In-situ-analysis of ice particles in the solar system: application, methods, instrument developement

外太阳系（大致从小行星带开始）的大部分凝聚态物质由水冰组成。目前关于冰表面和粒子组成的发现几乎完全是基于吸收光谱，特别是在红外范围内。然而，通过这种方式，嵌入在水冰基质中的化合物只能在一定程度上进行研究。这尤其适用于无机成分，它们在红外范围内通常只是轻微活跃甚至不活跃。许多有机化合物也很难识别，更不用说用吸收光谱法定量了。所请求的资金连同海森堡研究金的综合目标是用一种新方法来描述太阳系中冰体的化学特征。这是通过对太空中的冰粒进行原位质谱分析来完成的，这些冰粒会以高速与相应的探测器相撞。如果粒子的起源是已知的，那么母体的成分和地球化学也可以被表征。卡西尼号的宇宙尘埃分析仪（CDA）已经展示了这种方法的能力，它特别适合于冰冷的物质，并补充了吸收光谱。在拟议的研究计划框架内，将应用和进一步发展原位质谱法。为此目的，将分析当前太空任务（卡西尼号、罗塞塔号）的数据，并为未来的任务做好准备，以获得最佳的科学回报。这得到了一系列用冰模拟材料进行的实验室实验的支持。在子项目1中，先前使用卡西尼- cda数据的工作将在质量上扩大到一个新的水平。目标是对土星系统中冰质物质的组成进行全面、系统的描述。由此，可以全面了解土星环系统的组成及其低温火山活动的冰卫星土卫二。土卫二的冰泉，从月球冰层的温暖裂缝中出现，由液态水提供，可能提供有关月球天体生物学潜力的宝贵信息。解释CDA质谱的一个核心资源将是使用子项目2中描述的模拟实验。这些装置模拟冰粒对探测器板的高速撞击，对解释空间数据非常有帮助。然而，这种方法不仅适用于CDA光谱，也适用于其他当前或未来空间任务的数据，例如罗塞塔。现有的国家和国际合作和投资将得到利用和进一步扩大

The better part of condensed matter in the outer solar system (beginning roughly at the asteroid belt) consists of water ice. Current findings on the composition of icy surfaces and particles are almost exclusively based on absorption-spectroscopy, particularly in the infrared range. However, in this way, compounds that are embedded in a water ice matrix can only be investigated to a certain degree. This applies in particular to anorganic components, which are often only slightly active or even inactive in the infrared range. Many organic compounds are also difficult to identify, much less to quantify, by absorption-spectroscopy.The comprehensive goal of the requested funds, conjoint with a Heisenberg Fellowship, is the chemical characterisation of icy bodies in the solar system by means of a new method. This is done through in situ mass spectrometry of ice particles in space, which collide with the appropriate detectors at high speed. If the particles' origins are known, the composition and geochemistry of the mother body can also be characterised. This approach, the capabilities of which have been impressively shown through Cassini's Cosmic Dust Analyser (CDA), is particularly well suited to icy materials and complements absorption-spectroscopy. Within the framework of the proposed research programme, the in situ mass spectrometry shall be applied and further developed. For that purpose, data from current space missions (Cassini, Rosetta) will be analysed and future missions will be prepared for an optimal science return. This is supported by a series of lab experiments with icy analogue materials. In sub-project 1, the previous work with Cassini-CDA data will be expanded to a qualitatively new level. The target is a comprehensive, systematic description of the composition of icy materials in the Saturnian system. From this, comprehensive insights into the composition of Saturn's ring system and its cryo-volcanic active icy moon Enceladus can be derived. Enceladus ice fountains, which emerge through warm cracks in the moon's icy crust, are fed by liquid water and may provide valuable information about the moon's astrobiological potential. A core resource for the interpretation of CDA mass spectra will be the use of the analogue experiments as described in sub-project 2. These devices simulate high-speed impacts of ice particles onto the detector plate and are extremely helpful in the interpretation of space data. However, this method applies not only to CDA spectra, but also to the data of other current or future space missions, e.g. Rosetta. Existing national and international cooperations and investments will be used and further expanded