Calculation of Fe II atomic data required for the modeling of HST observations

Details Calculation of Fe II atomic data required for the modeling of HST observations Calculation of Fe II atomic data required for the modeling of HST observations

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003hst..prop.9923f&link_type=abstract

HST Proposal ID #9923

Physics

Hst Proposal Id #9923 Ism And Circumstellar Matter

Scientific paper

Emission lines of singly ionized iron {denoted Fe II} are observed from a wide variety of astronomical objects. A complete simulation of the physical processes affecting the Fe II ion would make it possible to deduce the density, temperature, and iron abundance of the emitting regions. This is a major goal, due to the ubiquity of Fe II emission, but is difficult because the physics governing Fe II emission is complex. We have embarked on a long-term project to develop the tools needed to fully interpret Fe II emission in astrophysical sources. This includes a complete simulation of the physics of the excitation and transport of Fe II, its incorporation into our spectral synthesis code CLOUDY, and a comparison of our calculations with HST and optical spectra of the symbiotic star RR Telescopii. For this object, the geometry, ionization sources, physical conditions and abundances are largely understood, and hence it offers an unique astrophysical laboratory to test and validate the completeness of our CLOUDY numerical simulations. However a vital requirement of our work is accurate Fe II atomic data, and in particular theoretical electron collisional excitation rates, as experimental results are not available for this process. This is the subject of the present proposal. Specifically, we wish to use our new code PRMAT, designed for accurate calculations of excitation rates for ions with open d-shells, to produce results for Fe II. We have already shown that existing atomic data for Fe II are in error. Calculations with PRMAT will allow Fe II emission lines in astronomical sources to be properly analysed, and in particular will permit the reliable modeling of UV spectra from HST.

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