Neutron-capture Elements in Planetary Nebulae: First Detections of Near-infrared [Te iii] and [Br v] Emission Lines

We have identified two new near-infrared (NIR) emission lines in the spectra of planetary nebulae arising from heavy elements produced by neutron-capture reactions: [Te iii ] 2.1019 μ m and [Br v ] 1.6429 μ m. [Te iii ] was detected in both NGC 7027 and IC 418, while [Br v ] was seen in NGC 7027. Th...

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Bibliographic Details
Published in:Astrophysical journal. Letters 2018-07, Vol.861 (1), p.L8
Main Authors: Madonna, Simone, Bautista, Manuel, Dinerstein, Harriet L., Sterling, N. C., García-Rojas, Jorge, Kaplan, Kyle F., Rubio-Díez, Maria del Mar, Castro-Rodríguez, Nieves, Garzón, Francisco
Format: Article
Language:English
Subjects:
Abundance
Asymptotic giant branch stars
Emission lines
Emission spectra
Gratings (spectra)
Heavy elements
Infrared spectrometers
Ions
Line spectra
Metallicity
Near infrared radiation
Nebulae
Nuclear capture
Planetary nebulae
Stellar evolution
Submerging
Tellurium
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Summary:We have identified two new near-infrared (NIR) emission lines in the spectra of planetary nebulae arising from heavy elements produced by neutron-capture reactions: [Te iii ] 2.1019 μ m and [Br v ] 1.6429 μ m. [Te iii ] was detected in both NGC 7027 and IC 418, while [Br v ] was seen in NGC 7027. The observations were obtained with the medium-resolution spectrograph Espectrógrafo Multiobjeto Infra-Rojo (EMIR) on the 10.4 m Gran Telescopio Canarias at La Palma, and with the high-resolution Immersion GRating INfrared Spectrometer (IGRINS) on the 2.7 m Harlan J. Smith telescope at McDonald Observatory. New calculations of atomic data for these ions, specifically A-values and collision strengths, are presented and used to derive ionic abundances of Te 2+ and Br 4+ . We also derive ionic abundances of other neutron-capture elements detected in the NIR spectra, and estimate total elemental abundances of Se, Br, Kr, Rb, and Te after correcting for unobserved ions. Comparison of our derived enrichments to theoretical predictions from asymptotic giant branch (AGB) evolutionary models shows reasonable agreement for solar metallicity progenitor stars of ∼2–4 M ⊙ . The spectrally isolated [Br v ] 1.6429 μ m line has advantages for determining nebular Br abundances over optical [Br iii ] emission lines that can be blended with other features. Finally, measurements of Te are of special interest because this element lies beyond the first peak of the s -process, and thus provides new leverage on the abundance pattern of trans-iron species produced by AGB stars.
ISSN:2041-8205
2041-8213
DOI:10.3847/2041-8213/aaccef