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Void galaxies are essential for understanding the physical processes thatdrive galaxy evolution because they are less affected by external factors thangalaxies in denser environments, that is, in filaments, walls, and clusters.The stellar metallicity of a galaxy traces the accumulated fossil record of thestar formation through the entire life of the galaxy. A comparison of thestellar metallicity of galaxies in various environments, including voids,filaments, walls, and clusters can provide valuable insights into how thelarge-scale environment affects the chemical evolution of the galaxy. Wepresent the first comparison of the relation of the total stellar mass versuscentral stellar metallicity between galaxies in voids, filaments, walls, andclusters with different star formation history (SFH) types, morphologies, andcolours for stellar masses between $10^{8.0}$ to $10^{11.5}$ solar masses andredshift $0.01<z<0.05$. We applied non-parametric full spectral fittingtechniques (pPXF and STECKMAP) to 10807 spectra from the SDSS-DR7 (987 invoids, 6463 in filaments and walls, and 3357 in clusters) and derived theircentral mass-weighted average stellar metallicity ($\rm [M/H]_M$). We find thatgalaxies in voids have slightly lower stellar metallicities on average thangalaxies in filaments and walls (by~$\sim~0.1$~dex), and they are much lowerthan those of galaxies in clusters (by~$\sim~0.4$~dex). These differences aremore significant for low-mass ($ \sim~10^{9.25}~{\rm M_\odot}$) than forhigh-mass galaxies, for long-timescale SFH (extended along time) galaxies thanfor short-timescale SFHs (concentrated at early times) galaxies, for spiralthan for elliptical galaxies, and for blue than for red galaxies.

Stellar mass-metallicity relation throughout the large-scale structure of the Universe: CAVITY mother sample