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Home All issues Volume 568 (August 2014) A&A, 568 (2014) A95 Full HTML
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Issue
A&A
Volume 568, August 2014
Article Number A95
Number of page(s) 8
Section Atomic, molecular, and nuclear data
DOI https://doi.org/10.1051/0004-6361/201424400
Published online 28 August 2014

© ESO, 2014

1. Introduction

Polycyclic aromatic hydrocarbons (PAHs) are one of the most interesting components of the interstellar medium (ISM). The infrared (IR) spectra of different astronomical objects such as HII regions, photodissociation regions (PDRs), or asymptotic giant branch (AGB) stars and planetary nebulae (PNe) are dominated by emission features in the region between 3.3−18 μm (Peeters 2011; Draine & Li 2007). It is thought that PAHs are also carriers of these diffuse interstellar bands, the so-called DIBs (Tielens 2008). But different from laboratory – the isolation of a single species is not possible. The spectra contain a superposition of many different molecules. Therefore a sophisticated understanding of all possible subtypes is required.

With the Infrared Space Observatory (ISO) and the Spitzer Space Telescope, a great variety of PAH bands was discovered (e.g., Spitzer Special Edition 2004; Peeters et al. 2004; Bauschlicher et al. 2009). The IR spectra are dominated by prominent emission features at 3.3, 6.2, 7.7, 8.6, and 11.2 μm, and many more. These bands are known as the unidentified infrared (UIR) bands (Tielens 2008), but the characteristics of emitting PAHs remain unclear so far. There is a clear variability in the PAH spectra from source to source and spatially within sources (Peeters 2011). The high sensitivity of the space-based observations have shown that the IR emission features are omnipresent and can be found in most astronomical objects (Peeters 2011).

A spectroscopic database of PAH molecules has been published by Bauschlicher et al. (2010), which has recently been updated (Bauschlicher et al. 2014). The web site1 contains over 800 spectra of PAHs in their neutral and charged states, experimentally measured and theoretically computed. The database contains positive and negative charged molecules, PAHs with different elements substituted, or metallic-cation PAH complexes, and all of the subgroups (e.g., Bakes et al. 2001; Knorke et al. 2009; Alvaro Galué et al. 2010; Hudgins et al. 2005; Bauschlicher et al. 2008; Simon & Joblin 2007).

The influence of size and symmetry on the IR spectra of the PAHs as well as PAHs with different elements added has been studied in the past (e.g., Pauzat & Ellinger 2002; Hudgins et al. 2005; Alvaro Galué et al. 2010; Bauschlicher et al. 2008, 2009; Ricca & Bauschlicher 2009; Knorke et al. 2009). These studies have provided many insights, and much knowledge about the observed PAHs was gained. The astrophysical environments were studied in detail, but there still are many unresolved questions.

thumbnail Fig. 1

PAH molecules studied in this work. Top: coronene and pyrene in their normal state. Bottom: the defected form. For C24H12d and C16H10d the 5-member rings and 7-member rings are shown.
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The PAHs are thought to be formed in the late stages of the AGB phase (Allamandola et al. 1989). Especially carbon-rich AGB stars are an ideal environment for PAH formation. During the growth of large, aromatic molecules, the (5, 7)-member ring defects play an important role.

The molecules chosen in this work are pyrene (C16H10) and coronene (C24H12), shown in Fig. 1. Both of them are unique for different reasons and can be considered to be limiting or prototypical cases. Coronene and pyrene are among the smallest hydrocarbons that can exhibit a (5, 7)-member ring defect, pyrene is the smallest one. Previous work on (5, 7)-member ring defects (Yu & Nyman 2012) has raised the suspicion that effects of such defects might be more intriguing with decreasing size of the PAHs. To study these small systems is thought to be an important step toward a substantial understanding of the role of (5, 7)-ring defects play for the IR spectra of PAHs. Another peculiarity of these two molecules appears by investigating the minimum energy pathway between the ground and (5, 7)-ring defected states, see Sect. 3. Coronene proceeds via a Stone-Wales transition (Harris 2009) from its ground to its defected state, but shows no Stone-Wales defect in the defected form. On the other hand, pyrene shows no Stone-Wales transition, but instead the defected pyrene exhibits a Stone-Wales defect. The latter is the underlying reason for the third respect in which the two studied molecules can be regarded as limiting and prototypical. Whereas pyrene retains some of its symmetry because of the symmetry exhibited by the Stone-Wales defect itself, coronene loses much more of its symmetry (see Fig. 1).

