Bruck 88: a young star cluster with an old age resemblance in the outskirts of the Small Magellanic Cloud

Piatti, Andrés E.

doi:10.1093/mnras/stu1917

Cited by 9 publications

(3 citation statements)

References 72 publications

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“…A striking feature of this young cluster sample is their uniformity in age. As determined from isochrone comparisons to observed CMDs (Alcaino et al 2003;Glatt, Grebel & Koch 2010;Piatti 2014), the cluster ages pile up around ∼ 160 Myr [log(age/yr)=8.2±0.1] and appear consistent with this single age, within current fitting uncertainties. We demonstrate the agreement with a single age by over-plotting an isochrone with log(age/yr)=8.2 on top of a summed SMASH CMD created for the nine cluster sample (see lower panel in Fig.…”

Section: Young Star Clustersmentioning

confidence: 60%

Nature of a shell of young stars in the outskirts of the Small Magellanic Cloud

Martínez–Delgado

Vivas

Grebel

et al. 2019

A&A

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Context. Understanding the evolutionary history of the Magellanic Clouds requires an in-depth exploration and characterization of the stellar content in their outer regions, which ultimately are key to tracing the epochs and nature of past interactions. Aims. We present new deep images of a shell-like over-density of stars in the outskirts of the Small Magellanic Cloud (SMC). The shell, also detected in photographic plates dating back to the fifties, is located at ∼ 1.9 • from the center of the SMC in the north-east direction. Methods. The structure and stellar content of this feature were studied with multi-band, optical data from the Survey of the MAgellanic Stellar History (SMASH) carried out with the Dark Energy Camera on the Blanco Telescope at Cerro Tololo Inter-American Observatory. We also investigate the kinematic of the stars in the shell using the Gaia Data Release 2.Results. The shell is composed of a young population with an age ∼ 150 Myr, with no contribution from an old population. Thus, it is hard to explain its origin as the remnant of a tidally disrupted stellar system. The spatial distribution of the young main-sequence stars shows a rich sub-structure, with a spiral arm-like feature emanating from the main shell and a separated small arc of young stars close to the globular cluster NGC 362. We find that the absolute g-band magnitude of the shell is M g,shell = −10.78 ± 0.02, with a surface brightness of µ g,shell = 25.81 ± 0.01 mag arcsec −2 Conclusions. We have not found any evidence that this feature is of tidal origin or a bright part of a spiral arm-like structure. Instead, we suggest that the shell formed in a recent star formation event, likely triggered by an interaction with the Large Magellanic Cloud and/or the Milky Way, ∼ 150 Myr ago.

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Section: Young Star Clustersmentioning

confidence: 60%

Nature of a shell of young stars in the outskirts of the Small Magellanic Cloud

Martínez–Delgado

Vivas

Grebel

et al. 2019

A&A

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“…The added noise by contaminating field stars is also a key issue, as this noise is very difficult to remove properly from integrated photometry data. A single overly bright field star can substantially modify the observed luminosity of the cluster, leading to incorrect estimates of its parameters (Baumgardt et al 2013;Piatti 2014). A detailed analysis of some of the issues encountered by integrated photometry studies and of the accuracy of their results is presented in Anders et al (2013).…”

Section: Databases Valuesmentioning

confidence: 99%

Astrophysical properties of star clusters in the Magellanic Clouds homogeneously estimated by ASteCA

Perren

Piatti

Vazquez

2017

A&A

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Aims. We seek to produce a homogeneous catalog of astrophysical parameters of 239 resolved star clusters, located in the Small and Large Magellanic Clouds, observed in the Washington photometric system. Methods. The cluster sample was processed with the recently introduced Automated Stellar Cluster Analysis (ASteCA) package, which ensures both an automatized and a fully reproducible treatment, together with a statistically based analysis of their fundamental parameters and associated uncertainties. The fundamental parameters determined for each cluster with this tool, via a color-magnitude diagram (CMD) analysis, are metallicity, age, reddening, distance modulus, and total mass. Results. We generated a homogeneous catalog of structural and fundamental parameters for the studied cluster sample and performed a detailed internal error analysis along with a thorough comparison with values taken from 26 published articles. We studied the distribution of cluster fundamental parameters in both Clouds and obtained their age-metallicity relationships. Conclusions. The ASteCA package can be applied to an unsupervised determination of fundamental cluster parameters, which is a task of increasing relevance as more data becomes available through upcoming surveys.

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“…Unfortunately, there is a small number of clusters with measured distances (see Section 2), which points to the need of observational campaigns in order to build a realistic spatial distribution of them (Piatti 2021b), and consequently, to trace more precisely the 3D SMC cluster population structure. Previous star cluster studies adopted, in general, a mean SMC distance when dealing with cluster colour-magnitudes diagrams (Piatti 2012(Piatti , 2014Piatti et al 2016, and references therein). This is because changes in the distance modulus by an amount equivalent to the average depth of the SMC (Crowl et al 2001;Ripepi et al 2017;Graczyk et al 2020), so that clusters can be placed in front or behind the SMC, leads to a smaller age difference than that resulting from the isochrones bracketing the observed star cluster features in the colour-magnitude diagram.…”

Section: Analysis and Discussionmentioning

confidence: 99%

Residual velocities of Small Magellanic Cloud star clusters

Piatti

2021

Preprint

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We analyzed the largest Small Magellanic Cloud (SMC) cluster sample (32) with proper motions and radial velocity measurements, from which we obtained their space velocity components. By adopting as a reference the recent best-fitted rotating disc of SMC star clusters as a function of the position angle, we computed their residual velocity vectors, and compared their magnitudes (∆V ) with that of a cluster with residual velocity components equal to the velocity dispersions along the three independent SMC rotating disc axes of motion (∆V = 60 km/s). We found that clusters that belong to SMC tidally induced structures have ∆V > 50 km/s, which suggests that space velocities of clusters in the process of escaping the rotating disc kinematics, are measurably different. Studied clusters pertaining to a northern branch of the Magellanic Bridge, the main Magellanic Bridge, the Counter-Bridge and the West halo give support to these findings. NGC 121, the oldest known SMC cluster, does not belong to any SMC tidal feature, and has ∆V = 64 km/s, slightly above the boundary between bound and kinematically perturbed clusters.

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Bruck 88: a young star cluster with an old age resemblance in the outskirts of the Small Magellanic Cloud

Cited by 9 publications

References 72 publications

Nature of a shell of young stars in the outskirts of the Small Magellanic Cloud

Nature of a shell of young stars in the outskirts of the Small Magellanic Cloud

Astrophysical properties of star clusters in the Magellanic Clouds homogeneously estimated by ASteCA

Residual velocities of Small Magellanic Cloud star clusters

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