Open Access
Volume 623, March 2019
Article Number A134
Number of page(s) 6
Section Interstellar and circumstellar matter
Published online 19 March 2019

© T. Pino et al. 2019

Licence Creative Commons
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

1 Introduction

It is strongly suspected that large carbonaceous molecules carry the aromatic infrared bands (AIBs) observed in many lines of sight throughout the interstellar medium (ISM). The mid-IR range of wavelengths of the AIBs points to an out-of-equilibrium radiative relaxation mechanism triggered by the absorption of a single UV-starlight photon. The position of the bands and the emission mechanism led to the so-called polycyclic aromatic hydrocarbon (PAH) hypothesis and the presence of a molecular component in the form of polycyclic aromatic aliphatic mixed hydrocarbons is now well accepted (Sloan 2017; Jones et al. 2017; Yang et al. 2017; Pilleri et al. 2015; Sloan et al. 2014, 2007; Carpentier et al. 2012; Acke et al. 2010; Pino et al. 2008). The size of these large molecules ranges from a few tens to a few hundred atoms. Recently, neutral C60 and C70 (Sellgren et al. 2010; Cami et al. 2010) and possibly cationic C (Berné et al. 2013) detected via their IR emission spectra confirmed the existence of such a large molecular component. The most recent assignment of five diffuse interstellar bands, observed in absorption in the near-infrared, to the vibronic bands of the first electronic transition in C (Campbell et al. 2015, 2016; Walker et al. 2015) definitely proved that the ISM is enriched by such large carbonaceous molecules.

A gap in abundance between the largest molecule detected by rotational spectroscopy (11 atoms), with a column density decreasing drastically with size, and the fullerenes suggests that different formation mechanisms are at work. For the small interstellar molecules, homogeneous chemistry, gas-surface heterogeneous chemistry, and chemistry in ices are usually considered. However, these reactions cannot produce an amount of molecules as large as the fullerenes and the interstellar PAHs. Top-down mechanisms are therefore invoked and some models explored the possibility of formation of C60 from the large PAH component (Berne et al. 2015), relying on the photostability of these compounds in the ISM (Montillaud et al. 2013). However, these scenarios question the ability of the dust nanograins to release the PAHs and fullerene components. High-energy interaction processes are at the core of these scenarios where UV irradiation, irradiation with light or heavy ions and shocks may lead to the release of the molecules (Léger et al. 1985). To date, these processes have been studied to better constrain the enrichment of the ISM with small molecules (Alata et al. 2014, 2015; Dartois et al. 2017). The goal of the present work is to provide experimentally a proof of principle that cosmic rays (CRs), where energy deposition is dominated by the electronic energy loss, can lead to the emission of PAHs and fullerenes. Our results provide strong evidence in favour of a top-down scenario for the formation of free-flying large carbonaceous molecules in space.

The paper is organised as follows. A brief description of the experimental set-up is given. The results are then presented and analysed to provide the molecular species released upon swift heavy ions simulating CR by laboratory experiments. Finally, a discussion on the astrophysical implication and concluding remarks are reported.

2 Experiment

2.1 Analogue production

The analogues were produced using the nanograins set-up already described in previous publications (Pino et al. 2008; Carpentier et al. 2012; Gavilan et al. 2016, 2017). In brief, the soot samples were produced ina low-pressure ethylene flame burning at 40 mbar with a C/O ratio of 1.05. Ethylene and O2 flowed through the McKenna burner at a constant flow rate of 4 sl min−1 and the shielding N2 flow at 3 sl min−1. The height above the burner to extract the soot was set to 24 mm. These conditions allow the production of the “young” soot. The sampling time was set to 10 min and the substrate was a plate of stainless steel (Omicron). Results from spectroscopy investigations of these soot particles in the IR-VUV range were reported recently (Gavilan et al. 2017). The study revealed that under these combustion conditions soot analogues of the circumstellar and interstellar polyaromatic dust are produced. The soot particles produced here were found to be good intermediates between classes B and C according to the AIB classification. A C/H ratio of about 25 was found for this soot sample, representative of the polyaromatic dust grains in these objects (Gavilan et al. 2017).

