How many components? Quantifying the complexity of the metallicity distribution in the Milky Way bulge with APOGEE

Alvaro Rojas-Arriagada, Gail Zasowski, Mathias Schultheis, Manuela Zoccali, Sten Hasselquist, Cristina Chiappini, Roger E. Cohen, Katia Cunha, José G. Fernández-Trincado, Francesca Fragkoudi, D. A. García-Hernández, Doug Geisler, Felipe Gran, Jianhui Lian, Steven Majewski, Dante Minniti, Antonela Monachesi, Christian Nitschelm, Anna B.A. Queiroz

Resultado de la investigación: Contribución a una revistaArtículorevisión exhaustiva

7 Citas (Scopus)

Resumen

We use data of ~13 000 stars from the Sloan Digital Sky Survey/Apache Point Observatory Galactic Evolution Experiment survey to study the shape of the bulge metallicity distribution function (MDF) within the region |l| = 11° and |b| = 13°, and spatially constrained to RGC = 3.5 kpc. We apply Gaussian mixture modelling and non-negative matrix factorization decomposition techniques to identify the optimal number and the properties of MDF components. We find that the shape and spatial variations of the MDF (at [Fe/H]=-1 dex) are well represented as a smoothly varying contribution of three overlapping components located at [Fe/H] = +0.32, -0.17, and -0.66 dex. The bimodal MDF found in previous studies is in agreement with our trimodal assessment once the limitations in sample size and individual measurement errors are taken into account. The shape of the MDF and its correlations with kinematics reveal different spatial distributions and kinematical structure for the three components co-existing in the bulge region. We confirm the consensus physical interpretation of metal-rich stars as associated with the secularly evolved disc into a boxy/peanut X-shape bar. On the other hand, metal-intermediate stars could be the product of in-situ formation at high redshift in a gas-rich environment characterized by violent and fast star formation. This interpretation would help us to link a present-day structure with those observed in formation in the centre of high-redshift galaxies. Finally, metal-poor stars may correspond to the metal-rich tail of the population sampled at lower metallicity from the study of RR Lyrae stars. Conversely, they could be associated with the metal-poor tail of the early thick disc.

Idioma originalInglés
Páginas (desde-hasta)1037-1057
Número de páginas21
PublicaciónMonthly Notices of the Royal Astronomical Society
Volumen499
N.º1
DOI
EstadoPublicada - 1 nov 2020

Áreas temáticas de ASJC Scopus

  • Astronomía y astrofísica
  • Ciencias planetarias y espacial

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