The unidentified infrared emission (UIE) features at 3.3, 6.2, 7.7, 8.6, and 11.3 μm, commonly attributed to polycyclic aromatic hydrocarbon (PAH) molecules, have recently been ascribed to mixed aromatic/aliphatic organic nanoparticles. More recently, an upper limit of <9% was placed on the aliphatic fraction (i.e., the fraction of carbon atoms in aliphatic form) of the UIE carriers based on the observed intensities of the 3.4 μm and 3.3 μm emission features by attributing them to aliphatic and aromatic C-H stretching modes, respectively, and assuming A 3.4/A 3.3 ≈ 0.68 derived from a small set of aliphatic and aromatic compounds, where A 3.4 and A 3.3 are, respectively, the band strengths of the 3.4 μm aliphatic and 3.3 μm aromatic C-H bonds. To improve the estimate of the aliphatic fraction of the UIE carriers, here we analyze 35 UIE sources exhibiting both the 3.3 μm and 3.4 μm C-H features and determine I 3.4/I 3.3, the ratio of the power emitted from the 3.4 μm feature to that from the 3.3 μm feature. We derive the median ratio to be 〈I 3.4/I 3.3〉 ≈ 0.12. We employ density functional theory to compute A 3.4/A 3.3 for a range of methyl-substituted PAHs. The resulting A 3.4/A 3.3 ratio well exceeds ~1.4, with an average ratio of A 3.4/A 3.3 ≈ 1.76. By attributing the 3.4 μm feature exclusively to aliphatic C-H stretch (i.e., neglecting anharmonicity and superhydrogenation), we derive the fraction of C atoms in aliphatic form from I 3.4/I 3.3 ≈ 0.12 and A 3.4/A 3.3 ≈ 1.76 to be ~2%. We therefore conclude that the UIE emitters are predominantly aromatic.
X. Yang et al., "The Carriers of the Interstellar Unidentified Infrared Emission Features: Constraints from the Interstellar C-H Stretching Features at 3.2-3.5 µm," Astrophysical Journal, vol. 776, no. 2, Institute of Physics Publishing, Oct 2013.
The definitive version is available at https://doi.org/10.1088/0004-637X/776/2/110
Keywords and Phrases
Dust; Extinction; ISM: lines and bands; ISM: molecules
International Standard Serial Number (ISSN)
Article - Journal
© 2013 Institute of Physics Publishing, All rights reserved.
01 Oct 2013