Identification of Organics in Ice Grains from Enceladus

Abstract:

The Cosmic Dust Analyzer (CDA) aboard the Cassini spacecraft performs in-situ measurements of the chemical composition of icy dust grains impinging onto the target surface. The instrument recorded cationic Time-of-Flight (ToF) mass spectra of organic-bearing ice grains emitted from Enceladus at different impact velocities causing different molecular fragmentation patterns [1,2].

Here we present a detailed analysis of these spectra (Type-2) to identify the composition of organic material embedded in Enceladus ice grains. The organic compounds display a great compositional diversity, which indicates varying contributions of several organic species. The spectra analysis is supported by a large-scale laboratory ground campaign yielding a library of analogue spectra for organic material embedded in a water ice matrix. To mimic the identified pattern of cationic fragments in organic enriched spectra we use a laboratory setup: Infrared Free Liquid MALDI ToF Mass Spectrometer (IR-FL-MALDI-ToF-MS). An infrared laser is used to disperse a liquid micro-beam of a water-solution to get cationic fragments. The laser energy is adjusted to simulate different impact velocities of ice particles on CDA [3].

So far we have identified characteristic fragment patterns of at least three classes of organic molecules: (i) aromatic species, (ii) amines, and (iii) carbonyl group species.

(i) ice grains containing aromatic species are identified by a series of characteristic aromatic fragment cations (ii) ice grains containing amines are identified by a pronounced ammonium cation and (iii) ice grains containing carbonyl compounds are specified by a characteristic acylium cation in conjunction with certain others mass lines. Besides aromatic, amine and carbonyl species, Type-2 spectra also show contributions from other, yet un-specified, organic species.

Typically, fragment cations of aromatic compounds are stable at impact velocities up-to 15km/s whereas cations of amines and carbonyl species are stable at velocities below 8km/s. Work is in progress to quantify concentrations of the identified species and to assign yet un-specified organic mass lines in Type 2 spectra.

Ref: [1]Postberg et al., Icarus-193,2008. [2]Postberg et al., Nature-459,2009. [3]Beinsen, A., University of Göttingen, Dissertation (2011).