$\mathsf{^{13}}$C isotope effects on infrared bands of quenched carbonaceous composite (QCC)

Wada, Setsuko; Onaka, Takashi; Yamamura, I.; Murata, Yuko; Tokunaga, A. T.

doi:10.1051/0004-6361:20030881

Cited by 16 publications

(13 citation statements)

References 52 publications

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“…Instead, the distribution of 3 μm band correlates to the BL distribution (Vijh et al 2005a). The filmy-QCC shows infrared absorption bands in the 3 μm region as shown in previous papers (Sakata et al 1990;Wada et al 2003). Why does the ERE carrier not emit the 3.3 μm band but emit ERE?…”

Section: Ere and Ief Carriers-decomposition Of Dust Particlesmentioning

confidence: 60%

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On the Carrier of the Extended Red Emission and Blue Luminescence

Wada¹,

Mizutani²,

Narisawa³

et al. 2008

ApJ

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Filmy-QCC, an organic material synthesized in the laboratory, exhibits red photoluminescence (PL). The peak wavelength of the PL ranges from 650 to 690 nm, depending on the mass distribution of polycyclic aromatic hydrocarbon (PAH) molecules, and the emission profile is a good match for that of the extended red emission (ERE) in the Red Rectangle (RR) nebula. The quantum yield of the PL ranges from 0.009 to 0.04. When filmy-QCC is dissolved in cyclohexane, it exhibits blue PL in the wavelength range of 400-500 nm with a quantum yield of 0.12-0.16. The large width of the red PL and the large wavelength difference between the PL of the filmy-QCC as a solid film and in a solution indicate that there is a strong interaction between the components of filmy-QCC. The major components of filmy-QCC are PAHs up to 500 amu. Our laboratory data suggest that the blue luminescence observed in the RR nebula is probably caused by small PAHs in a gaseous state, and the ERE is caused by larger PAHs in dust grains.

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Section: Ere and Ief Carriers-decomposition Of Dust Particlesmentioning

confidence: 60%

“…We detected peaks of aliphatic C-H hydrocarbons in a 3 μm region of the infrared absorption spectra of the filmy-QCC (Sakata et al 1990;Wada et al 2003). Odd m species in mass spectra can be explained by molecules with substituted PAHs with side groups of alkyl (methyl, ethyl, etc.…”

Section: Mass Spectroscopymentioning

confidence: 94%

On the Carrier of the Extended Red Emission and Blue Luminescence

Wada¹,

Mizutani²,

Narisawa³

et al. 2008

ApJ

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“…The variation in the peak wavelengths suggests possible processing of the band carriers in the ISM. The origin of the difference between class A and B objects may be attributed to the inclusion of hetero atoms (Peeters et al 2002) or carbon isotopes in the band carriers (Wada et al 2003). On the other hand, the UIR band spectrum observed in the diffuse Galactic radiation does not exhibit any systematic variations in the inner part of the Galaxy (Chan et al 2001;Kahanpää et al 2003), whereas Sakon et al (2004) detected small variations in the band ratio and the peak wavelength between the inner part of the Galaxy and the outer part.…”

Section: Introductionmentioning

confidence: 89%

Detection of unidentified infrared bands in a Hαfilament in the dwarf galaxy NGC 1569 with AKARI

Onaka

Matsumoto

Sakon

et al. 2010

A&A

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Context. We report the detection of unidentified infrared (UIR) bands in a filamentary structure associated with Hα emission in the starburst dwarf galaxy NGC 1569 based on imaging and spectroscopic observations of the AKARI satellite. Aims. We investigate the processing and destruction of the UIR band carriers in an outflow from NGC 1569. Methods. We performed observations of NGC 1569 for 6 infrared bands (3.2, 4.1, 7, 11, 15, and 24 μm) with the infrared camera (IRC) onboard AKARI. Near-to mid-infrared (2−13 μm) spectroscopy of a Hα filament was also carried out with the IRC. Results. The extended structure associated with a Hα filament appears bright at 7 μm. Since the IRC 7 μm band (S7) efficiently traces the 6.2 and 7.7 μm UIR band emission, the IRC imaging observations suggest that the filament is bright at the UIR band emission. Follow-up spectroscopic observations with the IRC confirm the presence of 6.2, 7.7, and 11.3 μm emission in the filament. The filament spectrum exhibits strong 11.3 μm UIR band emission relative to the 7.7 μm band compared to the galaxy disk observed with the infrared spectrograph on Spitzer. The near-infrared spectrum also suggests the presence of excess continuum emission in 2.5−5 μm in the filament. Conclusions. The presence of the UIR bands associated with a Hα filament is found by AKARI/IRC observations. The Hα filament is thought to have been formed by the galactic outflow originating from the star-formation activity in the disk of NGC 1569. The destruction timescale of the UIR band carriers in the outflow is estimated to be much shorter (∼1.3 × 10 3 yr) than the timescale of the outflow (∼5.3 Myr). Thus it is unlikely that the band carriers survive the outflow environment. Alternatively, we suggest that the band carriers in the filaments may be produced by the fragmentation of large carbonaceous grains in shocks, which produce the Hα emission. The NIR excess continuum emission cannot be accounted for by free-free emission alone and a hot dust contribution may be needed, although the free-free emission intensity estimated from H i recombination lines has a large uncertainty.

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“…For example PAH dimers, see Rapacioli et al (this volume) for specific structures. iv) Carbon isotope effects (Wada et al 2003). The presence of 13 C in PAHs redshifts the position of the CC stretching modes and thus it will move the band further away from the observed astronomical class A 6.2 µm PAH position.…”

Section: The Pah Band Profiles and The Composition Of The Pah Familymentioning

confidence: 97%

Astronomical observations of the PAH emission bands

Peeters

2011

EAS Publications Series

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Abstract. The infrared (IR) spectra of many galactic and extragalactic objects are dominated by emission features at 3. 3, 6.2, 7.7, 8.6 and 11.2 µm, generally attributed to the IR fluorescence of Polycyclic Aromatic Hydrocarbon molecules (PAHs). These PAH bands have been found in a wide variety of environments throughout the Universe and contain up to 10% of the total power output of starforming galaxies.Ground-based telescopes, the Infrared Space Observatory (ISO) and the Spitzer Space Telescope revealed a plethora of weaker PAH bands and provided extensive evidence for significant variability in the PAH spectrum from source to source and spatially within sources. Here we review the spectral characteristics of astronomical PAHs, their dependence on the local physical conditions and the implications for the physical and chemical characteristics of the carriers.

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$\mathsf{^{13}}$C isotope effects on infrared bands of quenched carbonaceous composite (QCC)

Cited by 16 publications

References 52 publications

On the Carrier of the Extended Red Emission and Blue Luminescence

On the Carrier of the Extended Red Emission and Blue Luminescence

Detection of unidentified infrared bands in a Hαfilament in the dwarf galaxy NGC 1569 with AKARI

Astronomical observations of the PAH emission bands

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