Galaxy evolution in the metric of the Cosmic Web

Abstract : The role of the cosmic web in shaping galaxy properties is investigated in the Galaxy And Mass Assembly (GAMA) spectroscopic survey in the redshift range 0.03 ≤ z ≤ 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. These 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.
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Article dans une revue
Mon.Not.Roy.Astron.Soc., 2018, 474 (1), pp.547-571. 〈10.1093/mnras/stx2638〉
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Soumis le : mercredi 20 décembre 2017 - 23:59:35
Dernière modification le : mercredi 12 décembre 2018 - 07:09:00

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K. Kraljic, S. Arnouts, C. Pichon, C. Laigle, S. De La Torre, et al.. Galaxy evolution in the metric of the Cosmic Web. Mon.Not.Roy.Astron.Soc., 2018, 474 (1), pp.547-571. 〈10.1093/mnras/stx2638〉. 〈hal-01669677〉



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