IR spectroscopy of gas-phase C60−

Kupser, Peter; Steill, Jeffrey D.; Meijer, Gerard; Helden, Gert von

doi:10.1039/b811862k

Cited by 20 publications

(19 citation statements)

References 41 publications

(69 reference statements)

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“…C − 60 is expected to be abundant in models and hence could be searched for in space. The strongest vibrational bands of C − 60 are around 17.5 and 7.3 µm (Kupser et al 2008). The 17.5 µm band is difficult to identify because of the presence of PAH emission at 17.4 µm.…”

Section: Abundances Of C 60mentioning

confidence: 99%

“…C60− is expected to be abundant in models and hence could be searched for in space. The strongest vibrational bands of C60− are around 17.5 and 7.3 μ m (Kupser et al 2008). The 17.5 μ m band is difficult to identify because of the presence of PAH emission at 17.4 μ m. A band at 7.3 μ m seems present in the spectrum of the Chamaeleon line of sight, however this region of the spectrum is quite noisy and higher sensitivity data will be required to confirm this.…”

Section: Abundances Of C60mentioning

confidence: 99%

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Detection of buckminsterfullerene emission in the diffuse interstellar medium

Berné

Cox

Mulas

et al. 2017

A&A

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Emission of fullerenes in their infrared vibrational bands has been detected in space near hot stars. The proposed attribution of the diffuse interstellar bands at 9577 and 9632 Å to electronic transitions of the buckminsterfullerene cation (i.e. C + 60 ) was recently supported by new laboratory data, confirming the presence of this species in the diffuse interstellar medium (ISM). In this Letter, we present the detection, also in the diffuse ISM, of the 17.4 and 18.9 µm emission bands commonly attributed to vibrational bands of neutral C 60 . According to classical models that compute the charge state of large molecules in space, C 60 is expected to be mostly neutral in the diffuse ISM. This is in agreement with the abundances of diffuse C 60 we derive here from observations.

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Section: Abundances Of C 60mentioning

confidence: 99%

Section: Abundances Of C60mentioning

confidence: 99%

Detection of buckminsterfullerene emission in the diffuse interstellar medium

Berné

Cox

Mulas

et al. 2017

A&A

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“…IR spectra have been reported in condensed and gas phases, [7][8][9][10] and spectra for ionized forms are available as well. 4,8,11,12 The high cosmic abundance of carbon combined with the high stability of fullerenes 13 initiated a quest for their detection in inter-and circumstellar environments. [14][15][16][17] This search culminated in the identifications of neutral C 60 and C 70 in a young planetary nebula (Tc1) 1 based on diagnostic IR features.…”

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confidence: 99%

The infrared spectrum of protonated buckminsterfullerene C60H+

2019

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Although fullerenes have long been hypothesized to occur in interstellar environments, their actual unambiguous spectroscopic identification is of more recent date. 1-4 C 60 , C 70 and C + 60 now constitute the largest molecular species individually identified in the interstellar medium (ISM). Fullerenes have significant proton affinities and it was suggested that C 60 H + is likely the most abundant interstellar analogue of C 60 . 5 We present here the first laboratory infrared (IR) spectrum of gaseous C 60 H + . Symmetry breaking relative to C 60 produces an IR spectrum that is much richer than that of C 60 . The experimental spectrum is used to benchmark theoretical spectra indicating that the B3LYP density functional with the 6-311+G(d,p) basis set accurately reproduces the spectrum. Comparison with IR emission spectra from two planetary nebulae, SMP LMC56 and SMC16, that have been associated with high C 60 abundances, indicate that C 60 H + is a plausible contributor to their IR emission.Buckminsterfullerene C 60 is undoubtedly one of the most iconic molecules of our time. Since its discovery in 1985, 6 its physico-chemical properties have been extensively characterized, including its ion chemistry and spectroscopic properties. IR spectra have been reported in condensed and gas phases, 7-10 and spectra for ionized forms are available as well. 4,8,11,12 The high cosmic abundance of carbon combined with the high stability of fullerenes 13 initiated a quest for their detection in inter-and circumstellar environments. [14][15][16][17] This search culminated in the identifications of neutral C 60 and C 70 in a young planetary nebula (Tc1) 1 based on diagnostic IR features. Accurate gas-phase laboratory spectra in the near-IR range led to the identification of C + 60 as carrier of two of the diffuse interstellar bands near 9600Å. 4 The question of whether or not fullerenes can form in H-rich regions of the interstellar medium (ISM) has been under debate. 1,3 Hydrogenation produces stable fullerene derivatives and partially hydrogenated fullerenes (fulleranes) have been suggested to occur in circumstellar envelopes and in the ISM 3,18,19 . On the other hand, hydrogenation and the concomitant change in orbital hybridization from sp 2 to sp 3 reduces the stability of the fullerene cage, which under the conditions of the ISM would likely lead to dehydrogenation and restoration of the original fullerene 20 or to breakdown of the carbon cage. 5 However, in this latter paper, Kroto also noted that protonation does not compromise cage stability and hypothesized that "protonated C 60 is likely to be the most abundant fullerene analogue," analogous to high abundances of protonated carbon monoxide, HCO + .Ion chemistry studies 21 have determined the proton affinity (PA) of C 60 at 860 kJ/mol. This relatively high value, just above the PA of ammonia, makes C 60 H + (Figure 1a) one of the most relevant stable fullerene derivatives and underpins Kroto's statement above. However, a) Corresponding author: j.oomens@science.ru.nl t...

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“…However, an additional sharp signal at 1397 cm –1 (indicated by an arrow) appears. The IR spectra of the fullerene anions are also dominated by four F 1u modes. − The first three bands at 527, 576, and 1183 cm –1 coincide with the modes of fullerene C 60 . However, a significant shift toward lower frequencies is observed for the fourth band.…”

Section: Resultsmentioning

confidence: 94%

Polypyrrole Nanoparticles Doped with Fullerene Uniformly Distributed in the Polymeric Phase: Synthesis, Morphology, and Electrochemical Properties

et al. 2018

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Composites of polypyrrole and fullerene C60 were prepared by the introduction of fullerene during polymerization of pyrrole initiated by the oxidation of pyrrole oligomers with C60. Composites were precipitated in the form of spherical particles, and their sizes ranged from 20 to 400 nm depending on the time of polymerization. Fullerene C60 nanocrystals with approximate size of 1 nm were uniformly distributed within the polymeric material. The amount of fullerene incorporated into polypyrrole depended on the C60 concentration in the solution used for the composite formation. An investigation of the composite using infrared spectroscopy indicated partial charge transfer between polypyrrole chains and fullerene nanocrystals. Such process was also confirmed by the theoretical investigation of electronic properties of composite. The composites were electrochemically active over a large potential window. At negative potentials, fullerene nanocrystals were reduced. In the positive potential range, polypyrrole chains were oxidized. Both processes were accompanied by complex ion transfer between supporting electrolyte solution and composite solid phase immobilized at the electrode surface.

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IR spectroscopy of gas-phase C60−

Cited by 20 publications

References 41 publications

Detection of buckminsterfullerene emission in the diffuse interstellar medium

Detection of buckminsterfullerene emission in the diffuse interstellar medium

The infrared spectrum of protonated buckminsterfullerene C60H+

Polypyrrole Nanoparticles Doped with Fullerene Uniformly Distributed in the Polymeric Phase: Synthesis, Morphology, and Electrochemical Properties

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