Study of Open Star Clusters Using the Gaia DR3: I- Poorly Studied King 2 and King 5

Abstract

In this study, we utilize photometric and kinematic data from \textit{Gaia} DR3 and the {\sc ASteCA} package to analyze the sparsely studied open clusters, King 2 and King 5. For King 2, we identify 340 probable members with membership probabilities exceeding 50\%. Its mean proper motion components are determined as $({\mu }_{\alpha }\cos \delta ,{\mu }_{\delta })=(-1.407\pm 0.008,-0.863\pm 0.012)$ mas yr${}^{-1}$, and its limiting radius is derived as $6.94_{-1.06}^{+0.22}$ arcminutes based on radial density profiles. The cluster has an estimated age of $4.80\pm 0.30$ Gyr, a distance of $6586\pm 164$ pc, and a metallicity of $\text{[Fe/H]}=-0.25$ dex ($z=0.0088$). We detect 17 blue straggler stars (BSSs) concentrated in its core, and its total mass is estimated to be $356\pm 19M_{\odot }$. The computed apex motion is $(A_o,D_o)=(-142^{\circ }.61\pm 0^{\circ }.08,-63^{\circ }.58\pm 0^{\circ }.13)$. Similarly, King 5 consists of 403 probable members with mean proper motion components $({\mu }_{\alpha }\cos \delta ,{\mu }_{\delta })=(-0.291\pm 0.005,-1.256\pm 0.005)$ mas yr${}^{-1}$ and a limiting radius of $11.33_{-2.16}^{+5.45}$ arcminutes. The cluster's age is determined as $1.45\pm 0.10$ Gyr, with a distance of $2220\pm 40$ pc and a metallicity of $\text{[Fe/H]}=-0.15$ dex ($z=0.0109$). We identify 4 centrally concentrated BSSs, and the total mass is estimated as $484\pm 22M_{\odot }$. The apex motion is calculated as $(A_o,D_o)=(-115^{\circ }.10\pm 0^{\circ }.09,-73^{\circ }.16\pm 0^{\circ }.12)$. The orbital analysis of King 2 and King 5 indicates nearly circular orbits, characterized by low eccentricities and minimal variation in their apogalactic and perigalactic distances. King 2 and King 5 reach maximum heights of $499\pm 25$ pc and $177\pm 2$ pc from the Galactic plane, respectively, confirming their classification as young stellar disc population.

27 pages, including 11 figures and 8 tables, accepted for publication in the Physica Scripta

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