The dependence of assembly bias on the cosmic web

For low-mass haloes (i.e. M-halo less than or similar to 10(13) h(-1) M-circle dot), the physical origins of halo assembly bias have been linked to the slowdown of accretion due to tidal forces, which are more dominant in some cosmic-web environments as compared to others. Here, we use publicly available data from the application of the Discrete Persistent Structures Extractor (DisPerSE) to the IllustrisTNG magnetohydrodynamical simulation to investigate the dependence of the related galaxy assembly bias effect on the cosmic web. We show that, at fixed halo mass, the galaxy population displays significant secondary bias when split by distance to DisPerSE critical points representing nodes (d(node)), filaments (d(skel)), and saddles (d(sadd)), with objects closer to these features being more tightly clustered (particularly at M-halo less than or similar to 10(12.5 )h(-1) M-circle dot). The secondary bias produced by some of these parameters exceeds the assembly bias signal considerably at some mass ranges, especially for d(sadd). We also demonstrate that the assembly bias signal is reduced significantly when clustering is conditioned to galaxies being close or far from these critical points. The maximum attenuation is measured for galaxies close to saddle points, where less than 35 per cent of the signal remains. Objects near voids, conversely, preserve a fairly pristine signal (almost 85 per cent). Our analysis confirms the importance of the tidal field in shaping assembly bias, but it is also consistent with the signal being the result of different physical mechanisms. Our work introduces new aspects of secondary bias where predictions from simulations can be directly tested with observational data.