Chemical evolution of ytterbium in the Galactic disk^★

¹ Kapteyn Astronomical Institute, University of Groningen, Landleven 12, 9747 AD Groningen, The Netherlands
e-mail: montelius@astro.rug.nl
² Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, 22100 Lund, Sweden
³ Materials Science and Applied Mathematics, Malmö University, 205 06 Malmö, Sweden
⁴ Department of Astronomy and Space Sciences, Ege University, 35100 Bornova, İzmir, Turkey
⁵ Center for Star and Planet Formation, GLOBE Institute University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen, Denmark
⁶ SOFIA Science Center - USRA, NASA Ames Research Center, Moffett Field, CA 94035, USA
⁷ Gemini Observatory/NOIRLab, Casilla 603, La Serena, Chile
⁸ Department of Astronomy and McDonald Observatory, The University of Texas, Austin, TX 78712, USA

Received: 17 January 2022
Accepted: 31 January 2022

Abstract

Context. Measuring the abundances of neutron-capture elements in Galactic disk stars is an important part of understanding key stellar and galactic processes. In the optical wavelength regime a number of different neutron-capture elements have been measured; however, only the s-process-dominated element cerium has been accurately measured for a large sample of disk stars from the infrared H band. The more r-process dominated element ytterbium has only been measured in a small subset of stars so far.

Aims. In this study we aim to measure the ytterbium (Yb) abundance of local disk giants using the Yb II line at λ_air = 16 498 Å. We also compare the resulting abundance trend with cerium and europium abundances for the same stars to analyse the s- and r-process contributions.

Methods. We analyse 30 K giants with high-resolution H band spectra using spectral synthesis. The very same stars have already been analysed using high-resolution optical spectra via the same method, but it was not possible to determine the abundance of Yb from those spectra due to blending issues for stars with [Fe/H] > −1. In the present analysis, we utilise the stellar parameters determined from the optical analysis.

Results. We determined the Yb abundances with an estimated uncertainty for [Yb/Fe] of 0.1 dex. By comparison, we found that the [Yb/Fe] trend closely follows the [Eu/Fe] trend and has clear s-process enrichment in identified s-rich stars. This comparison confirms both that the validity of the Yb abundances is ensured and that the theoretical prediction that the s-/r-process contribution to the origin of Yb of roughly 40/60 is supported.

Conclusions. These results show that, with a careful and detailed analysis of infrared spectra, reliable Yb abundances can be derived for a wider sample of cooler giants in the range −1.1 < [Fe/H] < 0.3. This is promising for further studies of the production of Yb and for the r-process channel, key for galactochemical evolution, in the infrared.