The normal chemistry of multiple stellar populations in the dense globular cluster NGC 6093 (M 80)

TL;DR

This study analyzes the chemical abundances of 82 stars in the dense, metal-poor globular cluster NGC 6093 (M 80), revealing star-to-star variations in proton-capture elements and insights into multiple stellar populations.

Contribution

First detailed abundance analysis of a large star sample in M 80, linking chemical variations to cluster properties and neutron-capture element contributions.

Findings

M 80 has a mean [Fe/H] of -1.791 with minimal scatter.

Star-to-star variations in Na and O indicate multiple populations.

A significant s-process contribution affects neutron-capture element distribution.

Abstract

We present the abundance analysis of 82 red giant branch stars in the dense, metal-poor globular cluster NGC 6093 (M 80), the largest sample of stars analyzed in this way for this cluster. From high resolution UVES spectra of 14 stars and intermediate resolution GIRAFFE spectra for the other stars we derived abundances of O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Y, Zr, Ba, La, Ce, Pr, Nd, Sm, Eu. On our UVES metallicity scale the mean metal abundance of M 80 is [Fe/H]=-1.791+/-0.006+/-0.076 (+/-statistical +/-systematic error) with rms=0.023 (14 stars). M 80 shows star to star variations in proton-capture elements, and the extension of the Na-O anticorrelation perfectly fit the relations with (i) total cluster mass, (ii) horizontal branch morphology, and (iii) cluster concentration previously found by our group. The chemistry of multiple stellar populations in M 80 does not look extreme. The cluster is also a typical representative of halo globular clusters for what concerns the pattern of alpha-capture and Fe-group elements. However we found that a significant contribution from the s-process is required to account for the distribution of neutron-capture elements. A minority of stars in M 80 seem to exhibit slightly enhanced abundances of s-process species, compatible with those observed in M 22 and NGC 1851, although further confirmation from larger samples is required.