Main physical properties of NGC 2298 stars. Left panel: Gaia optical CMD with membership probabilities color-coded as shown in the inset. RGB and AGB stars are denoted by open and filled symbols, respectively. A PARSEC isochrone of 12 Gyr and a metallicity of −1.75 is also overplotted with black solid lines. Middle panel: Gaia EDR3 vector point diagram (VPD). The three concentric dashed ellipses represent the 1-, 2-, and 3-σ level of the highest likelihood cluster members with > 90% membership probability. The two black dashed lines are shown for visual aids and show the nominal proper motions of the cluster taken from Vasiliev & Baumgardt (2021). Right panel: metallicity ([Fe/H]) versus radial velocity for 365 APOGEE-2S stars toward the NGC 2298 field. ASPCAP results are denoted by gray dots, while the BACCHUS results are denoted by navy blue star symbols for the 12 cluster members. The red box, which is arbitrarily limited between [Fe/H] = −2.1 and −1.6, centered on RV = 147.15 km s⁻¹ according to Baumgardt & Vasiliev (2021), and limited between ±10 km s⁻¹, encloses the highest likelihood cluster members with ASPCAP (gray dots) and BACCHUS (navy blue stars) determinations. The gray dotted and navy blue dash-dotted lines mark the average ⟨[Fe/H]⟩ of the 12 NGC 2298 stars analyzed in this work, and they are centered at ⟨[Fe/H]⟩ = −1.86 (ASPCAP results) and ⟨[Fe/H]⟩ = −1.76 (BACCHUS results), respectively. The 12 stars examined in this work are denoted by navy blue star symbols in all panels.