Infrared Emission from Interstellar Dust. IV. The Silicate‐Graphite‐PAH Model in the Post‐ Spitzer Era
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IR emission spectra are calculated for dust heated by starlight, for mixtures of amorphous silicate and graphitic grains, including varying amounts of PAH particles. The models are constrained to reproduce the average Milky Way extinction curve. The calculations include the effects of single-photon heating. Updated IR absorption properties for the PAHs are presented that are consistent with observed emission spectra, including those newly obtained by Spitzer . We find a size distribution for the PAHs giving emission band ratios consistent with the observed spectra of the Milky Way and other galaxies. Emission spectra are presented for a wide range of starlight intensities. We calculate how the efficiency of emission into different IR bands depends on PAH size; the strong 7.7 μm emission feature is produced mainly by PAH particles containing <10 3 C atoms. We also calculate how the emission spectrum depends on U , the starlight intensity relative to the local interstellar radiation field. The submillimeter and far-infrared emission is compared to the observed emission from the local interstellar medium. Using a simple distribution function, we calculate the emission spectrum for dust heated by a distribution of starlight intensities, such as occurs within galaxies. The models are parameterized by the PAH mass fraction q PAH , the lower cutoff U min of the starlight intensity distribution, and the fraction γ of the dust heated by starlight with U > U min . We present graphical procedures using Spitzer IRAC and MIPS photometry to estimate the parameters q PAH , U min , and γ, the fraction f PDR of the dust luminosity coming from photodissociation regions with U > 100, and the total dust mass M dust .
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Depending on shock velocity, a photon precursor can sufficiently heat dust to emit in the 12 μm band while dust inside the shock is heated by collisional processes and emits in both 12 and 22 μm bands.
“Depending on the shock velocity, such a photon precursor can sufficiently heat the dust to emit in the 12 µ m band (Draine & Li 2007; Draine 2011) while the dust inside the shock is heated by collisional processes, and therefore, emits in both 12 µ m and 22 µ m bands (Ponti et al. 2021).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Draine & Li 2007
Section 10.2 (page unavailable) says photons can excite PAHs enough to emit mid-infrared bands and identifies PAH features as the dominant contributor to IRAS 12 μm emission. It does not address photon precursors or how shock velocity affects that heating. The collisional-heating clause is attributed to a different citation and is not assessed here. (LLM, conf=0.88)
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Self-citationSAO 206462 - a solar-type star with a dusty, organically rich environment
Coulson, I. M., & Walther, D. M. (1995) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/274.4.977 · Cited by 35 · see citing works
Mid‐Infrared Spectropolarimetric Constraints on the Core‐Mantle Interstellar Dust Model
Li, A., & Greenberg, J. M. (2002) · The Astrophysical Journal · doi:10.1086/342222 · Cited by 35 · see citing works
Self-citationISO Beyond Point Sources: Studies of Extended Infrared Emission
Laureijs, R. J., Leech, K., & Kessler, M. F. (2000) · International Linear Collider · Cited by 35 · see citing works
Polycyclic Aromatic Hydrocarbons Orbiting HD 233517, an Evolved Oxygen-rich Red Giant
Jura, M. A., Bohac, C. J., Sargent, B., et al. (2006) · The Astrophysical Journal · doi:10.1086/500429 · Cited by 34 · see citing works
Spatially Resolved Sp it zer Spectroscopy of the Starburst Nucleus in NGC 5253
Beirão, P., Brandl, B. R., Devost, D., et al. (2006) · The Astrophysical Journal · doi:10.1086/505027 · Cited by 33 · see citing works
First Detection of PAHs and Warm Molecular Hydrogen in Tidal Dwarf Galaxies
Higdon, S. J. U., Higdon, J. L., & Marshall, J. A. (2006) · The Astrophysical Journal · doi:10.1086/500254 · Cited by 30 · see citing works
Graphite, Tubular PAHs, and the Diffuse Interstellar Bands
Zhou, Z., Sfeir, M. Y., Zhang, L., et al. (2006) · The Astrophysical Journal · doi:10.1086/501006 · Cited by 29 · see citing works
Spatial Separation of the 3.29 Micron Emission Feature and Associated 2 Micron Continuum in NGC 7023
An, J., & Sellgren, K. (2003) · The Astrophysical Journal · doi:10.1086/378630 · Cited by 28 · see citing works
Composition of interstellar gas and dust
Snow, T. P. (2000) · Journal of Geophysical Research Atmospheres · doi:10.1029/1999ja900270 · Cited by 24 · see citing works
Does the 3.3 Micron Polycyclic Aromatic Hydrocarbon Emission Feature Require Ultraviolet Excitation?
