Two MASS photometry of open star clusters: King 13 and Berkeley 53

Haroon, A. A.; Ismail, Hisham; Alnagahy, F. Y.

doi:10.1007/s10509-014-1990-z

Cited by 10 publications

(10 citation statements)

References 18 publications

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“…We apply the star counting technique based upon the clustering degree of neighbors around each star in the cluster region. Chen et al (2004) introduced this technique (see our applying procedure in Haroon et al 2014). …”

Section: Color-magnitude Diagramsmentioning

confidence: 99%

Photometry of three open star clusters: Juchert-Saloranta 1, Teutsch 1 and Teutsch 5

Ismail

Haroon

Alsslegy

2015

Astrophys Space Sci

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We present a photometric study for three rarely studied open star clusters; Juchert-Saloranta 1, Teutsch 1 and Teutsch 5 using the 2MASS-JHKs photometric data. Their structural and photometric parameters are determined. We obtained the distance from the Sun of 3.30 ± 0.30 kpc, 3.82 ± 0.25 kpc and 2.91 ± 0.34 kpc and their log(age) of 9.15, 8.75 and 8.9 at solar metallicity and the total mass of 215, 807 and 165 M for Juchert-Saloranta 1, Teutsch 1 and Teutsch 5 respectively. The three clusters lie in the galactic plane and about 11 kpc from the galactic center. The relaxation times of the clusters are smaller than the estimated cluster ages (∼ 0.01) that may be reflect the dynamical relaxation of these clusters.

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Section: Color-magnitude Diagramsmentioning

confidence: 99%

Photometry of three open star clusters: Juchert-Saloranta 1, Teutsch 1 and Teutsch 5

Ismail

Haroon

Alsslegy

2015

Astrophys Space Sci

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“…The resulting mass function is plotted in Fig 12. The mass function slope has been derived by using the relation log dN dM = −(1 + x) log(M)+constant, where dN is the number of stars in a mass bin dM with central mass M and x is the slope of MF. The derived MF slope (x = 1.46 ± 0.31) is more precise than Haroon et al (2014) because the current analysis is based on deep CCD V I data along with GAIA DR2 astrometry. Our derived value of MF slope for this cluster in the mass range 1.1-2.6M ⊙ is in good agreement with the value 1.35 given by Salpeter (1955) for field stars in the Solar neighbourhood.…”

Section: Mass Functionmentioning

confidence: 97%

Study of open cluster King 13 using CCD VI, 2MASS and Gaia DR2 Astrometry.

et al. 2020

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In this paper, we present astrophysical parameters of the open cluster King 13 based on the V I CCD and 2MASS JHK s photometric data. This is a poorly studied cluster, for which new results have been found in the present work. To identify probable members, we use proper motion data from Gaia DR2 catalogue. The mean proper motion of the cluster is determined as −2.8±0.2 and −0.88±0.14 mas yr −1 and cluster extent is derived as 3 ′ .2. Using color-magnitude diagrams, we estimate the age and distance of the cluster as 510 ± 60 Myr and 3.84 ± 0.15 kpc respectively. Interstellar reddening E(B − V) in the direction of the cluster is determined as 0.80 ± 0.2 mag using color-color diagram. Mass function slope of the cluster is found to be comparable with the Salpeter value. The total mass of this cluster is derived as 270 M ⊙ . The present analysis shows that King 13 is a dynamically relaxed cluster.

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“…We follow the procedure presented by many authors, e.g. Maciejewski and Niedzielski (2007), Maciejewski et al (2009), and Haroon et al (2014, into which two perpendicular strips were cut along the right ascension and declination at approximate center of the cluster, and then the Histograms of the star counts was built along each strip with bin size of 1 arcmin for the clusters with a diameter larger than 10 arcmin (Maciejewski and Niedzielski 2007), which fitted by Gaussian distribution function f(x) with mean  and standard deviation , i.e.…”

Section: Cluster Center Determinationmentioning

confidence: 99%

PPMXL and Gaia morphological analysis of Melotte 22 (Pleiades) and Melotte 25 (Hyades)

Elsanhoury¹,

Nouh²

2019

New Astronomy

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In this article, we present a morphological study of the well-known extended sized open clusters in the sky, Melotte 22 (Pleiades) and Melotte 25 (Hyades) with J, H, and Ks regions due to Gaia DR2 and PPMXL catalogues. Based on proper motions of these clusters, we extract our candidates and hence constructing fitting isochrones with Solar metallicity Z = 0.019, log (age) = 8.2 ± 0.05 for Melotte 22, and metallicity Z = 0.024, log (age) = 8.9 ± 0.10 for Melotte 25. Some photometric parameters are estimated, e.g. cluster heliocentric distances are 135 ± 3.6 and 47.51 ± 2.15 pc respectively, luminosity and mass functions with mass-luminosity relation MLR of the second order polynomial, and we have estimated the masses of Melotte 22 and Melotte 25 as 662.476 ± 25.73 M and 513.819 ± 22.65 M.The relaxation times of these clusters are smaller than the estimated cluster ages, which indicate that these clusters are dynamically relaxed.The second part is devoted to some kinematics of these clusters due to internal and/or motion of members, the apex position is 95 o .60 ± 0 o .10, -48 o .21 ± 0 o .14 for Melotte 22, and 96 o .72 ± 1 o .15, 5 o .66 ± 0 o .12 for Melotte 25. Also we have determined the components of space velocity and the cluster centers in pc as well as elements of the Solar motion. The results are in good agreement with those in the literature.

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Two MASS photometry of open star clusters: King 13 and Berkeley 53

Cited by 10 publications

References 18 publications

Photometry of three open star clusters: Juchert-Saloranta 1, Teutsch 1 and Teutsch 5

Photometry of three open star clusters: Juchert-Saloranta 1, Teutsch 1 and Teutsch 5

Study of open cluster King 13 using CCD VI, 2MASS and Gaia DR2 Astrometry.

PPMXL and Gaia morphological analysis of Melotte 22 (Pleiades) and Melotte 25 (Hyades)

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