Fullerene-containing MCPNe

The formation of fullerenes: clues from new C, C, and (possible) planar C detections in Magellanic Cloud Planetary Nebulae

D. A. García-Hernández11affiliation: Instituto de Astrofísica de Canarias, C/ Via Láctea s/n, 38200 La Laguna, Spain; agarcia@iac.es, amt@iac.es 22affiliation: Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38205 La Laguna, Spain , S. Iglesias-Groth11affiliation: Instituto de Astrofísica de Canarias, C/ Via Láctea s/n, 38200 La Laguna, Spain; agarcia@iac.es, amt@iac.es 22affiliation: Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38205 La Laguna, Spain , J. A. Acosta-Pulido11affiliation: Instituto de Astrofísica de Canarias, C/ Via Láctea s/n, 38200 La Laguna, Spain; agarcia@iac.es, amt@iac.es 22affiliation: Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38205 La Laguna, Spain , A. Manchado11affiliation: Instituto de Astrofísica de Canarias, C/ Via Láctea s/n, 38200 La Laguna, Spain; agarcia@iac.es, amt@iac.es 22affiliation: Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38205 La Laguna, Spain 33affiliation: Consejo Superior de Investigaciones Científicas, Spain , P. García-Lario44affiliation: Herschel Science Centre. European Space Astronomy Centre, Research and Scientific Support Department of ESA. Villafranca del Castillo, P.O. Box 50727. E-28080 Madrid. Spain; Pedro.Garcia-Lario@sciops.esa.int , L. Stanghellini55affiliation: National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA; shaw@noao.edu, letizia@noao.edu , E. Villaver66affiliation: Departamento de Física Teórica C-XI, Universidad Autónoma de Madrid, E-28049 Madrid, Spain; eva.villaver@uam.es , Richard A. Shaw55affiliation: National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA; shaw@noao.edu, letizia@noao.edu and F. Cataldo77affiliation: Istituto Nazionale di Astrofisica - Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy; franco.cataldo@fastwebnet.it 88affiliation: Actinium Chemical Research, Via Casilina 1626/A, 00133 Rome, Italy

We present ten new Spitzer detections of fullerenes in Magellanic Cloud Planetary Nebulae, including the first extragalactic detections of the C molecule. These new fullerene detections together with the most recent laboratory data permit us to report an accurate determination of the C and C abundances in space. Also, we report evidence for the possible detection of planar C in some of our fullerene sources, as indicated by the detection of very unusual emission features coincident with the strongest transitions of this molecule at 6.6, 9.8, and 20 m. The infrared spectra display a complex mix of aliphatic and aromatic species such as hydrogenated amorphous carbon grains (HACs), PAH clusters, fullerenes, and small dehydrogenated carbon clusters (possible planar C). The coexistence of such a variety of molecular species supports the idea that fullerenes are formed from the decomposition of HACs. We propose that fullerenes are formed from the destruction of HACs, possibly as a consequence of shocks driven by the fast stellar winds, which can sometimes be very strong in transition sources and young PNe. This is supported by the fact that many of our fullerene-detected PNe show altered [NeIII]/[NeII] ratios suggestive of shocks as well as P-Cygni profiles in their UV lines indicative of recently enhanced mass loss.

astrochemistry — circumstellar matter — infrared: stars — planetary nebulae: general — stars: AGB and post-AGB
slugcomment: To appear in ApJ

1 Introduction

Fullerenes had been predicted since the 70s (Osawa et al. 1970) as a possible carbon assemblage in the Universe, but have remained elusive in the astrophysical context until recently, when C and C were detected in the young Planetary Nebula (PN) Tc 1 (Cami et al. 2010) under conditions which were claimed to be in agreement with the original laboratory studies on the formation of fullerenes (Kroto et al. 1985; Kratschmer et al. 1990; de Vries et al. 1993), this is under hydrogen-poor conditions. More recently, García-Hernández et al. (2010, 2011) have challenged our understanding of the fullerene formation in space, showing that, contrary to general expectation, fullerenes (usually accompanied by polycyclic aromatic hydrocarbon (PAH) emission) are efficiently formed in H-rich circumstellar environments. The suggestion was made that both fullerenes and PAHs can be formed by the photochemical processing of hydrogenated amorphous carbon grains (HACs), which should be a major constituent in the circumstellar envelope of C-rich evolved stars. The detection of fullerenes in a larger sample of PNe is essential to answer key questions about fullerene formation in space. In this context, we must note that C has also been detected in the interstellar medium (Sellgren et al. 2010), and in a proto-PN (Zhang & Kwok 2011). The latter raises the exciting possibility that considerable gas-phase physical and chemical processing of dust occurs just after the Asymptotic Giant Branch (AGB) phase, during which most of the circumstellar dust is formed (e.g., Wallerstein & Knapp 1998). Fullerenes, being relatively hardy molecules (Cataldo et al. 2009), may survive indefinitely in space playing an important role in circumstellar/interstellar chemistry.

