“船底座耀斑”超壳层：探测星系烟囱中的原子和分子ISM
The "Carina Flare" Supershell: Probing the Atomic and Molecular ISM in a Galactic Chimney
摘要：
“船底座耀斑”超壳层GSH 287+04-17，是一个分子超壳层，最初是用NANTEN 4米望远镜在12 CO（J=1-0）中发现的。我们提出的第一个研究壳的原子ISM，使用HI 21厘米线数据从帕克斯64米望远镜南银河平面调查。这些数据揭示了一个温和膨胀的~ 230 x 360 pc HI超壳层，显示了银道面爆发的强有力证据，其主体在z ~ 280 pc处破裂，并且高纬度延伸达到z ~ 450 pc。分子云形成了原子壳层的共同运动部分，两相的形态反映了超壳层对ISM结构的影响。我们还报告了第一次发现的超壳层的电离成分，在形式上微妙的，流光般的细丝对齐与建议的方向井喷。我们重新检验了到壳的距离估计，发现了强有力的证据来支持最初的建议，即它位于隆凸臂，距离为2.6 +- 0.4 kpc。相关的HI和H2质量估计为M（HI）~ 7 +- 3 x 10^5 Msol和M（H2）~ 2.0 +- 0.6 x 10^5 Msol，膨胀壳层的动能估计为E ~ 1 x 10^51 erg。我们检查了分析和数值模型的结果，估计所需的形成能量为10^51至10^52尔格，年龄为10^7年。这个年龄与分子云形成的时间尺度是兼容的，我们简要地考虑了超壳层引发的分子成分起源的可行性。
英文摘要：
The "Carina Flare" supershell, GSH 287+04-17, is a molecular supershell originally discovered in 12CO(J=1-0) with the NANTEN 4m telescope. We present the first study of the shell's atomic ISM, using HI 21 cm line data from the Parkes 64m telescope Southern Galactic Plane Survey. The data reveal a gently expanding, ~ 230 x 360 pc HI supershell that shows strong evidence of Galactic Plane blowout, with a break in its main body at z ~ 280 pc and a capped high-latitude extension reaching z ~ 450 pc. The molecular clouds form co-moving parts of the atomic shell, and the morphology of the two phases reflects the supershell's influence on the structure of the ISM. We also report the first discovery of an ionised component of the supershell, in the form of delicate, streamer-like filaments aligned with the proposed direction of blowout. The distance estimate to the shell is re-examined, and we find strong evidence to support the original suggestion that it is located in the Carina Arm at a distance of 2.6 +- 0.4 kpc. Associated HI and H2 masses are estimated as M(HI) ~ 7 +- 3 x 10^5 Msol and M(H2) ~ 2.0 +- 0.6 x 10^5 Msol, and the kinetic energy of the expanding shell as E ~ 1 x 10^51 erg. We examine the results of analytical and numerical models to estimate a required formation energy of several 10^51 to ~ 10^52 erg, and an age of ~ 10^7 yr. This age is compatible with molecular cloud formation time-scales, and we briefly consider the viability of a supershell-triggered origin for the molecular component.
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