The determination of abundances in the interstellar medium from infrared fine-structure lines

Details The determination of abundances in the interstellar medium from infrared fine-structure lines The determination of abundances in the interstellar medium from infrared fine-structure lines

Mar 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iraj...16..219j&link_type=abstract

(Astronomical Science Group of Ireland, Meeting, University College, Dublin, Ireland, Sept. 29, 1983) Irish Astronomical Journal

Astronomy and Astrophysics

Astronomy

1

Abundance, Astronomical Spectroscopy, Infrared Astronomy, Interstellar Gas, Planetary Nebulae, Electron Density (Concentration), Fine Structure, Line Spectra, Neon

Scientific paper

Infrared fine-structure lines used to obtain ionic abundances, electron densities, and electron temperatures in the interstellar medium are discussed. There are several advantages in using the infrared lines which include the following: the lines suffer much less from extinction than optical forbidden lines, thus reducing the need for corrections; excitation energies for these levels are small (less than 0.25 eV); and they are insensitive to the electron temperature. To obtain an ionic abundance relative to hydrogen, the ionic line flux and either a hydrogen-line flux or the radio-continuum flux must be measured. The calculation of atomic data for the most abundant ions which is carried out at QUB is considered. The observations of the Ne V 2428 micron line from three planetary nebulae by Shure et al. (1983) are reinterpreted using the atomic data of Aggarwal (1983, 1984). The results indicate that to obtain Ne V abundances for the three planetary nebulae NGC 7027, NGC 7354, and NGC 7662, using the 3P1-3P0 transition, a specific electron density and temperature must be assumed.

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