A Study of the Blue Straggler Population of the Old Open Cluster Collinder 261

Rain, M. J.; Carraro, G.; Ahumada, J. A.; Villanova, S.; Boffin, H. M. J.; Monaco, L.; Beccari, G.

doi:10.3847/1538-3881/ab5f0b

Cited by 20 publications

(7 citation statements)

References 54 publications

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“…The CMDs of the clusters have been very useful tool in identification of the member stars and determination of the cluster parameters. These are also used in the study of blue stragglers, rotation of stars, and multi-population in the clusters (Cordoni et al 2018;Piatti & Bonatto 2019;Rain et al 2020). In this study we used (B-V)/V CMDs to derive age of the clusters.…”

Section: Age Through Cmdmentioning

confidence: 99%

Photometric study of the young open clusters IC 1442, King 21, and Trumpler 7

Maurya,

Joshi,

Gour

2020

Preprint

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We carried out UBVR c I c photometric study of three poorly studied young open clusters IC 1442, King 21, and Trumpler 7 (Tr 7). We obtained 263, 244, and 128 member stars using Gaia DR2 proper motions and parallaxes in IC 1442, King 21, and Tr 7, respectively. The reddening, E(B − V), was derived to be 0.54±0.04, 0.76±0.06, and 0.38±0.04 mag for these clusters. The comparison of observed colour-magnitude diagrams (CMDs) with solar metallicity isochrones yields log(Age) = 7.40±0.30, 7.70±0.20, and 7.85±0.25 yr and corresponding distances 2847±238, 2622±156, and 1561±74 pc for IC 1442, King 21, and Tr 7, respectively. The estimated mass function (MF) slopes are found to be -1.94±0.18, -1.54±0.32, and -2.31±0.29 for IC 1442, King 21, and Tr 7, respectively. The study of MF slopes determined separately in the inner and the outer regions of these clusters gives a steeper slope in outer region which suggests spatial variation in slope and mass segregation in the clusters. We found evidence of mass segregation after dynamical study in these clusters. The obtained relaxation time, T E , is 74, 26, and 34 Myr for the clusters IC 1442, King 21, and Tr 7, respectively. The mass segregation in IC 1442 may be caused by early dynamical relaxation. The estimated T E is well below to the ages of King 21 and Tr 7 which indicates that these clusters are dynamically relaxed.

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Section: Age Through Cmdmentioning

confidence: 99%

Photometric study of the young open clusters IC 1442, King 21, and Trumpler 7

Maurya,

Joshi,

Gour

2020

Preprint

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“…For Berkeley 17, the BSS distribution was found to be similar to the family II globular clusters (Bhattacharya et al 2019). Rain et al (2020) found a flat distribution (family I) for Collinder 261.…”

Section: The Bss Of King 11mentioning

confidence: 77%

A Gaia based photometric and kinematic analysis of the old open cluster King 11

Sariya,

Jiang,

Bisht

et al. 2021

Preprint

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This paper presents an investigation of an old age open cluster King 11 using Gaia's Early Data Release 3 (EDR3) data. Considering the stars with membership probability (P µ ) > 90%, we identified 676 most probable cluster members within the cluster's limiting radius. The mean proper motion (PM) for King 11 is determined as: µ x = −3.391 ± 0.006 and µ y = −0.660 ± 0.004 mas yr −1 . The blue straggler stars (BSS) of King 11 show a centrally concentrated radial distribution. The values of limiting radius, age, and distance are determined as 18.51 arcmin, 3.63±0.42 Gyr and 3.33 ± 0.15 kpc, respectively. The cluster's apex coordinates (A = 267.84 • ± 1.01 • , D = −27.48 • ± 1.03 • ) are determined using the apex diagram (AD) method and verified using the (µ U ,µ T ) diagram. We also obtained the orbit that the cluster follows in the Galaxy and estimated its tentative birthplace in the disk. The resulting spatial velocity of King 11 is 60.2 ± 2.16 km s −1 . A significant oscillation along the Z-coordinate up to 0.556±0.022 kpc is determined.

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“…Using the WIYN data from the WOCS collaboration (see Mathieu & WOCS Collaboration (2013), for example, for more details) would be ideal for this experiment, since it focuses on old open clusters and, at least for clusters like NGC 188, M67 and a few others, extensive studies have been done over the last several decades to thoroughly quantify the issue of cluster membership, and even provide BS binary fractions in some clusters (e.g. Mathieu & Geller 2009;Rain et al 2020). In order to increase the sample size for the number of clusters with known BS binary fractions, these WIYN data can be combined with the GC data coming from double BS sequences.…”

Section: Blue Stragglersmentioning

confidence: 99%

The mean free path approximation and stellar collisions in star clusters: Numerical exploration of the analytic rates and the role of perturbations on binary star mergers

Reinoso,

Leigh,

Barrera-Retamal

et al. 2021

Preprint

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In this paper we compute predictions for the number of stellar collisions derived from analytic models based on the mean free path (MFP) approximation and compare them to the results of 𝑁-body simulations. Our goal is to identify the cluster conditions under which the MFP approximation remains valid. Adopting a range of particle numbers (100 ≤ 𝑁 ≤ 5000) and different combinations of particle masses and radii, we explore three different channels leading to stellar collisions, all of which are expected to occur in realistic stellar environments. At high densities, binaries form from isolated three-body interactions of single stars. Hence, we consider collisions between single stars and collisions involving binary stars, after they form in our simulations. For the latter, we consider two channels for mergers, namely direct stellar collisions during chaotic single-binary interactions and perturbation-driven mergers of binaries due to random walks in eccentricity approaching unity. In the densest systems considered here, a very massive object is formed at the cluster centre, causing local stellar orbits to become increasingly Keplerian and the assumptions going into our analytic model to break down. Before reaching this limit, we obtain excellent agreement between our theoretical predictions and the simulations: the analytic rates are typically accurate to within one standard deviation for the entire parameter space considered here, but the agreement is best for short integration times. Our results have direct implications for blue straggler formation in dense star clusters, and stellar mergers in galactic nuclei hosting massive black holes.

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A Study of the Blue Straggler Population of the Old Open Cluster Collinder 261

Cited by 20 publications

References 54 publications

Photometric study of the young open clusters IC 1442, King 21, and Trumpler 7

Photometric study of the young open clusters IC 1442, King 21, and Trumpler 7

A Gaia based photometric and kinematic analysis of the old open cluster King 11

The mean free path approximation and stellar collisions in star clusters: Numerical exploration of the analytic rates and the role of perturbations on binary star mergers

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