We present a comprehensive analysis (photometric and kinematical) of the poorly studied open cluster NGC 4337 using 2MASS, WISE, APASS, and Gaia DR2 databases. By determining the membership probabilities of stars, we identified the 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 and μ _y = 1.49 ± 0.006 mas yr⁻¹. We find the normal interstellar extinction toward the cluster region. The radial distribution of members provides a cluster radius of 7.′75 (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 within the mass range 0.75−2.0 , 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.°27 ± 0.°10, 13.°14 ± 0.°27) and (A _◦, D _◦) = (100.°282 ± 0.°10, 9.°577 ± 0.°323) respectively. We also computed the Velocity Ellipsoid Parameters, matrix elements (μ _ij ), direction cosines (l _j , m _j , n _j ), and the Galactic longitude of the vertex (l ₂).

In this study, we utilize photometric and kinematic data from Gaia DR3 and the 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 ( μ α cos δ , μ δ ) = ( − 1.407 ± 0.008 , − 0.863 ± 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 ± 0.30 Gyr, a distance of 6586 ± 164 pc, and a metallicity of [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 ± 19M _⊙. The computed apex motion is ( A o , D o ) = ( − 14 2 . ∘ 61 ± 0 . ∘ 08 , − 6 3 . ∘ 58 ± 0 . ∘ 13 ) . Similarly, King 5 consists of 403 probable members with a mean proper motion components ( μ α cos δ , μ δ ) = ( − 0.291 ± 0.005 , − 1.256 ± 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 ± 0.10 Gyr, with a distance of 2220 ± 40 pc and a metallicity of [Fe/H] = −0.15 dex (z = 0.0109). We identify 4 centrally concentrated BSSs, and the total mass is estimated as 484 ± 22M _⊙. The apex motion is calculated as ( A o , D o ) = ( − 11 5 . ∘ 10 ± 0 . ∘ 09 , − 7 3 . ∘ 16 ± 0 . ∘ 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 ± 25 pc and 177 ± 2 pc from the Galactic plane, respectively, confirming their classification as young stellar disc population.

The kinematical parameters, spatial shape and structure of the open cluster IC 2391 and the associated stellar stream are studied here using Gaia Data Release 2 (GDR2) astrometry data. The apex positions are determined for the open cluster IC 2391 (data taken from Cantat-Gaudin et al.) and for the kinematical stream’s stars mentioned in Montes et al. employing both convergent point and AD-diagram methods. The values of apex coordinates are: ( A , D ) _CP = ( 6 . h 17 ± 0 . h 004 , − 6 . ° 88 ± 0 . ° 381 ; for cluster) and ( 6 . h 07 ± 0 . h 007 , − 5 . ° 00 ± 0 . ° 447 ; stream), and ( A ₀ , D ₀ ) = ( 6 . h 12 ± 0 . h 004 , − 3 . ° 4 ± 0 . ° 3 ; cluster) and ( 6 . h 21 ± 0 . h 007 , − 11 . ° 895 ± 0 . ° 290 ; stream). The results are in good agreement with the previously calculated values. The positions of the stars in the disk and the spatial dispersion velocities are determined. The paths of cluster and associated stream are traced in the disk by orbit calculation back in time to their places of formation. A possible genetic relationship between the cluster and stream has been detected. The approximation of the spatial and kinematical shape of the stream and the cluster is made. According to this study, even though currently the cluster and stream seem to have a spatial difference in their locations, they appear to have formed in the same region of the Galactic disk.