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26 April 2024
 
  » arxiv » 1710.2676

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Galaxy evolution in the metric of the Cosmic Web
K. Kraljic ; S. Arnouts ; C. Pichon ; C. Laigle ; S. de la Torre ; D. Vibert ; C. Cadiou ; Y. Dubois ; M. Treyer ; C. Schimd ; S. Codis ; V. de Lapparent ; J. Devriendt ; H.S. Hwang ; D. Le Borgne ; N. Malavasi ; B. Milliard ; M. Musso ; D. Pogosyan ; M. Alpaslan ; J. Bland-Hawthorn ; A. H. Wright ;
Date 7 Oct 2017
AbstractThe role of the cosmic web in shaping galaxy properties is investigated in the GAMA spectroscopic survey in the redshift range $0.03 leq z leq 0.25$. The stellar mass, $u - r$ dust corrected colour and specific star formation rate (sSFR) of galaxies are analysed as a function of their distances to the 3D cosmic web features, such as nodes, filaments and walls, as reconstructed by DisPerSE. Significant mass and type/colour gradients are found for the whole population, with more massive and/or passive galaxies being located closer to the filament and wall than their less massive and/or star-forming counterparts. Mass segregation persists among the star-forming population alone. The red fraction of galaxies increases when closing in on nodes, and on filaments regardless of the distance to nodes. Similarly, the star-forming population reddens (or lowers its sSFR) at fixed mass when closing in on filament, implying that some quenching takes place. Comparable trends are also found in the state-of-the-art hydrodynamical simulation Horizon-AGN. These results suggest that on top of stellar mass and large-scale density, the traceless component of the tides from the anisotropic large-scale environment also shapes galactic properties. An extension of excursion theory accounting for filamentary tides provides a qualitative explanation in terms of anisotropic assembly bias: at a given mass, the accretion rate varies with the orientation and distance to filaments. It also explains the absence of type/colour gradients in the data on smaller, non-linear scales.
Source arXiv, 1710.2676
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