Spectroscopy of polycyclic aromatic hydrocarbons and very small grains in photodissociation regions

By Mathias Rapacioli, Christine Joblin, P. Boissel, F. Calvo, F. Spiegelman. 2005

210 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/3069e1af8adaff07c1cf6cc6f45c7cbb56ab1237

How researchers see this paper

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In Astronomy and Astrophysics

1. E. D. Cunha
2. S. Charlot
3. D. Elbaz
4. E. Peeters
5. L. Allamandola
6. John-David T. Smith
7. C. Bauschlicher
8. C. Conroy

In Atmospheric Science

1. E. Peeters
2. L. Allamandola
3. N. Ysard
4. A. Jones
5. C. Bauschlicher
6. L. Verstraete
7. J. Bernard
8. D. Elbaz

Citations in the corpus

• THE INFRARED SPECTRA OF VERY LARGE IRREGULAR POLYCYCLIC AROMATIC HYDROCARBONS (PAHs): OBSERVATIONAL PROBES OF ASTRONOMICAL PAH GEOMETRY, SIZE, AND CHARGE (2009, background): “…of this emission vary between different objects and spatially within extended objects (e.g., Peeters et al. 2002a, 2004; Bregman & Temi 2005; Rapacioli et al. 2005; Berné et al. 2007; Sellgren et al. 2007, and references therein), revealing the nature of the specific PAH molecules present…”
• A simple model to interpret the ultraviolet, optical and infrared emission from galaxies (2008, background): “…emission tends to peak in the ‘photo-dissociation regions’ (PDRs) at the interface between ionised and molecular gas in the outskirts of H ii regions, where PAH molecules can survive and transient heating is most efficient (e.g., Cesarsky et al. 1996; Verstraete et al. 1996; Rapacioli et al. 2005).”
• Polycyclic aromatic hydrocarbon processing in interstellar shocks (2009, background): “The observed spectra also show evidence for PAH clusters containing a few hundred C-atoms (Bregman et al. 1989; Rapacioli et al. 2005; Berné et al. 2007) as well as very small dust grains (∼30 Å; Désert et al. 1990).”
• The global dust SED: tracing the nature and evolution of dust with DustEM (2010, background): “…grain growth and fragmentation), which are primarily reflected in the variation of the dust size distribution and, in particular, in the ratio of the abundance small grains (a <∼ 10 nm) to large grains (e.g. Stepnik et al. 2003; Paradis et al. 2009a; Rapacioli et al. 2005; Berné et al. 2007).”
• FORMATION OF FULLERENES IN H-CONTAINING PLANETARY NEBULAE (2010, background): “The only difference is the clear presence of a broad 6–9 μm emission feature in SMP SMC 16 which is not seen in Tc 1 and attributable to hydrogenated amorphous carbon (HAC), very small grains, or PAH clusters (Tielens 2008; Buss et al. 1993; Rapacioli et al. 2005).”
• Analysis of the emission of very small dust particles from Spitzer spectro-imagery data using blind signal separation methods (2007, methodology): “Applying SVD to the observations of different PDRs, Boissel et al. (2001) and then Rapacioli et al. (2005) (RJB hereafter) were able to extract the spectra of different types of very small dust particles: PAH-like speciesand VSGs.”