From the experimental point of view, it is important to know the temperature dependence of the wavelength (and width) and of the strength (e.g., molar absorptivity) of the C and C infrared bands. Very recent laboratory spectroscopy of C and C (Iglesias-Groth et al. 2011) has provided this detailed information. Moreover, PNe in the Magellanic Clouds (MCPNe hereafter) offer the opportunity of obtaining an accurate determination of the fullerene abundances in space. In this letter, we report ten new Spitzer detections of C and C fullerenes in MCPNe together with the first possible detection of planar C in space, which provide us with crucial information about fullerene formation in PNe.

2 Infrared spectra of fullerene-containing MCPNe

García-Hernández et al. (2010) reported that SMP-SMC 16 showed obvious C bands in its Spitzer/IRS spectrum, acquired by Stanghellini et al. (2007) within a sample of 41 MCPNe. Here we have re-analized in more detail the full sample of IRS spectra mentioned above and those from an additional sample of 25 MCPNe also observed with Spitzer/IRS (Bernard-Salas et al. 2009). We have obtained the corresponding residual spectra by subtracting the dust continuum emission between 5 and 38 m, which is represented by 3-7 order polynomials fitted at spectral locations free from any dust or gas feature. A careful inspection of the residual spectra reveals the fullerene signatures in 10 additional objects (6 SMC and 4 LMC PNe, see Table 1). Flux measurements (errors 3040%) were done in the residual spectra by subtracting a local baseline and fitting gaussians (García-Hernández et al., in preparation; hereafter, GH2011). We list our targets in Table 1, where we also provide the central star temperatures, the H fluxes, carbon abundances, electron temperatures and densities, total hydrogen and carbon masses of the nebulae. Most of these newly detected C-containing MCPNe also show broad dust emission features at 11.5 and 30 m, which sometimes are accompanied by other broad dust features at 6-9 and 15-20 m (see Stanghellini et al. 2007; Bernard-Salas et al. 2009). Bernard-Salas et al. (2009) found that the strength of the 11.5 m feature decreases with increasing [NeIII]/[NeII]111The ratio of the flux from [Ne III] m to that of [Ne II] m (hereafter, [Ne III]/[Ne II]). ratio (taken as an indicator of the radiation field hardness). However, SMC 16 and LMC 02 display the lowest [NeIII]/[NeII] ratios (Table 2) in our sample and the 11.5m feature is barely detected in SMC 16 and completely absent in LMC 02. A low [NeIII]/[NeII] ratio may be explained if the [NeII] 12.8m line is excited by shocks (see Sect. 3).

In Fig. 1 we display the residual spectra, where the expected positions of the four C bands are marked with dashed vertical lines. A few of the C sources also display relatively strong and isolated C features at 12.6, 13.8, 14.9, 15.6, 17.3, 17.6, and 18.7 m. In particular, C is clearly detected in SMC 24 and LMC 02 for which high-resolution (R600) Spitzer spectra are available (Fig. 2). We can neither confirm nor exclude the presence of C in other sources because of the much lower resolution of their Spitzer spectra, similarly to what we discovered for SMC 16 (García-Hernández et al. 2010). SMC 24 and LMC 02 display an infrared spectrum richer than Tc 1 (Fig.2) with several unidentified features such as those at 16.0, 16.1, 16.6, 18.0, 18.3, and 18.4 m. The identification of these features will be studied elsewhere

The Spitzer spectra of fullerene MCPNe show that a complex mixture of aliphatic and aromatic species is usually present. A broad 69 m emission, which can be attributed to HACs, large PAH clusters or very small grains (Tielens 2008), is seen with different strengths in most of our sources (Fig. 1). The 69 m feature is more intense in SMC 16, 24, and LMC 02222Bernard-Salas et al. (2009) identified the 69 m emission in SMC 24 and LMC 02 with HACs. and displays a shape different to the other sources. Narrower features at 6.3 and 7.87.9 m are also detected (e.g., SMC 20, 13, LMC 25, 48, 99). The latter features are seen in a few Galactic post-AGB stars and can be attributed to large PAHs or to hydrocarbons (as a relatively unprocessed mixture of aliphatics and aromatics; Sloan et al. 2007). Additional weak features at 6.9 and 7.3 m that have been identified with aliphatic hydrocarbons and/or HACs (Sloan et al. 2007 and references therein) are also detected in SMC 24.

