The Organic Refractory Material in the Diffuse Interstellar Medium: Mid-Infrared Spectroscopic Constraints

By Y. Pendleton, L. Allamandola. 2002

275 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/ee50238a84f0bd07e3ca4345d29fdfc63cf9ff0d

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In Astronomy and Astrophysics

1. R. Genzel
2. F. Eisenhauer
3. D. Lutz
4. S. Gillessen
5. T. Ott
6. E. Jenkins
7. O. Pfuhl
8. E. Dishoeck

In Atmospheric Science

1. E. Jenkins
2. A. Fraisse
3. L. Kaltenegger
4. A. Jones
5. E. Dishoeck
6. L. Verstraete
7. B. Draine
8. N. Ysard

In Spectroscopy

1. B. Draine
2. R. Genzel
3. E. Dishoeck
4. A. Jones
5. A. Fraisse
6. Simon Bruderer
7. Cecilia Ceccarelli
8. R. Garrod

Citations in the corpus

• Scattering by Interstellar Dust Grains. I. Optical and Ultraviolet (2003, background): “From the observed 3.4 lmC-H stretch feature, Pendleton & Allamandola (2002) estimate that 85% of the C is aromatic and 15% is aliphatic (chainlike).”
• POLARIZED FAR-INFRARED AND SUBMILLIMETER EMISSION FROM INTERSTELLAR DUST (2008, methodology): “Based on the profile of the 3.4 µm C-H stretching mode, Pendleton & Allamandola (2002) estimate that about 85% of the carbon is in aromatic structures.”
• The global dust modelling framework THEMIS (The Heterogeneous dust Evolution Model for Interstellar Solids) (2017, background): “These materials are consistent with the observed infrared absorption bands (e.g., Pendleton & Allamandola 2002; Dartois et al. 2004b; Dartois & Muñoz-Caro 2007) and show temperaturedependent luminescence (e.g., Robertson 1986) consistent with the observed interstellar luminescence in the red, the…”
• The nature of molecular cloud material in interplanetary dust (2004, background): “Our FTIR spectra from both Semarkona and Murchison meteorite residues are consistent with this estimate when the intrinsic band strengths for each of the hydrocarbon species are considered (Pendleton et al., 1995; Pendleton and Allamandola, 2002 ).”
• ISO Spectroscopy of Gas and Dust: From Molecular Clouds to Protoplanetary Disks (2004, background): “The C-H stretching mode of aliphatic (chain-like) hydrocarbons at 3.4 µm has been detected from the ground along many diffuse lines of sight with extinctions > ∼ 10 mag (e.g., Pendleton & Allamandola 2002).”
• INTERSTELLAR DUST GRAINS (2003, unknown): “…variation in the C-H band strength, so it has not been possible to use the measured 3.4µm feature to determine the abundance of aliphatic hydrocarbon material in the interstellar grain population, nor is it possible to identify the specific hydrocarbon material (Pendleton & Allamandola 2002).”
• What makes a planet habitable? (2009, background): “Several allotropes of carbon, among them diamond, graphite and fullerenes have been identified in space environments, in particular in meteorites (Ehrenfreund and Charnley 2000; Pendleton and Allamandola 2002).”
• What Is the Total Deuterium Abundance in the Local Galactic Disk? (2006, background): “From the relative strengths and profiles of different C-H stretching modes, Pendleton & Allamandola (2002) estimate that ∼85% of the carbon in dust is in aromatic form, with H/C≈0.35, and ∼15% of the carbon is aliphatic, with H/C≈2.1.”
• LINE DERIVED INFRARED EXTINCTION TOWARD THE GALACTIC CENTER (2011, background): “In molecular clouds it is not detected (Pendleton & Allamandola 2002).”