Infrared radiation of very small dust grains in the Rho Ophiuchi region

Details Infrared radiation of very small dust grains in the Rho Ophiuchi region Infrared radiation of very small dust grains in the Rho Ophiuchi region

Nov 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...186..312r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 186, no. 1-2, Nov. 1987, p. 312-318. Research supported by the Observatoire de

Astronomy and Astrophysics

Astronomy

58

Cosmic Dust, Infrared Astronomy Satellite, Infrared Radiation, Infrared Spectra, Interstellar Matter, Molecular Clouds, Radiation Distribution, Spiral Galaxies

Scientific paper

The IRAS Sky-flux maps have been used to study the colours of interstellar dust in the Rho Oph region. The 12 μm and 60 μm band intensities relative to the dust emission at longer wavelengths have been obtained in the south-east extension of the molecular cloud and in the surrounding of the stars σ Sco, τ Sco, and HD 147889. It is found that the 60 μm to 100 μm intensity ratio increases gradually with the starlight radiation density heating the dust, as expected. In the reflection nebula NGC 2023, the 12 μm flux is shown to be entirely produced by the "aromatic infrared features" (namely at λ = 7.7, 8.6, 11.3 μm) encompassed in the band, which is thus interpreted as the tracer of the source of the features, believed to be polycyclic aromatic hydrocarbons (PAHs). A strong 12 μm intensity is detected almost everywhere. However, in a radiation field of order 100 eV cm-3, the 12 μm emission is depressed by a factor of order five, which is attributed to a destruction of the polycyclic aromatic hydrocarbons. It is concluded that the particles should in general be made of about 20 to 40 carbon atoms.

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