Interstellar Polycyclic Aromatic Hydrocarbon Molecules

By A. Tielens. 2008

1,446 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/0e08cb69527d23769731a3c3019c1299f53232c8

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In Astronomy and Astrophysics

1. R. Garrod
2. E. Herbst
3. Mark R. Krumholz
4. B. McGuire
5. S. Ioppolo
6. H. Cuppen
7. K. Menten
8. C. Walsh

In Atmospheric Science

1. S. Ioppolo
2. R. Garrod
3. H. Cuppen
4. E. Herbst
5. T. Lamberts
6. C. Walsh
7. C. Walmsley
8. B. McGuire

In Atomic and Molecular Physics, and Optics

1. R. Garrod
2. B. McGuire
3. C. Walsh
4. S. Ioppolo
5. Steven B. Charnley
6. D. Semenov
7. H. Cuppen
8. E. Herbst

Citations in the corpus

• THE PdBI ARCSECOND WHIRLPOOL SURVEY (PAWS). I. A CLOUD-SCALE/MULTI-WAVELENGTH VIEW OF THE INTERSTELLAR MEDIUM IN A GRAND-DESIGN SPIRAL GALAXY (2013, background): “The impact of radiation onto molecular gas is typically described in the form of a photodominated (or -dissociation) region (PDR) that is nowadays defined as a region where far-UV photons dominate the energy balance or chemistry of the gas (e.g. Tielens 2008).”
• Present-day cosmic abundances - A comprehensive study of nearby early B-type stars and implications for stellar and Galactic evolution and interstellar dust models (2012, background): “From observations of the photodissociation region in the Orion nebula it is known that polycyclic aromatic hydrocarbons (PAHs) disappear as the gas becomes ionized (e.g. Tielens 2008).”
• THE NASA AMES POLYCYCLIC AROMATIC HYDROCARBON INFRARED SPECTROSCOPIC DATABASE: THE COMPUTED SPECTRA (2010, neutral): “…et al. 1973) and attributed to molecular-sized species by Sellgren (1984), is now generally attributed to polycyclic aromatic hydrocarbons (PAHs; e.g., Puget & Leger 1989; Allamandola et al. 1989; van Dishoeck 2004; Peeters et al. 2004a; Draine & Li 2007; Tielens 2008, and references therein).”
• EXTENDING THE NEARBY GALAXY HERITAGE WITH WISE: FIRST RESULTS FROM THE WISE ENHANCED RESOLUTION GALAXY ATLAS (2012, background): “The IRAC-4 band is centered on the 7.7 µm PAH band (and includes the 6.2 µm PAH band), which are small and charged molecules, while the W3 band is centered on the 11.3 PAH band, which are larger and tend toward neutralcharge molecules (cf. Tielens 2008; Draine 2011).”
• THE WISE CATALOG OF GALACTIC H ii REGIONS (2013, background): “The IRAC 8.0 μm band contains strong PAH emission at 7.7 μm and 8.6 μm, whereas the WISE 12 μm band contains PAH emission at 11.2 μm and 12.7 μm (see Tielens 2008, for a review).”
• 2018 Census of Interstellar, Circumstellar, Extragalactic, Protoplanetary Disk, and Exoplanetary Molecules (2018, background): “A substantial body of literature now seems to favor the assignment of these emission features to polyclic aromatic hydrocarbons (PAHs) (Tielens 2008), or at the very least sp2-hybridized aromatic carbon structures.”
• Grain Surface Models and Data for Astrochemistry (2017, background): “Even larger macromolecules, polyaromatic hydrocarbons (PAHs), consisting of between tens and hundreds of carbon atoms, are identifiable in space as a distinct class of species through their characteristic infrared bands (see the review by Tielens 2008).”
• Prokaryotic Hydrocarbon Degraders (2010, background): “Lentinus Fries 1825 Phenanthrene Valentı́n et al. (2006) Lenzites Fries 1836 Anthracene Gramss et al.”
• Discovery of the Pure Polycyclic Aromatic Hydrocarbon Indene (c-C9H8) with GOTHAM Observations of TMC-1 (2021, background): “H bonds of the full range of PAHs in a given source, thus precluding any unique identifications (Tielens 2008; Bauschlicher et al. 2018).”
• 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).”