1. Belén Maté, Miguel Jiménez-Redondo, Isabel Tanarro, Miguel Moreno, and Victor Herrero Instituto de Estructura de la Materia (IEM-CSIC), Serrano 123, 28006, Madrid, Spain belen.mate@csic.es ISMS - 70TH MEETING - JUNE 22-26, 2015 - CHAMPAIGN-URBANA, ILLINOIS Investigation of carbonaceous interstellar dust analogues by infrared spectroscopy: Effects of energetic processing Funding: CDS2009-00038, FIS20012 -38175, FIS2013-48087-C2-1-P, ERC-2013-Syg 610256 INSTITUTO DE ESTRUCTURA DE LA MATERIA

2. Interstellar hydrocarbon dust IR absorption features 3.4  m band J. Chiar et al. ApJ 2013, 770, 78 A. P. Jones ASP Conf. Ser. 414, 2009

3. Carbonaceous dust in the diffuse ISM E. Dartois et al. A&A, 2007, 463, 635 Hydrogenated amorphous carbon (HAC or a-C:H) produced in the laboratory CH aromatic (upper limit) CC aromatic + olefinic CH Aliphatic stretchings CH aliphatic bendings Structure estimates by Dartois et al. suggest an important contribution of hydrogen rich aliphatic carbon Aliphatic features are more prominent their absorption strengths are much higher

4. Amorphous C/H ternary diagram PAHs E. Dartois et al. A&A, 2007, 463, 635

5. Carbonaceous dust in the diffuse ISM J. Chiar et al. ApJ, 2013, 770, 78 Left: weighted average of the spectra of the six quintuplet lines of sight. Right: ISO spectra UKIRT spectra toward the Galactic center Quintuplet Cluster Structure estimates by Chiar et al. suggest that the dust is hydrogen poor and highly aromatic

6. HAC film deposition in CH 4 /He plasma IEM-CSIC CH 4 (40%)/He 0.3 mbar 40 W, 13.56 MHz outside the coil HAC1 inside the coil HAC2 Inductively coupled RF discharge reactor Film thickness ~ 3 µm 1 hour

7. IR spectra of the deposits CH stretch C=C stretch CHx bend Aromatics Aliphatics Outside the coil Inside the coil x5 6.9 µm 6.2 µm 11.3 µm CH3 CH2 7.2 µm CH 3 CH 2 CH 3 3.4 µm B. Maté et al. Faraday Disc. 2014, 168, 267 HAC 1 HAC 2

8. Analysis of HAC spectra H0.33 sp 2 0.55 sp 3 0.11 3200 3800 2800 1700 1500 1300 Wavelength/ cm -1 0.4 0.2 0.1 Absorbance CH 2, CH 3 sp 3 CC sp 2 CH sp 2 HAC 1 HAC 2 H0.13 sp 2 0.83 sp 3 0.04 Using absorption strengths from Chiar et al. ApJ 2013, 770, 78 CO? HAC2 HAC1

9. Comparison with observations in the diffuse ISM Infrared Galaxy IRAS 08572+3915 Dartois et al. A&A 2007 Galactic center Quintuplet Cluster. Chiar et al. ApJ, 2013, Optical depth Wavelength µm

10. Comparison with observations in the diffuse ISM Infrared Galaxy IRAS 08572+3915 Dartois et al. A&A 2007 Galactic center Quintuplet Cluster. Chiar et al. ApJ, 2013, Optical depth Wavelength µm HAC 1 spectrum scaled to the maximum

11. Comparison with observations in the diffuse ISM Infrared Galaxy IRAS 08572+3915 Dartois et al. A&A 2007 Galactic center Quintuplet Cluster. Chiar et al. ApJ, 2013, Optical depth Wavelength µm HAC 1 spectrum scaled to the maximum HAC 2 spectrum scaled to the maximum

12. Deposit growth and structure The H/C and sp 3 /sp 2 ratios decrease with growing thickness Inside the coil 3 min ~ 100 nm 6 min ~ 200 nm 12 min ~ 400 nm growth

13. H 2 plasma 0.25 mbar, 40 W 0 min 4 min 10 min Processing in H 2 plasma The CC stretch band remains unchanged CC bonds polyaromatic rather than olefinic The CH x stretch band decreases with processing CC

14. Summary and conclusions Carbonaceous dust analogues have been grown in inductively coupled RF discharges of He+CH 4. The position in the plasma reactor affects the structure of the deposited hydrocarbon. Inside coil deposits are good analogues to interstellar medium dust. Processing with H 2 plasma do not affect the aromatic component of the carbonaceous material. Belén Maté, belen.mate@csic.es INSTITUTO DE ESTRUCTURA DE LA MATERIA