KLEINER, DANEDANEKLEINERPimbblet, Kevin A.Kevin A.PimbbletJones, D. HeathD. HeathJonesKoribalski, Bärbel S.Bärbel S.KoribalskiSERRA, PAOLOPAOLOSERRA2021-04-192021-04-1920170035-8711http://hdl.handle.net/20.500.12386/30801We examine the H I-to-stellar mass ratio (H I fraction) for galaxies near filament backbones within the nearby Universe (d < 181 Mpc). This work uses the 6-degree Field Galaxy Survey and the Discrete Persistent Structures Extractor to define the filamentary structure of the local cosmic web. H I spectral stacking of H I Parkes all sky survey observations yields the H I fraction for filament galaxies and a field control sample. The H I fraction is measured for different stellar masses and fifth nearest neighbour projected densities (Σ<SUB>5</SUB>) to disentangle what influences cold gas in galaxies. For galaxies with stellar masses log(M<SUB>⋆</SUB>) ≤ 11 M<SUB>☉</SUB> in projected densities 0 ≤ Σ<SUB>5</SUB> < 3 galaxies Mpc<SUP>-2</SUP>, all H I fractions of galaxies near filaments are statistically indistinguishable from the control sample. Galaxies with stellar masses log(M<SUB>⋆</SUB>) ≥ 11 M<SUB>☉</SUB> have a systematically higher H I fraction near filaments than the control sample. The greatest difference is 0.75 dex, which is 5.5σ difference at mean projected densities of 1.45 galaxies Mpc<SUP>-2</SUP>. We suggest that this is evidence for massive galaxies accreting cold gas from the intrafilament medium that can replenish some H I gas. This supports cold mode accretion where filament galaxies with a large gravitational potential can draw gas from the large-scale structure.STAMPAenArticle10.1093/mnras/stw33282-s2.0-85032830676https://academic.oup.com/mnras/article/466/4/4692/27338592017MNRAS.466.4692KFIS/05 - ASTRONOMIA E ASTROFISICA