English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We use the data-driven method, The Cannon, to bring 21,000 stars from theARGOS bulge survey, including 10,000 red clump stars, onto the parameter andabundance scales of the cross-Galactic survey, APOGEE, obtaining rms precisionsof 0.10 dex, 0.07 dex, 74 K, and 0.18 dex for [Fe/H], [Mg/Fe], Teff, andlog(g), respectively. The re-calibrated ARGOS survey - which we refer to as theA2A survey - is combined with the APOGEE survey to investigate the abundancestructure of the Galactic bulge. We find X-shaped [Fe/H] and [Mg/Fe]distributions in the bulge that are more pinched than the bulge density, asignature of its disk origin. The mean abundance along the major axis of thebar varies such that the stars are more [Fe/H]-poor and [Mg/Fe]-rich near theGalactic center than in the long bar/outer bulge region. The vertical [Fe/H]and [Mg/Fe] gradients vary between the inner bulge and long bar with the innerbulge showing a flattening near the plane that is absent in the long bar. The[Fe/H]-[Mg/Fe] distribution shows two main maxima, an ``[Fe/H]-poor [Mg/Fe]-rich'' maximum and an ``[Fe/H]-rich [Mg/Fe]-poor'' maximum, that vary instrength with position in the bulge. In particular, the outer long bar close tothe Galactic plane is dominated by super-solar [Fe/H], [Mg/Fe]-normal stars.Stars composing the [Fe/H]-rich maximum show little kinematic dependence on[Fe/H], but for lower [Fe/H] the rotation and dispersion of the bulge increaseslowly. Stars with [Fe/H]<-1 dex have a very different kinematic structure thanstars with higher [Fe/H]. Comparing with recent models for the Galacticboxy-peanut bulge, the abundance gradients and distribution, and the relationbetween [Fe/H] and kinematics suggest that the stars comprising each maximumhave separate disk origins with the ``[Fe/H]-poor [Mg/Fe]-rich'' starsoriginating from a thicker disk than the ``[Fe/H]-rich [Mg/Fe]-poor'' stars.

A2A: 21,000 bulge stars from the ARGOS survey with stellar parameters on the APOGEE scale