通过成像禁止线发射绘制天体物理星云中的低密度和高密度云
Mapping low and high density clouds in astrophysical nebulae by imaging forbidden line emission
摘要：
发射线比率对于确定天体物理学气体星云中的气体温度和密度等物理参数至关重要。随着全景光谱设备的出现，原则上也可以产生具有与这些物理参数相关的发射线的区域的图像。我们表明，从现代仪器的观测，它是可能的转换图像从密度敏感的禁线到图像的发射从高和低密度的云通过应用一个转换矩阵。为了实现这一点，必须观察和组合密度敏感线对以及相邻连续体的图像。我们计算了红外、可见光、紫外和X射线波段的一系列线对的临界密度，并在4能级和5能级原子近似下计算了高密度极限和低密度极限下的线对强度比。为了说明该方法，我们将其应用到两个星系核的GMOS-IFU数据。我们的结论是，这种方法提供了新的天体物理学感兴趣的信息，特别是映射低密度和高密度云，因为这个原因，我们称之为“ld/hd成像方法”。
英文摘要：
Emission line ratios have been essential for determining physical parameters such as gas temperature and density in astrophysical gaseous nebulae. With the advent of panoramic spectroscopic devices, images of regions with emission lines related to these physical parameters can, in principle, also be produced. We show that, with observations from modern instruments, it is possible to transform images taken from density sensitive forbidden lines into images of emission from high and low-density clouds by applying a transformation matrix. In order to achieve this, images of the pairs of density sensitive lines as well as the adjacent continuum have to be observed and combined. We have computed the critical densities for a series of pairs of lines in the infrared, optical, ultraviolet and X-rays bands, and calculated the pair line intensity ratios in the high and low-density limit using a 4 and 5 level atom approximation. In order to illustrate the method we applied it to GMOS-IFU data of two galactic nuclei. We conclude that this method provides new information of astrophysical interest, especially for mapping low and high-density clouds; for this reason we call it "the ld/hd imaging method".
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