CRIRES-POP: A library of high resolution spectra in the near-infrared

Abstract

Context. High-resolution spectra in the near-infrared (NIR) are an important tool for the detailed study of stellar atmospheres. The accurate identification of elements and molecules in these spectra can be used to determine chemical abundances and physical conditions in the photosphere of the observed star. Such identifications require precise line positions and strengths of both atomic and molecular features. Aims. This work focusses on the full identification of absorption lines in the NIR spectrum of the K-giant 10 Leo, including previously unidentified lines. The large number and complexity of the observed absorption lines require a deep search for potential spectral signatures to enable an unambiguous assignment to specific elements or molecular species. We aim to improve the published line lists of metals, some of which are determined by model calculations only, and many of which presently lack the completeness and accuracy of line parameters. Methods. The CRIRES-POP project provided high-resolution, high signal-to-noise ratio (S/N) spectra of several bright stars in the 1–5 μm range. For the K-giant 10 Leo, a spectrum corrected for telluric absorption and with precise wavelength calibration is available. This has been analysed by comparison with model spectra and up-to-date line lists. Results. We identified lines of 29 elements and eight molecular species. While the positions of many known lines could be confirmed, about 6% of all lines detected in 10 Leo could not be attributed to any known feature. For CO and its isotopologues, molecular constants could be derived and several additional lines identified. We report major inconsistencies for some prominent lines. In addition, abundances for several key elements in 10 Leo are provided.

Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star

“…Rotation rates of stars have been used to trace stellar activity (e.g., Browning 2008). For low-mass stars and brown dwarfs, specifically, it appears that these objects are common rapid rotators, with a dependence on the object's temperature, age, and mass (e.g., Mohanty & Basri 2003;Zapatero Osorio et al 2006;Reiners & Basri 2008;Konopacky et al 2012;Snellen et al 2014;Bryan et al 2020;Hsu et al 2021b;Tannock et al 2021;Wang et al 2021;Zendel et al 2023;Landman et al 2024, Hsu et al 2024. For younger objects (≈10-100 Myr), the rapid rotation can be explained by the gravitational contraction of these objects, which causes them to spin up as they age due to the conservation of angular momentum.…”