2.2 Ion irradiations

The ion irradiations with swift heavy ions (SHI) were performed at the M1 branch of the UNILAC of GSI Helmholtzzentrum für Schwerionenforschung (Darmstadt, Germany). During the experiments, we used a 48 Can+ at 4.8 MeV u−1 swift heavy ion (SHI) beam (July 2016) with an ion current on the target of about 40 nA cm−2. Equilibrium charge states were obtained by inserting a carbon foil in the 48 Ca10+ beam delivered by the accelerator. The accelerator was operated at a frequency of 2 Hz and the length of the beam pulse was 5 ms. The electronic stopping power, 19.91 MeV (mg cm−2)−1, was calculated using the SRIM-2013 code (Stopping and Range of Ions in Matter; Ziegler et al. 2010), with a C/H of 25 and a density of 1.7 g cm−3. The range of the ions (40 μm) is much larger than the thickness of the film (few μm), ensuring homogeneous interaction with the target along the ion trajectory. The samples were exposed under a beam incidence of 45°.

2.3 TOF mass spectrometry

Mass spectra were monitored using a recently installed time-of-flight mass spectrometry (TOFMS) unit operating in reflectron mode (Meinerzhagen et al. 2016). The optical axis of the TOFMS is set normal to the sample surface and the pulsed ion extraction is synchronised to the SHI pulsed beam. The MCP detector is floated at a post-acceleration potential of −4 kV with respect to the ground. In combination with the stage extraction potential of 1500 V, this yields an ion impact energy of 5.3 keV onto the MCP surface. We have not measured the detection efficiency as a function of the post-acceleration potential, but we woule like to note that the detection was performed in the so-called analogue mode, where the MCP output was performed by directly digitising the MCP output using a transient digitiser. In this operation mode, the measured signal will always increase with increasing post-acceleration voltage. All triggering events are described in detail in a previous publication (Meinerzhagen et al. 2016) where the complete chronograph is displayed. Secondary ions and secondary neutral mass spectra (SIMS and SNMS, respectively) are monitored within a single SHI pulse of 5 ms duration. In addition, each mass spectrum acquired during the UNILAC pulse is complemented by a blank spectrum taken during beam-off times between the ion pulses, but under otherwise identical experimental conditions. This is done by gating the acquisition with a pulse of the same length as the UNILAC pulses, but delayed by five times its width. For the SNMS, a photoionisation nanosecond pulsed laser operating at157 nm (7.9 eV photon energy) is fired few mm above the sample holder and parallel to it, typically 300 μs after the beginning of the SHI pulse (and blank pulse). Since the TOFMS extraction is running at 1.2 kHz, it enables the accumulation of several SIMS spectra without laser (called repetitions), as compared to the SNMS spectra within the same acquisition cycle (event). Five hundred events were necessary to obtain a good SNMS signal-to-noise ratio (S/N). The mass resolution of the SNMS was found to be about 500 at mass 300 u (corresponding to the mass of the coronene C24 H12 molecule) and lower for the SIMS due to the large velocity dispersion of the ions and the better spatially defined ion cloud of the photoionised neutral molecules in the extraction zone of the TOFMS. The mass window was restricted to 0–1500 u for this first set of experiments. With this experimental set-up, the secondary ion mass spectrum emitted shortly after the SHI impact was detected, as were the neutral species (Breuer et al. 2016). This unique design gives access to the detection of large neutral molecules and radicals released during the irradiation. The photoionisation wavelength for SNMS is particularly efficient and can perform the direct ionisation of species with an ionisation potential below 7.9 eV, i.e. conjugated molecules such as the PAHs.

3 Results and analysis

3.1 Mass spectra

The mass spectra are presented in Fig. 1 for the masses below 100 u, in Fig. 2 for the mass range between 100 and 600 u, and in Fig. 3 for the masses above 600 u. For the last, only the SIMS is shown because no species are detected in the SNMS. A data treatment was applied to normalise the intensities in counts per repetition. The normalised SIMS intensities were obtained by dividing the accumulated SIMS spectra by the total number of repetitions (NTOT = Nevents ×Nrepet); the normalised SNMS intensities were obtained by dividing the accumulated “laser on” spectra by Nevents and subtracting the normalised SIMS spectra. Integration of the peaks around each mass unit was performed to plot the intensities directly. Because the soot target is composed mainly of carbon and hydrogen, a contribution of 13 C was taken into account. The natural abundance and all possible combinations were computed to perform the isotopic deconvolution. Because the structure of the SNMS can easily be identified with well-separated groups of peaks of species containing the same number of carbon atoms, the decomposition can be done as in Weilmunster et al. (1999) and every mass peak can be assigned to a chemical formula. For the SIMS data up to mass 600 u, the lower mass resolution and the presence of many peaks prevent the application of this simple protocol. We thus hypothesised that the species distribution were identical to those of the neutral for the 100–600 u mass range in order to perform the 13 C deconvolution of the SIMS. This was performed after background subtraction, as explained below.

thumbnail Fig. 1

SIMS and SNMS measured in the 0–100 u (unified atomic mass unit) mass range.

