A WFC3/HST VIEW OF THE THREE STELLAR POPULATIONS IN THE GLOBULAR CLUSTER NGC 6752

By A. Milone, A. Marino, G. Piotto, L. Bedin, Jay Anderson, A. Aparicio, Andrea Bellini, Santi Cassisi, F. D’Antona, F. Grundahl and 2 more. 2013

133 citations recorded by the source corpus.

Multi-band Hubble Space Telescope photometry reveals that the main sequence, sub-giant, and the red-giant branch of the globular cluster NGC 6752 splits into three main components in close analogy with the three distinct segments along its horizontal branch stars. These triple sequences are consistent with three stellar groups: a stellar population with a chemical composition similar to field-halo stars (Population a), a Population (c) with enhanced sodium and nitrogen, depleted carbon and oxygen, and an enhanced helium abundance (ΔY ∼ 0.03), and a Population (b) with an intermediate (between Populations a and c) chemical composition and slightly enhanced helium (ΔY ∼ 0.01). These components contain ∼25% (Population a), ∼45% (Population b), and ∼30% (Population c) of the stars. No radial gradient for the relative numbers of the three populations has been identified out to about 2.5 half-mass radii.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f97f2a8e6d70abeab4d663773a92b9c1b5029db5

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In Astronomy and Astrophysics

1. Jay Anderson
2. G. Piotto
3. L. Bedin
4. A. Milone
5. A. Renzini
6. F. D’Antona
7. Santi Cassisi
8. A. Aparicio

In Instrumentation

1. Jay Anderson
2. L. Bedin
3. G. Piotto
4. A. Milone
5. F. D’Antona
6. A. Renzini
7. A. Aparicio
8. Santi Cassisi

Citations in the corpus

• THE HUBBLE SPACE TELESCOPE UV LEGACY SURVEY OF GALACTIC GLOBULAR CLUSTERS. I. OVERVIEW OF THE PROJECT AND DETECTION OF MULTIPLE STELLAR POPULATIONS (2014, methodology): “1 Milone et al. (2013) defined a pseudo-colorCF275W,F336W,F438W=(mF275W−mF336W)−(mF336W−mF438W), which maximizes the virtue of both F336W− F438W and F275W− F336W, and has proven to be quite efficient in separation of multiple sequences.”
• A stellar census in globular clusters with MUSE: multiple populations chemistry in NGC 2808 (2019, background): “…multiple RGBs, SGBs, and MSs are related to differences in the abundances of some specific elements (mostly He, C, N, and O), and in fewer cases by differences in iron abundances (see, e.g., Marino et al. 2012; Milone et al. 2013, 2018; Yong et al. 2015; Bellini et al. 2017a; Lardo et al. 2018).”
• The Hubble Space Telescope UV Legacy Survey of Galactic globular clusters – IX. The Atlas of multiple stellar populations (2016, methodology): “tical HSTphotometry, as documented by pilot studies by our group (e.g., Milone et al. 2012b, 2013; Piotto et al. 2013).”
• THE AGES OF 55 GLOBULAR CLUSTERS AS DETERMINED USING AN IMPROVED METHOD ALONG WITH COLOR–MAGNITUDE DIAGRAM CONSTRAINTS, AND THEIR IMPLICATIONS FOR BROADER ISSUES (2013, background): “Indeed, support for this possibility is provided by the very recent discovery of three distinct sequences in HST/WFC3 CMDs of NGC 6752, which are characterized by ∆Y values ranging from 0.01 to 0.03 (see Milone et al. 2013).”