Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood

Abstract

Abstract 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.