Spatial structure of the old open cluster NGC 2420

Peikov, Z. I.; Rusev, R. M.; Ruseva, T. S.

doi:10.1134/1.1471393

Cited by 3 publications

(3 citation statements)

References 2 publications

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“…We are also interested in the classification of globular clusters according to the degree of concentration of stars to the center, which was first considered in in the work of Shapley and Sawyer [11]. Despite the fact that for almost a century after the work of [11] many authors [12][13][14][15][16][17][18][19][20][21][22][23][24] have carried out serious studies, unfortunately, a satisfactory solution to the Shapley-Sawyer problem has not been found. Since the stellar number density increases rapidly as we approach the center of the GC, it is difficult for ground-based telescopes to analyze their central region (for details, see, for example, in [25]), and CCD observations are necessary.…”

Section: Introductionmentioning

confidence: 99%

Analysis of Observational Data of Globular Clusters within the Framework of Gaia Dr2

Turaev,

Nuritdinov,

Rastorguev

et al. 2023

Preprint

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This article is a logical continuation of the work of Nuritdinov et al. (2021). We analyzed space observations of the apparent surface density of 81 globular clusters (GCs) observed by GAIA DR2 and published in de Boer et al (2019). First, we studied the features of the quality of the GC surface density data, including comparing them with the HST data. Using our 3-parameter model, previously tested on the example of HST space observations, we found the values of the stellar concentration parameter towards the center of the cluster. As a result, we found good correlations of this parameter with the physical characteristics of the GCs. We have also found the corresponding empirical formulas for this parameter.

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Section: Introductionmentioning

confidence: 99%

Analysis of Observational Data of Globular Clusters within the Framework of Gaia Dr2

Turaev,

Nuritdinov,

Rastorguev

et al. 2023

Preprint

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“…Photometry of M12 can be found in various research articles (e.g. Nassau & Hynek 1946;Racine 1971;Buonanno et al 1976;Mironov et al 1978;Peikov & Rusev 1988;Brocato et al. 1996;Sato et al 1989;von Braun et al 2002;Hargis et al 2004).…”

Section: Introductionmentioning

confidence: 99%

“…Photometry of M12 can be found in various research articles (e.g. Nassau & Hynek 1946;Racine 1971;Buonanno et al 1976;Mironov et al 1978;Peikov & Rusev 1988;Brocato et al 1996;Sato et al 1989;von Braun et al 2002;Hargis et al 2004). von Braun et al (2002) presented an extinction map and reported small differential reddening across the cluster.…”

Section: Introductionmentioning

confidence: 99%

A proper motion study of the globular cluster M12 (NGC 6218)

Sariya

Jiang

Yadav

2018

Res. Astron. Astrophys.

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Using astrometric techniques developed by Anderson et al., we determine proper motions (PMs) in ∼14.60×16.53 arcmin 2 area of the kinematically "thick-disk" globular cluster M12. The cluster's proximity and sparse nature makes it a suitable target for ground-based telescopes. Archive images with time gap of ∼ 11.1 years were observed with wide-field imager (WFI) mosaic camera mounted on ESO 2.2 m telescope. The median value of PM error in both components is ∼ 0.7 mas yr −1 for the stars having V ≤ 20 mag. PMs are used to determine membership probabilities and to separate field stars from the cluster sample. In electronic form, a membership catalog of 3725 stars with precise coordinates, PMs, BV RI photometry is being provided. One of the possible applications of the catalog was shown by gathering the membership information of the variable stars, blue stragglers and X-ray sources reported earlier in the cluster's region.

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The longevity of the oldest open clusters

Alvarez-Baena,

Carrera,

Thompson

et al. 2024

A&A

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The dynamical evolution of open clusters is driven by stellar evolution, internal dynamics, and external forces, which according to dynamical simulations will lead to their evaporation over a timescale of about 1\,Ga. However, about 10<!PCT!> of the known open clusters are older. These latter are special systems whose detailed properties are related to their dynamical evolution and the balance between mechanisms of cluster formation and dissolution. We investigated the spatial distribution and structural parameters of six open clusters older than 1\,Ga in order to constrain their dynamical evolution and longevity. We identified members using EDR3 data up to a distance of 150\,pc from the centre of each cluster. We investigated the spatial distribution of stars inside each cluster to understand their degree of mass segregation. Finally, in order to interpret the obtained radial density profiles, we reproduced them using the lowered isothermal model explorer with and the spherical potential escapers stitched ( models. All the studied clusters appear to be more extended than previously reported in the literature. The spatial distributions of three of them show some structures aligned with their orbits. These structures may be related to the existence of extra tidal stars. Moreover, we find that about 20<!PCT!> of their members have sufficient energy to leave the systems or are already unbound. Together with their initial masses, their distances to the Galactic plane may play significant roles in their survival. We find clear evidence that the most dynamically evolved clusters do not fill their Roche volumes, appearing more concentrated than the others. Finally, we find a cusp--core dichotomy in the central regions of the studied clusters, which shows some similarities to that observed among globular clusters.

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Spatial structure of the old open cluster NGC 2420

Cited by 3 publications

References 2 publications

Analysis of Observational Data of Globular Clusters within the Framework of Gaia Dr2

Analysis of Observational Data of Globular Clusters within the Framework of Gaia Dr2

A proper motion study of the globular cluster M12 (NGC 6218)

The longevity of the oldest open clusters

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