Age – metallicity relation in the Magellanic Clouds clusters

Livanou, E.; Dapergolas, A.; Kontizas, M.; Nordström, B.; Kontizas, E.; Andersen, J.; Dirsch, B.; Karampelas, A.

doi:10.1051/0004-6361/201220926

Cited by 16 publications

(24 citation statements)

References 33 publications

(34 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Our results are in agreement with Livanou et al (2013), who analyzed a sample of 15 LMC clusters spread all over the galaxy. On the other hand, the field stars AMR relation from Carrera et al (2011) lead to higher metallicities at a fixed age than those typically inferred for our sample of outer LMC clusters, at least for ages > 3 Gyr.…”

Section: Des-sv Lmc Clusterssupporting

confidence: 93%

“…(x) The age-metallicity relationship for LMC clusters differs from LMC field stars AMR (from Piatti & Geisler 2013) in the sense that the latter form an upper envelope in metallicity for age distribution. The same feature is shown in Livanou et al (2013), as the presence of young clusters (1Gyr) filling the range from most metal rich down to [Fe/H] ≃ -1.2.…”

Section: Discussion and Summarysupporting

confidence: 73%

See 1 more Smart Citation

Physical properties of star clusters in the outer LMC as observed by the DES

Pieres

Santiago

Balbinot

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

The Large Magellanic Cloud (LMC) harbors a rich and diverse system of star clusters, whose ages, chemical abundances, and positions provide information about the LMC history of star formation. We use Science Verification imaging data from the Dark Energy Survey to increase the census of known star clusters in the outer LMC and to derive physical parameters for a large sample of such objects using a spatially and photometrically homogeneous data set. Our sample contains 255 visually identified cluster candidates, of which 109 were not listed in any previous catalog.We quantify the crowding effect for the stellar sample produced by the DES Data c 2015 The Authors Management pipeline and conclude that the stellar completeness is < 10% inside typical LMC cluster cores. We therefore develop a pipeline to sample and measure stellar magnitudes and positions around the cluster candidates using DAOPHOT. We also implement a maximum-likelihood method to fit individual density profiles and colour-magnitude diagrams. For 117 (from a total of 255) of the cluster candidates (28 uncatalogued clusters), we obtain reliable ages, metallicities, distance moduli and structural parameters, confirming their nature as physical systems. The distribution of cluster metallicities shows a radial dependence, with no clusters more metal-rich than [F e/H] ≃ −0.7 beyond 8 kpc from the LMC center. The age distribution has two peaks at ≃ 1.2 Gyr and ≃ 2.7 Gyr.

show abstract

Section: Des-sv Lmc Clusterssupporting

confidence: 93%

Section: Discussion and Summarysupporting

confidence: 73%

Physical properties of star clusters in the outer LMC as observed by the DES

Pieres

Santiago

Balbinot

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

“…The possible explanation is the adopted calibration of Strömgren colors with metallicity. Data points based on Strömgren photometry from Livanou et al (2013), Piatti (2018), andPiatti et al (2019) were obtained with different calibrations (Hilker, Richtler & Gieren 1995;Grebel & Richtler 1992;Calamida et al 2007, respectively). Hilker (2000) pre-sented an extended calibration of Grebel & Richtler (1992) for cluster and field red giants for a wide range of metallicities (−2.0 < [Fe/H] < 0.0 dex).…”

Section: Discussionmentioning

confidence: 99%

Metallicities and ages for 35 star clusters and their surrounding fields in the Small Magellanic Cloud

Narloch,

Pietrzyński,

Gieren

et al. 2021

Preprint

View full text Add to dashboard Cite

Aims. In this work we study 35 stellar clusters in the Small Magellanic Cloud (SMC) in order to provide their mean metallicities and ages. We also provide mean metallicities of the fields surrounding the clusters. Methods. We used Strömgren photometry obtained with the 4.1 m SOAR telescope and take advantage of (b − y) and m1 colors for which there is a metallicity calibration presented in the literature. Results. The spatial metallicity and age distributions of clusters across the SMC are investigated using the results obtained by Strömgren photometry. We confirm earlier observations that younger, more metal-rich star clusters are concentrated in the central regions of the galaxy, while older, more metal-poor clusters are located farther from the SMC center. We construct the age-metallicity relation for the studied clusters and find good agreement with theoretical models of chemical enrichment, and with other literature age and metallicity values for those clusters. We also provide the mean metallicities for old and young populations of the field stars surrounding the clusters, and find the latter to be in good agreement with recent studies of the SMC Cepheid population. Finally, the Strömgren photometry obtained for this study is made publicly available.

show abstract

“…Studies linking epochs of enhanced star formation with the MCs' approach are numerous (e.g. Bica et al 1998;Subramaniam 2004;Glatt et al 2010;Livanou et al 2013;Rubele et al 2015;Strantzalis et al 2019).…”

Section: Introductionmentioning

confidence: 99%

“…6; g taken from (1) Piatti et al (2005), (2) Mould et al (1992), (3) Glatt et al (2010), (4) Matteucci et al (2002), (5) Nayak et al (2018), (6) Dias et al (2016), (7) Maia et al (2019), (8) Parisi et al (2014), (9) Piatti (2014), (10) Chiosi et al (2006), (11) Maia et al (2014), (12) Santos et al (2010), (13) Piatti (2011b), (14) Piatti et al (2015), (15) Kalari et al (2018), (16) Dias et al (2014), (17) Geisler et al (1997), (18) Piatti (2012), (19)Piatti (2011a), (20)Livanou et al (2013) …”

mentioning

confidence: 99%

The VISCACHA survey – II. Structure of star clusters in the Magellanic Clouds periphery

Santos

Maia

Dias

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We provide a homogeneous set of structural parameters of 83 star clusters located at the periphery of the Small Magellanic Cloud (SMC) and the Large Magellanic Cloud (LMC). The clusters’ stellar density and surface brightness profiles were built from deep, AO assisted optical images, and uniform analysis techniques. The structural parameters were obtained from King and Elson et al. model fittings. Integrated magnitudes and masses (for a subsample) are also provided. The sample contains mostly low surface brightness clusters with distances between 4.5 and 6.5 kpc and between 1 and 6.5 kpc from the LMC and SMC centres, respectively. We analysed their spatial distribution and structural properties, comparing them with those of inner clusters. Half-light and Jacobi radii were estimated, allowing an evaluation of the Roche volume tidal filling. We found that: (i) for our sample of LMC clusters, the tidal radii are, on average, larger than those of inner clusters from previous studies; (ii) the core radii dispersion tends to be greater for LMC clusters located towards the southwest, with position angles of ∼200 degrees and about ∼5 degrees from the LMC centre, i.e., those LMC clusters nearer to the SMC; (iii) the core radius evolution for clusters with known age is similar to that of inner clusters; (iv) SMC clusters with galactocentric distances closer than 4 kpc are overfilling; (v) the recent Clouds collision did not leave marks on the LMC clusters’ structure that our analysis could reveal.

show abstract

Age – metallicity relation in the Magellanic Clouds clusters

Cited by 16 publications

References 33 publications

Physical properties of star clusters in the outer LMC as observed by the DES

Physical properties of star clusters in the outer LMC as observed by the DES

Metallicities and ages for 35 star clusters and their surrounding fields in the Small Magellanic Cloud

The VISCACHA survey – II. Structure of star clusters in the Magellanic Clouds periphery

Contact Info

Product

Resources

About