论文标题
微型Quasars GRS 1758-258和1E 1740.7-2942附近的喷气主义互动
Jet-ISM Interactions near the Microquasars GRS 1758-258 and 1E 1740.7-2942
论文作者
论文摘要
我们提出了Atacama大型毫米/次毫米阵列观测值，该候选喷气式互动区域附近的黑洞X射线二进制区GRS 1758 $ - $ 258和1E 1740.7 $ - $ 2942。使用这些数据，我们绘制区域中的分子线排放，检测HCN [$ j = 1-0 $]，HCO $^+$ [$ J = 1-0 $]，SIO [$ J = 2-1 $]，CS [$ J = 2-1 $] [$ j = 4_ {0,4} -3_ {0,3} $]，hnco [$ j = 5_ {0,5} -4_ {0,4} $]和ch $ _3 $ oh [$ j = 2_ = 2_ {1,1,1} -1,1_ {1,0,0} $]分子过渡。通过检查这种发射的形态，光谱和运动学特性，我们确定了可能在这些系统周围气体中追踪喷气驱动腔的分子结构。我们的GRS 1758 $ - $ 258地区的结果与最近的工作一致，该工作假定该地区深度无线电连续图中存在喷气式茧结构。使用这些新发现的分子结构作为量热法，我们估计这些系统的时间平均时间，找到$（1.1-5.7）\ times10^{36} {\ rm erg \，s}^{ - 1} $超过$ 0.12-0.31 $ for GRS 1758 $ 258 $ 258 $ 258 $ 258 $ - 1} $ $（0.7-3.5）\ times10^{37} {\ rm erg \ \，s}^{ - 1} $超过$ 0.10-0.26 $ MYR，for 1e 1740.7 $ - $ 2942。此外，检测到的发射的光谱线特性将这些分子结构放在我们星系的中央分子区域中，从而将距离限制为黑洞X射线二进制文件为$ 8.0 \ pm1.0 $ kpc。总体而言，我们的分析巩固了分子线的诊断能力，并突出了Astro化学如何识别出射流X射线二进制文件的喷气主义相互作用区域和探测喷射反馈。
We present Atacama Large Millimeter/Sub-millimeter Array observations of the candidate jet-ISM interaction zones near the black hole X-ray binaries GRS 1758$-$258 and 1E 1740.7$-$2942. Using these data, we map the molecular line emission in the regions, detecting emission from the HCN [$J=1-0$], HCO$^+$ [$J=1-0$], SiO [$J=2-1$], CS [$J=2-1$], $^{13}$CO [$J=1-0$], C$^{18}$O [$J=1-0$], HNCO [$J=4_{0,4}-3_{0,3}$], HNCO [$J=5_{0,5}-4_{0,4}$], and CH$_3$OH [$J=2_{1,1}-1_{1,0}$] molecular transitions. Through examining the morphological, spectral, and kinematic properties of this emission, we identify molecular structures that may trace jet-driven cavities in the gas surrounding these systems. Our results from the GRS 1758$-$258 region in particular, are consistent with recent work, which postulated the presence of a jet-blown cocoon structure in deep radio continuum maps of the region. Using these newly discovered molecular structures as calorimeters, we estimate the time averaged jet power from these systems, finding $(1.1-5.7)\times10^{36}{\rm erg\,s}^{-1}$ over $0.12-0.31$ Myr for GRS 1758$-$258 and $(0.7-3.5)\times10^{37}{\rm erg\,s}^{-1}$ over $0.10-0.26$ Myr for 1E 1740.7$-$2942. Additionally, the spectral line characteristics of the detected emission place these molecular structures in the central molecular zone of our Galaxy, thereby constraining the distances to the black hole X-ray binaries to be $8.0\pm1.0$ kpc. Overall, our analysis solidifies the diagnostic capacity of molecular lines, and highlights how astro-chemistry can both identify jet-ISM interaction zones and probe jet feedback from Galactic X-ray binaries.
