Travel support for two observers to conduct astronomical observations at the LBT during the LBTB observing block in April 2018

1)未演化的星系应该具有低质量、低金属度和强辐射场，这是由于最近的星暴和基本上不存在的老恒星所致。因此，它们应该在更长的波长和极强的发射线上发射出强的UV连续谱和非常弱的连续谱。在高红移的情况下，这些矮小星系极难研究，因此我们需要好的替代物来更详细地观察相关的过程。这样的极端发射线星系和极蓝星系已经在中等红移时被探测到，其中许多具有很低的金属丰度(低于0.1Z_SOLAR)。因此，我们找到了原星系的合适替代品，从而可以进行详细的分析。2)Z~7星系中星云CIII和CIV发射线的观测引起了人们对产生这些发射线所需的硬辐射场性质的新兴趣。由于不仅非常大质量、低金属丰度的恒星，而且大质量的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谱光子的来源，因此定义一组非常局部的代理是必要的，其中空间分辨率和灵敏度允许详细研究气体和单独的电离源。3)盘状星系外流和扩散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得到了很好的证实(但还没有完全理解)，但观测到的电离气体的电离机制并没有受到很好的限制：虽然光致电离肯定起到了作用，但观测到的谱线比及其与圆盘距离的变化需要光子场的变化和另外一个目前未知的加热机制的存在。4)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，可以获取表观中心恒星的光谱，令人惊讶的是，这些恒星往往被证明是演化的大质量恒星(Wolf-Rayet恒星，发光蓝变星的候选者，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目标定位，以更公正的方式对气泡中可能被高度吸收的部分进行分类，并研究其演化状态和中心恒星。

1) Unevolved galaxies should have low-masses, low-metallicities, and a strong radiation fields due to recent starbursts and largely absent older stars. Therefore, they should emit strong UV continuum but very weak continua at longer wavelengths and extremely strong emission lines. At high redshifts these dwarfish galaxies are extremely hard to study, so we need good proxies for a more detailed looks at the involved processes. Such extreme emission line galaxies and extremely blue galaxies have been detected at intermediate redshifts, many have very low metallicity (below 0.1 Z_solar). We therefore have found decent proxies for protogalaxies, allowing detailed analyses. 2) 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. 3) 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. 4) 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.