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           CO2 produced after ion irradiation of ice mixture

Through the links given below you will obtain the spectra relative to the CO2 bands formed after ion irradiation of the ice mixtures as indicated. Each file gives wavenumber (in units of cm^-1) and optical depth (tau). The optical depth is tau = - ln T where T is the transmittance after baseline correction. The names of the spectra files are structured in such a way that the first letter (B or S) indicates if the file refers to the bending (B) mode band (at about 660 cm-1) or to the stretching (S) mode band (at about 2340 cm-1). A sequence of numbers (and occasionally the letter L) identify the spectrum in our database. The final letter (P) if present, indicates that a polarizer was placed in the path of the IR beam in front of the detector of the spectrometer. With the polarizer it is possible to select and analyze the P and S components of the IR beam separately. Spectra labeled P are relative to the P polarized component of the IR beam.

We point out that, as discussed in Baratta et al. (2000, A&A 357, 1045), if the P component of the laboratory spectrum is different from the S component then laboratory spectra are not representative of small particle cross section and cannot be used to fit observed astronomical spectra. We have verified that all the spectra inserted in this database can be directly compared with observed spectra. If letter P is not present it means that the polarizer was not used.

All the experimental details relative to the spectra here available can be found in Ioppolo et al. 2008, A&A submitted. Please cite this paper if you use these spectra.

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CH3OH + 30 keV He+ irradiated at 12.5 K + warm up.

CO:NH3 (2:1) + 30 keV He+ irradiated at 12.5 K.

CO + 200 keV H+ irradiated at 16 K + warm up.

CO:N2 (1:1) + 200 keV H+ irradiated at 16 K + warm up.

CO:N2 (8:1) + 200 keV H+ irradiated at 16 K + warm up.

CO2 formed after irradiation of CO + 200 keV H+ irradiated at 70 K.

CO:H2O (10:1) + 200 keV H+ irradiated at 16 K + warm up.