Other
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...19916102s&link_type=abstract
American Astronomical Society, 199th AAS Meeting, #161.02; Bulletin of the American Astronomical Society, Vol. 34, p.572
Other
Scientific paper
Deep, high-resolution emission spectra of emission-line regions reveal literally hundreds of weak lines which may not be quickly or accurately identifiable manually. We present software, dubbed ``EMILI'' for Emission Line Identifier, currently under development, that can aid in making such identifications, specifically in planetary nebulae and H \small II \normalsize regions. This software will become public domain in the near future. EMILI begins with a user-supplied list of line wavelengths, fluxes, and associated errors. The observed object's systemic velocity, and a model of the ionization energy dependence of the expansion velocity are calculated from user pre-identified strong lines. These line's strengths are also used to calculate the ionization corrections for all ions Z<=30 and ionization stage up to 30, and consequent ionic abundances as modified from base solar values. For each observed unidentified line, a master transition list (van Hoof 2001, Atomic Line List v2.04) is consulted for all transitions within a certain multiple of the line's wavelength uncertainty. The observed line's wavelength is then corrected for systemic motion and the ionization dependent expansion velocity. A predicted flux is calculated for each transition based upon the transition's parent ion's abundance and other attributes. For the transitions with the strongest predicted flux, the input line-list is searched for other lines of the same multiplet which have ratios of observed fluxes approximately equal to the ratios of statistical weights and Einstein coefficients. Finally each transition is ranked on the basis of how well its calculated flux matches the observed value, the agreement between the corrected wavelength of the observed line and the transition's rest wavelength, and on the numbers of other multiplet lines identified within the input list. This determines a set of likely identifications for each line which is presented to the user.
Baldwin John
Sharpee Brian
van Hoof Peter A. M.
Williams Robert E.
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