Fluorine variations in the globular cluster NGC 6656 (M22): implications for internal enrichment timescales

TL;DR

This study investigates fluorine abundance variations in globular cluster M22, revealing correlations with other elements and constraining the timescale of internal chemical enrichment through spectroscopic analysis.

Contribution

It provides the first detailed fluorine abundance measurements in M22, linking them to multiple populations and chemical enrichment timescales.

Findings

F varies among stars beyond measurement errors

F correlates with O and anticorrelates with Na

Differences in F content between sub-groups suggest enrichment by 4-5 solar mass AGB stars

Abstract

Observed chemical (anti)correlations in proton-capture elements among globular cluster stars are presently recognized as the signature of self-enrichment from now extinct, previous generations of stars. This defines the multiple population scenario. Since fluorine is also affected by proton captures, determining its abundance in globular clusters provides new and complementary clues regarding the nature of these previous generations, and supplies strong observational constraints to the chemical enrichment timescales. In this paper we present our results on near-infrared CRIRES spectroscopic observations of six cool giant stars in NGC 6656 (M22): the main objective is to derive the F content and its internal variation in this peculiar cluster, which exhibits significant changes in both light and heavy element abundances. We detected F variations across our sample beyond the measurement uncertainties and found that the F abundances are positively correlated with O and anticorrelated with Na, as expected according to the multiple population framework. Furthermore, our observations reveal an increase in the F content between the two different sub-groups, s-process rich and s-process poor, hosted within M22. The comparison with theoretical models suggests that asymptotic giant stars with masses between 4 and 5 Msun are responsible for the observed chemical pattern, confirming evidence from previous works: the difference in age between the two sub-components in M22 must be not larger than a few hundreds Myr.