This work is structured as follows: in Sect. 2, we briefly describe the methodology and the computational methods used in this work. In Sect. 3.1, we discuss the effect of (5, 7)-membered ring defects on the IR absorption spectra of pyrene, coronene, and their (singly charged) cations and anions. This is followed by an exploration of parts of the potential energy surface of the neutral species to investigate their thermodynamic stability in Sect. 3.2. In Sect. 4 we present an alternative pathway that could lead to the formation of these defected PAHs in the interstellar matter and discuss their stability, observability and detectability from an astrophysical point of view.

2. Models and computational methods

Pyrene (C16H10) consists in its original condition of four 6-membered rings. In the defected state, all four rings are changed into two 5-membered and two 7-membered rings. The size of the molecule remains the same. The defected state is referred to as C16H10d. The normal coronene (C24H12) consists of a 6-membered ring in the center, surrounded by a ring of six more 6-membered rings. The defect changes the ring in the center into a 7-membered ring, and two adjacent rings are changed into 5-membered rings. Coronene with defect is denoted as C24H12d.

The geometry optimizations and harmonic frequency calculations were performed using the B3LYP density functional, which uses Becke’s three parameter hybrid exchange functional (Becke 1993) and a correlation functional of Lee et al. comprising both local and nonlocal terms (Lee et al. 1988), in conjunction with the 4-31G basis set (Frisch et al. 1984). It has been shown previously (Langhoff 1996; Bauschlicher & Langhoff 1997; Boersma et al. 2010a) that this combination of a functional basis set and a single-scale factor of 0.958 leads to harmonic frequencies that agree excellently well with experiments. IR spectra, calculated using this level of theory, of molecules for which no experimental data exists are at least consistent with the data of other PAH molecules of the same size and charge (Ricca et al. 2011). For the (5, 7)-ring defected molecules no experimental data exists for comparison. Furthermore, it has been shown in previous work that diffuse functions do not need to be included even for the investigation of anions (Ricca et al. 2011). However, considering intensities, it has been reported that B3LYP might yield erroneous results if there are two electronic states with essentially the same energy (Ricca et al. 2011). In such cases it is known that HF calculations might favor an asymmetric wave-function, which can lead to the consequence that hybrid functionals are more likely to have problems than generalized gradient approximation (GGA) functionals because of the inclusion of HF exchange (Sherrill 1999). For this reason we repeated our harmonic frequency calculations with the GGA functional of Becke and Perdew, that is, BP86 (Becke 1988; Perdew 1986) using a single-scale factor of 0.986. However, when B3LYP encounters no problems, it is usually more accurate than GGA functionals. Hence, we report results using the BP86 functional only when the B3LYP results deviate strongly in terms of intensities. Otherwise, the B3LYP data are taken.

thumbnail Fig. 2

Theoretical IR spectra of coronene and pyrene and the defected forms in the region of 6−10 μm. Cations, neutrals, and anions are shown from left to right. The calculations were performed using the B3LYP density functional. The changes in intensity and shifts in position of the bands are clearly visible. UIR bands at 6.2 μm, 6.9 μm, 7.7 μm and 8.6 μm are indicated by dashed lines.
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thumbnail Fig. 3

Theoretical IR spectra of coronene and pyrene and the defected forms in the region of 10−15 μm. Cations, neutrals, and anions are shown from left to right. The calculations were performed using the B3LYP density functional. The changes in intensity and shifts in position of the bands are small, but still visible. UIR bands at 11.0 μm, 12.8 μm, and 13.6 μm are indicated by dashed lines.
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All spectra are IR absorption spectra. The observations of the PAHs in space deal with the emission lines of the molecules. To be able to compare our theoretical spectra with the observed spectra, different line widths were taken for the different bands, in a similar manner as in Ricca et al. 2011. The synthetic IR spectra were generated via folding the frequencies and intensities with a normalized Gaussian line-shape function. Typically, a FWHM of 30 cm-1 was taken as the natural line width of emission lines of molecules in the ISM (Bauschlicher et al. 2009). For bands shorter than 10 μm, we used this value (see Fig. 2). To obtain better resolved spectra, we adopted a value of 10 cm-1 for the line with in the region between 10 and 15 μm (see Fig. 3). It is thought that this value is more consistent with current observations as well as theoretical calculations (Bauschlicher et al. 2009). To continue to match the observations (Van Kerckhoven et al. 2000) in the 15−20 μm bands, a FWHM of 5 cm-1 was used there (see Fig. 4). For longer wavelengths, the FWHM will decrease even more. We adopted a value of 1 cm-1 for all wavelengths above 20 μm (see Fig. 5). This is sufficient for our purposes in this region, because we focus on the impact of the defects in the spectra.