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3.2 Secondary molecular ions

Regarding the SIMS, few masses dominate the distribution: C2 H2, C2 H4, C3 H3, C3 H8, and C4 H2. The broad distribution of masses at smaller intensities suggests contribution of intense dissociation of emitted molecular fragments. In principle, fragmentation of molecular ions during their flight along the field-free drift path of the mass spectrometer may also contribute additional peaks to the measured spectrum. While such contributions could in principle be identified by re-tuning the flight time focusing properties of the reflectron (see Boesl et al. 1982), such an analysis was not attempted here due to the limited beam time available. In addition to the mass resolved peaks, a broad unresolved background is detected which arises from fragmentation processes within the extraction region and/or incomplete flight time focusing of secondary ions extracted from regions outside the focal volume of the mass spectrometer (Meinerzhagen et al. 2016). For this background, no identification may be performed. Therefore, for the subsequent analysis, only the superimposed peaks revealing a regular pattern are discussed. Subtraction of the underlying continuum was performed in the SIMS data above 100 u and only the remaining ion peaks were considered further (Figs. 2 and 3).

For the larger masses, the number of counts is by far smaller than those of the dominating peaks. However, the hydrogenation pattern remains with groups of peaks. These recall a typical distribution whose hydrogenation is found close to the most compact PAHs (such as coronene, ovalene, circumcoronene), although the H/C ratios are slightly higher. Starting at mass 720 u, the SIMS data exhibit a regular distribution of peaks separated by 24 mass units. This is characteristic of a fullerene distribution (Kroto et al. 1985), the smallest one detected here being C. Owing to the chosen mass window during this first set of experiments (below 1500 u), the complete distribution of the emitted fullerenes was not monitored and an instrumental cut-off at C124 is observed. It is noticeable that the mass spectrum exhibits the magic numbers of 60 and 70 carbon atoms and a broad distribution peaking above 100 carbon atoms.

3.3 Secondary neutral molecules

The SNMS in the low-mass range is dominated by species with an odd numbered hydrogenation. This is suggestive of a fragmentation pattern of larger species produced upon photoionisation because the ionisation potential of species containing a number of carbon atoms in this small mass range, even for the small aromatic molecules, is higher than the 7.9 eV of the laser photon, and thus cannot be directly photoionised (Desgroux et al. 2013). Species released in metastable electronic states could also contribute via direct photoionisation. The number of counts/rep is found to be comparable to that of the ions (Fig. 1). However, the multiphoton ionisation process implies a much more efficient neutral emission of small species.

Above about 100 u, the distribution resembles typical PAH distributions that can be extracted from flames or observed by nanosecond laser desorption followed by laser ionisation (Apicella et al. 2009; Faccinetto 2009; Faccinetto et al. 2011). For instance, peaks at the masses of pyrene and coronene are found to dominate. Even numbers of carbon and even numbers of hydrogen are the structures that are measured to be the most abundant, as expected for a PAH distribution. Compared to the emitted ions, the number of counts/rep for neutral molecules is found to be much higher (Fig. 2). For instance the neutral to cation ratio at the mass of coronene (300 u) is found to be about 50.

The H/C distribution is plotted in Fig. 4, where the intensity of the peaks is traced as a function of the number of C and H in a 3D plot. The most intense species exhibit hydrogenation that closely follows that of the most compact PAHs, with one or two species dominating for a given number of C, as illustrated by the inset in Fig. 2. The intensity distribution of species with lower H content probably arises either from fragmentation of the emitted PAHs after the SHI impact and/or is due to the photoionisation process. The intensity ratios were found not to depend strongly upon variation of the laser intensity, confirming a weak contribution of photodissociation. Therefore, the hydrogen distribution probably reflects the release process, and the dominating 2H-loss channel at the mass of coronene (see inset in Fig.2) helps to constrain the effective temperature of emission to about 2200 K (Chen et al. 2015).

