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arXiv 1504.01534astro-ph.SR
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Hα表面亮度-半径关系：行星状星云的一个可靠的统计距离指示器

The Hα surface brightness - radius relation: a robust statistical distance indicator for planetary nebulae

David J. Frew, Q. A. Parker, I. S. Bojicic

备注：
49 pages, 17 tables, 8 figures. Published in MNRAS; supplementary tables are included at end of this manuscript
发表信息：
MNRAS, 455, 1459 (2016)
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摘要：

测量银河系行星状星云（PNE）的距离几十年来一直是一个棘手的问题。我们现在已经建立了一个强大的光学统计距离指标，H $α$表面亮度-半径或S-r关系，它解决了这个问题。我们开发了这个关系，从一个严格评估的样品的主要校准PNe。该方法的鲁棒性结果从我们修订的校准距离显着降低系统的不确定性，和最近的高质量的数据，包括更新的星云直径和综合H $α$通量。S-r技术应用简单，只需要角尺寸、积分Hα通量和红化到PN。从这些量中，计算出内半径，当与角尺寸结合时，直接产生距离。此外，我们还发现，光学厚PNe倾向于填充趋势的上限，而光学薄PNe沿S-r平面的下边界下降。这使得能够开发出子趋势，在确定距离时提供更好的精度，在光学薄，高激发PNe的情况下高达18%。这比以往任何一个统计指标都要好。我们使用这种技术来创建一个目录的统计距离超过1100银河PNE，最大的这样的汇编文献中的日期。最后，在附录中，我们调查了一组过渡PNE和一系列PN模拟在S-r平面，以证明其作为诊断工具的用途。有趣的是，大质量恒星周围的恒星喷出物在S-r空间中的一个紧密轨迹上，有可能作为这些物体的单独距离指示器。

英文摘要：

Measuring the distances to Galactic planetary nebulae (PNe) has been an intractable problem for many decades. We have now established a robust optical statistical distance indicator, the H$α$ surface brightness- radius or S-r relation, which addresses this problem. We developed this relation from a critically evaluated sample of primary calibrating PNe. The robust nature of the method results from our revised calibrating distances with significantly reduced systematic uncertainties, and the recent availability of high-quality data, including updated nebular diameters and integrated H$α$ fluxes. The S-r technique is simple in its application, requiring only an angular size, an integrated Hα flux, and the reddening to the PN. From these quantities, an intrinsic radius is calculated, which when combined with the angular size, yields the distance directly. Furthermore, we have found that optically thick PNe tend to populate the upper bound of the trend, while optically-thin PNe fall along the lower boundary in the S-r plane. This enables sub-trends to be developed which offer even better precision in the determination of distances, as good as 18 per cent in the case of optically-thin, high-excitation PNe. This is significantly better than any previous statistical indicator. We use this technique to create a catalogue of statistical distances for over 1100 Galactic PNe, the largest such compilation in the literature to date. Finally, in an appendix, we investigate both a set of transitional PNe and a range of PN mimics in the S-r plane, to demonstrate its use as a diagnostic tool. Interestingly, stellar ejecta around massive stars plot on a tight locus in S-r space with the potential to act as a separate distance indicator for these objects.

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