Abstract:
In this paper, we carried out photometric and kinematic study of two poorly studied open clusters NGC 7031 and NGC 7086 utilizing the optical wavelength of Gaia DR3. We identified 613 and 226 candidates for respective clusters as highly probable astrometric members. Fitting King's profile within RDPs, we estimate both core and limiting radii. For each cluster, we construct CMDs and fit them with suitable isochrones with metallicities (Z = 0.01189 ± 0.00023 & 0.01121 ± 0.00025) and different ages (8.468 ± 0.007 & 8.617 ± 0.021; log yr-1), therefore, the heliocentric distances are 701 ± 26 & 942 ± 31 pc for NGC 7031 and NGC 7086, respectively. Moreover, the collective mass (MC) in solar mass units may be deduced with MLR of 1072 ± 33 & 598 ± 25 and LF concluded that the average absolute (MG) magnitudes are 7.51 ± 0.36 & 6.54 ± 0.39 for respective clusters. The overall mass function reflects the slopes (α) for Salpeter's value (2.35) within the uncertainty, i.e., αNGC 7031 = 2.73 ± 0.25 & αNGC 7086 = 2.67 ± 0.32.
The present study and the dynamical analysis for different evolving times demonstrate that the clusters are dynamically relaxed, where the dynamical evolution parameter τ≫1. According to a kinematical analysis, we have obtained that the coherent convergent point (Ao, Do) is (-83.99 ° ± 0.11 °, -24.02 ° ± 0.20 °; NGC 7031) & (-80.69 ° ± 0.11 °, -17.51 ° ± 0.24 °; NGC 7086). Finally, we have computed their linear separation distance to be about 55.08 ± 7.42 pc, which reflects that the clusters are not binary and/or pair clusters.
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; Elsanhoury, W.H.
