Stellar Ejecta: Macro-Molecule and Dust Formation and Evolution

Details Stellar Ejecta: Macro-Molecule and Dust Formation and Evolution Stellar Ejecta: Macro-Molecule and Dust Formation and Evolution

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sptz.prop...77r&link_type=abstract

Spitzer Proposal ID #77

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Scientific paper

Mass ejected into the interstellar medium during the early and late stages of stellar evolution -- protostellar jets, asymptotic giant branch (AGB) stellar mass loss, novae, and supernovae -- is the primary source of chemically enriched material to the interstellar medium (e.g. Jura 1987, in ISP). Dust and large "macro" molecules (polycyclic aromatic hydrocarbons or PAHs) are a major constituent of the interstellar medium, and strongly influence the physics and chemistry of the ISM. The origin and evolution of these key components are not well known. With IRAC we will determine the detailed structure in various tracers, such as the warm dust component and PAHs, molecular hydrogen (v=0-0), and various ionized species. The IRAC bands are well placed to be able to detect large scale emission in the IR PAH bands. Some confusion with other species will be present, but IRS spectroscopy will quickly resolve any issues. Its large field of view allows rapid study of some of the most well known, but poorly observed objects. MIPS will give us access to extended shells and ISM interactions, the cold and very cold components, interaction interfaces, with efficient wide field mapping and fast/accurate photometry with a wide FOV. MIPS SED mode will provide information on the temperature and composition of the cold and very cold components and the dust. IRS will be used for detailed composition and temperature studies of the dust, PAHs, and numerous atomic and molecular species available in the IRS wavelength ranges of the high and low resolution modules.

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