We present VLT-ISAAC medium resolution spectroscopy of the HH34 and HH1 jets. Our aim is to derive the kinematics and the physical parameters and to study how they vary with jet velocity. We use several important diagnostic lines such as [FeII] 1.644um, 1.600um and H2 2.122um. In the inner jet region of HH34 we find that both the atomic and molecular gas present two components at high and low velocity. The [FeII] LVC in HH34 is detected up to large distances from the source (>1000 AU), at variance with TTauri jets. In H2 2.122um, the LVC and HVC are spatially separated. We detect, for the first time, the fainter red-shifted counterpart down to the central source. In HH1, we trace the jet down to ~1" from the VLA1 driving source: the kinematics of this inner region is again characterised by the presence of two velocity components, one blue-shifted and one red-shifted with respect to the source LSR velocity. In the inner HH34 jet region, ne increases with decreasing velocity. Up to ~10" from the driving source, and along the whole HH1 jet an opposite behaviour is observed instead, with ne increasing with velocity. In both jets the mass flux is carried mainly by the high-velocity gas. A comparison between the position velocity diagrams and derived electron densities with models for MHD jet launching mechanisms has been performed for HH34. While the kinematical characteristics of the line emission at the jet base can be, at least qualitatively, reproduced by both X-winds and disc-wind models, none of these models can explain the extent of the LVC and the dependence of electron density with velocity that we observe. It is possible that the LVC in HH34 represents gas not directly ejected in the jet but instead denser ambient gas entrained by the high velocity collimated jet.
Theoretical overview on high-energy emission in microquasars
微类星体喷流是粒子加速和同步辐射的场所。这种同步辐射已经被探测到来自不同空间尺度的喷流区域，对于现在工作的仪器来说，这些喷流区域看起来像是紧凑的射电核心，稍微分辨的射电喷流，或者（非常）扩展的结构。由于相对论粒子和密集的光子，磁场和物质场的存在，这些外流也是产生来自其中两个物体LS 5039和LS I +61 303的甚高能量（VHE）伽马射线的最佳候选者，并且可能对MQ核心发射的X射线做出重大贡献。此外，除了电磁辐射外，不同尺度的喷流还产生了一定量的轻子和强子宇宙射线（CR），这些天体中可能存在中微子产生的证据。能够产生大量不同波长的发射的喷流区域已经减少到喷流底部，喷流的尺度为系统轨道半长轴的大小，喷流中间尺度（解析的射电喷流）和喷流终止点。喷流的周围环境也可能是多波长发射的场所，也值得深入了解。我们专注于这些情况下，无论是强子或轻子，它似乎更合理的产生光子从无线电VHE和高能中微子。我们简要地评论以及MQ的相关性，可能的贡献者银河CR在GeV-PeV范围。
