The near-infrared excess continuum in the Orion Bar splits into a roughly 700 K component that tracks the 3.3 micron aromatic band and a hotter, poorly constrained component that does not, with water and CO2 ice absorption from a deeper layer.
Low-Resolution Spectrum of the Diffuse Galactic Light and 3.3 um PAH emission with AKARI InfraRed Camera
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abstract
We first obtained the spectrum of the diffuse Galactic light (DGL) at general interstellar space in 1.8-5.3 um wavelength region with the low-resolution prism spectroscopy mode of the AKARI Infra-Red Camera (IRC) NIR channel. The 3.3 um PAH band is detected in the DGL spectrum at Galactic latitude |b| < 15 deg, and its correlations with the Galactic dust and gas are confirmed. The correlation between the 3.3 um PAH band and the thermal emission from the Galactic dust is expressed not by a simple linear correlation but by a relation with extinction. Using this correlation, the spectral shape of DGL at optically thin region (5 deg < |b| < 15 deg) was derived as a template spectrum. Assuming that the spectral shape of this template spectrum is uniform at any position, DGL spectrum can be estimated by scaling this template spectrum using the correlation between the 3.3 um PAH band and the thermal emission from the Galactic dust.
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PDRs4All XXII. Near-Infrared continuum in the Orion Bar
The near-infrared excess continuum in the Orion Bar splits into a roughly 700 K component that tracks the 3.3 micron aromatic band and a hotter, poorly constrained component that does not, with water and CO2 ice absorption from a deeper layer.