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With a hydrodynamical simulation using a simple galaxy formation modelwithout taking into account feedback, our previous work has shown that denseand massive filaments at high redshift can provide potential wells to trap andcompress gas, and hence affect galaxy formation in their resident low-masshaloes. In this paper, we make use of the Auriga simulations, a suite ofhigh-resolution zoom-in hydrodynamical simulations of Milky Way-like galaxies,to study whether the conclusion still holds in the simulations with asophisticated galaxy formation model. In agreement with the results of ourprevious work, we find that, comparing to their counterparts with similar halomasses in field, dwarf galaxies residing in filaments tend to have higherbaryonic and stellar fractions. At the fixed parent halo mass, the filamentdwarfs tend to have slightly higher star formation rates than those of fieldones. But overall we do not find a clear difference in galaxy g - r coloursbetween the filament and field populations. We also show that at highredshifts, the gas components in dwarf galaxies tend to have their spinsaligned with the filaments in which they reside. Our results support a picturein which massive filaments at high redshift assist gas accretion and enhancestar formation in their resident dwarf sized dark matter haloes.

The impact of filaments on dwarf galaxy properties in the Auriga simulations