The harmonic frequency calculations provide as unit for the synthetic spectra cm-1 on the x-axis. Since the astrophysical observations are commonly presented in μm, we converted the x-axis to μm to compare the results. The y-axis indicates the integrated intensities, given as a cross-section in units of 105 cm2 mol-1.

thumbnail Fig. 4

Theoretical IR spectra of coronene and pyrene and the defected forms in the region of 15−20 μm. Cations, neutrals, and anions are shown from left to right. The calculations were performed using the B3LYP density functional. There are hardly any similarities between normal and defected form. UIR bands at 16.4 μm, 17.4 μm, and 17.8 μm are indicated by dashed lines.
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thumbnail Fig. 5

Theoretical IR spectra of coronene and pyrene and the defected forms in the region of 20−100 μm. The calculations were performed using the B3LYP density functional. Additionally, there is the cm-1 axis on the top. The changes in intensity and shifts in position of the bands are clearly visible.
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To explore the parts of the potential energy surface that connect the ground-state geometries with those corresponding to the (5, 7)-ring defected states, we used the STQN method, which uses a quadratic synchronous-transit approach to find the transition state and then completes the optimization using a quasi-Newton algorithm (Peng & Schlegel 1993; Peng et al. 1996). Subsequently, we performed frequency calculations to verify that we found a transition state of first order (yielding one and only one imaginary frequency), and then the reaction path was followed by integrating the intrinsic reaction coordinate (IRC; Fukui 1981) to verify that the transition state connects the ground and defected states. To assess the energetics more accurately, we performed these calculations again using the B3LYP functional, but now in conjunction with Dunning’s cc-pVTZ basis set (Dunning 1989). The energies of the ground, (5, 7)-ring defected and transition states were then calculated even more accurately using the G4(MP2) extrapolation approach (Curtiss et al. 2007), including a zero-point energy correction. These types of calculations were only performed for the neutral species, however.

All electronic structure calculations were performed with the software Gaussian 09 (Frisch et al. 2009).

3. Results

3.1. IR spectra

The resulting spectra of both coronene and pyrene and for the defected state of the molecules and their cations and anions are given in Figs. 2−5. All spectra of the unmodified coronene and pyrene were compared with the NASA Ames PAH IR Spectroscopic Database (Bauschlicher et al. 2010). We obtained exactly the same IR spectra for both molecules, which is at least an indication for the reliability of all our computed data.

The first part of the spectra is the 6−10 μm region, shown in Fig. 2. In this region, the vibrations are in accordance with CC stretches and CH in-plane bends. Especially in the 6−10 μm area it is thought that the influence of ionization is very strong, the IR emission can increase sharply. The emission originates from vibrationally excited cations, proceeding via electronic excitation and intersystem crossing to highly excited vibrational levels of the ground state (Allamandola et al. 1989). Our spectra follow this trend, the cations as well as the anions show clearly increased intensities compared with the neutral molecule. The cations show a peak near the 6.2 μm band, whether defected or not. But the typical bands at 7.7 μm and 8.6 μm cannot be found for our molecules. Only the defected form of coronene shows peaks near these bands. In general, for cations, neutrals, and anions, the intensities of the defected molecules seem to exceed the results of the normal molecules. The positions of the lines are shifted in the defect state. The addition of defects leads to more bands than are found in the normal molecules. For better comparison with the UIR bands, dashed lines are drawn at 6.2 μm, 6.9 μm, 7.7 μm, and 8.6 μm.

In Fig. 3 the 10−15 μm region of the spectra is shown. The lines in this area originate from C-H out-of-plane bending motion. It is expected that the undefected molecules show bands near 11.2 μm, wherein the peaks of the cations occur at shorter wavelengths, of the anions at longer wavelengths. Our spectra confirm this, even the molecules with defect follow this trend. We note that the differences between defected and defect-free molecules is not that big than in the 6−10 μm region, but still not negligible. The cationic molecules still have clearly higher intensities than the others in this region. Again, for better comparison with the UIR bands, dashed lines are drawn at 11.0 μm, 12.8 μm, and 13.6 μm.

Figure 4 shows the 15−20 μm region of the spectra. In this region, the intensities strongly decrease, but cations and anions still have higher intensities than the neutrals. The changes produced by adding the defects are strong, the molecules with defects have no similarities with the molecules without defects. There seems to be a charge effect on the 16.4 μm UIR band of the defected PAHs, it can be seen for the defected coronene, whereas pyrene has a strong peak at lower wavelengths. Dashed lines are drawn at 16.4 μm, 17.4 μm, and 17.8 μm because UIR bands at these positions have been thought to originate from PAHs.

The 20−100 μm region of the spectra in the far-IR is shown in Fig. 5. Only the neutral species are included because the influence of ionization is very weak at these wavelengths. In this region changes caused by the defects in intensities and positions of the lines can be found as well.

