Galaxy evolution in the metric of the Cosmic Web
The 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...
| Päätekijät: | , , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Aineistotyyppi: | Journal article |
| Julkaistu: |
Oxford University Press
2017
|
| _version_ | 1826286661963612160 |
|---|---|
| author | Kraljic, K Arnouts, S Pichon, C Laigle, C de la Torre, S Vibert, D Cadiou, C Dubois, Y Treyer, M Schimd, C Codis, S de Lapparent, V Devriendt, J Hwang, H Le Borgne, D Malavasi, N Milliard, B Musso, M Pogosyan, D Alpaslan, M Bland-Hawthorn, J Wright, A |
| author_facet | Kraljic, K Arnouts, S Pichon, C Laigle, C de la Torre, S Vibert, D Cadiou, C Dubois, Y Treyer, M Schimd, C Codis, S de Lapparent, V Devriendt, J Hwang, H Le Borgne, D Malavasi, N Milliard, B Musso, M Pogosyan, D Alpaslan, M Bland-Hawthorn, J Wright, A |
| author_sort | Kraljic, K |
| collection | OXFORD |
| description | The 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. |
| first_indexed | 2024-03-07T01:47:04Z |
| format | Journal article |
| id | oxford-uuid:98c56900-40f3-43bc-aa21-4955a1f7bea1 |
| institution | University of Oxford |
| last_indexed | 2024-03-07T01:47:04Z |
| publishDate | 2017 |
| publisher | Oxford University Press |
| record_format | dspace |
| spelling | oxford-uuid:98c56900-40f3-43bc-aa21-4955a1f7bea12022-03-27T00:09:28ZGalaxy evolution in the metric of the Cosmic WebJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:98c56900-40f3-43bc-aa21-4955a1f7bea1Symplectic Elements at OxfordOxford University Press2017Kraljic, KArnouts, SPichon, CLaigle, Cde la Torre, SVibert, DCadiou, CDubois, YTreyer, MSchimd, CCodis, Sde Lapparent, VDevriendt, JHwang, HLe Borgne, DMalavasi, NMilliard, BMusso, MPogosyan, DAlpaslan, MBland-Hawthorn, JWright, AThe 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. |
| spellingShingle | Kraljic, K Arnouts, S Pichon, C Laigle, C de la Torre, S Vibert, D Cadiou, C Dubois, Y Treyer, M Schimd, C Codis, S de Lapparent, V Devriendt, J Hwang, H Le Borgne, D Malavasi, N Milliard, B Musso, M Pogosyan, D Alpaslan, M Bland-Hawthorn, J Wright, A Galaxy evolution in the metric of the Cosmic Web |
| title | Galaxy evolution in the metric of the Cosmic Web |
| title_full | Galaxy evolution in the metric of the Cosmic Web |
| title_fullStr | Galaxy evolution in the metric of the Cosmic Web |
| title_full_unstemmed | Galaxy evolution in the metric of the Cosmic Web |
| title_short | Galaxy evolution in the metric of the Cosmic Web |
| title_sort | galaxy evolution in the metric of the cosmic web |
| work_keys_str_mv | AT kraljick galaxyevolutioninthemetricofthecosmicweb AT arnoutss galaxyevolutioninthemetricofthecosmicweb AT pichonc galaxyevolutioninthemetricofthecosmicweb AT laiglec galaxyevolutioninthemetricofthecosmicweb AT delatorres galaxyevolutioninthemetricofthecosmicweb AT vibertd galaxyevolutioninthemetricofthecosmicweb AT cadiouc galaxyevolutioninthemetricofthecosmicweb AT duboisy galaxyevolutioninthemetricofthecosmicweb AT treyerm galaxyevolutioninthemetricofthecosmicweb AT schimdc galaxyevolutioninthemetricofthecosmicweb AT codiss galaxyevolutioninthemetricofthecosmicweb AT delapparentv galaxyevolutioninthemetricofthecosmicweb AT devriendtj galaxyevolutioninthemetricofthecosmicweb AT hwangh galaxyevolutioninthemetricofthecosmicweb AT leborgned galaxyevolutioninthemetricofthecosmicweb AT malavasin galaxyevolutioninthemetricofthecosmicweb AT milliardb galaxyevolutioninthemetricofthecosmicweb AT mussom galaxyevolutioninthemetricofthecosmicweb AT pogosyand galaxyevolutioninthemetricofthecosmicweb AT alpaslanm galaxyevolutioninthemetricofthecosmicweb AT blandhawthornj galaxyevolutioninthemetricofthecosmicweb AT wrighta galaxyevolutioninthemetricofthecosmicweb |