Dust continuum and features in ISO-SWS 2.5--45μ m spectra of galaxies -- templates for SIRTF and other missions.

Details Dust continuum and features in ISO-SWS 2.5--45μ m spectra of galaxies -- templates for SIRTF and other missions. Dust continuum and features in ISO-SWS 2.5--45μ m spectra of galaxies -- templates for SIRTF and other missions.

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...195.7407s&link_type=abstract

American Astronomical Society, 195th AAS Meeting, #74.07; Bulletin of the American Astronomical Society, Vol. 31, p.1479

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Scientific paper

We present an inventory of mid-infrared spectral features detected in high resolution (R 1500) ISO-SWS 2.4--45μ m spectra of the galaxies {M 82}, {NGC 253}, {Circinus}, {NGC 1068}, and the {30 Doradus} region of the LMC. We discuss their identifications and highlight possible relations between these features and the physical state of the interstellar medium in galaxies. In the 5--13μ m region, emission from unidentified infrared bands (UIBs), usually ascribed to aromatic molecules, and apparent silicate absorption dominate the spectrum. The density of features makes it difficult to determine the continuum, particularly in ground-based data of limited wavelength coverage. In fact the apparent depth of the 9.7μ m silicate absorption may be overestimated in the presence of UIB emission, as we demonstrate by comparing the spectrum of M 82 to the (absorption free) spectrum of the reflection nebula {NGC 7023}. No strong silicate absorption is present in M 82. The (very small grain) dust continuum under the UIB emission in our starburst templates can be modeled by a simple power law, starting at wavelengths between 8 and 9μ m. Differences in absorption features point to different physical conditions in the obscuring regions of active galaxies compared to starburst galaxies. The spectra are valuable templates for other mid-infrared missions. We smooth our data to simulate low resolution spectra as obtained with ISOCAM-CVF, ISOPHOT-S, and in the future with the low resolution mode of SIRTF-IRS, and use our high spectral resolution information to highlight possible identification problems at low resolving power that are caused by coincidences of lines and features.

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