Thus all areas of the spectra show more significant deviations than was reported in previous works. Yu & Nyman (2012) have hypothesized that there is a size dependence for the effects of the (5, 7)-member ring defect on the IR spectra of PAHs. The impact of such defects could increase with decreasing size of the PAHs. Ricca et al. (2011) also found that the differences appear to become smaller as the size of the PAH increases. Boersma et al. (2010b) and Ricca et al. (2010) discussed the difficulties of drawing any definitive conclusions about the specific PAH species that might be responsible for the UIR bands attributed to the PAHs. Our investigations represent the limiting cases with respect to the size of the PAHs. The investigation of these small systems is assumed to be an important step to a significant understanding of the role of the (5, 7)-member ring defects for IR spectra of PAHs.

Table 1

Ground-state energies and energy differences for neutral (q = 0), anionic (q = −1), and cationic (q = + 1) species.

Table 2

Adiabatic ionization energies and electron affinities.

thumbnail Fig. 6

Relative energies (in eV) for the structures along the minimum energy pathway connecting defect-free and defected a) pyrene and b) coronene. Note that for pyrene two transition structures are involved (TS1 and TS2) that are separated by a shallow local minimum (LM), see also Fig. 7. In contrast, the barrier separating coronene and the (5, 7)-ring defected coronene corresponds to a Stone-Wales-transition structure, see also Fig. 7.
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thumbnail Fig. 7

Possible formation pathways of the (5, 7)-member ring defects depicted for a)–e) pyrene and f)–h) coronene.
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3.2. Energetics

Table 1 summarizes the ground-state energies and the energy difference between (5, 7)-member ring defected and ground states. Adiabatic ionization energies and electron affinities as obtained at the B3LYP/4-31G level of theory for pyrene and coronene are shown in Table 2. Literature values for the ionization energies and electron affinities of pyrene and coronene are 7.7, 7.21, 0.59, and 0.47 eV, respectively (Kazakov et al. 1999; Schroeder et al. 2001; Chen & Cooks 1995; Duncan et al. 1999). By comparison, both are underestimated by 0.5−1 eV for both molecules. This is not surprising since the 4-31G basis set is far from being complete. For the energy difference between ground and defected states we note, however, that the estimates yielded by the B3LYP/4-31G model chemistry are close to those resulting from a more accurate treatment using G4(MP2) extrapolations to investigate the minimum energy reaction paths on the potential energy surfaces (PES) for the neutral species. These accurate calculations results in energy differences of 2.23 eV for pyrene and 2.31 eV for coronene. The reaction pathways on the PES connecting ground and defected states are schematically depicted in Fig. 6 for the two neutral molecules pyrene and coronene. For pyrene we do not observe a Stone-Wales transition that would lead to the Stone-Wales defect, but a more complicated path via two vastly nonplanar transition states (TS1 and TS2 in Figs. 6 and 7) and a shallow local minimum (LM) configuration in between (LM in Figs. 6 and 7) that is almost the same as the two transition structures, see Fig. 7. To find this pathway it has been necessary to replace the usual 6-31G(2df, p) basis set (Ditchfield et al. 1971) used in the G4(MP2) theory by the slightly larger cc-pVTZ basis set, because with the former one it was not possible to achieve convergence for the local minimum structure. Furthermore, the geometry that is achieved when the central C-C bond in pyrene is just rotated by 45 degrees, corresponding to a transition structure of second order that exhibits two imaginary frequencies. For coronene we observe that the transition between the ground and defected state proceeds via the Stone-Wales transition, but as is obvious from the structure of the molecule, do not result in a Stone-Wales defect (see Fig. 7). The minimum activation barriers for transforming pyrene and coronene into their (5, 7)-ring defected forms are found to be 8.21 and 8.41 eV. The corresponding reverse barriers are 5.92 and 6.10 eV, and are thus close to the 6.47 and 6.41 eV found for the neutral and cationic C48H18 PAH model studied in an earlier investigation (Yu & Nyman 2012). Hence, the energy required to build (5, 7)-ring defects seems to be insensitive to the actual size of the PAH molecule, which is in line with the explanation given for the high barriers in the previous study of Yu & Nyman (2012). Therein, it was shown that for the transformation two π C-C bonds have to be broken, which requires much energy. The latter should obviously be quite insensitive to the size of the molecule.

4. Discussion

4.1. Formation

The environment of carbon-rich AGB stars seems to be the perfect place for PAH formation (Allamandola et al. 1989). One of the most important molecules in carbon-rich environments is C2H2, which is presumably the parent molecule in PAH formation (Allamandola et al. 1989). A detailed study on the growth of carbon molecules was made by Whitesides & Frenklach (2010), who also discussed the role of 5-member rings.

