8-13 micron spectra of NGC 7027, BD +30 3639 and NGC 6572.

Gillett, F. C.; Forrest, W. J.; Merrill, K. M.

doi:10.1086/152211

Cited by 298 publications

(166 citation statements)

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“…The spectrum in Figure 12 is somewhat puzzling because none of the features can be readily identified with the usual features found in dust: silicates, unidentified infrared (UIR; Gillett et al 1973) or polycyclic aromatic hydrocorbon (PAH; Allamandola et al 1985) bands, etc. The feature at 11.3 μm-or one very much like it-occurs in both oxygen-rich dust (olivine feature) and carbon-rich dust (UIR bands and some PAH features), though the common wavelength between the two is a coincidence.…”

Section: Dustmentioning

confidence: 99%

NOVA V2362 CYGNI (NOVA CYGNI 2006):SPITZER,SWIFT, AND GROUND-BASED SPECTRAL EVOLUTION

Lynch

Woodward

Gehrz

et al. 2008

The Astronomical Journal

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Nova V2362 Cygni has undergone a number of very unusual changes. Ground-based spectroscopy initially revealed a normal sequence of events: the object faded and its near-infrared emission lines gradually shifted to higher excitation conditions until about day 100 when the optical fading reversed and the object slowly brightened. This was accompanied by a rise in the Swift X-ray telescope flux and a sudden shift in excitation of the visible and IR spectrum back to low levels. The new lower excitation spectrum revealed broad line widths and many P-Cygni profiles, all indicative of the ejection of a second shell. Eventually, dust formed, the X-ray brightnessapparently unaffected by dust formation-peaked and then declined, and the object faded at all wavelengths. The Spitzer dust spectra revealed a number of solid-state emission features that, at this time, are not identified.

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Section: Dustmentioning

confidence: 99%

NOVA V2362 CYGNI (NOVA CYGNI 2006):SPITZER,SWIFT, AND GROUND-BASED SPECTRAL EVOLUTION

Lynch

Woodward

Gehrz

et al. 2008

The Astronomical Journal

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“…Although spectral features in the visible to UV range of wavelengths are observed and carried by carbonaceous materials (Désert et al 1990;Draine 2003;Zubko et al 2004), this fraction of cosmic dust is mainly observed through remote infrared (IR) spectroscopy. In particular, the mid-IR emission features observed in many astronomical objects (Gillett et al 1973), often called the aromatic infrared bands (AIBs), trace carbonaceous particles of a few nanometers often attributed to PAHs in most of the astrophysical literature (Léger & Puget 1984;Crawford et al 1985;Tielens 2008). Heated by UV and visible starlight, these nanoparticles emit through their vibrational bands thanks to an out-of-equilibrium process known as the transient heating mechanism (Puget & Léger 1989;Allamandola et al 1989;Draine & Li 2001).…”

Section: Introductionmentioning

confidence: 99%

Nanostructuration of carbonaceous dust as seen through the positions of the 6.2 and 7.7μm AIBs

Carpentier

Féraud

Dartois

et al. 2012

A&A

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“…First detected in two planetary nebulae by Gillett et al (1973), UIBs have since been ubiquitously observed in dusty environments along a large number of interstellar sight-lines covering a wide range of excitation conditions (see e.g. Allamandola et al 1989).…”

Section: Introductionmentioning

confidence: 99%

Testing the “strong” PAHs hypothesis

Mulas

Malloci

Benvenuti

2003

A&A

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Abstract. In Paper I (Malloci et al. 2003) we proved the profile invariance of the first permitted electronic transition of the typical Polycyclic Aromatic Hydrocarbon cation C 32 H 14 + as a first necessary check for the "strong" PAHs hypothesis. In this paper we derive a quantitative relation between the intensities of the former band, which ought to be observable in absorption in the visible range, and those of the far-IR bands, which are predicted by the PAH model to be simultaneously present in emission. Contrary to the mid-IR bands, collectively known as "Unidentified Infrared Bands" (UIBs), which do not discriminate specific molecules, the far IR, skeletal bands can be expected to be a fingerprint of each single species. This fact provides a number of independent constraints which must be simultaneously fulfilled for a successful PAH identification. Our approach thus offers a powerful criterion for the identification of specific PAHs, both in the presently available ISO data and in those of the forthcoming SIRTF and Herschel missions. As an interesting by-product, we quantitatively evaluate the impact of isotopic substitutions ( 13 C→ 12 C and D →H) on the resulting infrared emission bands.

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8-13 micron spectra of NGC 7027, BD +30 3639 and NGC 6572.

Cited by 298 publications

References 0 publications

NOVA V2362 CYGNI (NOVA CYGNI 2006):SPITZER,SWIFT, AND GROUND-BASED SPECTRAL EVOLUTION

NOVA V2362 CYGNI (NOVA CYGNI 2006):SPITZER,SWIFT, AND GROUND-BASED SPECTRAL EVOLUTION

Nanostructuration of carbonaceous dust as seen through the positions of the 6.2 and 7.7μm AIBs

Testing the “strong” PAHs hypothesis

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