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We study the physical properties of a spectroscopic sample of 28 star-forminggalaxies in a large filamentary structure in the COSMOS field at $z\sim$0.53,with spectroscopic data taken with the Keck/DEIMOS spectrograph, and comparethem with a control sample of 30 field galaxies. We spectroscopically confirmthe presence of a large galaxy filament ($\sim$ 8 Mpc), along which fiveconfirmed X-ray groups exist. We show that within the uncertainties, theionization parameter, equivalent width (EW), EW versus specific star-formationrate (sSFR) relation, EW versus stellar mass relation, line-of-sight velocitydispersion, dynamical mass, and stellar-to-dynamical mass ratio are similar forfilament and field star-forming galaxies. However, we show that on average,filament star-forming galaxies are more metal-enriched ($\sim$ 0.1$-$0.15 dex),possibly due to the inflow of the already enriched intrafilamentary gas intofilament galaxies. Moreover, we show that electron densities are significantlylower (a factor of $\sim$17) in filament star-forming systems compared to thosein the field, possibly because of a longer star-formation timescale forfilament star-forming galaxies. Our results highlight the potentialpre-processing role of galaxy filaments and intermediate-density environmentson the evolution of galaxies, which has been highly underestimated.

Spectroscopic Study of Star-forming Galaxies in Filaments and the Field at $z\sim$0.5: Evidence for Environmental Dependence of Electron Density