The defect may not only be formed in the growing process of the PAHs. In addition, transitions between the ground state and the defected form might play a role (see Fig. 7). As we have discussed in Sect. 3.2, the minimum activation barriers for transforming pyrene and coronene into their (5, 7)-member ring defected forms are 8.21 eV for pyrene and 8.41 eV for coronene. The energy required to build (5, 7)-member ring defects seems to be insensitive to the size of the PAH molecule. We now discuss how these barriers can be overcome. A very recent study of Champeaux et al. (2014) discussed the physical interactions of PAHs with stellar particle radiation, especially the interaction of coronene with protons. An interaction will not necessarily destroy or fragment the molecules. If the particle has enough energy and exactly hits on a knot of the molecule, a change of the ring structure from 6-membered rings into pentagons and heptagons may occur (Huber et al. 2013). The particle has to have at least enough energy to overcome the activation barrier. Clearly, not every hit with sufficient energy will cause a deformation, but also maybe ionization, dissociation, or hydrogenation. Too much energy will lead to the destruction of the molecule. The spatial angle for the hit should be around 90°, ± 10°, but this parameter was not investigated in detail and may also vary. Possible candidate particles can be found in different environments such as stellar winds, AGB stars and winds, or PNe. The probability for a collision in such environments can be estimated as follows: from energy and momentum conservation and the parameters of a typical C-rich AGB stellar wind, the collision probability can be calculated. Even these very simplified calculations show a few hits per second for a simple stellar wind up to a distance of about 20 R⊙. Recent observations showed evidence of mixed chemistry with emission from both silicate dust and PAHs (Guzman-Ramirez et al. 2011) or the simultaneous presence of mid-IR features attributed to neutral fullerene molecules (i.e., C60) and PAHs (García-Hernández et al. 2013). A very recent study discussed that PAHs are located and even formed at the outer edge of dense tori (Guzman-Ramirez et al. 2014). The presence of a dense torus has been strongly associated with the rich and mixed chemistry seen in these regions. All these observed environments strongly enable the transition from the ground state to the defect state of the molecules.

thumbnail Fig. 8

Comparison between the IR spectra of pyrene (green) and pyrene exhibiting the (5, 7)-member ring defect (blue), both neutral. The changes in intensity and shifts in positions of the lines in the spectrum are clearly visible. In gray we show the transmission curve of the atmosphere for conditions common for Paranal.
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4.2. Observations

To sketch the possibilities of observing the effects of the (5, 7)-member ring defects, Figs. 8 and 9 show a comparison of the defected molecule with the normal one in the region from 0−20 μm. In addition, the transmission curve of the Earth’s atmosphere is plotted, calculated with the code LNFL/LBLRTM (Clough et al. 2004) for airmass =1 and a one-year averaged atmospheric profile scaled to 3 mm PWV (precipitable water vapor), a typical PWV value for Paranal. This conveys an impression of the best detectable lines and bands best suited for a study. Figure 8 shows pyrene and its defected form, Fig. 9 shows coronene and its defected form, all of them in their neutral states.

thumbnail Fig. 9

Comparison between the IR spectra of coronene (green) and coronene exhibiting the (5, 7)-member ring defect (blue), both neutral. Same as for pyrene, the lines change in intensity and position within the spectrum. In gray we plot again the transmission curve of our atmosphere to indicate observability and detectability.
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5. Conclusions

The PAHs observed in astrophysical environments are thought to be formed mainly in the surroundings of C-rich AGB stars. The growth of the aromatic hydrocarbon rings includes effects of 5- and 7-member ring defects (Whitesides & Frenklach 2010). The still unidentified IR features seen in the observations require additional computational, laboratory, and observational investigations. We have performed a theoretical study of the IR spectra of PAHs containing (5, 7)-member ring defects. Using the density functional theory, we investigated the effect of these defects on the IR spectra of pyrene (C16H10) and coronene (C24H12) and their cations and anions. In addition, we explored parts of the potential energy surface of the neutral species.

