EDP Sciences
Free Access
Volume 412, Number 1, December II 2003
Page(s) 121 - 132
Section Formation, structure and evolution of stars
DOI https://doi.org/10.1051/0004-6361:20031408

A&A 412, 121-132 (2003)
DOI: 10.1051/0004-6361:20031408

UV-photoprocessing of interstellar ice analogs: New infrared spectroscopic results

G. M. Muñoz Caro1, 2 and W. A. Schutte1

1  Raymond and Beverly Sackler Laboratory for Astrophysics, Leiden Observatory, 2300 RA Leiden, The Netherlands
2  Institut d'Astrophysique Spatiale, UMR 8617, Bât. 121, Campus Paris XI, 91405 Orsay, France

(Received 14 November 2002 / Accepted 20 August 2003 )

We simulate experimentally the physical conditions present in dense clouds by means of a high vacuum experimental setup at low temperature T  $\approx$ 12 K. The accretion and photoprocessing of ices on grain surfaces is simulated in the following way: an ice layer with composition analogous to that of interstellar ices is deposited on a substrate window, while being irradiated by ultraviolet (UV) photons. Subsequently the sample is slowly warmed up to room temperature; a residue remains containing the most refractory products of photo- and thermal processing. In this paper we report on the Fourier transform-infrared (FT-IR) spectroscopy of the refractory organic material formed under a wide variety of initial conditions (ice composition, UV spectrum, UV dose and sample temperature). The refractory products obtained in these experiments are identified and the corresponding efficiencies of formation are given. The first evidence for carboxylic acid salts as part of the refractory products is shown. The features in the IR spectrum of the refractory material are attributed to hexamethylenetetramine (HMT, [ (CH 2) 6N 4] ), ammonium salts of carboxylic acids [ (R-COO -)(NH +4)] , amides [ H 2NC(=O)-R] , esters [ R-C(=O)-O-R '] and species related to polyoxymethylene (POM, [ (-CH 2O-) n] ). Furthermore, evidence is presented for the formation of HMT at room temperature, and the important role of H 2O ice as a catalyst for the formation of complex organic molecules. These species might also be present in the interstellar medium (ISM) and form part of comets. Ongoing and future cometary missions, such as Stardust and Rosetta, will allow a comparison with the laboratory results, providing new insight into the physico-chemical conditions present during the formation of our solar system.

Key words: infrared: ISM -- ISM: lines and bands -- methods: laboratory -- ultraviolet: ISM -- ISM: dust, extinction

Offprint request: G. M. Muñoz Caro, Guillermo.Munoz-Caro@ias.u-psud.fr

© ESO 2003

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