Interestingly, some of our sources (SMC 13, 16, 24, LMC 48, 02) display an unidentified infrared feature (UIR) at 6.6 m. This feature is accompanied by other unidentified features at 9.8 and 20 m in SMC 24 and LMC 02 (see Fig. 1). The wavelength position of the three UIR features seen in SMC 24 and LMC 02 agree very well with the strongest transitions of planar C as recently reported by Kuzmin & Duley (2011) from calculated infrared spectra using first principles density functional techniques. In SMC 24, the observed flux ratios are F(6.6)/F(9.8)=3.3 and F(6.6)/F(20.0)=1.5, which compare well with the theoretical integrated intensity (km/mole) ratios of 3.8 and 2, respectively (Kuzmin & Duley 2011). However, the 6.6 m feature is not clearly distinguised from the 69m emission in LMC 02 and the observed 9.8 m feature is 3 times more intense than that at 20 m. As in the case of the C and C fullerenes (Iglesias-Groth et al. 2011), one expects the intensity, width, and position of the infrared features of planar C to be temperature dependent. Planar C is a very stable molecule (more than the C fullerene although Jones & Seyfert (1997) show that other C conformations may be more stable than planar C). The detection of these very unusual 6.6, 9.8, and 20 m features in fullerene sources represents the first possible detection of planar C in space. However, this can only be confirmed through laboratory infrared spectroscopy at different temperatures, which is extremely difficult because of the high reactivity of C.

3 CLOUDY simulations

Recent laboratory spectroscopy of C and C fullerenes show that C displays a strong transition at 7.0 m (Iglesias-Groth et al. 2011). The 7.0m C transition is one of the strongest (with a strength very similar to the other 15.6 and 18.7m C transitions). The 7.0m C band is, however, less intense (a factor of 3) than that at 18.9 m. Indeed, the 7.0m line intensity observed in fullerene PNe cannot be explained by C alone and it has been assumed to be strongly contaminated by [ArII]6.99m (Cami et al. 2010; García-Hernández et al. 2010). We show here that the 7.0m emission seen in our sample can not be assigned to [ArII] only, rather, it should be attributed to a combination of C and C, in agreement with the recent laboratory data. To this end, we have used a photoionization code to model the relative intensity of the mid-infrared lines observed in the Spitzer/IRS spectra. Calculations were performed with CLOUDY (Ferland et al. 1998). We do not intend to find the best solution for each of the observed PNe but to make general predictions using the models. As ionizing continuum we assumed blackbody and synthetic stellar spectra (Rauch 2003) with temperatures from 25,000 to 50,000 K. Typical PN values for the bolometric luminosity (10 L) and for the radius of the photoionized region (0.1 pc) are adopted (Mendez et al. 1992; Villaver et al. 2002, 2007). There is no way to explain the extremely low [NeIII]/[NeII] ratios observed in some of our sources (see below), even taking into account large variations of these parameters (GH2011). We also assumed a density of 1800 cm at r=0.1 pc, which varies as r along the nebula and the chemical abundances by Shaw et al.(2010).

Our model predictions are compared with the observed line intensity ratios ([ArIII]/[HI] vs. [ArII/HI] and [SIV]/[SIII] vs. [NeIII]/[NeII]) in Fig. 3. The 7.0m feature cannot be explained by [ArII]6.99m emission (even taking into account maximum errors of 40% in the observed line flux ratios) and the observed 7.0m emission is much higher than expected from photoionization from the central stars (T31,000 K; Table 1). Assuming that the 7.0m emission is due to the Ar lines, the Ar abundances for these PNe would be unrealistically high. Another important conclusion can be extracted from the plot [SIV]/[SIII] vs. [NeIII]/[NeII] (Fig.3). The low [NeIII]/[NeII] ratios333Note that the [SIV]/[SIII] ratio in LMC 02 is much lower than expected for its T because the observed 18.7m emission is dominated by C. observed in many of our PNe cannot be explained by photoionization. This discrepancy can be explained if the [NeII] 12.8m line is shock-excited by the fast stellar winds from the central stars (e.g., Hartigan et al. 1987; Molinari & Noriega-Crespo 2002; van Boekel et al. 2009). A [NeII] shock-excited origin is also suggested from the common detection of P-Cygni profiles in the UV lines of our PNe (see Sect.5); a clear indication of recently enhanced mass loss and thus, of possible shocks.