The addition of (5, 7)-member ring defects into the skeleton of these small PAH molecules has an astonishing strong effect on the IR spectra. Pyrene and coronene that exhibited a (5, 7)-member ring defect lost their typical spectroscopic signature. There is a clear difference in the spectrum of the unmodified molecule and the one exhibiting the (5, 7)-member ring defect. Coronene and pyrene are amongst the smallest PAHs that exhibit such ring defects. This implies that the internal heat quantity taken by other parts after a hit is smallest in these molecules, and therefore the probability of reaching the energy of the barrier is high. In this study we represented the boundaries in terms of the size of the PAHs. The minimum energy pathways between the ground and (5, 7)-member ring defected states exhibit lowest activation barriers of 8.21 eV for pyrene and 8.41 eV for coronene for the transformation. The corresponding reverse barriers are 5.92 eV for pyrene and 6.10 eV for coronene, which agrees well with the results of Yu et al. (2012). The size of the PAH molecule seems to have no influence on the energy required to build (5, 7)-ring defects. Whereas pyrene retains some of its symmetry because of the symmetry exhibited by the Stone-Wales defect itself, coronene loses much more of its symmetry. The formation of these (5, 7)-ring defects in PAHs may be well supported in AGB stars or PNe. These environments strongly enable the transition from the ground state to the defect state. Therefore the knowledge of the IR spectra of these molecules can facilitate future investigations in understanding of the unidentified IR emission bands. To study the (5, 7)-membered ring defects in other PAH molecules is believed to be an important step to a significant understanding of the UIR bands and the IR spectra of PAHs, although the defects in astronomical PAH molecules will be extremely difficult to detect with current instruments and tools. But future telescopes and instruments are promising a chance for observing these molecules and their defects. High-resolution IR spectrographs of the European Extremely Large Telescope (E-ELT) type telescopes will allow a spatial and wavelength segregation from telluric lines in even highly obscured wavelength domains (e.g., METIS-IFU with a spectral resolution of R ~ 100 000, Brandl et al. 2012). The James Webb Space Telescope (JWST) will allow completing studies of the bright stars observed the IR with extremely high signal-to-noise ratios (e.g., MIRI at the JWST, Wright et al. 2010).

Acknowledgments

S.Ö. and S.E.H. acknowledge support by the Austrian Fonds zur Wissenschaftlichen Forschung, FWF DK+ project Computational Intersiciplinary Modelling W1227-N16. This work was supported by the Austrian Ministry of Science BMWF as part of the UniInfrastrukturprogramm of the Focal Point Scientific Computing at the University of Innsbruck.

