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 Tools annual

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 monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

We present the first reconstruction of the star formation history (SFH) ofthe Large and Small Magellanic Clouds (LMC and SMC) using Long Period Variablestars. These cool evolved stars reach their peak luminosity in thenear-infrared; thus, their K-band magnitudes can be used to derive their birthmass and age, and hence the SFH can be obtained. In the LMC, we found a 10-Gyrold single star formation epoch at a rate of $\sim1.5$ M$_\odot$ yr$^{-1}$,followed by a relatively continuous SFR of $\sim0.2$ M$_\odot$ yr$^{-1}$,globally. In the core of the LMC (LMC bar), a secondary, distinct episode isseen, starting 3 Gyr ago and lasting until $\sim0.5$ Gyr ago. In the SMC, twoformation epochs are seen, one $\sim6$ Gyr ago at a rate of $\sim0.28$M$_\odot$ yr$^{-1}$ and another only $\sim0.7$ Gyr ago at a rate of $\sim0.3$M$_\odot$ yr$^{-1}$. The latter is also discernible in the LMC and may thus belinked to the interaction between the Magellanic Clouds and/or Milky Way, whilethe formation of the LMC bar may have been an unrelated event. Star formationactivity is concentrated in the central parts of the Magellanic Clouds now, andpossibly has always been if stellar migration due to dynamical relaxation hasbeen effective. The different initial formation epochs suggest that the LMC andSMC did not form as a pair, but at least the SMC formed in isolation.

The star formation history of the Magellanic Clouds derived from long-period variable star counts