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

In some scenarios for the formation of the Milky Way bulge the stellarpopulation at the edges of the boxy bulge may be younger than those on theminor axis, or close to the Galactic center. So far the only bulge region wheredeep color-magnitude diagrams have been obtained is indeed along the minoraxis. To overcome this limitation, we aim at age-dating the bulge stellarpopulations far away from the bulge minor axis. Color-magnitude diagrams andluminosity functions have been obtained from deep near-IR VLT/HAWK-I imagestaken at the two Southern corners of the boxy bulge, i.e., near the oppositeedges of the Galactic bar. The foreground disk contamination has beenstatistically removed using a pure disk field observed with the same instrumentand located approximately at similar Galactic latitudes of the two bulgefields, and 30deg in longitude away from the Galactic center. For each bulgefield, mean reddening and distance are determined using the position of redclump stars, and the metallicity distribution is derived photometrically usingthe color distribution of stars in the upper red giant branch. The resultingmetallicity distribution function of both fields peaks around [Fe/H] -0.1 dex,with the bulk of the stellar population having a metallicity within the range:-1 dex < [Fe/H] <+0.4 dex, quite similar to that of other inner bulge fields.Like for the inner fields previously explored, the color-magnitude diagrams ofthe two bar fields are consistent with their stellar population being olderthan ~10 Gyr, with no obvious evidence for the presence of a youngerpopulation.

Stellar Ages through the Corners of the Boxy Bulge