The diffuse galactic emission at 6.2 micrometer

Details The diffuse galactic emission at 6.2 micrometer The diffuse galactic emission at 6.2 micrometer

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...286l..23r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 286, no. 2, p. L23-L26

Astronomy and Astrophysics

Astronomy

40

Cosmic Dust, Diffuse Radiation, Emission Spectra, Infrared Astronomy, Infrared Spectra, Interstellar Extinction, Interstellar Matter, Polycyclic Aromatic Hydrocarbons, Balloon-Borne Instruments, French Space Program, Molecules

Scientific paper

We present the observation of the 6.2 micrometer emission toward the inner galactic disk, obtained with the AROME balloon-borne experiment with an angular resolution of 0.9 deg. The galactic coordinates of the observed region are -5 deg less than or equal to LII less than or equal to 35 deg and -6 deg less than or equal to BII less than or equal to 6 deg. The measurements reveal the existence of an emission feature at 6.2 micrometer all over this region. The averaged 6.2 micrometer surface brightness (-1 deg less than or equal to BII less than or equal to 1 deg, 8 deg less than or equal to LII less than or equal to 35 deg) is lambda x Ilambda = (1.2 +/- 0.3) 10-5 W/sq m/sr with a continuum lambda x Ilambda = (5.9 +/- 1.2) 10-6 W/sq m/sr and a feature intensity Delta lambda x Ilambda = (6.1 +/- 1.3) 10-7 W/sq m/sr. If we take into account the effect of dust extinction along the line of sight, we obtain respectively for the 6.2 micrometer to 3.3 micrometer emission feature ratio and the 6.2 micrometer feature to 12 micrometer emissivity ratio: Delta lambda x Ilambda (6.2)/Delta lambda x Ilambda (3.3) = 9 +/- 2 and Delta lambda x Ilambda (6.2)/lambda x Ilambda (12) = 0.09 +/- 0.02; these color ratios are similar to those obtained on UV excited nebulae, despite very different radiation field intensities and spectra. We show that the 6.2 micrometer can only arise from the diffuse interstellar medium. In consequence, it supports an emission process involving transiently heated very small grains or large molecules like polycyclic aromatic hydrocarbons (PAHs), as it was originally proposed by Puget et al. (1985).

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