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We present a novel method for identifying cosmic web filaments using theIllustrisTNG (TNG100) cosmological simulations and investigate the impact offilaments on galaxies. We compare the use of cosmic density field estimatesfrom the Delaunay Tessellation Field Estimator (DTFE) and the Monte CarloPhysarum Machine (MCPM), which is inspired by the slime mold organism, in theDisPerSE structure identification framework. The MCPM-based reconstructionidentifies filaments with higher fidelity, finding more low-prominence/diffusefilaments and better tracing the true underlying matter distribution than theDTFE-based reconstruction. Using our new filament catalogs, we find that mostgalaxies are located within 1.5-2.5 Mpc of a filamentary spine, with littlechange in the median specific star formation rate and the median galactic gasfraction with distance to the nearest filament. Instead, we introduce thefilament line density, {\Sigma}fil(MCPM), as the total MCPM overdensity perunit length of a local filament segment, and find that this parameter is asuperior predictor of galactic gas supply and quenching. Our results indicatethat most galaxies are quenched and gas-poor near high-line density filamentsat z<=1. At z=0, quenching in log(M*/Msun)>10.5 galaxies is mainly driven bymass, while lower-mass galaxies are significantly affected by the filament linedensity. In high-line density filaments, satellites are strongly quenched,whereas centrals have reduced star formation, but not gas fraction, at z<=0.5.We discuss the prospect of applying our new filament identification method togalaxy surveys with SDSS, DESI, Subaru PFS, etc. to elucidate the effect oflarge-scale structure on galaxy formation.

Filaments of The Slime Mold Cosmic Web And How They Affect Galaxy Evolution