We present photometric, astrometric, and kinematic studies of the old open star clusters NGC 1193 and NGC 1798. Both of the clusters are investigated by combining data sets from Gaia Early Data Release 3 (EDR3) and CCD UBV observational data. E(B − V) color excesses are derived for NGC 1193 as 0.150 ± 0.037 and for NGC 1798 as 0.505 ± 0.100 mag through the use of two-color diagrams. Photometric metallicities are also determined from twocolor diagrams with the results of [Fe/H]=‑0.30 ± 0.06 dex for NGC 1193 and [Fe/H]=−0.20 ± 0.07 dex for NGC 1798. The isochrone fitting distance and age of NGC 1193 are 5562 ± 381 pc and 4.6 ± 1 Gyr, respectively. For NGC 1798, these parameters are 4451 ± 728 pc and 1.3 ± 0.2 Gyr. Kinematic and dynamic orbital calculations indicate that NGC 1193 and NGC 1798 belong to the thick-disk and thin-disk populations, respectively.

We present a multimethod investigation of four metal-poor G-type main-sequence stars to resolve their Galactic origins. By combining high-resolution spectroscopy from PolarBase, photometric/astrometric data from Gaia DR3, and spectral energy distribution modeling, we derive precise stellar parameters, chemical abundances, kinematics, and Galactic orbital parameters. The stars HD 22879, HD 144579, HD 188510, and HD 201891 show effective temperatures of 5855 ± 110, 5300 ± 160, 5370 ± 60, and 5880 ± 90 K; surface gravities of 4.40 ± 0.18, 4.52 ± 0.37, 4.57 ± 0.13, and 4.48 ± 0.18 cgs; and metallicities of −0.86 ± 0.08, −0.55 ± 0.12, −1.60 ± 0.07, and −1.15 ± 0.07 dex, respectively. Kinematic analysis suggests that HD 22879, HD 144579, and HD 201891 are potential bulge-origin escapees, possibly ejected by the Galactic bar or spiral arm perturbations. HD 188510, however, shows halo-like dynamics, including a retrograde orbit. Chemical abundance trends ([α/Fe] versus [Fe/H]) reveal mixed origins, challenging kinematic classifications. This discrepancy highlights the importance of integrative methodologies in Galactic archaeology. We associate HD 22879, HD 144579, and HD 201891 with the bulge globular cluster NGC 6441, NGC 5927, and NGC 6544, respectively. HD 188510’s retrograde motion and low metallicity align with ejection from the halo globular cluster NGC 5139 (ω Cen). These results illustrate the complex interplay of dynamical processes—including bar resonances, spiral arm perturbations, and tidal stripping—in depositing metal-poor stars into the solar neighborhood.

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.

To understand the nature of the NGC 146–King 14 cluster pair, we conducted a detailed photometric, astrometric, and dynamical study using multiwavelength data from Gaia DR3, Pan-STARRS1, WISE, and TESS. Using a probabilistic approach, we identified 770 and 690 high-probability members of NGC 146 and King 14, respectively. Both clusters exhibit well-defined radial density profiles consistent with King models. We estimate the cluster ages as 20 ± 5 Myr and 50 ± 10 Myr from isochrone fitting, and distances of 2.98 ± 0.33 kpc and 2.51 ± 0.23 kpc from parallaxes after applying the Bailer-Jones criteria. The clusters show consistent mean proper motions. The mass function slopes (1.51 ± 0.18 and 1.50 ± 0.15) are close to the Salpeter value, and the extinction follows a normal Galactic reddening law ( R _V ≈ 3.1). Three-dimensional mapping gives a projected separation of ∼9 pc. Orbit integration using the galpy MWPotential2014 model shows that NGC 146 and King 14 move in nearly circular, disk-like orbits with similar mean orbital radii ( R _m ∼ 9 kpc) and orbital periods of roughly 255 Myr. A dynamical separation of ∼32 pc indicates that both clusters share a common spatial and kinematic association, consistent with a comoving pair. However, their relative velocity exceeds the escape velocity set by their combined mass, indicating they are not gravitationally bound. TESS light curves reveal seven variable stars, including γ Doradus, SPB stars, and eclipsing binaries, though only one is a likely member. Overall, the clusters likely formed within the same giant molecular cloud and now exist as an unbound comoving pair.