通过LBT-LUCI在[ FeII ] 1.64 um中观察到的PDKEEPAAA流出
The HH34 outflow as seen in [FeII]1.64um by LBT-LUCI
摘要：
致密的原子喷流从年轻的恒星大量发射[FeII]红外线，这可以，因此，被用来跟踪嵌入的原恒星的直接环境。我们想研究在源HH 34 IRS的喷流中的明亮的[Fe II] 1.64 μ m线的形态，并将其与最常用的光学示踪剂[SII]进行比较。我们分析了一个1.64 μ m的窄带滤波图像获得的大双目望远镜（LBT）LUCI仪器，其中包括HH 34喷流和反喷流。应用点扩散函数（PSF）反卷积算法来提高空间分辨率，并使IR图像与同源的[SII] HST图像直接可比。从喷流、（弱）反喷流以及HH 34-S和HH 34-N弓形激波中都检测到了[Fe II]发射。去卷积图像使我们能够分辨出距离中心源约1 \arcsec的喷流结。[Fe II]发射的形态与[SII]发射的形态非常相似，并且[Fe II]和[SII]峰的相对位置根据先前从HST图像导出的自行测量而移位。[Fe Ⅱ]/[SII]排放比的分析表明，Fe气体丰度远低于太阳值高达90%的Fe亏损的内部喷流结。这证实了以前的研究结果，尘埃射流，冲击是不够有效的，以消除耐火材料从谷物。
英文摘要：
Dense atomic jets from young stars copiously emit in [FeII] IR lines, which can, therefore, be used to trace the immediate environments of embedded protostars. We want to investigate the morphology of the bright [FeII] 1.64um line in the jet of the source HH34 IRS and compare it with the most commonly used optical tracer [SII]. We analyse a 1.64um narrow-band filter image obtained with the Large Binocular Telescope (LBT) LUCI instrument, which covers the HH34 jet and counterjet. A Point Spread Function (PSF) deconvolution algorithm was applied to enhance spatial resolution and make the IR image directly comparable to a [SII] HST image of the same source. The [FeII] emission is detected from both the jet, the (weak) counter-jet, and from the HH34-S and HH34-N bow shocks. The deconvolved image allows us to resolve jet knots close to about 1\arcsec from the central source. The morphology of the [FeII] emission is remarkably similar to that of the [SII] emission, and the relative positions of [FeII] and [SII] peaks are shifted according to proper motion measurements, which were previously derived from HST images. An analysis of the [FeII]/[SII] emission ratio shows that Fe gas abundance is much lower than the solar value with up to 90% of Fe depletion in the inner jet knots. This confirms previous findings on dusty jets, where shocks are not efficient enough to remove refractory species from grains.
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