A prime site of astrobiological interest within the Solar System is the interior ocean of Enceladus. This ocean has already been shown to contain organic molecules and is thought to have the conditions necessary for more complex organic biomolecules to emerge and potentially even life itself. This sub-surface ocean has been accessed by Cassini, an unmanned spacecraft that interacted with the water plumes ejected naturally from Enceladus. The encounter speed with these plumes and their contents was 5 km s −1 and above. Encounters at such speeds allow analysis of vaporised material from submicron-sized particles within the plume, but sampling micron-sized particles remains an open question. The latter particles can impact metal targets exposed on the exterior of future spacecraft, producing impact craters lined with impactor residue, which can then be analysed. Although there is considerable literature on how mineral grains behave in such high-speed impacts, and also on the relationship between the crater residue and the original grain composition, far less is known regarding the behaviour of organic particles. Here we consider a deceptively simple yet fundamental scientific question: for impacts at speeds of around 5-6 kms −1 would the impactor residue alone be sufficient to enable us to recognise the signature conferred by organic particles? Furthermore, would it be possible to identify the organic molecules involved, or at least distinguish between aromatic and aliphatic chemical structures? For polystyrene (aromatic-rich) and poly (methyl methacrylate) (solely aliphatic) latex particles impinging at around 5 km s −1 onto metal targets, we found that sufficient residue is retained at the impact site to permit identification of a carbon-rich projectile, but not of the particular molecules involved, nor is it currently possible to discriminate between aromatic-rich and solely aliphatic particles. This suggests that an alternative analytical method to simple impacts on metal targets is required to enable successful collection of organic samples in a fly-by Enceladus mission. that not only does life evolve, but also that it may even generate intelligence and contact us. This possibility can be expressed as a series of independent terms, the probability of each of which can be estimated, and the terms then multiplied together to produce an overall possibility (see [2] for a discussion). More recently, the Drake equation has been revisited, adding time dependences to the terms, etc. [3,4]. Indeed, one can go further and say that each of the terms in such an equation is not given by a single discrete value but is best represented by a distribution [5]. However, this does not advance our understanding of what actually occurs in each step. Indeed, the actual appearance of life is usually a single step in such equations; this is, however, a very big step.The reason approaches such as the Drake equation work, is because the Universe has great homogeneity from a scientific viewpoint. There are many stars, arranged in many g...