4 Discussion

4.1 PAHs and fullerenes released by cosmic radiation

By irradiating soot samples with swift heavy ions, we identified neutral and cationic PAHs as well as cationic fullerenes. Using the geometrical configuration of the set-up, the photoionisation cross section at 7.9 eV of coronene of about 10 Mbarn (Johansson et al. 2017; Verstraete et al. 1990), and a 20 mJ cm−2 pulse−1 energy density, a rough estimation of the photoionisation efficiency gives 0.1. Using this efficiency and the measured neutral to cation ratio for coronene, the ratio of emitted cation to neutral is deduced to be about 2 × 10−3. This value iscomparable to the emission of secondary cations and neutrals measured for a coronene film (Breuer et al. 2016). PAHs could be present at the surface of the soot, although in low concentration. Because the neutral PAH distribution is very close to that measured from flames, for example using laser induced desorption in the nanosecond regime (Faccinetto et al. 2011, 2015; Alfe et al. 2008), the SNMS may be dominated by these adsorbed PAHs.

A striking point is the detection of cationic fullerenes with no evidence of neutral ones. It raises questions about the emission/production mechanism of these species. Detection of ionic fullerenes upon MeV ion irradiations has already been reported (Brinkmalm et al. 1992, 1993; Bitensky et al. 1993, 1994; Demirev et al. 1994; Akhtar et al. 1997; Qayyum et al. 1998). Influence of the nature of the target was shown with cluster growth starting from C60 when it was already present in the material (Bitensky et al. 1994; Demirev et al. 1994; Papaleo et al. 1996). Our SIMS shows a fullerene distribution starting at C60, suggesting that the present soot material may already contain fullerenic structures. According to its spectroscopy (Gavilan et al. 2017), this soot is made of sp2 carbons with defects causing curvature and tortuosity. In Carpentier et al. (2012), the soot was also consistently shown to possess curved structures. The initial structure of the soot particle may thus favour the formation and emission of fullerenes, although it does not contain such fullerenic structures. It is also noteworthy that in the present experiment, the electronic stopping power was 19.91 MeV (mg cm−2)−1, just above the threshold for fullerene formation and emission upon SHI impact that was predicted to be in the range 10–20 MeV (mg cm−2)−1 (Bitensky et al. 1993). In addition, their release was demonstrated to originate from the core region of the tracks (Brinkmalm et al. 1993; Bitensky et al. 1993, 1994; Demirev et al. 1994; Papaleo et al. 1996). Moreover, for an indium and silver targets, the ionisation probability were shown to depend on the projectile impact angle, with ionisation being enhanced for large angles of beam incidence (Mai et al. 2013). Therefore, the detection of fullerenic neutral species is probably unfavoured compared to cationic species; incident ions impacting at 45° with respect to the TOF axis have obviously a larger ion yield and favours the emission of the neutral fullerenes along the ion track and not normal to the surface. This also implies that that they may escape the post-photoionisation zone of the TOFMS. In addition, formation of ionised metastable fullerene fragments may actually be preferred as a result of the competition between thermionic electron emission (Campbell et al. 1991, 1992; Walder et al. 1993) and dissociation through C2 emission during relaxation of the emitted hot fullerenes from the ion track. In the ISM, the formation of the fullerenes may be triggered by the cosmic rays and subsequently emitted from the highly excited core region of the ion tracks.

thumbnail Fig. 2

SIMS and SNMS measured in the 100–600 u mass range. Insets are zoom-ins around mass 300 corresponding to the mass of coronene C24H12.

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thumbnail Fig. 3

SIMS measured in the mass range above 620 u. Note that a linear background was removed.

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thumbnail Fig. 4

Number of carbon NC and hydrogen NH in the neutral PAH mass range. The colours scale with the intensity of the peaks increasing from black to red and finally yellow. The open green circles mark the H and C composition of compact PAHs up tocircumcoronene. Lower H content probably arises from emitted partially dehydrogenated fragments, while higher probably traces less compact structures.

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4.2 Plausible top-down scenario?

