BROAD BAND INFRARED SPECTROSCOPY OF MASSIVE YOUNG STELLAR OBJECTS
BROAD BAND INFRARED SPECTROSCOPY OF MASSIVE YOUNG STELLAR OBJECTS
复制标题
大质量年轻恒星物体的宽带红外光谱
DOI：
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发表时间：
1998
期刊：
影响因子：
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通讯作者：
S. Lumsden
中科院分区：
文献类型：
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作者：
J. Porter;J. Drew;S. Lumsden
我们给出了12颗高度红化恒星的0.9-2.5 μm中等分辨率红外光谱，其中包括一些已知的和一些不熟悉的来源。采用了一种从标准星星数据中提取定标曲线的新方法，并取得了很好的效果。对每个物体的红化进行了充分的讨论，并从连续谱（分为短波长区λλ < 1.5μm和长波长区λλ > 1.5μm）和Hi线计算。我们发现，通常情况下，有来自H i线和短波长连续的值之间的一致性，但不是从长波长连续的值。这种差异是由于在λλ <$1.5 μm处的红外过量，这与热尘埃的发射一致（我们推导出尘埃温度在750- 1500 K范围内）。我们注意到，我们的一些源具有高度不一致的帕邢递减，并且对于λλ < 1.5μm可能具有大量的散射光。光谱显示了各种金属发射线和一些证据，在同一个源不同的发射区域。源之间的谱线到连续谱对比度范围很大，在以前进行观测的地方，有证据表明某些源的发射谱线强度存在变异性。
We present intermediate resolution 0.9–2.5 μm IR spectra of 12 highly reddened stars, including some well known and some unfamiliar sources. A new technique for extracting calibration curves from standard star data is employed, and is found to be very successful. The reddening to each object is fully discussed and is calculated from both the continua (which was split into shortand long-wavelength regions λλ < 1.5μm andλλ > 1.5μm ) and the Hi lines. We find that, typically, there is consistency between the values derived from the H i lines and the short-wavelength continua, but not with the value from the long-wavelength continua. This discrepancy is due to an IR excess at λλ ∼ 1.5μm , which is consistent with emission from hot dust (we derive dust temperatures in the range 750–1500K). We note that some of our sources have highly discrepant Paschen decrements, and may have a significant amount of scattered light forλλ < 1.5μm . The spectra show a variety of metallic emission lines and some evidence for different distinct emission regions in the same source. The range of line-to-continuum contrast between the sources is high, and where previous observations have been taken, there is evidence of variability of emission line strength in some sources.