Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001apj...562..515d&link_type=abstract
The Astrophysical Journal, Volume 562, Issue 1, pp. 515-520.
Astronomy and Astrophysics
Astronomy
9
Infrared: Ism, Ism: Lines And Bands, Line: Identification, Ism: Planetary Nebulae: General, Planetary Nebulae: Individual (Ic 5117, Ngc 7027), Stars: Agb And Post-Agb
Scientific paper
We have identified a line at 3.625 μm in the planetary nebulae (PNs) NGC 7027 and IC 5117 as the 2D3/2-2D5/2 fine-structure transition of the 3d9 ion Zn+3. Zinc (N=30) is believed to be made primarily by explosive nucleosynthesis and r-process neutron capture reactions, and because Zn/H closely tracks Fe/H in metal-poor stars and is relatively undepleted into dust in the ISM, Zn/H has been used as a surrogate for Fe/H in the high-redshift universe. However, some isotopes of Zn are also produced as part of the s-process in asymptotic giant branch stars, the progenitors of PNs. Although there is currently no published calculation of the collision strength for [Zn IV] 3.625 μm, for plausible values the observed line fluxes do not require Zn/H greater than solar, suggesting that these two PNs, which have elevated abundances of other s-process elements and C, are not significantly self-enriched in Zn. Consequently, Zn/H determined from emission lines should be a good indicator of elemental Fe/H in PNs, where gas-phase Fe/H values cannot be used directly because of depletion effects, enabling comparisons between nebular and stellar Fe/H abundances. We also report an upper limit on the strength of the 1-0 P(2) line of HeH+ at 3.608 μm in NGC 7027.
Dinerstein Harriet L.
Geballe Thomas Ronald
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