The astrophysical relevance of the electronic sputtering induced by CRs on interstellar carbonaceous dust to the production of large molecular species in the ISM relies on the efficiency of the process. While it is not yet measurable in the laboratory, astrophysical constraints can be set to explore its likelihood. Previous sputtering yield measurements can be used to infer the C sputtering rate in an interstellar Galactic cosmic ray exposed environment. The sputtering rate for carbon RC (given in C atom cm−2 s−1) can be evaluated by integrating the product of the yield with the cosmic ray flux over their energy and abundance distribution following (1)

where is the differential flux of the cosmic ray element of atomic number Z and energy per nucleon E, with a cut-off in energy Emin set at 100 eV. Moving the cut-off from 10 eV to 1 keV does not change the results significantly. The sputtering yield is evaluated by combining Ys(Se) established experimentally and the calculated electronic stopping cross section Se(E, Z) using the SRIM code (Ziegler et al. 2010) as a function of atomic number Z and energy per nucleon E. For the differential flux, we adopt the functional form given by Webber & Yushak (1983), also described in Shen et al. (2004), (2)

where C is a normalisation constant and E0 a form parameter allowing us to account for the low-energy cosmic ray distribution.

To perform a calculation on the rate in interstellar space, we adopt the sputtering yield measurements given by Ghosh et al. (2004) for amorphous carbon, measured at 100 MeV (mg cm−2)−1, of 1.8 × 104 C atoms/ion and assuming a quadratic dependency of the sputtering yield with the stopping power in the electronic regime. The SRIM stopping power cross sections for the different interstellar ions are calculated with a density of 1.7 g cm−3, corresponding to typical soot value. The corresponding rate gives 1.24 C atom cm−2 s−1 /1016ζ, where ζ (s−1) is the cosmic ray ionisation rate. The Jones et al. (2017) model predicts a carbonaceous nanoparticle surface density of about 1.7 × 10−20 cm2 per hydrogen atom. The overall production rate is therefore 2.1 C atom 10−36/ζ H−1 s−1.

The rate of production of a species corresponds therefore to this rate multiplied by the fraction η of a species produced in the sputtering process. The C fraction locked in the fullerene from diffuse absorption bands in the visible is about 0.05–0.1% of the carbon abundance, i.e. ~ 10−7H. Adopting an ionisation rate of ζ = 10−16 s−1, waiting 100 My would require η ~ 1.5 × 10−3 to explain the observed abundance. This efficiency is that of the sputtered carbon finally locked into the interstellar fullerenes. This value cannot rule out the contribution of electronic sputtering and calls for quantitative studies.

5 Concluding remarks

Emitted molecular fragments from a laboratory analogue of carbonaceous interstellar dust irradiated by swift heavy ion simulating cosmic ray effects were measured. Large PAHs have been detected with the neutral population dominating over the cations. This experimental results highlights the importance of the post-photoionisation facility to monitor the release of neutral molecules. The distribution of the neutral PAHs suggests desorption of rather intact adsorbed PAHs even with sizes as high as PAHs containing up to 50 carbon atoms. Cationic fullerenes up to 120 carbon atoms were observed with a broad mass distribution. Geometrical constraints probably prevented the detection of neutral fullerenes, but this has still to be proven. These experiments provide a proof of principle of a top-down scenario for the production of large carbonaceous molecules in the ISM involving cosmic radiation of interstellar dust and electronic sputtering. Efficiencies have to be measured to quantify the effective contribution of this energetic process.


Financial support from the CNRS/INSU French national program on Physics and Chemistry of the Interstellar Medium is acknowledge. This work has been supported by the European Union’s Horizon 2020 research and innovation program and grant agreement number 6544002.


