑造CO喷流提供了新证据，也为微类星体的发现开辟了新窗口。
AI 中文摘要
我们展示了ALMA对DEM L241/LMC P3的CO发射观测结果，DEM L241/LMC P3是由一个致密天体和一颗O型恒星组成的最亮γ射线双星。我们发现了一个单侧的类喷流CO结构，长度为8秒差距，宽度为1秒差距，同时还伴随另一个取向略有不同的较弱CO喷流候选体。该单侧CO喷流与LMC P3显著对齐，表明该喷流由LMC P3驱动。我们测定该CO喷流的动力学温度为33-60K，显著高于附近非喷流CO云的约15K，且未发现任何辐射热源。我们解释该高温是由γ射线双星驱动的微类星体喷流的激波加热所致，其中致密天体拥有由O型恒星风供给的吸积盘。该CO喷流与现有磁流体动力学模拟的预测结果相符，模拟显示CO喷流可由微类星体喷流与周围星际介质云的相互作用形成。这些结果为CO喷流是微类星体喷流塑造的特征提供了有力证据，支持LMC P3的质量吸积作为γ射线起源的观点。该结果表明，除了最近在银河系中发现的微类星体候选体HESS J1023-575中的CO喷流外，这是第二个可能由微类星体驱动的CO喷流案例。此外，我们的结果表明可利用亚毫米观测来识别微类星体，为其发现和研究开辟了新的可能窗口。
英文摘要
We present ALMA observations of DEML 241/LMC P3, the most luminous $γ$-ray binary consisting of a compact object and an O star, in CO emission. We have found an one-sided jet-like CO feature of 8 pc length and 1 pc width, which accompanies another weaker CO jet candidate with slightly different orientation. The one-sided CO jet exhibits striking alignment with LMC P3, suggesting that the jet was driven by LMC P3. We have determined kinetic temperature of the CO jet to be significantly high at 33$-$60 K as compared with $\sim$15 K in the nearby non-jet CO cloud whereas no radiative heat source is found. We interpret that the high temperatures are due to shock heating of a microquasar jet driven by the $γ$-ray binary, where the compact object has an accretion disk fed by the O star winds. The CO jet matches existing predictions from magneto-hydrodynamical simulations, which show that CO jet can form from the interaction of the microquasar jet and an ambient ISM cloud. These results provide strong evidence that CO jets are a signature sculptured by microquasar jets, lending support for mass accretion in LMC P3 as the $γ$-ray origin. The results suggest a second case of CO jets potentially driven by a microquasar along with the CO jets in the microquasar candidate HESS J1023-575 recently identified in the Milky Way. Further, our results suggest the use of sub-mm observations for identifying microquasars, opening a new possible window for their discovery and study.
CommentsAccepted for publication in ApJL