References

  1. Allamandola, L. J., Tielens, A. G. G. M., & Barker, J. R. 1989, ApJS, 71, 733 [NASA ADS] [CrossRef] [Google Scholar]
  2. Alvaro Galué, H., Pirali, O., & Oomens, J. 2010, A&A, 517, A15 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  3. Bakes, E. L. O., Tielens, A. G. G. M., Bauschlicher, C. W., Hudgins, D. M., & Allamandola, L. J. 2001, ApJ, 560, 261 [NASA ADS] [CrossRef] [Google Scholar]
  4. Bauschlicher, C. W., & Langhoff, S. R. 1997, Spectrochim. Acta A, 53, 1225 [NASA ADS] [CrossRef] [Google Scholar]
  5. Bauschlicher, C. W., Peeters, E., & Allamandola, L. J. 2008, ApJ, 678, 316 [NASA ADS] [CrossRef] [Google Scholar]
  6. Bauschlicher, C. W., Peeters, E., & Allamandola, L. J. 2009, ApJ, 697, 311 [NASA ADS] [CrossRef] [Google Scholar]
  7. Bauschlicher, C. W., Boersma, C., Ricca, A., et al. 2010, ApJS, 189, 341 [NASA ADS] [CrossRef] [Google Scholar]
  8. Becke, A. D. 1988, Phys. Rev. A, 38, 3098 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
  9. Becke, A. 1993, J. Chem. Phys., 98, 5648 [NASA ADS] [CrossRef] [Google Scholar]
  10. Boersma, A. J., Coquière, D., & Geerdink, D., 2010a, Nature Chem., 2, 991 [NASA ADS] [CrossRef] [Google Scholar]
  11. Boersma, C., Bauschlicher, C. W., Allamandola, L. J., et al. 2010b, A&A, 511, A32 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  12. Boersma, C., Bauschlicher, C. W., Ricca, A., et al. 2014, ApJS, 211, 8 [NASA ADS] [CrossRef] [Google Scholar]
  13. Brandl, B. R., Lenze, R., Pantin, E., et al. 2012, SPIE, 8446, 13 [Google Scholar]
  14. Champeaux, J. P., Moretto-Capelle, P., Cafarelli, P., et al. 2014, MNRAS, 441, 1479 [NASA ADS] [CrossRef] [Google Scholar]
  15. Chen, G., & Cooks, R. G. 1995, J. Mass Spectr., 30, 1167 [CrossRef] [Google Scholar]
  16. Clough, S. A., Shephard, M. W., Mlawer, E. J., et al. 2004, JQRST, 91, 233 [Google Scholar]
  17. Curtiss, L. A., Redfern, P. C., & Raghavachari, K. 2007, J. Chem. Phys., 127, 124105 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
  18. Ditchfield, R., Hehre, W. J., & Pople, J. A. 1971, J. Chem. Phys., 54, 724 [NASA ADS] [CrossRef] [Google Scholar]
  19. Draine, B. T., & Li, A. 2007, ApJ, 657, 810 [NASA ADS] [CrossRef] [Google Scholar]
  20. Duncan, M. A., Knight, A. M., Negishi, Y., et al. 1999, Chem. Phys. Lett., 309, 49 [NASA ADS] [CrossRef] [Google Scholar]
  21. Dunning, Jr., T. H. 1989, J. Chem. Phys., 90, 1007 [NASA ADS] [CrossRef] [Google Scholar]
  22. Frisch, M. J., Pople, J. A., & Binkley, J. S. 1984, J. Chem. Phys., 80, 3265 [NASA ADS] [CrossRef] [Google Scholar]
  23. Frisch, M. J., Trucks, G. W., Schlegel, H. B., et al. 2009, Gaussian 09, Revision A.1, Gaussian, Inc., Wallingford CT [Google Scholar]
  24. Fukui, K. 1981, Accounts of Chemical Research, 14, 363 [CrossRef] [Google Scholar]
  25. García-Hernández, D. A., Cataldo, F., & Manchado, A. 2013, MNRAS, 434, 415 [NASA ADS] [CrossRef] [Google Scholar]
  26. Guzman-Ramirez, L., Zijlstra, A. A., Níchuimín, R., et al. 2011, MNRAS, 414, 1667 [NASA ADS] [CrossRef] [Google Scholar]
  27. Guzman-Ramirez, L., Lagadec, E., Jones, D., Zijlstra, A. A., & Gesicki, K. 2014, MNRAS, 441, 1, 364 [NASA ADS] [CrossRef] [Google Scholar]
  28. Harris, P. J. F. 2009, Carbon Nanotube Science: Synthesis, Properties and Applications (Cambridge University Press) [Google Scholar]
  29. Huber, S. E., Mauracher, A., & Probst, M. 2013, AIP Advances, 3, 122104 [NASA ADS] [CrossRef] [Google Scholar]
  30. Hudgins, D. M., Bauschlicher, C. W., & Allamandola, L. J. 2005, ApJ, 632, 3116 [NASA ADS] [CrossRef] [Google Scholar]
  31. Kazakov, S. M., Kaputerko, M. N., & Suchkov, V. A. 1999, J. Appl. Spectr., 66, 375 [NASA ADS] [CrossRef] [Google Scholar]
  32. Knorke, H., Langer, J., Oomens, J., & Dopfer, O. 2009, ApJ, 706, L66 [NASA ADS] [CrossRef] [Google Scholar]
  33. Langhoff, S. R. 1996, J. Chem. Phys., 100, 2819 [CrossRef] [Google Scholar]
  34. Lee, C., Yang, W., & Parr, R. G. 1988, Phys. Rev. B, 37, 785 [NASA ADS] [CrossRef] [Google Scholar]
  35. Pauzat, F., & Ellinger, Y. 2002, Chem. Phys., 280, 267 [NASA ADS] [CrossRef] [Google Scholar]
  36. Peeters, E. 2011, EAS Pub. Ser., 46, 137 [CrossRef] [EDP Sciences] [Google Scholar]
  37. Peeters, E., Allamandola, L. J., Hudgins, D. M., Hony, S., & Tielens, A. G. G. M. 2004, ASP Conf. Ser., 309, 141 [NASA ADS] [Google Scholar]
  38. Peng, C., & Schlegel, H. B. 1993, Israel J. Chem., 33, 449 [CrossRef] [Google Scholar]
  39. Peng, C., Ayala, P. Y., Schlegel, H. B., & Frisch, M. J. 1996, J. Comput. Chem., 17, 49 [CrossRef] [Google Scholar]
  40. Perdew, J. P. 1986, Phys. Rev. B, 33, 8822 [NASA ADS] [CrossRef] [Google Scholar]
  41. Ricca, A., & Bauschlicher, C. W. 2009, ApJ, 698, 275 [NASA ADS] [CrossRef] [Google Scholar]
  42. Ricca, A., Bauschlicher, C. W., Mattioda, A. L., Boersma, C., & Allamandola, L. J. 2010, ApJ, 709, 42 [NASA ADS] [CrossRef] [Google Scholar]
  43. Ricca, A., Bauschlicher, C. W., & Allamandola, L. J. 2011, ApJ, 729, 94 [NASA ADS] [CrossRef] [Google Scholar]
  44. Schroeder, D., Loos, J., Schwarz, H., et al. 2001, Helvet. Chim. Acta, 84, 1625 [CrossRef] [Google Scholar]
  45. Sherrill, C. D., Lee, M. S., & Head-Gordon, M. 1999, Chem. Phys. Lett., 302, 425 [NASA ADS] [CrossRef] [Google Scholar]
  46. Simon, A., & Joblin, C. 2007, J. Phys. Chem. A, 111, 9745 [CrossRef] [PubMed] [Google Scholar]
  47. Spitzer First Observations Special Edition 2004, ApJS, 154 [Google Scholar]
  48. Tielens, A. G. G. M. 2008, ARA&A, 46, 289 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  49. Van Kerckhoven, C., Hony, S., Peeters, E., et al. 2000, A&A, 357, 1013 [Google Scholar]
  50. Whitesides, R., & Frenklach, M. 2010, J. Phys. Chem. A, 2010, 689 [CrossRef] [Google Scholar]
  51. Wright, G. S., Rieke, G., Boeker, T., et al. 2010, SPIE, 7731, 10 [NASA ADS] [Google Scholar]
  52. Yu, H. G., & Nyman, G. 2012, ApJ, 751, 7 [NASA ADS] [CrossRef] [Google Scholar]

