猎户座大星云惠更斯区、扩展猎户座大星云和M~43的分光光度学研究散射光系统地扭曲由发射线导出的条件
Spectrophotometry of the Huygens Region of the Orion Nebula, the Extended Orion Nebula, and M~43; Scattered Light Systematically Distorts Conditions Derived from Emission-Lines
摘要：
本文报道了猎户座星云区的中分辨率分光光度测量结果，其中首次包括猎户座大星云及其附近的M~43。49个长缝观测被分成99个较小的样本，这些样本允许确定整个复杂区域的消光量、消光校正的\Hbeta \表面亮度、电子温度（来自[S~II]、[N~II]和[O~III]）和电子密度（来自[S~II]和[Cl~III]）。我们证实了一个早期的结论，即在距离\ori约5 \arcmin之后，局部辐射开始被M~42更亮的惠更斯中心区的光的光的散射所污染，并且这种散射光在远距离处占主导地位。这种污染意味着外部区域的导出属性不准确。通过比较M~43中主要恒星发出的光与该星云的连续光谱（几乎完全是散射的恒星光），可以确定散射光在蓝色区域增强，这可能导致观测到的巴耳末线比率在理论上是不可能的，并且错误的电子温度。发射线的这种蓝色散射即使在惠更斯区也很重要，因为这意味着除了非常高的光谱分辨率外，观察到的线是原始光和散射光的混合，较短波长的线被人为增强。这可能导致过度估计的电子温度来自星云和极光的禁行线比。这种现象可能也适用于其它许多H~II区。
英文摘要：
We report on medium resolution spectrophotometry of the Orion Nebula region, including for the first time the Extended Orion Nebula and the nearby M~43. The 49 long slit observations were divided into 99 smaller samples, which have allowed determinations of the amount of extinction, extinction corrected \Hbeta\ surface brightness, electron temperatures (from [S~II], [N~II], and [O~III]), and electron densities (from [S~II] and [Cl~III]) throughout much of this complex region. We verify an earlier conclusion from a radio/optical study that beyond about 5\arcmin\ from \ori\ local emission begins to be contaminated by scattering of light from the much brighter central Huygens Region of M~42 and this scattered light component becomes dominant at large distances. This contamination means that the derived properties for the outer regions are not accurate. From comparison of the light from the dominant star in M~43 with the continuum of that nebula (which is almost entirely scattered star light) it is determined that scattered light is enhanced in the blue, which can lead to observed Balmer line ratios that are theoretically impossible and erroneous electron temperatures. This blue scattering of emission-lines is important even in the Huygens Region because it means that at anything except very high spectroscopic resolution the observed lines are a blend of the original and scattered light, with shorter wavelength lines being artificially enhanced. This can lead to over-estimates of the electron temperatures derived from the nebular and auroral line ratios of forbidden lines. This phenomenon is probably applicable to many other H~II regions.
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