Smith, T. L., Clayton, G. C., & Valencic, L. A. (2004) · The Astronomical Journal · doi:10.1086/421745 · Cited by 22 · see citing works
The vibrations of C60H60 and the unidentified infrared emission
Webster, A. S. (1993) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/264.1.121 · Cited by 21 · see citing works
Elbaz, D., Floc'h, E. L., Dole, H., & Marcillac, D. (2005) · Astronomy and Astrophysics · doi:10.1051/0004-6361:200500095 · Cited by 18 · see citing works
UIR Bands in Carbon Star Spectra
Speck, A. K., & Barlow, M. J. (1997) · Astrophysics and Space Science · doi:10.1023/a:1000768102477 · Cited by 17 · see citing works
The Prominent Dust Emission Feature near 8.9 μm in Four H ii Regions
Peeters, E., Tielens, A. G. G. M., Boogert, A. C. A., et al. (2005) · The Astrophysical Journal · doi:10.1086/427143 · Cited by 16 · see citing works
New developments of the coal model of interstellar dust
Papoular, R., Ellis, K., Guillois, O., Reynaud, C., & Nenner, I. (1993) · Journal of the Chemical Society Faraday Transactions · doi:10.1039/ft9938902289 · Cited by 14 · see citing works
Far-Infrared Surveyor: design, operation, and performance
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The infrared camera (IRC) on board the ASTRO-F: laboratory tests and expected performance
Onaka, T., Fujishiro, N., Ihara, C., et al. (2004) · Proceedings of SPIE, the International Society for Optical Engineering/Proceedings of SPIE · doi:10.1117/12.550857 · Cited by 10 · see citing works
Flagged first, then by citations
Research works printed but not linked: 6
- Draine, B. T. 1994, in ASP Conf. Ser. 58, The First Symposium on the Infrared Cirrus and Diffuse Interstellar Clouds, ed. R. M. Cutri & W. B. Latter (San Francisco: ASP), 227
- ---. 2006, in ASP Conf. Ser. 348, Astrophysics in the Far Ultraviolet, ed.
- ---. 2005, in IAU Symp. 231, Astrochemistry, ed. D. C. Lis, G. A. Blake, & E. Herbst (Cambridge: Cambridge Univ. Press), 443
- Kawada, M., Shibai, H., Kaneda, H., & Nakagawa, T. 2004, Proc. SPIE, 5487, 359
- Mason, R. E., Wright, G. S., Adamson, A., & Pendleton, Y. 2007, ApJ, in press
- Onaka, T., et al. 2004, Proc. SPIE, 5487, 338
Cited by
Sorted by citations
On the duration of the embedded phase of star formation
Kim, J., Chevance, M., Kruijssen, J. M. D., Schruba, A., Sandstrom, K., Barnes, A. T., Bigiel, F., Blanc, G. A., Cao, Y., Dale, D. A., et al. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab878 · Cited by 95 · see citing works
MAIN-SEQUENCE STARS MASQUERADING AS YOUNG STELLAR OBJECTS IN THE CENTRAL MOLECULAR ZONE
Koepferl, C. M., Robitaille, T. P., Morales, E. F. E., & Johnston, K. G. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/799/1/53 · Cited by 50 · see citing works
The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way
Sarkar, K. C. (2024) · The Astronomy and Astrophysics Review · doi:10.1007/s00159-024-00152-1 · Cited by 34 · see citing works
Lewis, A. R., Simones, J. E., Johnson, B. D., Dalcanton, J. J., Skillman, E. D., Weisz, D. R., Dolphin, A. E., Williams, B. F., Bell, E. F., Fouesneau, M., et al. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/834/1/70 · Cited by 16 · see citing works
- Authors
- Draine, B. T., & Li, A.
- Affiliations
- Princeton University (US)
- University of Missouri (US)
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2007-03-10
- Volume
- 657
- Issue
- 2
- Pages
- 810-837
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2048274049
- Cited by
- 2,122
- References
- 123
- Citations by year
- 2026: 79 · 2025: 124 · 2024: 149 · 2023: 124 · 2022: 111 · 2021: 128 · 2020: 115 · 2019: 133 · 2018: 127 · 2017: 124 · 2016: 137 · 2015: 117 · 2014: 114 · 2013: 110 · 2012: 99
- FWCI
- 46.24
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- CERN Document Server (European Organization for Nuclear Research) (submittedVersion)
- arXiv (Cornell University)
- Funders
- National Science Foundation (0406883)
- National Aeronautics and Space Administration
- University of Missouri
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
- Keywords
- interstellar dust, infrared emission spectra, polycyclic aromatic hydrocarbons, graphite grains, dust size distribution, photodissociation regions, dust mass estimation
About these checks
Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.
Statistics and arithmetic are recomputed, not judged.
Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.
What counts as a claim ›How we measure confidence ›How we check this ›
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