All Tables

Table 1

Ground-state energies and energy differences for neutral (q = 0), anionic (q = −1), and cationic (q = + 1) species.

In the text
Table 2

Adiabatic ionization energies and electron affinities.

In the text

All Figures

thumbnail Fig. 1

PAH molecules studied in this work. Top: coronene and pyrene in their normal state. Bottom: the defected form. For C24H12d and C16H10d the 5-member rings and 7-member rings are shown.
Open with DEXTER
In the text
thumbnail Fig. 2

Theoretical IR spectra of coronene and pyrene and the defected forms in the region of 6−10 μm. Cations, neutrals, and anions are shown from left to right. The calculations were performed using the B3LYP density functional. The changes in intensity and shifts in position of the bands are clearly visible. UIR bands at 6.2 μm, 6.9 μm, 7.7 μm and 8.6 μm are indicated by dashed lines.
Open with DEXTER
In the text
thumbnail Fig. 3

Theoretical IR spectra of coronene and pyrene and the defected forms in the region of 10−15 μm. Cations, neutrals, and anions are shown from left to right. The calculations were performed using the B3LYP density functional. The changes in intensity and shifts in position of the bands are small, but still visible. UIR bands at 11.0 μm, 12.8 μm, and 13.6 μm are indicated by dashed lines.
Open with DEXTER
In the text
thumbnail Fig. 4

Theoretical IR spectra of coronene and pyrene and the defected forms in the region of 15−20 μm. Cations, neutrals, and anions are shown from left to right. The calculations were performed using the B3LYP density functional. There are hardly any similarities between normal and defected form. UIR bands at 16.4 μm, 17.4 μm, and 17.8 μm are indicated by dashed lines.
Open with DEXTER
In the text
thumbnail Fig. 5

Theoretical IR spectra of coronene and pyrene and the defected forms in the region of 20−100 μm. The calculations were performed using the B3LYP density functional. Additionally, there is the cm-1 axis on the top. The changes in intensity and shifts in position of the bands are clearly visible.
Open with DEXTER
In the text
thumbnail Fig. 6

Relative energies (in eV) for the structures along the minimum energy pathway connecting defect-free and defected a) pyrene and b) coronene. Note that for pyrene two transition structures are involved (TS1 and TS2) that are separated by a shallow local minimum (LM), see also Fig. 7. In contrast, the barrier separating coronene and the (5, 7)-ring defected coronene corresponds to a Stone-Wales-transition structure, see also Fig. 7.
Open with DEXTER
In the text
thumbnail Fig. 7

Possible formation pathways of the (5, 7)-member ring defects depicted for a)–e) pyrene and f)–h) coronene.
Open with DEXTER
In the text
thumbnail Fig. 8

Comparison between the IR spectra of pyrene (green) and pyrene exhibiting the (5, 7)-member ring defect (blue), both neutral. The changes in intensity and shifts in positions of the lines in the spectrum are clearly visible. In gray we show the transmission curve of the atmosphere for conditions common for Paranal.
Open with DEXTER
In the text
thumbnail Fig. 9

Comparison between the IR spectra of coronene (green) and coronene exhibiting the (5, 7)-member ring defect (blue), both neutral. Same as for pyrene, the lines change in intensity and position within the spectrum. In gray we plot again the transmission curve of our atmosphere to indicate observability and detectability.
Open with DEXTER
In the text

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