A chromosome map to unveil stellar populations with different magnesium abundances. The case of ω Centauri. Issue 3 (20th July 2020)

• Record Type: Journal Article
• Authors: Milone, A P; Marino, A F; Renzini, A; Li, C; Jang, S; Lagioia, E P; Tailo, M; Cordoni, G; Carlos, M; Dondoglio, E
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 497:Issue 3(2020)
• Page Start: 3846
• Page End: 3859
• Publication Date: 2020-07-20
• Subjects: techniques: photometric -- stars: abundances -- stars: population II -- globular clusters: general; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa2119
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: Historically, photometry has been largely used to identify stellar populations [multiple populations (MPs)] in globular clusters (GCs) by using diagrams that are based on colours and magnitudes that are mostly sensitive to stars with different metallicities or different abundances of helium, carbon, nitrogen, and oxygen. In particular, the pseudo-two-colour diagram called chromosome map (ChM), allowed the identification and the characterization of MPs in about 70 GCs by using appropriate filters of the Hubble Space Telescope ( HST ) that are sensitive to the stellar content of He, C, N, O, and Fe. We use here high precision HST photometry from F 275 W, F 280 N, F 343 N, F 373 N, and F 814 W images of ω Centauri to investigate its MPs. We introduce a new ChM whose abscissa and ordinate are mostly sensitive to stellar populations with different magnesium and nitrogen, respectively, in monometallic GCs. This ChM is effective in disentangling the MPs based on their Mg chemical abundances, allowing us to explore, for the first time, possible relations between the production of these elemental species for large samples of stars in GCs. By comparing the colours of the distinct stellar populations with the colours obtained from appropriate synthetic spectra we provide 'photometric-like' estimates of the chemical composition of each population. Our results show that, in addition to first-generation (1G) stars, the metal-poor population of ω Cen hosts four groups of second-generation stars with different [N/Fe], namely, 2GA–D . 2GA stars share nearly the same [Mg/Fe] as the 1G, whereas 2GB, 2GC, and 2GD are Mg depleted by ∼0.15, ∼0.25, and ∼0.45 dex, respectively. We provide evidence that the metal-intermediate populations host stars with depleted [Mg/Fe].