arXiv 0807.11292008-07-07astro-ph

银河系行星状星云距离尺度的麦哲伦云刻度

The Magellanic Cloud Calibration of the Galactic Planetary Nebula Distance Scale

Letizia Stanghellini, Richard A. Shaw, Eva Villaver

备注：: The Astrophysical Journal, in press
DOI：: 10.1086/592395

摘要：

银河系行星状星云（PN）的距离推导，除了在少数情况下，通过校准的统计特性的PNe。这样的校准是有限的，由几个非均匀的方法，每个携带自己的负债集获得的个人PN距离的准确性。在本文中，我们使用的物理性质的PNE在麦哲伦云，和他们的准确已知的距离，重新校准的Shklovsky/Daub距离技术。我们的新校准与Cahn等人（1992）常用的距离尺度非常相似（在1%以内），尽管存在重要的差异。我们发现，无论是距离规模工程以及与经典的PNe（“蝴蝶”）双极形态，虽然银河和麦哲伦云校准中的辐射约束PN序列具有相似的斜率，从光学厚到光学薄的转变似乎发生在比Cahn等人所采用的更高的表面亮度和更小的尺寸下。在确定标度因子时的色散表明，通过这种方法得出的PN距离至少有30%的不确定性，并且这种分散性不能通过使用更好的校准器来显着降低。我们提出了一个目录的银河PN距离使用我们的重新校准，可用于未来的应用程序，并比较最好的个人银河PN距离我们的新的和其他几个距离尺度，无论是在文献中，我们新重新校准，发现我们的规模是最可靠的日期。

英文摘要：

Galactic planetary nebula (PN) distances are derived, except in a small number of cases, through the calibration of statistical properties of PNe. Such calibrations are limited by the accuracy of individual PN distances which are obtained with several non-homogeneous methods, each carrying its own set of liabilities. In this paper we use the physical properties of the PNe in the Magellanic Clouds, and their accurately known distances, to recalibrate the Shklovsky/Daub distance technique. Our new calibration is very similar (within 1 percent) of the commonly used distance scale by Cahn et al. (1992), although there are important differences. We find that neither distance scale works well for PNe with classic ("butterfly") bipolar morphology, and while the radiation bounded PN sequences in both the Galactic and the Magellanic Cloud calibration have similar slopes, the transition from optically thick to optically thin appears to occur at higher surface brightness and smaller size than that adopted by Cahn et al. The dispersion in the determination of the scale factor suggests that PN distances derived by this method are uncertain by at least 30 percent, and that this dispersion cannot be reduced significantly by using better calibrators. We present a catalog of Galactic PN distances using our re-calibration which can be used for future applications, and compare the best individual Galactic PN distances to our new and several other distance scales, both in the literature and newly recalibrated by us, finding that our scale is the most reliable to date.

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