2020
DOI: 10.1093/mnras/staa029
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Abstract: We present a comprehensive photometric analysis of a young open cluster NGC 1960 (= M36) along with the long-term variability study of this cluster. Based on the kinematic data of Gaia DR2, the membership probabilities of 3871 stars are ascertained in the cluster field among which 262 stars are found to be cluster members. Considering the kinematic and trigonometric measurements of the cluster members, we estimate a mean cluster parallax of 0.86±0.05 mas and mean proper motions of µ RA = -0.143±0.008 mas yr −1… Show more

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Cited by 29 publications
(29 citation statements)
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“…The mass segregation is the phenomenon in which massive stars are more centrally concentrated than low mass stars in clusters and has been reported in many clusters (e.g., Joshi et al 2014;Piatti 2016;Zeidler et al 2017;Dib et al 2018;Joshi et al 2020). The mass segregation effect can be triggered due to the dynamical evolution of the cluster or may be imprint of star formation process itself (Sagar et al 1988).…”
Section: Mass Segregationmentioning
confidence: 99%
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“…The mass segregation is the phenomenon in which massive stars are more centrally concentrated than low mass stars in clusters and has been reported in many clusters (e.g., Joshi et al 2014;Piatti 2016;Zeidler et al 2017;Dib et al 2018;Joshi et al 2020). The mass segregation effect can be triggered due to the dynamical evolution of the cluster or may be imprint of star formation process itself (Sagar et al 1988).…”
Section: Mass Segregationmentioning
confidence: 99%
“…In the right panels of Figure 5, we show these probable members by small region within the red circle in the VPDs which are the same stars those lie exactly on the Main-sequence and shown by filled circles in the CMDs of the same figure. To quantify membership of stars we assigned membership probabilities to stars in the clusters which were estimated using a statistical method based on PMs of stars as described in previous studies (Sanders 1971;Michalska 2019;Joshi et al 2020). In this method i th star is assigned with membership probability calculated as…”
Section: Proper Motion Membershipmentioning
confidence: 99%
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“…Unlike compact halo counterparts (i.e., globular clusters), open clusters have a looser spatial distribution, and the interaction among the stars in an open cluster leads to the energy exchange(Inagaki & Saslaw, 1985;Baumgardt & Makino, 2003). This phenomenon has been recently reported for many open clusters (e.g Dib & Basu 2018;Bisht et al 2020;Joshi et al 2020)…”
mentioning
confidence: 84%
“…We calculated membership probabilities for the stars present in the observed regions of the selected clusters through statistical method using PMs of stars as given in previous studies (Sanders 1971;Joshi et al 2020). The equations used in membership calculation using this method are given in our previous study .…”
Section: Membershipmentioning
confidence: 99%