Travel support for two observers to conduct astronomical observations at the LBT during in September/October 2018

1)在z~7星系中观测到的星云CIII和CIV发射线引发了人们对产生这些发射线所需的硬辐射场性质的新兴趣。由于不仅是非常大质量、低金属丰度的恒星，而且还有大质量x射线双星、吸积的超大质量黑洞，甚至冲击波都可能是硬连续体光子的可能来源，因此必须定义一组非常局部的代理，其中空间分辨率和灵敏度允许对气体和单个电离源进行详细研究。2)盘状星系中喷流和弥漫性电离气体晕的电离过程仍然是一个未解之谜。虽然与恒星形成活动的联系似乎很好地建立了（但尚未完全理解），但观测到的电离气体的电离机制并没有得到很好的约束：虽然光电离肯定有贡献，但观测到的线比及其随距离的变化需要光子场的变化以及目前未知的额外加热机制的存在。3)斯皮策和赫歇尔揭示了银河系中大量的小气泡。在一些情况下，有可能获得明显中心恒星的光谱，令人惊讶的是，这些恒星往往是进化的大质量恒星（沃尔夫-拉叶星，发光蓝变量的候选者，以及OB超巨星）。我们利用LUCI近红外光谱对气泡及其中心恒星进行了分类，对气泡中可能被高度吸收的部分进行了分类，并以更公正的方式研究了它们的演化状态和中心恒星。

1) The observation of nebular CIII] and CIV emission lines in z~7 galaxies triggered new interest in the nature of the hard radiation field needed for this emission lines to occur. Since not only very massive, low metallicity stars, but also massive X-ray binaries,accreting supermassive black hole, and even shocks may be possible sources of the hard continuum photons, the definition of a set of very local proxies is imperative, where spatial resolution and sensitivity allow a detailed study of the gas and individual ionization sources. 2) The ionization process of outflows and diffuse ionized gas halos in disk galaxies is still an unsolved puzzle. While a connection to star formation activity seems to be well established (but not fully understood), the ionization mechanism of the observed ionized gas is not well constrained: while photo-ionization certainly contributes, the observed line ratios and their change with distance from the disk require changes in the photon field and the presence of an additional currently unknown heating mechanism. 3) Spitzer and also HERSCHEL revealed a significant number of small bubbles in the Milky Way. In a couple of cases, it was possible to take optical spectra of the apparent central stars, which surprisingly often turned out to be evolved massive stars (Wolf-Rayet stars, candidates for Luminous Blue Variables, and OB supergiants). We target the bubbles and their central stars with LUCI NIR spectroscopy to classify the potentially highly absorbed part of the bubbles and investigate their evolutionary state and their central stars in a more unbiased way.