4 Excitation mechanism and abundances

Previous works suggest that the fullerene emission in PNe does not originate from free gas-phase fullerene molecules, but from molecular carriers attached to solid material (Cami et al. 2010; García-Hernández et al. 2010). However, the fullerene emission seen in sources with cooler stars (T25,000 K) such as reflection nebulae (Sellgren et al. 2010), RCB stars (García-Hernández et al. 2011), and proto-PNe (Zhang & Kwok 2011) may be explained by UV-excited C molecules in the gas phase. Sellgren et al.’s (2010) calculations indicate that the intensities of the C 7.0 and 8.5 m bands versus the 18.9 m band are very sensitive to the energy of the absorbed UV photons; with the C F(17.4)/F(18.9) ratio being not sensitive to the absorbed photon energy. Assuming a solid-state origin for the observed C bands instead, we have determined the fluxes that are actually due to the 7.0 and 8.5 m C transitions444The observed 8.5m fluxes cannot be completely explained by C in four PNe (SMC 13, 24, LMC 02, 99). from the corresponding excitation diagrams (see below). The C F(7.0)/F(18.9) and F(8.5)/F(18.9) ratios are listed in Table 2 for a proper comparison with Sellgren et al.’s (2010) predictions. Interestingly, the C F(7.0)/F(18.9) and F(8.5)/F(18.9) ratios indicate typical photon energies of 5 eV for all sources in our sample independently of the effective temperature (31,000 K, when available) of the central star (see Sect.5).

We determine the fullerene temperatures for each PN from the flux measurements of the C and C transitions and adopting the temperature dependence of the absorptivity for each C and C transition (Iglesias-Groth et al. 2011). We developed an iterative process to find the best correlation coefficient of the linear relation in the Boltzmann excitation diagram, from which the temperature and the total number of emitting fullerene molecules can be estimated (GH2011). The initial temperatures were assumed in the range 1001000 K and a few iterations were required for a quick convergence. The four mid-IR transitions of C were considered, allowing the fraction of the flux of the 7m C transition as a free parameter. In the case of C, we considered the 3 or 4 transitions less contaminated by other species, obtaining also the fraction of the 7m C flux. We found very good correlation coefficients (0.890.99) for the C and C fullerenes. The temperatures and the C and C contributions to the observed 7m flux are listed in Table 2. The derived fullerene excitation temperatures are in the range 200600 K and the emission may come from solid-state fullerenes (e.g., molecules attached to dust grains). Our excitation temperatures indicate that C is cooler than C.

The fullerene-sources in the MCs provide a reliable estimate of the C and C abundances in PNe because the distances to the SMC (61 kpc; Hilditch 2005) and LMC (48.5 kpc; Freedman & Madore 2010) are accurately known, and because reliable C atomic abundances from UV spectra are available for many of these sources in the literature (Table 1). By using the above distances and following García-Hernández et al. (2010)555The H masses are estimated from the available electronic temperatures and densities and the observed H fluxes (Table 1)., the C/C and C/C abundances were estimated. We find C/C0.0030.29 (average of 0.07) and C/C0.0010.07 (average of 0.03). Our average C/C0.07 is consistent with the C abundance recently derived in a proto-PN (Zhang & Kwok 2011). By assuming a distance of 2 kpc for Tc 1 (as Cami et al. 2010), we estimate C/C=0.04 and C/C=0.005.

5 Formation of fullerenes

Laboratory studies show that the C/C ratio can tell us whether the formation of fullerenes is “bottom-up” or “top-down”, meaning growth from smaller to larger, or decay from larger to smaller units, respectively (e.g., Mansurov 2011). In combustion, one can get a high ratio (0.268.8), while in carbon vapor condensation the ratio is usually low (0.020.18) (e.g., Mansurov 2011). In addition, vapor carbon condensation experiments under H-poor conditions indicate that C fullerenes are more than 50% of total large carbon clusters (Kroto et al. 1985). The low C/C of 0.020.2 (Table 2) seems to indicate that fullerenes are formed from vapor carbon condensation. However, the fact that all known fullerene-containing PNe are H-rich and that C only represents a very small percentage of the total carbon in these stars is against the idea that fullerenes are formed under H-poor conditions. García-Hernández et al. (2010, 2011) have suggested that fullerenes can be formed from the decomposition of HACs in order to explain the simultaneous detection of C and PAHs in H-rich circumstellar envelopes. Unfortunately, the C/C ratio cannot be measured in the laboratory when fullerenes are produced from laser vaporization of HACs films. This is because it is common to see variations in the relative intensities of the C and C mass peaks even in mass spectra recorded on the same sample and under the same experimental conditions (W. Duley 2011, private communication).