  1. Acke, B., Bouwman, J., Juhasz, A., et al. 2010, ApJ, 718, 558 [NASA ADS] [CrossRef] [Google Scholar]
  2. Akhtar, M., Ahmad, B., & Ahmad, S. 1997, Phys. Lett. A, 234, 367 [NASA ADS] [CrossRef] [Google Scholar]
  3. Alata, I., Cruz-Diaz, G. A., Munoz Caro, G. M., & Dartois, E. 2014, A&A, 569, A119 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  4. Alata, I., Jallat, A., Gavilan, L., et al. 2015, A&A, 584, A123 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  5. Alfe, M., Apicella, B., Tregrossi, A., & Ciajolo, A. 2008, Carbon, 46, 2059 [CrossRef] [Google Scholar]
  6. Apicella, B., Wang, X., Armenante, M., Bruno, A., & Spinelli, N. 2009, in Proceedings of the 32nd Meeting on Combustion, Naples, Italy, I–12 [Google Scholar]
  7. Berné, O., Mulas, G., & Joblin, C. 2013, A&A, 550, L4 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  8. Berne, O., Montillaud, J., & Joblin, C. 2015, A&A, 577, A133 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  9. Bitensky, I., Demirev, P., & Sundqvist, B. 1993, Nucl. Instrum. Methods Phys. Res. B, 82, 356 [NASA ADS] [CrossRef] [Google Scholar]
  10. Bitensky, I., Brinkmalm, G., Demirev, P., et al. 1994, Int. J. Mass Spectrom. Ion Process., 138, 159 [NASA ADS] [CrossRef] [Google Scholar]
  11. Boesl, U., Neusser, H., Weinkauf, R., & Schlag, E. 1982, J. Phys. Chem., 86, 4857 [CrossRef] [Google Scholar]
  12. Breuer, L., Meinerzhagen, F., Herder, M., et al. 2016, J. Vac. Sci. Technol. B, 34, 03H130 [CrossRef] [Google Scholar]
  13. Brinkmalm, G., Barofsky, D., Demirev, P., et al. 1992, Chem. Phys. Lett., 191, 345 [NASA ADS] [CrossRef] [Google Scholar]
  14. Brinkmalm, G., Demirev, P., Fenyo, D., et al. 1993, Phys. Rev. B, 47, 7560 [NASA ADS] [CrossRef] [Google Scholar]
  15. Cami, J., Bernard-Salas, J., Peeters, E., & Malek, S. 2010, Science, 329, 1180 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
  16. Campbell, E., Ulmer, G., & Hertel, I. 1991, Phys. Rev. Lett., 67, 1986 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
  17. Campbell, E., Ulmer, G., & Hertel, I. 1992, Z. Phys. D. Atom. Mol. Cluster., 24, 81 [NASA ADS] [CrossRef] [Google Scholar]
  18. Campbell, E., Holz, M., Gerlich, D., & Maier, J. 2015, Nature, 523, 322 [NASA ADS] [CrossRef] [Google Scholar]
  19. Campbell, E., Holz, M., Maier, J., et al. 2016, ApJ, 822, 17 [NASA ADS] [CrossRef] [Google Scholar]
  20. Carpentier, Y., Féraud, G., Dartois, E., et al. 2012, A&A, 548, A40 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  21. Chen, T., Gatchell, M., Stockett, M. H., et al. 2015, J. Chem. Phys., 142, 144305 [NASA ADS] [CrossRef] [Google Scholar]
  22. Dartois, E., Chabot, M., Pino, T., et al. 2017, A&A, 599, A130 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  23. Demirev, P., Brinkmalm, G., Eriksson, J., et al. 1994, Carbon, 32, 809 [CrossRef] [Google Scholar]
  24. Desgroux, P., Mercier, X., & Thomson, K. 2013, Proc. Combust. Inst., 34, 1713 [CrossRef] [Google Scholar]
  25. Faccinetto, A. 2009, PhD Thesis, Université Lille 1, France [Google Scholar]
  26. Faccinetto, A., Desgroux, P., Ziskind, M., Therssen, E., & Focsa, C. 2011, Combust. Flame, 158, 227 [CrossRef] [Google Scholar]
  27. Faccinetto, A., Focsa, C., Desgroux, P., & Ziskind, M. 2015, Environ. Sci. Technol., 49, 10510 [NASA ADS] [CrossRef] [Google Scholar]
  28. Gavilan, L., Alata, I., Le, K. C., et al. 2016, A&A, 586, A106 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  29. Gavilan, L., Le, K. C., Pino, T., et al. 2017, A&A, 607, A73 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  30. Ghosh, S., Avasthi, D. K., Tripathi, A., et al. 2004, Nucl. Instrum. Methods Phys. Res. B, 219, 973 [NASA ADS] [CrossRef] [Google Scholar]
