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arXiv 0802.3813astro-ph
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行星状星云及其晕的空间分辨光谱学I。五个星系盘状天体

Spatially resolved spectroscopy of planetary nebulae and their halos I. Five galactic disk objects

Christer Sandin, Detlef Schönberner, Martin M. Roth, Matthias Steffen, Petra Böhm, Ana Monreal-Ibero

备注：
27 pages, 29 figures, A&A (in press), Abridged abstract, Corrected and clarified various minor issues; the section on scattered light is significantly clarified
发表信息：
Astron. Astrophys. 486 (2008), 545-567
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摘要：

渐近巨星分支（AGB）顶端恒星的强烈质量损失深刻地影响了这些恒星及其周围环境的性质，包括随后的行星状星云（PN）阶段。在这项研究中，我们希望通过研究弱发射晕来确定质量损失的物理特性，重点是星系盘中的物体。光环围绕着PNE的中心区域，亮度高达数千倍。年轻的晕，特别是，仍然包含的信息之前的最后质量损失阶段的AGB。在观测中，我们使用了积分场光谱的方法与PMAS仪器。这是第一次使用这种技术对PNe晕进行研究。我们通过几个步骤改进了我们的数据分析。在一项关于散射光影响的研究中，我们发现内晕中有一部分强度源自相邻区域。由于我们结合了远距离波长的线强度，并且由于径向强度梯度很陡，我们校正了差分大气折射的影响。为了提高弱发射线的信噪比，我们引入了一种专用的方法来对单个空间元素的光谱进行分块。我们还开发了一种通用的技术来减去大地线-而不使用单独的天空曝光。通过这些步骤，我们避免了在晕中的温度测量中引入几千开尔文的误差。对于IC 3568，我们检测到晕。我们发现M2-2的晕半径是M2 - 2的2.5倍。（节略）

英文摘要：

Strong mass loss off stars at the tip of the asymptotic giant branch (AGB) profoundly affects properties of these stars and their surroundings, including the subsequent planetary nebula (PN) stage. With this study we wanted to determine physical properties of mass loss by studying weakly emitting halos, focusing on objects in the galactic disk. Halos surround the, up to several thousand times, brighter central regions of PNe. Young halos, specifically, still contain information of the preceeding final mass loss stage on the AGB. In the observations we used the method of integral field spectroscopy with the PMAS instrument. This is the first committed study of halos of PNe that uses this technique. We improved our data analysis by a number of steps. In a study of the influence of scattered light we found that a moderate fraction of intensities in the inner halo originate in adjacent regions. As we combine line intensities of distant wavelengths, and because radial intensity gradients are steep, we corrected for effects of differential atmospheric refraction. In order to increase the signal-to-noise of weak emission lines we introduced a dedicated method to bin spectra of individual spatial elements. We also developed a general technique to subtract telluric lines - without using separate sky exposures. By these steps we avoided introducing errors of several thousand Kelvin to our temperature measurements in the halo. For IC3568 we detected a halo. For M2-2 we found a halo radius that is 2.5 times larger... (abridged)

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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