Chemical characterisation of the globular cluster NGC 5634 associated to the Sagittarius dwarf spheroidal galaxy

Carretta, E.; Bragaglia, A.; Lucatello, S.; D’Orazi, V.; Gratton, R.; Donati, P.; Sollima, A.; Sneden, Christopher

doi:10.1051/0004-6361/201630004

Cited by 25 publications

(26 citation statements)

References 68 publications

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“…Kayser et al 2008;Smolinsky et al 2011), O and Na, and Mg and Al (see e.g. Carretta et al 2009a,b;Bragaglia et al 2015;Carretta et al 2017 and references therein for our FLAMES survey of more than 25 MW GCs). Photometrically, light element variations manifest in colour-magnitude diagrams (CMD) as sequence broadening and splitting (e.g.…”

Section: Introductionmentioning

confidence: 88%

“…To increase the sample studied with high-resolution spectroscopy, we obtained data for a few old and massive open clusters (OCs; i.e. Berkeley 39, NGC 6791: Bragaglia et al 2012Bragaglia et al , 2014 and low-mass GCs, which are also connected with the Sgr dSph (Terzan 8, NGC 6139, and NGC 5634;Carretta et al 2014a;Bragaglia et al 2015;Carretta et al 2017).…”

Section: Introductionmentioning

confidence: 99%

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NGC 6535: the lowest mass Milky Way globular cluster with a Na-O anti-correlation?

Bragaglia

Carretta

D’Orazi

et al. 2017

A&A

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To understand globular clusters (GCs) we need to comprehend how their formation process was able to produce their abundance distribution of light elements. In particular, we seek to figure out which stars imprinted the peculiar chemical signature of GCs. One of the best ways is to study the light-element anti-correlations in a large sample of GCs that are analysed homogeneously. As part of our spectroscopic survey of GCs with FLAMES, we present here the results of our study of about 30 red giant member stars in the low-mass, low-metallicity Milky Way cluster NGC 6535. We measured the metallicity (finding [Fe/H]=−1.95, rms=0.04 dex in our homogeneous scale) and other elements of the cluster and, in particular, we concentrate here on O and Na abundances. These elements define the normal Na-O anti-correlation of classical GCs, making NGC 6535 perhaps the lowest mass cluster with a confirmed presence of multiple populations. We updated the census of Galactic and extragalactic GCs for which a statement on the presence or absence of multiple populations can be made on the basis of high-resolution spectroscopy preferentially, or photometry and low-resolution spectroscopy otherwise; we also discuss the importance of mass and age of the clusters as factors for multiple populations.

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Section: Introductionmentioning

confidence: 88%

Section: Introductionmentioning

confidence: 99%

NGC 6535: the lowest mass Milky Way globular cluster with a Na-O anti-correlation?

Bragaglia

Carretta

D’Orazi

et al. 2017

A&A

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“…Two other clusters, NGC 5024 and NGC 5053, have at some point been linked to Sagittarius, although recent proper motion measurements have demonstrated this association is unlikely (see Law & Majewski 2010;Sohn et al 2018;Gaia Collaboration, Helmi et al 2018). Also NGC 5634 has been related to Sagittarius (Law & Majewski 2010;Carretta et al 2017) based on its position and radial velocity. However, the proper motion of the system measured by Gaia Collaboration, Helmi et al (2018) is very different from the prediction by for example, the Law & Majewski (2010) model of the Sagittarius streams.…”

Section: Association With Globular Clustersmentioning

confidence: 99%

Characterization and history of the Helmi streams with Gaia DR2

Koppelman

Helmi

Massari

et al. 2019

A&A

157

199

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Context. The halo of the Milky Way has long been hypothesized to harbour significant amounts of merger debris. This view has been supported over more than a decade by wide-field photometric surveys which have revealed the outer halo to be lumpy. Aims. The recent release of Gaia DR2 is allowing us to establish that mergers also have been important and possibly built up the majority of the inner halo. In this work we focus on the Helmi streams, a group of streams crossing the Solar vicinity and known for almost two decades. We characterize their properties and relevance for the build-up of the Milky Way's halo. Methods. We identify new members of the Helmi streams in an unprecedented dataset with full phase-space information combining Gaia DR2, and the APOGEE DR2, RAVE DR5 and LAMOST DR4 spectroscopic surveys. Based on the orbital properties of the stars, we find new stream members up to a distance of 5 kpc from the Sun, which we characterize using photometry and metallicity information. We also perform N-body experiments to constrain the time of accretion and properties of the progenitor of the streams. Results. We find nearly 600 new members of the Helmi streams. Their HR diagram reveals a broad age range, from approximately 11 to 13 Gyr, while their metallicity distribution goes from −2.3 to −1.0, and peaks at [Fe/H] ∼ −1.5. These findings confirm that the streams originate in a dwarf galaxy. Furthermore, we find 7 globular clusters to be likely associated, and which follow a well-defined age-metallicity sequence whose properties suggest a relatively massive progenitor object. Our N-body simulations favour a system with a stellar mass of ∼ 10 8 M accreted 5 − 8 Gyr ago. Conclusions. The debris from the Helmi streams is an important donor to the Milky Way halo, contributing approximately 15% of its mass in field stars and 10% of its globular clusters.

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“…NGC 5634 was first proposed to be associated to an ancient wrap of the stream by Bellazzini et al (2002) and Bellazzini et al (2003a). Later Law & Majewski (2010b) and Carretta et al (2017) confirmed it as a good candidate. In the metalpoor regime the abundance patterns of the Milky Way and of Sgr dSphs are very similar.…”

Section: Ngc 5634mentioning

confidence: 99%

Globular Clusters in the Sagittarius stream. Revising members and candidates with Gaia DR2

Bellazzini,

Ibata,

Malhan

et al. 2020

Preprint

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We reconsider the case for the association of Galactic globular clusters (GCs) to the tidal stream of the Sagittarius dwarf spheroidal galaxy (Sgr dSph), using Gaia DR2 data. We use RR Lyrae to trace the stream in 6D and we select clusters matching the observed stream in position and velocity. In addition to the clusters residing in the main body of the galaxy (M 54, Ter 8, Ter 7, Arp 2) we confirm the membership of Pal 12 and Whiting 1 to the portion of the trailing arm populated by stars lost during recent perigalactic passages. NGC 2419, NGC 5634 and NGC 4147 are very interesting candidates, possibly associated to more ancient wraps of the stream. We note that all these clusters, with the exception of M 54, that lies within the stellar nucleus of the galaxy, are found in the trailing arm of the stream. The selected clusters are fully consistent with the [Fe/H] vs. [Mg/Fe], [Ca/Fe] patterns and the age-metallicity relation displayed by field stars in the main body of Sgr dSph.

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Chemical characterisation of the globular cluster NGC 5634 associated to the Sagittarius dwarf spheroidal galaxy

Cited by 25 publications

References 68 publications

NGC 6535: the lowest mass Milky Way globular cluster with a Na-O anti-correlation?

NGC 6535: the lowest mass Milky Way globular cluster with a Na-O anti-correlation?

Characterization and history of the Helmi streams with Gaia DR2

Globular Clusters in the Sagittarius stream. Revising members and candidates with Gaia DR2

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