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Gaia photometric and kinematics studies of fouropen star clusters: King 13, Juchert-Saloranta 1,Teutsch 1, and Teutsch 5
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Abstract
This paper presents the results of the studying photometric, and kinematics offour open star clusters; namely King 13, Juchert-Saloranta 1, Teutsch 1, andTeutsch 5 utilizing the most recent data of Gaia EDR3. The most probable ofthe star members was computed using the ASteCA code and the numbers ofmembers of the clusters (N); (521) King 13, (429) Juchert-Saloranta 1, (414)Teutsch 1, and (191) Teutsch 5. The parameter structure of each object suchas cluster radii range from 3.00 to 7.00 arcmin. We obtained the distance fromSun 3.000±0.100 kpc, 4.891±0.554 kpc, 3.885±0.225 kpc, and 2.979±0.167 kpc,respectively. The values of age 0.818±0.043 Gyr, 0.9754±0.123 Gyr, 0.539±0.038Gyr, and 0.899±0.159 Gyr, respectively. The kinematical parameters have beencomputed; The position of the cluster convergent is computed by the AD diagrammethod, cluster velocity, center of the cluster, elements of solar motion, and spacevelocity components.
Title: Gaia photometric and kinematics studies of fouropen star clusters: King 13, Juchert-Saloranta 1,Teutsch 1, and Teutsch 5
Description:
Abstract
This paper presents the results of the studying photometric, and kinematics offour open star clusters; namely King 13, Juchert-Saloranta 1, Teutsch 1, andTeutsch 5 utilizing the most recent data of Gaia EDR3.
The most probable ofthe star members was computed using the ASteCA code and the numbers ofmembers of the clusters (N); (521) King 13, (429) Juchert-Saloranta 1, (414)Teutsch 1, and (191) Teutsch 5.
The parameter structure of each object suchas cluster radii range from 3.
00 to 7.
00 arcmin.
We obtained the distance fromSun 3.
000±0.
100 kpc, 4.
891±0.
554 kpc, 3.
885±0.
225 kpc, and 2.
979±0.
167 kpc,respectively.
The values of age 0.
818±0.
043 Gyr, 0.
9754±0.
123 Gyr, 0.
539±0.
038Gyr, and 0.
899±0.
159 Gyr, respectively.
The kinematical parameters have beencomputed; The position of the cluster convergent is computed by the AD diagrammethod, cluster velocity, center of the cluster, elements of solar motion, and spacevelocity components.
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