Laboratory experiments show that the decomposition of HACs is sequential with small dehydrogenated PAH molecules released first, and then fullerenes and large PAH clusters (Scott et al. 1997). We have shown here that fullerene MCPNe show a complex mixture of aliphatic and aromatic species such as HACs, PAH clusters, fullerenes, and small dehydrogenated carbon clusters (possible planar C). The coexistence of this large variety of molecular species in PNe with fullerenes is strongly supported by the laboratory results obtained by Scott and colleagues, indicating that fullerenes (and PAHs) are formed from the vaporization of HACs.

However, the excitation mechanism of the fullerene emission is still not clear. Neutral fullerenes in MCPNe seem to be not excited by the bulk of UV photons coming from the central star (T31,000 K, when available); the photon energies involved to explain the observed C intensity ratios (Table 2) should be 5 eV according to Sellgren et al. (2010). Our results are not consistent with Sellgren et al. (2010) who concluded that the fullerene emission observed in the reflection nebula NGC 7023 is due to gas-phase C molecules excited by UV photons of 10 eV, in agreement with the bulk of UV photons coming from the exciting star with T=21,000 K. An alternative explanation may be that fullerenes are collisionally excited during the HACs vaporization process (i.e., grain-grain collisions) and emit even when they are still attached to the HACs surface. Other possibilities are the dehydrogenation of the molecules present in the HACs surface, before they are released to the gas phase or even shock-excited gas-phase fullerenes666Possibly this is also the case for the planar C emission observed..Presumably shocks are not energetic enough to ionize the fullerenes, but this is an open question and the shock-excited hypothesis needs further more detailed modeling work. The lack of mid-IR C features in fullerene-containing sources, may imply that fullerenes are either quickly destroyed in the gas phase or never leave the grains as free molecules. This ambiguity arises because fullerenes may be created in the vaporization process, rather than being pre-existing molecules in the original HACs sample. Indeed, the laboratory experiments use a laser at 4 eV to simulate HACs vaporization by interstellar shocks. Our Fig. 3. show that the observed [NeIII]/[NeII] ratios in many of the circumstellar shells of fullerene-containing PNe cannot be explained by photoionization and they may be strongly altered by shocks. Five fullerene-containing sources (SMC 15, 16, 20, LMC 25, 48) display P-cygni profiles in their UV lines, which are indicative of on-going mass loss with high-velocity (1000 kms) strong winds, as confirmed by HST UV spectroscopy (Stanghellini et al. 2005, 2009). Furthermore, given the low S/N in the HST ACS spectra, the presence of P-cygni profiles in SMC 24 and SMC 18 is hinted although could not be confirmed. LMC 99 and LMC 02 lack the necessary diagnostics to determine the presence of P-Cygni profiles in the UV. SMC 13, which does not show any P-Cygni profiles, displays the lowest C/C abundance, suggesting that fullerene formation is less efficient. On the other hand, fullerene production seems to be more efficient in SMC 16 and LMC 02777SMC 24 with intense 69m emission also displays a [NeIII]/[NeII] ratio lower than expected for its T of 37,800 K with the stronger outflows (as indicated by their extremely low [NeIII]/[NeII] ratios) and this is the subset of sources which display as well the more intense 69 m emission that may be attributed to HACs or PAH clusters.

In summary, we propose that shocks (i.e., grain-grain collisions) driven by the strong stellar winds are triggering the HACs processing and that fullerenes (as well as other complex aromatic and aliphatic species like possibly planar C molecules that may have been detected for the first time) evolved from the vaporization of HACs. Our interpretation can be observationally tested through high-resolution (R30,000) observations around [Ne II]12.8m, which will confirm/refute the possible [Ne II] shock-excited origin in fullerene-containing PNe.

We thank the anonymous referee and W. Duley for suggestions that help to improve the paper. Facilities: Spitzer:IRS.


