The Prince and the Pauper: Evidence for the early high-redshift formation of the Galactic α-poor disc population^⋆,⋆⋆

¹ Max-Planck Institute for Astronomy, 69117 Heidelberg, Germany
e-mail: gent@mpia.de
² Ruprecht-Karls-Universität, Grabengasse 1, 69117 Heidelberg, Germany
³ Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK
⁴ Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Martii i Franques, 1, 08028 Barcelona, Spain
⁵ Institute of Space Sciences (ICE, CSIC), Carrer de Can Magrans s/n, 08193 Cerdanyola del Valles, Spain
⁶ Institut Estudis Espacials de Catalunya (IEEC), Carrer Gran Capita 2, 08034 Barcelona, Spain
⁷ Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK
⁸ Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
⁹ Niels Bohr International Academy, Niels Bohr Institute, University of Copenhagen, Blegdamsvej 17, 2100 Copenhagen, Denmark
¹⁰ Universität Heidelberg, Interdisziplinäres Zentrum für Wissenschaftliches Rechnen, Im Neuenheimer Feld 205, 69120 Heidelberg, Germany
¹¹ Universität Heidelberg, Zentrum für Astronomie, Institut für Theoretische Astrophysik, Albert-Ueberle-Straße 2, 69120 Heidelberg, Germany

Received: 31 May 2022
Accepted: 28 November 2023

Abstract

Context. The presence of [α/Fe]–[Fe/H] bi-modality in the Milky Way disc has intrigued the Galactic archaeology community over more than two decades.

Aims. Our goal is to investigate the chemical, temporal, and kinematical structure of the Galactic discs using abundances, kinematics, and ages derived self-consistently with the new Bayesian framework SAPP.

Methods. We employed the public Gaia-ESO spectra, as well as Gaia EDR3 astrometry and photometry. Stellar parameters and chemical abundances are determined for 13 426 stars using NLTE models of synthetic spectra. Ages were derived for a sub-sample of 2898 stars, including subgiants and main-sequence stars. The sample probes a large range of Galactocentric radii, ∼3 to 12 kpc, and extends out of the disc plane to ±2 kpc.

Results. Our new data confirm the known bi-modality in the [Fe/H]–[α/Fe] space, which is often viewed as the manifestation of the chemical thin and thick discs. The over-densities significantly overlap in metallicity, age, and kinematics and none of them offer a sufficient criterion for distinguishing between the two disc populations. In contrast to previous studies, we find that the α-poor disc population has a very extended [Fe/H] distribution and contains ∼20% old stars with ages of up to ∼11 Gyr.

Conclusions. Our results suggest that the Galactic thin disc was in place early, at lookback times corresponding to redshifts of z ∼ 2 or more. At ages of ∼9 to 11 Gyr, the two disc structures shared a period of co-evolution. Our data can be understood within the clumpy disc formation scenario that does not require a pre-existing thick disc to initiate the formation of the thin disc. We anticipate that a similar evolution can be realised in cosmological simulations of galaxy formation.