IDENTIFICATION OF MORE INTERSTELLAR ${{\rm{C}}}_{60}^{+}$ BANDS

Walker, G. A. H.; Bohlender, D.; Maier, John P.; Campbell, E. K.

doi:10.1088/2041-8205/812/1/l8

Cited by 148 publications

(162 citation statements)

References 16 publications

(19 reference statements)

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“…The power density (flux) is determined with a calibrated profile meter. interstellar absorption of + C 60 was reported by Walker et al (2015).…”

Section: Absorption Cross-sectionsmentioning

confidence: 78%

“…This led to the first unequivocal identification of a molecular ion as a carrier of two DIBs . The observation of two more DIBs consistent with laboratory measurements of weaker + C 60 absorption bands was then reported (Walker et al 2015). With the discovery of + C 60 in the interstellar medium, long-standing interest in fullerenes (Kroto 1988) and derivatives (Kroto & Jura 1992) and their role in astrochemistry has reawakened.…”

Section: Introductionmentioning

confidence: 84%

“…At high laser fluence, the curves decrease to a common asymptotic value, N 1 , which is due to the number of C C Telluric water lines (WV) seriously contaminate the spectral regions covered by the laboratory bands for + C 60 (see Figure 1 in Walker et al 2015). To first order, these can be eliminated by normalization using spectra of an unreddened, rapidly rotating star taken at the same air mass.…”

Section: Absorption Cross-sectionsmentioning

confidence: 99%

“…An unreddened standard matching as closely as possible the spectral type and luminosity of the reddened target star was also observed to correct for weak stellar features. Details of HD 183143 and the standard stars are given in Table 1 of Walker et al (2015).…”

Section: Absorption Cross-sectionsmentioning

confidence: 99%

“…Full details of the reductions are given in Walker et al (2015). Attempts to correct for WV by chopping between the target and the WV standard were not entirely successful as significant residuals for the stronger WV lines remain.…”

Section: Absorption Cross-sectionsmentioning

confidence: 99%

See 4 more Smart Citations

Gas Phase Absorption Spectroscopy of and in a Cryogenic Ion Trap: Comparison With Astronomical Measurements*

Campbell

Holz

Maier

et al. 2016

ApJ

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114

144

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Recent low-temperature laboratory measurements and astronomical observations have proved that the fullerene cation + C 60 is responsible for four diffuse interstellar bands (DIBs). These absorptions correspond to the strongest bands of the lowest electronic transition. The gas phase spectrum below 10 K is reported here for the full wavelength range encompassed by the electronic transition. The absorption spectrum of + C 70 , with its origin band at Å 7959.2 , has been obtained under similar laboratory conditions. Observations made toward the reddened star HD 183143 were used in a specific search for the absorption of these fullerene cations in diffuse clouds. In the case of + C 60 , one further band in the astronomical spectrum at Å 9348.5 is identified, increasing the total number of assigned DIBs to five. Numerous other + C 60 absorptions in the laboratory spectrum are found to lie below the astronomical detection limit. Special emphasis is placed on the laboratory determination of absolute absorption cross-sections. For + C 60 this directly yields a column density, ( ) + N C 60 , of´-2 10 cm 13 2 in diffuse clouds, without the need to rely on theoretical oscillator strengths. The intensity of the + C 70 electronic transition in the range 7000-8000 Å is spread over many features of similar strength. Absorption cross-section measurements indicate that even for a similar column density, the individual absorption bands of + C 70 will be too weak to be detected in the astronomical spectra, which is confirmed giving an upper limit of 2 mÅ to the equivalent width.

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“…The power density (flux) is determined with a calibrated profile meter. interstellar absorption of + C 60 was reported by Walker et al (2015).…”

Section: Absorption Cross-sectionsmentioning

confidence: 78%

Section: Introductionmentioning

confidence: 84%

Section: Absorption Cross-sectionsmentioning

confidence: 99%

Section: Absorption Cross-sectionsmentioning

confidence: 99%

Section: Absorption Cross-sectionsmentioning

confidence: 99%

See 3 more Smart Citations

Gas Phase Absorption Spectroscopy of and in a Cryogenic Ion Trap: Comparison With Astronomical Measurements*

Campbell

Holz

Maier

et al. 2016

ApJ

Self Cite

114

144

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Fullerene im Weltraum

Maier¹,

Campbell²

2017

Angewandte Chemie

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Abbildung 1. Die diffusen interstellaren Banden setzen sich aus etwa fünfhundert Absorptionsbanden zusammen, die in den Spektren von durch interstellare Wolken laufendem Sternenlicht beobachtetwerden. Als Ursache nimmt man Elektronenübergänge von mehratomigen Molekülen an, die dort vorkommen. Dieses astronomische Rätsel ist zwar schon seit hundert Jahren bekannt, doch hier wurden erstmals mehrere Absorptionen dem Buckminsterfulleren-Kation C 60 + zugeordnet. Angewandte ChemieAufsätze 5001

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Fullerenes in Space

Maier

Campbell

2017

Angew Chem Int Ed

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In 1985 the football structure of C , buckminsterfullerene was proposed and subsequently confirmed following its macroscopic synthesis in 1990. From the very beginning the role of C and C in space was considered, particularly in the context of the enigmatic diffuse interstellar bands. These are absorption features found in the spectra of reddened star light. The first astronomical observations were made around one hundred years ago and despite significant efforts none of the interstellar molecules responsible have been identified. The absorption spectrum of C was measured in a 5 K neon matrix in 1993 and two prominent bands near 9583 Å and 9645 Å were observed. On the basis of this data the likely wavelength range in which the gas phase C absorptions should lie was predicted. In 1994 two diffuse interstellar bands were found in this spectral region and proposed to be due to C . It took over 20 years to measure the absorption spectrum of C under conditions similar to those prevailing in diffuse clouds. In 2015, sophisticated laboratory experiments led to the confirmation that these two interstellar bands are indeed caused by C , providing the first answer to this century old puzzle. Here, we describe the experiments, concepts and astronomical observations that led to the detection of C in interstellar space.

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IDENTIFICATION OF MORE INTERSTELLAR ${{\rm{C}}}_{60}^{+}$ BANDS

Cited by 148 publications

References 16 publications

Gas Phase Absorption Spectroscopy of and in a Cryogenic Ion Trap: Comparison With Astronomical Measurements*

Gas Phase Absorption Spectroscopy of and in a Cryogenic Ion Trap: Comparison With Astronomical Measurements*

Fullerene im Weltraum

Fullerenes in Space

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