Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VI. M3 (NGC 5272) Is Not a Prototypical Normal Globular Cluster*
               
               †

Lee, Jae-Woo; Sneden, Christopher

doi:10.3847/1538-4357/abd948

Cited by 12 publications

(44 citation statements)

References 79 publications

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“…The cn JWL CMD shows discrete double RGB sequences (see also Lee 2017Lee , 2019a. On the other hand, our ch JWL , nh JWL , and m1 CMDs show very broad RGB sequences, due to spreads in the carbon and nitrogen abundances as we will discuss later (also see Lee & Sneden 2021).…”

Section: Color-magnitude Diagramsmentioning

confidence: 70%

“…Throughout this work, we will use our own photometric indices already defined in our previous works (Lee 2017(Lee , 2019aLee & Sneden 2021),…”

Section: Color-magnitude Diagramsmentioning

confidence: 99%

“…The nh JWL , cn JWL , and ch JWL are excellent measures of the NH band at λ3360, the CN band at λ3883, and the CH G band at λ4250, respectively, for cool stars (Lee 2017(Lee , 2019b(Lee , 2020Lee & Sneden 2021). We made use of the proper motions from the Gaia EDR3 to select the cluster's membership stars, following the method similar to those used in our previous studies (see, e.g., Lee 2020; Lee & Sneden 2021, and references therein).…”

Section: Color-magnitude Diagramsmentioning

confidence: 99%

“…Our new Ca-CN-CH-NH observations of the cluster reveal new population with interesting physical properties that we were not able to detect in our previous study. Lee 2015Lee , 2017Lee , 2019aLee & Sneden 2021, for our new filter system). Our method can avoid the crowding effects with potential contamination by neighboring stars, which is one of the limitations in the classical spectroscopic study of the GC stars, in particular, in the central part of GCs.…”

Section: Introductionmentioning

confidence: 99%

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Formation of Multiple Populations of M5 (NGC 5904)

Lee

2021

Preprint

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With our new Ca-CN-CH-NH photometry, we revisit the globular cluster (GC) M5. We find that M5 is a mono-metallic GC with a small metallicity dispersion. Our carbon abundances show that the σ[C/Fe] of the M5 CN-s population, with depleted carbon and enhanced nitrogen abundances, is significantly large for a single stellar population. Our new analysis reveals that the M5 CN-s population is well described by the two stellar populations: the CN-s I , being the major CN-s component, with the intermediate carbon and nitrogen abundance and the CN-s E with the most carbon-poor and nitrogen-rich abundance. We find that the CN-s E is significantly more centrally concentrated than the others, while CN-w and CN-s I have similar cumulative radial distributions. The red giant branch bump V magnitude, the helium abundance barometer in mono-metallic populations, of individual populations appears to be correlated with their mean carbon abundance, indicating that carbon abundances are anticorrelated with helium abundances. We propose that the CN-s E formed out of gas that experienced proton-capture processes at high temperatures in the innermost region of the proto-GC of M5 that resided in a dense ambient density environment. Shortly after, the CN-s I formed out of gas diluted from the pristine gas in the more spatially extended region, consistent with the current development of numerical simulations by others.

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Section: Color-magnitude Diagramsmentioning

confidence: 70%

“…Throughout this work, we will use our own photometric indices already defined in our previous works (Lee 2017(Lee , 2019aLee & Sneden 2021),…”

Section: Color-magnitude Diagramsmentioning

confidence: 99%

Section: Color-magnitude Diagramsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Formation of Multiple Populations of M5 (NGC 5904)

Lee

2021

Preprint

Self Cite

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“…If nitrogen becomes more abundant than carbon as a result of this process, the CN band strength no longer scale monotonically with N abundance and can even decline with rising luminosity (e.g. Smith & Bell 1986;Martell et al 2008a;Lee & Sneden 2021). As a consequence, in the low-metallicity regime, the CN index has only limited sensitivity to variations in nitrogen (see Fig.…”

Section: Discussionmentioning

confidence: 99%

Evidence for C, O, Al and Mg variations in the GD-1 stellar stream

Balbinot,

Cabrera-Ziri,

Lardo

2021

Preprint

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Dynamically cold stellar streams are the relics left over from globular cluster dissolution. These relics offer a unique insight into a now fully disrupted population of ancient clusters in our Galaxy. Using a combination of Gaia eDR3 proper motions, optical and near-UV colours we select a sample of likely Red Giant Branch stars from the GD-1 stream for medium-low resolution spectroscopic follow-up. Based on radial velocity and metallicity, we are able to find 14 new members of GD-1, 5 of which are associated with the spur and blob/cocoon off-stream features. We measured C-abundances to probe for the abundance variations known to exist in globular clusters. These variations are expected to manifest in a subtle way in globular clusters with such low masses (∼ 10 4 M ) and metallicities ([Fe/H] ∼ −2.1 dex). We find that the C-abundances of the stars in our sample display a small but significant (3σ level) spread. Furthermore, we find ≥ 4σ variations in Al-and Mg-abundances as well as a ∼ 2σ O-abundance variation among the stars in our sample that have been observed by APOGEE. These abundance patterns match the ones found in Galactic globular clusters of similar metallicity. Our results suggest that GD-1 represents the first fully disrupted globular cluster where light-element abundance spreads have been found.

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Kinematic differences between multiple populations in Galactic globular clusters

Martens

Kamann

Göttgens

et al. 2023

A&A

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Aims. The formation process of multiple populations in globular clusters is still up for debate. These populations are characterized by different light-element abundances. Kinematic differences between the populations are particularly interesting in this respect, because they allow us to distinguish between single-epoch formation scenarios and multi-epoch formation scenarios. We derive rotation and dispersion profiles for 25 globular clusters and aim to find kinematic differences between multiple populations in 21 of them to constrain the formation process. Methods. We split red-giant branch (RGB) stars in each cluster into three populations (P1, P2, P3) for the type-II clusters and two populations (P1 and P2) otherwise using Hubble photometry. We derive the global rotation and dispersion profiles for each cluster by using all stars with radial velocity measurements obtained from MUSE spectroscopy. We also derive these profiles for the individual populations of each cluster. Based on the rotation and dispersion profiles, we calculate the rotation strength in terms of ordered-overrandom motion (v/σ) HL evaluated at the half-light radius of the cluster. We then consistently analyse all clusters for differences in the rotation strength of their populations. Results. We detect rotation in all but four clusters.

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Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH–NH Photometry. VI. M3 (NGC 5272) Is Not a Prototypical Normal Globular Cluster* †

Cited by 12 publications

References 79 publications

Formation of Multiple Populations of M5 (NGC 5904)

Formation of Multiple Populations of M5 (NGC 5904)

Evidence for C, O, Al and Mg variations in the GD-1 stellar stream

Kinematic differences between multiple populations in Galactic globular clusters

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