Analysis of binary star cluster candidates with Gaia DR2

Naufal, A.; Arifyanto, M. I.; Aprilia,

doi:10.1088/1742-6596/1523/1/012013

Cited by 4 publications

(4 citation statements)

References 17 publications

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“…Collinder 394 and NGC 6716 were confirmed to be physically interacting binaries by Angelo et al (2022). The pair was discovered by Pang (2019), andNaufal et al (2020) were the first to analyze their morphology, age estimates, photometric mass, and kinematics using Gaia DR2 for the first time. This is the oldest (age > 90 Myr) and closest (Sep = 11.49 pc) pair compared to the other clusters in this work.…”

Section: Known Binary Open Clustersmentioning

confidence: 99%

Binary open clusters in the Gaia data

Song

Esamdin

et al. 2022

A&A

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Context. Observations indicate that the fraction of potential binary star clusters in the Milky Way is either the same or lower than that of the Magellanic Clouds. The unprecedented precision in the parallax measurements by Gaia has allowed for the discovery of a growing number of new binary open clusters (OCs). Aims. We aim to survey the candidates of truly binary open clusters that are formed simultaneously, using information from the Gaia database. Methods. Based on the most recent catalog of open clusters, we investigated the interactions of adjacent binary open clusters in our Galaxy within separations of 50 pc. We compared their coordinates, proper motions, parallaxes, and color-magnitude diagrams (CMDs) via binary plots for all candidate pairs. The candidates of truly binary open clusters are selected on the basis of their common proper motions and consistent behaviors in the CMDs of different clusters that are limited to a separation of 50 pc. Results. About ten pairs of the selected binary open clusters appear to be the same clusters, based on evidence that almost half of the cluster members are shared. Fourteen pairs are possibly true binaries, implying that they may come from the same clouds, among which five pairs are newly discovered. In addition, two clusters, UBC 46 and UBC 192, were found to be part of the stellar complex LISCA I. Our results confirm that OCs born in groups are usually composed of young open clusters.

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Section: Known Binary Open Clustersmentioning

confidence: 99%

Binary open clusters in the Gaia data

Song

Esamdin

et al. 2022

A&A

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“…After performing the total mass estimates, we checked if each of the potentially interacting pairs are gravitationally bound (i.e, genuine binary clusters) by comparing their relative velocity (v rel ) and the system's escape velocity (vesc). An order of magnitude estimate of vesc can be obtained from the expression (e.g., Naufal et al 2020)…”

Section: Escape Velocitymentioning

confidence: 99%

“…Collinder 394−NGC 6716 Naufal et al (2020) employed Gaia DR2 data to investigate three binary cluster candidates, including the pair Collinder 394−NGC 6716. They found that both OCs present very similar proper motions, compatible heliocentric distances and ages, thus entailing an interacting pair.…”

Section: Comparison With Recent Cataloguesmentioning

confidence: 99%

Investigating Galactic binary cluster candidates with Gaia EDR3

Angelo,

Santos,

Maia

et al. 2021

Preprint

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A number of stellar open cluster (OC) pairs in the Milky Way occupy similar positions in the phase space (coordinates, parallax and proper motions) and therefore may constitute physically interacting systems. The characterization of such objects based on observational data is a fundamental step towards a proper understanding of their physical status and to investigate cluster pair formation in the Galaxy. In this work, we employed Gaia EDR3 data to investigate a set of 16 OCs distributed as seven stellar aggregates. We determined structural parameters and applied a decontamination technique that allowed to obtain unambiguous lists of member stars. The studied OCs span Galactocentric distances and ages in the ranges 7 R G (kpc) 11 and 7.3 log t 9.2. Eight OCs were found to constitute 4 gravitationally bound pairs (NGC 5617−Trumpler 22, Collinder 394−NGC 6716, Ruprecht 100−Ruprecht 101, NGC 659−NGC 663, the latter being a dynamically unevolved binary) and other 4 clusters constitute 2 interacting, but gravitationally unbound, pairs (King 16−Berkeley 4, NGC 2383−NGC 2384, the latter being a dissolving OC). Other 4 OCs (Dias 1, Pismis 19, Czernik 20, NGC 1857) seem not associated to any stellar aggregates. Apparently, clusters within bound and dynamically evolved pairs tend to present ratios of half-light to tidal radius larger than single clusters located at similar R G , suggesting that mutual tidal interactions may possibly affect their structural parameters. Unbound or dynamically unevolved systems seems to present less noticeable signature of tidal forces on their structure. Moreover, the core radius seems more importantly correlated with the clusters' internal dynamical relaxation process.

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“…Such a large separation indicates that the influence of external tidal fields has dissociated the constituent star clusters, which have detacheded on a relatively short time scale (Sugimoto & Makino 1989;Bhatia 1990). More interestingly, Naufal et al (2020) have identified new three candidates of double cluster in the LMC with separations ∼ 13 pc, i.e. ASCC 16/ASCC 21, NGC 6716/Collinder 394, and NGC 2547/Pozzo 1 from the second data release of GAIA.…”

Section: Introductionmentioning

confidence: 97%

The Formation of Binary Star Clusters in the Milky Way and Large Magellanic Cloud

Darma,

Arifyanto,

Kouwenhoven

2021

Preprint

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Recent observations of young embedded clumpy clusters and statistical identifications of binary star clusters have provided new insights into the formation process and subsequent dynamical evolution of star clusters. The early dynamical evolution of clumpy stellar structures provides the conditions for the origin of binary star clusters. Here, we carry out 𝑁-body simulations in order to investigate the formation of binary star clusters in the Milky Way and in the Large Magellanic Cloud (LMC). We find that binary star clusters can form from stellar aggregates with a variety of initial conditions. For a given initial virial ratio, a higher degree of initial substructure results in a higher fraction of binary star clusters. The number of binary star clusters decreases over time due to merging or dissolution of the binary system. Typically, ∼ 45% of the aggregates evolve into binary/multiple clusters within 𝑡 = 20 Myr in the Milky Way environment, while merely ∼ 30% survives beyond 𝑡 = 50 Myr, with separations 50 pc. On the other hand, in the LMC, ∼ 90% of the binary/multiple clusters survive beyond 𝑡 = 20 Myr and the fraction decreases to ∼ 80% at 𝑡 = 50 Myr, with separations 35 pc. Multiple clusters are also rapidly formed for highly-substructured and expanding clusters. The additional components tend to detach and the remaining binary star cluster merges. The merging process can produce fast rotating star clusters with mostly flat rotation curves that speed up in the outskirts.

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Analysis of binary star cluster candidates with Gaia DR2

Cited by 4 publications

References 17 publications

Binary open clusters in the Gaia data

Binary open clusters in the Gaia data

Investigating Galactic binary cluster candidates with Gaia EDR3

The Formation of Binary Star Clusters in the Milky Way and Large Magellanic Cloud

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