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 investigate the frequency of occurrence of Galactic carbon stars as afunction of progenitor mass using Gaia data. Small number statistics limitfidelity, but C star frequency agrees with that observed in the MagellanicClouds (MCs) down to $m \approx1.67$ M$_\odot$. At $m \approx 1.38$ M$_\odot$,the frequency rises by a factor of three even though the frequency appears todrop to zero for the MCs. In fact this is due to a lack of clusters at the keyage range in the MCs. At $m \approx 1.24$ M$_\odot$ and below, no C stars areobserved, corresponding to ages older than 4 Gyr. Within uncertainties, C~starfrequency in M 31 is consistent with that of the Galaxy and the MCs. We find anambiguous C-star candidate at $\sim$7 M$_\odot$.

The frequency by mass of Galactic carbon stars inferred from Gaia measurements of star cluster members