Some Astrometric and Kinematic Characteristics of the M67 Open Cluster

Elsanhoury, W. H.

doi:10.1007/s10511-015-9405-6

Cited by 4 publications

(5 citation statements)

References 23 publications

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“…l2 with our series of articles (e.g. Elsanhoury et al, 2015Elsanhoury et al, , 2016. Thus, we conclude that is that the longitude of the vertex l2 differs slightly from zero.…”

Section: Discussionsupporting

confidence: 55%

“…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 estimated the cluster's position (X, Y, Z, in pc, Mihalas & Binney 1981) and its velocity components (V x , V y , V z km/s) along x, y, and z-axes in the coordinate system centered at the Sun using the formulae given by Smart (1968). Elsanhoury et al (2016) also has been explained the equations to estimate velocity components.…”

Section: Kinematical Structurementioning

confidence: 99%

“…To compute VEPs for NGC 4337, we follow a computational algorithm (Elsanhoury et al 2013(Elsanhoury et al , 2018Elsanhoury 2015;Postnikova et al 2020). Depending on the matrix that controls the eigenvalue problem for the velocity ellipsoid, we established an analytical expressions of some parameters in terms of the matrix elements mu ij .…”

Section: Parametersmentioning

confidence: 99%

“…Therefore, the solar elements with spatial velocities considered (w.s.v.c.) have been estimated using the equations given by Elsanhoury et al (2016).…”

Section: Parametersmentioning

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

Preprint

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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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“…l2 with our series of articles (e.g. Elsanhoury et al, 2015Elsanhoury et al, , 2016. Thus, we conclude that is that the longitude of the vertex l2 differs slightly from zero.…”

Section: Discussionsupporting

confidence: 55%

Section: Kinematical Structurementioning

confidence: 99%

Section: Kinematical Structurementioning

confidence: 99%

Section: Parametersmentioning

confidence: 99%

“…Therefore, the solar elements with spatial velocities considered (w.s.v.c.) have been estimated using the equations given by Elsanhoury et al (2016).…”

Section: Parametersmentioning

confidence: 99%

See 3 more Smart Citations

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

Bisht,

Elsanhoury,

Zhu

et al. 2020

Preprint

Self Cite

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Photometric and kinematical analysis of Koposov 12 and Koposov 43 open clusters

Elsanhoury

2021

J Astrophys Astron

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We present a photometric and kinematical analysis of two and poorly studied open clusters; Koposov 12 (FSR 802) and Koposov 43 (FSR 848) by using cross-matched data from PPMXL and Gaia DR2 catalog. We use astrometric parameters to identify 285 and 310 cluster members for Koposov 12 and Koposov 43, respectively. Using the extracted member candidates and isochrone fitting to near-infrared (J, H, K s ) and Gaia DR2 bands (G, G BP , G RP ), and Color Magnitude Diagrams (CMDs), we have estimated ages: log (age/yr) = 9.00  0.20 and 9.50  0.20, and distances d = 1850  43 pc and 2500  50 pc for Koposov 12 and Koposov 43, respectively, assuming Solar metallicity (Z=0.019). The estimated masses of the cluster derived using initial mass function and synthetic CMD are 364  19 M ⨀ and 352  19 M ⨀ . We have also computed their velocity ellipsoid parameters based on (3 × 3) matrix elements (μ ij ).

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2MASS photometry and kinematical studies of open cluster NGC 188

Elsanhoury

Haroon²,

Чупина

et al. 2016

New Astronomy

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In this paper, we present our results for the photometric and kinematical studies of old open cluster NGC 188. We determined various astrophysical parameters like limited radius, core and tidal radii, distance, luminosity and mass functions, total mass, relaxation time etc. for the cluster using 2MASS catalog. We obtained the cluster's distance from the Sun as 1721±41 pc and log (age)= 9.85±0.05 at Solar metallicity. The relaxation time of the cluster is smaller than the estimated cluster age which suggests that the cluster is dynamically relaxed. Our results agree with the values mentioned in the literature. We also determined the clusters apex coordinates as (281• .88, −44• .76) using AD-diagram method. Other kinematical parameters like space velocity components, cluster center and elements of Solar motion etc. have also been computed.

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Some Astrometric and Kinematic Characteristics of the M67 Open Cluster

Cited by 4 publications

References 23 publications

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

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

Photometric and kinematical analysis of Koposov 12 and Koposov 43 open clusters

2MASS photometry and kinematical studies of open cluster NGC 188

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