Stellar properties as a function of ZAMS mass and metallicity. Left: The main-sequence lifetime (τ_⋆) as a function of ZAMS mass and metallicity. The color of the curves from light to dark indicates the metallicity from low (${10}^{-8}{\mathrm{Z}}_{\odot }$) to high (1 Z_⊙). Middle: Photon production rate (Q) of radiation bins from optical to He II ionizing band as a function of ZAMS mass and metallicity. Similarly, the color of the curves from light to dark indicates the metal abundance from low (${10}^{-8}{\mathrm{Z}}_{\odot }$) to high (1 Z_⊙). We shifted the curves of the Opt., FUV, LW, and EUV1 bands by multiplying constants of 10⁴, 10³, 10², and 10, respectively, to avoid overlapping different bins. Right: Similar to left but for the wind mass-loss rate (${\dot{m}}_{\mathrm{w}}$) and wind velocity (v_w). The color of the curves from light to dark indicates the metal abundance from low (${10}^{-6}{\mathrm{Z}}_{\odot }$) to high (1 Z_⊙). The main-sequence stellar winds from extremely metal-poor stars with $Z<{10}^{-6}{\mathrm{Z}}_{\odot }$ are negligible and not considered in our model.