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2013MNRAS.429.2791F - Mon. Not. R. Astron. Soc., 429, 2791-2851 (2013/March-2)
Very deep spectroscopy of the bright Saturn nebula NGC 7009 - II. Analysis of the rich optical recombination spectrum.
FANG X. and LIU X.-W.
Abstract (from CDS):
The possibility of plasma diagnostics using the ORLs of various heavy-element ions is discussed in detail. The line ratios that can be used to determine electron temperature are presented for each ion, although there is still a lack of adequate atomic data and some of the lines are still not detected in the spectrum of NGC 7009 due to weakness and/or line blending. Plasma diagnostics based on the Nii and Oii recombination spectra both yield electron temperatures close to 1000K, which is lower than those derived from the collisionally excited line (CEL) ratios (e.g. the [Oiii] and [Nii] nebular-to-auroral line ratios; see Paper I for details) by nearly one order of magnitude. The very low temperatures yielded by the Oii and Nii ORLs indicate that they originate from very cold regions. The C2+/H+, N2+/H+, O2+/H+ and Ne2+/H+ ionic abundance ratios derived from ORLs are consistently higher, by about a factor of 5, than the corresponding values derived from CELs. In calculating the ORL ionic abundance ratios, we have used the newly available high-quality effective recombination coefficients, and adopted an electron temperature of ∼ 1000K, as given by the ORL diagnostics and as a consequence presumably representing the physical conditions prevailing in the regions where the heavy-element ORLs arise. Measurements of the ultraviolet (UV) and infrared (IR) CELs from the literature are used to calculate CEL ionic abundance ratios when optical data are not available for the ionic species. A comparison of results of plasma diagnostics and abundance determinations for NGC 7009 points to the existence of `cold', metal-rich (i.e. H-deficient) inclusions embedded in the hot, diffuse ionized gas, first postulated by Liu et al.
At electron temperatures yielded by the Nii and Oii ORLs, the predicted relative intensities of ORLs agree well with the observed values, indicating that the current quantum calculations of the recombination spectra of those two ionic species well represent the recombination processes under nebular conditions. Deviations from the LS coupling, noticed in an earlier quantitative spectroscopy by Liu et al. for the same object, are again confirmed, especially for recombination lines of the 4f-3d transition array. For Nii, as well as for Oii, the ionic abundances derived from different J-resolved transitions within a multiplet, or from the transitions belonging to different multiplets, agree with each other. This is another evidence that the new effective recombination coefficients are reliable. New calculations of the effective recombination coefficients for the Neii lines at nebular temperatures and densities are needed.
Abstract Copyright: © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2013)
Journal keyword(s): atomic data - atomic processes - ISM: abundances - planetary nebulae: individual: NGC 7009
Simbad objects: 14
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