  31. Johansson, K. O., Dillstrom, T., Elvati, P., et al. 2017, Proc. Combust. Inst., 36, 799 [CrossRef] [Google Scholar]
  32. Jones, A. P., Kohler, M., Ysard, N., Bocchio, M., & Verstraete, L. 2017, A&A, 602, A46 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  33. Kroto, H., Heath, J., O’Brien, S., Curl, R., & Smalley, R. 1985, Nature, 318, 162 [NASA ADS] [CrossRef] [Google Scholar]
  34. Léger, A., Jura, M., & Omont, A. 1985, A&A, 144, 147 [NASA ADS] [Google Scholar]
  35. Mai, M., Weidtmann, B., Marpe, M., & Wucher, A. 2013, Nucl. Instrum. Methods Phys. Res. B, 317, 130 [NASA ADS] [CrossRef] [Google Scholar]
  36. Meinerzhagen,F., Breuer, L., Bukowska, H., et al. 2016, Rev. Sci. Instrum. Inst., 87 [Google Scholar]
  37. Montillaud, J., Joblin, C., & Toublanc, D. 2013, A&A, 552, A15 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  38. Papaleo, R., Demirev, P., Eriksson, J., Hakansson, P., & Sundqvist, B. 1996, Int. J. Mass Spectrom. Ion Process., 152, 193 [NASA ADS] [CrossRef] [Google Scholar]
  39. Pilleri, P., Joblin, C., Boulanger, F., & Onaka, T. 2015, A&A, 577, A16 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  40. Pino, T., Dartois, E., Cao, A.-T., et al. 2008, A&A, 490, 665 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  41. Qayyum, A., Ahmad, B., Akhtar, M., & Ahmad, S. 1998, Eur. Phys. J. D, 3, 267 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  42. Sellgren, K., Werner, M., Ingalls, J., et al. 2010, ApJ, 722, L54 [NASA ADS] [CrossRef] [Google Scholar]
  43. Shen, C. J., Greenberg, J. M., Schutte, W. A., & van Dishoeck E. F. 2004, A&A, 415, 203 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  44. Sloan, G. C. 2017, Planet. Space Sci., 149, 32 [NASA ADS] [CrossRef] [Google Scholar]
  45. Sloan, G., Jura, M., Duley, W., et al. 2007, ApJ, 664, 1144 [NASA ADS] [CrossRef] [Google Scholar]
  46. Sloan, G. C., Lagadec, E., Zijlstra, A. A., et al. 2014, ApJ, 791 [Google Scholar]
  47. Verstraete, L., Léger, A., DHendecourt, L., Dutuit, O., & Defourneau, D. 1990, A&A, 237, 436 [NASA ADS] [Google Scholar]
  48. Walder, G., Kennedy, K., & Echt, O. 1993, Z. Phys. D. Atom. Mol. Cluster., 26, S288 [NASA ADS] [CrossRef] [Google Scholar]
  49. Walker, G., Bohlender, D., Maier, J., & Campbell, E. 2015, ApJ, 812, L8 [NASA ADS] [CrossRef] [Google Scholar]
  50. Webber, W. R., & Yushak, S. M. 1983, ApJ, 275, 391 [NASA ADS] [CrossRef] [Google Scholar]
  51. Weilmunster, P., Keller, A., & Homann, K. 1999, Combust. Flame, 116, 62 [CrossRef] [Google Scholar]
  52. Yang, X. J., Glaser, R., Li, A., & Zhong, J. X. 2017, New Astron. Rev., 77, 1 [NASA ADS] [CrossRef] [Google Scholar]
  53. Ziegler, J. F., Ziegler, M. D., & Biersack, J. P. 2010, Nucl. Instrum. Methods Phys. Res. B, 268, 1818 [NASA ADS] [CrossRef] [Google Scholar]

All Figures

thumbnail Fig. 1

SIMS and SNMS measured in the 0–100 u (unified atomic mass unit) mass range.

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In the text
thumbnail Fig. 2

SIMS and SNMS measured in the 100–600 u mass range. Insets are zoom-ins around mass 300 corresponding to the mass of coronene C24H12.

Open with DEXTER
In the text
thumbnail Fig. 3

SIMS measured in the mass range above 620 u. Note that a linear background was removed.

Open with DEXTER
In the text
thumbnail Fig. 4

Number of carbon NC and hydrogen NH in the neutral PAH mass range. The colours scale with the intensity of the peaks increasing from black to red and finally yellow. The open green circles mark the H and C composition of compact PAHs up tocircumcoronene. Lower H content probably arises from emitted partially dehydrogenated fragments, while higher probably traces less compact structures.

Open with DEXTER
In the text

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