Metal-poor stars observed with the Magellan Telescope

• Verfasst von: Mardini, Mohammad K. [VerfasserIn]
• Verfasst von: Frebel, Anna [VerfasserIn]
• Verfasst von: Betre, Leyatt [VerfasserIn]
• Verfasst von: Jacobson, Heather [VerfasserIn]
• Verfasst von: Norris, John E [VerfasserIn]
• Verfasst von: Christlieb, Norbert [VerfasserIn]
• Titel: Metal-poor stars observed with the Magellan Telescope
• Titelzusatz: IV. Neutron-capture element signatures in 27 main-sequence stars
• Verf.angabe: Mohammad K. Mardini, Anna Frebel, Leyatt Betre, Heather Jacobson, John E. Norris and Norbert Christlieb
• E-Jahr: 2024
• Jahr: February 2024
• Umfang: 18 S.
• Illustrationen: Illustrationen
• Fussnoten: Gesehen am 23.07.2024
• Titel Quelle: Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
• Ort Quelle: Oxford : Oxford Univ. Press, 1827
• Jahr Quelle: 2024
• Band/Heft Quelle: 528(2024), 2 vom: Feb., Seite 2912-2929
• ISSN Quelle: 1365-2966
• DOI: doi:10.1093/mnras/stad3925
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1896144675

Abstract

We present a chemo-dynamical analysis for 27 near main-sequence turnoff metal-poor stars, including 20 stars analysed for the first time. The sample spans a range in [Fe/H] from −2.5 to −3.6, with 44 per cent having [Fe/H]<−2.9. We derived chemical abundances for 17 elements, including strontium and barium. We derive Li abundances for the sample, which are in good agreement with the ‘Spite Plateau’ value. The lighter elements (Z < 30) generally agree well with those of other low-metallicity halo stars. This broadly indicates chemically homogeneous gas at the earliest times. We used the [Sr/Ba] versus [Ba/Fe] diagram to classify metal-poor stars into five populations based on their observed ratios. We find HE 0232 − 3755 to be a likely main r-process star, and HE 2214 − 6127 and HE 2332 − 3039 to be limited-r stars. CS30302-145, HE 2045 − 5057, and CD −24°17504 plausibly originated in long-disrupted early dwarf galaxies. We also find that the derived [Sr/H] and [Ba/H] values for CD −24°17504 are not inconsistent with the predicted yields of the s-process in massive rotating low-metallicity stars models. Further theoretical explorations will be helpful to better understand the earliest mechanisms and time scales of heavy element production for comparison with these and other observational abundance data. Finally, we investigate the orbital histories of our stars. Most display halo-like kinematics although three stars (CS 29504-018, HE 0223 − 2814, and HE 2133 − 0421) appear to be disc-like in nature. This confirms the extragalactic origin for CS 30302-145, HE 2045 − 5057, and, in particular, CD −24°17504 which likely originated from a small accreted stellar system as one of the oldest stars.