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Object T log(F(H)) A(C) T N Ref. M M
(K) log(C/H)+12 (10 K) (cm) (M) (10 M)
SMC 13 31,300 -12.59 8.73 1.28 2900 (1,2,3,4,4) 0.702 4.520
SMC 15 -12.45 8.26 1.41 7500 (,5,3,6,7) 0.270 0.588
SMC 16 -12.74 8.19 1.18 4400 (,5,3,6,7) 0.210 0.392
SMC 18 -12.66 8.31 1.18 3600 (,2,3,4,4) 0.381 0.934
SMC 20 -12.47 8.25 1.38 3900 (,2,3,4,4) 0.497 1.061
SMC 24 37,800 -12.66 8.18 1.16 2800 (1,2,3,4,4) 0.411 0.747
SMC 27 43,300 -12.51 1.27 3650 (1,2,,4,4) 0.471
LMC 02 39,000 -13.18 8.14 1.21 5000 (8,7,9,6,8) 0.048 0.079
LMC 25 33,700 -12.39 8.29 1.56 3300 (10,11,12,13,13) 0.626 1.465
LMC 48 -12.48 8.40 1.00 1900 (,5,12,,6) 0.844 2.540
LMC 99 -12.54 8.77 1.22 3600 (,14,15,6,6) 0.434 3.040
Tc 1 34,100 -10.73 8.59 0.90 3000 (16,17,18,18,18) 0.0535 0.250
aafootnotetext: References for T, log(F(H)), C abundance, T, and N.bbfootnotetext: T for LMC 48 is assumed to be 10 K.ccfootnotetext: High-resolution Spitzer/IRS spectra were obtained and it was possible to detect C unambiguously.

References. – (1) Villaver et al. (2004); (2) Stanghellini et al. (2003); (3) Stanghellini et al. (2009); (4) Shaw et al. (2010); (5) Shaw et al. (2006); (6) Leisy & Dennefeld (2006); (7) Dopita et al. (1988); (8) Herald & Bianchi (2004); (9) Milanova & Kholtygin (2009); (10) Villaver et al. 2003; (11). Stanghellini et al. (2002); (12) Stanghellini et al. (2005); (13) Shaw et al. (2011, in prep.); (14) R. Shaw (2011, priv. comm.); (15) Leisy & Dennefeld (1996); (16) Preite-Martínez et al.(1989; (17) Cahn et al. (1992); (18) Williams et al. (2008).

Table 1: The sample of fullerene-containing MCPNe.
Object F(7.0)/F(18.9) F(8.5)/F(18.9) F(17.4)/F(18.9) [NeIII]/[NeII] C/C f T C/C f T C/C
(%) (%) (K) (%) (%) (K)
SMC 13 0.16 0.32 0.21 2.89 0.003 1510 45350
SMC 15 0.20 0.30 0.30 0.49 0.07 1510 29020
SMC 16 0.24 0.33 0.45 0.21 0.12 3010 41450
SMC 18 0.16 0.52 0.44 1.16 0.03 1510 36535
SMC 20 0.05 0.13 0.41 0.03 1010 22830
SMC 24 0.47 0.18 0.53 3.33 0.07 6020 51430 0.001 2010 38360 0.02
SMC 27 0.58 0.48 0.50 9.69 5010 55340
LMC 02 0.48 0.37 0.71 0.42 0.29 3010 50220 0.07 1010 32410 0.21
LMC 25 0.08 0.26 0.69 13.19 0.02 5020 30025
LMC 48 0.07 0.22 1.13 11.46 0.01 2010 27020
LMC 99 0.30 0.56 0.72 16.82 0.02 5010 44625
Tc 1 0.26 0.36 0.53 0.05 0.04 2510 41530 0.005 4010 31430 0.10
aafootnotetext: The ratio of fluxes in the C bands with the wavelenghts in brackets.bbfootnotetext: C and C contributions to the observed 7m flux.
Table 2: C intensity ratios and fullerene abundances and temperatures.
Figure 1: Residual spectra (523 m) of fullerene-MCPNe. The band positions of C (dashed) and planar C (dotted) are marked. The spectra are displaced for clarity.
Figure 2: Residual spectra (1023 m) for C-MCPNe (in comparison with Tc 1) where the C (dashed) and C (dotted) band positions are marked.
Figure 3: CLOUDY predictions vs. observations. Predictions for different ionizing continua such as blackbody spectra (red dotted line) and synthetic stellar spectra (black dashed line) at several temperatures are shown (see text).
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