Photometric, kinematic, and variability study in the young open cluster NGC 1960

Joshi, Y. C.; Maurya, Jayanand; John, Ancy Anna; Panchal, Alaxender; Joshi, Santosh; Kumar, Brijesh

doi:10.1093/mnras/staa029

Cited by 30 publications

(30 citation statements)

References 94 publications

(141 reference 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%

“…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%

“…There are many methods to determine the membership of cluster stars using photometric, proper motions, radial velocities, polarimetric data and their combinations (Joshi et al 2012;Medhi & Tamura 2013;Gao 2014). Recently, with the availability of the Gaia DR2 catalog (Gaia Collaboration et al 2018) having unprecedented astrometric precision, the membership determination based on kinematic method (proper motions or radial velocities) becomes a reliable tool to identify the cluster members (e.g., Cantat-Gaudin et al 2018Castro-Ginard et al 2018Bisht et al 2019;Joshi et al 2020). The precise knowledge of cluster membership helps us to study the distribution of stellar mass, also known as MF, which has a fundamental importance in the study of dynamic evolution of star clusters.…”

Section: Introductionmentioning

confidence: 99%

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Photometric and kinematic study of the three intermediate age open clusters NGC 381, NGC 2360, and Berkeley 68

Maurya

Joshi

2020

Monthly Notices of the Royal Astronomical Society

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We present UBVR c I c photometric study of three intermediate age open star clusters NGC 381, NGC 2360, and Berkeley 68 (Be 68). We examine the cluster membership of stars using recently released Gaia DR2 proper motions and obtain a total of 116, 332, and 264 member stars in these three clusters. The mean reddening of E(B − V) = 0.36±0.04, 0.08±0.03, and 0.52±0.04 mag are found in the direction of these clusters where we observe an anomalous reddening towards NGC 381. We fitted the solar metallicity isochrones to determine age and distance of the clusters which are found to be log(Age) = 8.65±0.05, 8.95±0.05, and 9.25±0.05 yr with the respective distance of 957±152, 982±132, and 2554±387 pc for the clusters NGC 381, NGC 2360, and Be 68. A two-stage power law in the mass function (MF) slope is observed in the cluster NGC 381, however, we observe only a single MF slope in the clusters NGC 2360 and Be68. To study a possible spatial variation in the slope of MF we estimate slopes separately in the inner and the outer regions of these clusters and notice a steeper slope in outer region. The dynamic study of these clusters reveals deficiency of lowmass stars in their inner regions suggesting the mass segregation process in all these clusters. The relaxation times of 48.5, 78.9, and 87.6 Myr are obtained for the clusters NGC 381, NGC 2360, and Be 68, respectively which are well below to their respective ages. This suggests that all the clusters are dynamically relaxed.

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Section: Mass Segregationmentioning

confidence: 99%

Section: Proper Motion Membershipmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Photometric and kinematic study of the three intermediate age open clusters NGC 381, NGC 2360, and Berkeley 68

Maurya

Joshi

2020

Monthly Notices of the Royal Astronomical Society

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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%

A comprehensive photometric and kinematical characteristic of the newly discovered QCs clusters with Gaia EDR3

Elsanhoury,

Amin,

Haroon

et al. 2022

Preprint

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This study reports the first comprehensive astrometric, photometric and kinematical analysis of four newly discovered open clusters; namely QC1, QC2, QC3, and QC4, using astrometric and photometric data from the most recent Gaia EDR3 for G < 17 mag. Utilizing the ASteCA code, we identified the most probable (P ≥ 50%) star candidates and found the numbers of star members (N) to be 118 (QC1), 142 (QC2), 210 (QC3), and 110 (QC4). By fitting King's density profile to the cluster's RDPs, we found the internal structural parameters of each cluster such as the cluster radii that are in the range 7.00 to 11.00 arcmin. For each cluster we constructed the CMD and by fitting them with suitable isochrones we found that the metallicity range is (0.0152 -0.0199) which is in line with the Solar value, the logarithmic age (in yrs) range between 6.987 and 8.858. The distances derived from CMD are 1674±41, 1927±44, 1889±43, and 1611±40 (pc) for QC1, QC2, QC3, and QC4, respectively, and they are in good agreement up to 85% with the values obtained from the astrometric data. In addition, from the MLR of the clusters, we obtained a total mass, M C in Solar units, of 158, 177, 232, and 182 and an absolute magnitude M G (mag) of 4. 33, 3.80, 4.25, and 4.10 for QC1, QC2, QC3, and QC4, respectively. The dynamical analysis and evolution parameters of the cluster members indicated that all the four clusters are dynamically relaxed; except QC1 which has an evolution parameter τ ∼ 0.82 that indicates a dynamical activity within the cluster. From the kinematical analysis of the cluster data, we computed the space velocity, the coordinates of the apex point (A, D) using the AD -diagram method, as well as the Solar elements (S , l A , b A , α A , δ A ).

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“…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%

Photometric and Kinematic study of the open clusters SAI 44 and SAI 45

Maurya¹,

C.²,

Elsanhoury³

et al. 2021

Preprint

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We carry out detailed photometric and kinematic study of the poorly studied sparse open clusters SAI 44 and SAI 45 using ground based BVR c I c data supplemented by archival data from Gaia eDR3 and Pan-STARRS. The stellar membership are determined using a statistical method based on Gaia eDR3 kinematic data and we found 204 members in SAI 44 while only 74 members are identified in SAI 45. The average distances to SAI 44 and SAI 45 are calculated as 3670±184 and 1668±47 pc. The logarithmic age of the clusters are determined as 8.82±0.10 and 9.07±0.10 years for SAI 44 and SAI 45, respectively. The color-magnitude diagram of SAI 45 hosts an extended main-sequence turn-off (eMSTO) which may be originated through differential rotation rates of member stars. The mass function slopes are obtained as -1.75±0.72 and -2.58±3.20 in the mass rages 2.426-0.990 M and 2.167-1.202 M for SAI 44 and SAI 45, respectively. SAI 44 exhibit the signature of mass segregation while we found a weak evidence of the mass segregation in SAI 45 possibly due to tidal striping. The dynamical relaxation times of these clusters indicate that both the clusters are in dynamically relaxed state. Using AD-diagram method, the apex coordinates are found to be (69. • 79 ± 0. • 11, -30. • 82 ± 0. • 15) for SAI 44 and (-56. • 22 ± 0. • 13, -56. • 62 ± 0. • 13) for SAI 45. The average space velocity components of the clusters SAI 44 and SAI 45 are calculated in units of km s −1

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Photometric, kinematic, and variability study in the young open cluster NGC 1960

Cited by 30 publications

References 94 publications

Photometric and kinematic study of the three intermediate age open clusters NGC 381, NGC 2360, and Berkeley 68

Photometric and kinematic study of the three intermediate age open clusters NGC 381, NGC 2360, and Berkeley 68

A comprehensive photometric and kinematical characteristic of the newly discovered QCs clusters with Gaia EDR3

Photometric and Kinematic study of the open clusters SAI 44 and SAI 45

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