Abstract
The role played by large-scale structures in galaxy evolution is not very well understood yet. In this study, we investigated properties of galaxies in the range 0.1 < z < 0.3 from a value-added version of the WISExSCOS catalogue around cosmic filaments detected with DisPerSE. We fitted a profile of galaxy over-density around cosmic filaments and found a typical radius of rm = 7.5 ± 0.2 Mpc. We measured an excess of passive galaxies near to the spine of the filament that was higher than the excess of transitioning and active galaxies. We also detected star formation rates (SFR) and stellar mass (M⋆) gradients pointing towards the spine of the filament. We investigated this result and found an M⋆ gradient for each type of galaxy, that is active, transitioning, and passive; we found a positive SFR gradient for passive galaxies. We also linked the galaxy properties and gas content in the cosmic web. To do so, we investigated the quiescent fraction fQ profile of galaxies around the cosmic filaments. Based on recent studies about the effect of the gas and the cosmic web on galaxy properties, we modelled fQ with a β model of gas pressure. The slope obtained in this work, β = 0.54 ± 0.18, is compatible with the scenario of projected isothermal gas in hydrostatic equilibrium (β = 2/3) and with the profiles of gas fitted in Sunyaev-Zel’dovich data from the Planck satellite.
Highlights
The matter distribution in the Universe is very non-linear and very complex, structured into a cosmic web composed of voids, walls, filaments, and nodes (e.g. Zel’Dovich 1970; Bond et al 1996; Libeskind et al 2018)
We investigated properties of galaxies in the range 0.1 < z < 0.3 from a value-added version of the WISExSCOS catalogue around cosmic filaments detected with DisPerSE
We present a statistical study of galaxy properties from the value-added catalogue based on the WISExSCOS catalogue, around cosmic filaments at low redshift extracted with DisPerSE in a spectroscopic sample of galaxies from the Sloan Digital Sky Survey (SDSS)
Summary
The matter distribution in the Universe is very non-linear and very complex, structured into a cosmic web composed of voids, walls, filaments, and nodes (e.g. Zel’Dovich 1970; Bond et al 1996; Libeskind et al 2018). Understanding the evolution and physical properties of the matter around the largest scale structures remains one of the main challenges in observational and theoretical cosmology Nowadays, numerical simulations such as Millenium (Springel 2005), Illustris-TNG (Springel et al 2018), HorizonAGN (Dubois et al 2014), or Magneticum (Hirschmann et al 2014) allow us to trace and characterise all the matter (i.e. dark matter, hot gas, cold gas, and galaxies) of the largescale Universe. While galaxy clusters are relatively easy to detect, study, and characterise, other cosmic web structures, such as cosmic filaments, are not defined because of their low densities. We present a statistical study of galaxy properties from the value-added catalogue based on the WISExSCOS catalogue, around cosmic filaments at low redshift (in the range 0.1 < z < 0.3) extracted with DisPerSE in a spectroscopic sample of galaxies from the SDSS. We present the combination of galaxy cluster catalogues used to remove the cluster galaxy members
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