The kinematical and space structures of IC 2391 open cluster and moving group with Gaia-DR2

Postnikova, E. S.; Elsanhoury, W. H.; Sariya, Devesh P.; Чупина, Н. В.; Верещагин, С. В.; Jiang, Ing-Guey

doi:10.1088/1674-4527/20/2/16

Cited by 19 publications

(10 citation statements)

References 44 publications

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“…The CP method: This method assumes that all the member stars of a cluster possess the same space velocities. The velocity components along the x, y, and z axes (V x , V y , V z ) for a cluster having coordinates (α,δ) with proper motions (µ α * ; µ δ ) and radial velocity V r at a distance of d i (in pc) in the heliocentric coordinate system are given by Smart (1968) as described in Postnikova et al (2020). We found the coordinates of the apex (A CP , D CP ) to be (77. ii).…”

Section: Apex Of the Clustersmentioning

confidence: 99%

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

Maurya¹,

C.²,

Elsanhoury³

et al. 2021

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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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Section: Apex Of the Clustersmentioning

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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“…The VEPs for the most probable cluster members are computed using a computational algorithm (see Elsanhoury 2015;Elsanhoury et al 2018;Postnikova et al 2020). We cross-matched cluster members with the catalog given by Soubiran et al (2018).…”

Section: Kinematical Structurementioning

confidence: 99%

“…We aim to derive apex coordinates (A, D) of the cluster on the celestial sphere (Vereshchagin et al 2014, Postnikova et al 2020 based on 2MASS and Gaia DR2 catalogs. The apex demonstrates the actual direction where the object moves.…”

Section: The Apex Of the Clustermentioning

confidence: 99%

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An investigation of poorly studied open cluster NGC 4337 using multi-color photometric and Gaia DR2 astrometric data

Bisht,

Elsanhoury,

Zhu

et al. 2020

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We present a comprehensive analysis (photometric and kinematical) of poorly studied open cluster NGC 4337 using 2MASS, WISE, APASS, and Gaia DR2 database. By determining the membership probabilities of stars, we identified 624 most probable members with membership probability higher than 50% by using proper motion and parallax data taken from Gaia DR2. The mean proper motion of the cluster is obtained as µ x = −8.83 ± 0.01 and µ y = 1.49 ± 0.006 mas yr −1 . We find the normal interstellar extinction towards the cluster region. The radial distribution of members provides a cluster radius of 7.75 arcmin (5.63 pc). The estimated age of 1600 ± 180 Myr indicates that NGC 4337 is an old open cluster with a bunch of red giant stars. The overall mass function slope for main-sequence stars is found as 1.46 ± 0.18 within the mass range 0.75−2.0 M ⊙ , which is in fair agreement with Salpeter's value (x=1.35) within uncertainty. The present study demonstrates that NGC 4337 is a dynamically relaxed open cluster. Using the Galactic potential model, Galactic orbits are obtained for NGC 4337. We found that this object follows a circular path around the Galactic center. Under the kinematical analysis, we compute the apex coordinates (A, D) by using two methods: (i) the classical convergent point method and (ii) the AD-diagram method. The obtained coordinates are: (A conv , D conv ) = (96 o .27 ± 0 o .10, 13 o .14 ± 0 o .27) & (A • , D • ) = (100 o .282 ± 0 o .10, 9 o .577 ± 0 o .323) respectively. We also computed the Velocity Ellipsoid Parameters (VEPs), matrix elements (µ ij ), direction cosines (l j , m j , n j ) and the Galactic longitude of the vertex (l 2 ).

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“…We used the distribution of individual apexes of cluster members in the equatorial coordinate system. Also, some kinematical parameters and velocity ellipsoid parameters (VEPs) are presented here with the computational algorithm presented in our previous papers (Elsanhoury et al 2015, Postnikova et al 2020, Bisht et al 2020.…”

Section: Introductionmentioning

confidence: 99%

Detailed analysis of the poorly studied northern open cluster NGC 1348 using multi-color photometry and GAIA EDR3 astrometry

Bisht,

Zhu,

Elsanhoury

et al. 2021

Preprint

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The membership determination for open clusters in noisy environments of the Milky Wayis still an open problem. In this paper, our main aim is provide the membership probability of stars using proper motions and parallax values of stars using Gaia EDR3 astrometry.Apart from the Gaia astrometry, we have also used other photometric data sets like UKIDSS, WISE, APASS and Pan-STARRS1 in order to understand cluster properties from optical to mid-infrared regions. We selected 438 likely members with membership probability higher 1 than 50% and G≤20 mag. We obtained the mean value of proper motion as µ x = 1.27 ± 0.001 and µ y = −0.73 ± 0.002 mas yr −1 . The cluster's radius is determined as 7.5 arcmin (5.67 pc) using radial density profile. Our analysis suggests that NGC 1348 is located at a distance of 2.6 ± 0.05 kpc. The mass function slope is found to be 1.30 ± 0.18 in the mass range 1.0−4.1 M ⊙ , which is in fair agreement with Salpeter's value within the 1σ uncertainty. The present study validates that NGC 1348 is a dynamically relaxed cluster. We computed the apex coordinates (A, D) for NGC 1348 as (A • , D • ) = (−23 o .815 ± 0 o .135, −22 o .228 ± 0 o .105). In addition, calculations of the velocity ellipsoid parameters (VEPs), matrix elements µ ij , direction cosines (l j , m j , n j ) and the Galactic longitude of the vertex have been also conducted in this analysis.

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The kinematical and space structures of IC 2391 open cluster and moving group with Gaia-DR2

Cited by 19 publications

References 44 publications

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

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

An investigation of poorly studied open cluster NGC 4337 using multi-color photometric and Gaia DR2 astrometric data

Detailed analysis of the poorly studied northern open cluster NGC 1348 using multi-color photometry and GAIA EDR3 astrometry

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