The impact of the connectivity of the cosmic web on the physical properties of galaxies at its nodes
We investigate the impact of the number of filaments connected to the nodes of the cosmic web on the physical properties of their galaxies using the Sloan Digital Sky Survey. We compare these measurements to the cosmological hydrodynamical simulations Horizon-(no)AGN and Simba. We find that more mas...
| Autori principali: | , , , , , , , , , , , , , |
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| Natura: | Journal article |
| Lingua: | English |
| Pubblicazione: |
Oxford University Press
2019
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| _version_ | 1826283367856865280 |
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| author | Kraljic, K Pichon, C Codis, S Laigle, C Davé, R Dubois, Y Hwang, HS Pogosyan, D Arnouts, S Devriendt, J Musso, M Peirani, S Slyz, A Treyer, M |
| author_facet | Kraljic, K Pichon, C Codis, S Laigle, C Davé, R Dubois, Y Hwang, HS Pogosyan, D Arnouts, S Devriendt, J Musso, M Peirani, S Slyz, A Treyer, M |
| author_sort | Kraljic, K |
| collection | OXFORD |
| description | We investigate the impact of the number of filaments connected to the nodes
of the cosmic web on the physical properties of their galaxies using the Sloan
Digital Sky Survey. We compare these measurements to the cosmological
hydrodynamical simulations Horizon-(no)AGN and Simba. We find that more massive
galaxies are more connected, in qualitative agreement with theoretical
predictions and measurements in dark matter only simulation. The star formation
activity and morphology of observed galaxies both display some dependence on
the connectivity of the cosmic web at fixed stellar mass: less star forming and
less rotation supported galaxies also tend to have higher connectivity. These
results qualitatively hold both for observed and virtual galaxies, and can be
understood given that the cosmic web is the main source of fuel for galaxy
growth. The simulations show the same trends at fixed halo mass, suggesting
that the geometry of filamentary infall impacts galaxy properties beyond the
depth of the local potential well. Based on simulations, it is also found that
AGN feedback is key in reversing the relationship between stellar mass and
connectivity at fixed halo mass. Technically, connectivity is a practical
observational proxy for past and present accretion (minor mergers or diffuse
infall). |
| first_indexed | 2024-03-07T00:57:51Z |
| format | Journal article |
| id | oxford-uuid:88b2c4d9-1c38-45e5-baf3-9ba65472e667 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-07T00:57:51Z |
| publishDate | 2019 |
| publisher | Oxford University Press |
| record_format | dspace |
| spelling | oxford-uuid:88b2c4d9-1c38-45e5-baf3-9ba65472e6672022-03-26T22:19:16ZThe impact of the connectivity of the cosmic web on the physical properties of galaxies at its nodesJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:88b2c4d9-1c38-45e5-baf3-9ba65472e667EnglishSymplectic ElementsOxford University Press2019Kraljic, KPichon, CCodis, SLaigle, CDavé, RDubois, YHwang, HSPogosyan, DArnouts, SDevriendt, JMusso, MPeirani, SSlyz, ATreyer, MWe investigate the impact of the number of filaments connected to the nodes of the cosmic web on the physical properties of their galaxies using the Sloan Digital Sky Survey. We compare these measurements to the cosmological hydrodynamical simulations Horizon-(no)AGN and Simba. We find that more massive galaxies are more connected, in qualitative agreement with theoretical predictions and measurements in dark matter only simulation. The star formation activity and morphology of observed galaxies both display some dependence on the connectivity of the cosmic web at fixed stellar mass: less star forming and less rotation supported galaxies also tend to have higher connectivity. These results qualitatively hold both for observed and virtual galaxies, and can be understood given that the cosmic web is the main source of fuel for galaxy growth. The simulations show the same trends at fixed halo mass, suggesting that the geometry of filamentary infall impacts galaxy properties beyond the depth of the local potential well. Based on simulations, it is also found that AGN feedback is key in reversing the relationship between stellar mass and connectivity at fixed halo mass. Technically, connectivity is a practical observational proxy for past and present accretion (minor mergers or diffuse infall). |
| spellingShingle | Kraljic, K Pichon, C Codis, S Laigle, C Davé, R Dubois, Y Hwang, HS Pogosyan, D Arnouts, S Devriendt, J Musso, M Peirani, S Slyz, A Treyer, M The impact of the connectivity of the cosmic web on the physical properties of galaxies at its nodes |
| title | The impact of the connectivity of the cosmic web on the physical properties of galaxies at its nodes |
| title_full | The impact of the connectivity of the cosmic web on the physical properties of galaxies at its nodes |
| title_fullStr | The impact of the connectivity of the cosmic web on the physical properties of galaxies at its nodes |
| title_full_unstemmed | The impact of the connectivity of the cosmic web on the physical properties of galaxies at its nodes |
| title_short | The impact of the connectivity of the cosmic web on the physical properties of galaxies at its nodes |
| title_sort | impact of the connectivity of the cosmic web on the physical properties of galaxies at its nodes |
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