Connecting the cosmic web to the spin of dark halos: implications for galaxy formation
We investigate the alignment of the spin of dark matter halos relative (i) to the surrounding large-scale filamentary structure, and (ii) to the tidal tensor eigenvectors using the Horizon 4pi dark matter simulation which resolves over 43 million dark matter halos at redshift zero. We detect a cle...
| Main Authors: | , , , , , , |
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| Format: | Journal article |
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Oxford University Press
2012
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| _version_ | 1826299105831288832 |
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| author | Codis, S Pichon, C Devriendt, J Slyz, A Pogosyan, D Dubois, Y Sousbie, T |
| author_facet | Codis, S Pichon, C Devriendt, J Slyz, A Pogosyan, D Dubois, Y Sousbie, T |
| author_sort | Codis, S |
| collection | OXFORD |
| description | We investigate the alignment of the spin of dark matter halos relative (i) to the surrounding large-scale filamentary structure, and (ii) to the tidal tensor eigenvectors using the Horizon 4pi dark matter simulation which resolves over 43 million dark matter halos at redshift zero. We detect a clear mass transition: the spin of dark matter halos above a critical mass tends to be perpendicular to the closest filament, and aligned with the intermediate axis of the tidal tensor, whereas the spin of low-mass halos is more likely to be aligned with the closest filament. Furthermore, this critical mass of 5 10^12 is redshift-dependent and scales as (1+z)^-2.5. We propose an interpretation of this signal in terms of large-scale cosmic flows. In this picture, most low-mass halos are formed through the winding of flows embedded in misaligned walls; hence they acquire a spin parallel to the axis of the resulting filaments forming at the intersection of these walls. On the other hand, more massive halos are typically the products of later mergers along such filaments, and thus they acquire a spin perpendicular to this direction when their orbital angular momentum is converted into spin. We show that this scenario is consistent with both the measured excess probabilities of alignment w.r.t. the eigen-directions of the tidal tensor, and halo merger histories. On a more qualitative level, it also seems compatible with 3D visualization of the structure of the cosmic web as traced by "smoothed" dark matter simulations or gas tracer particles. Finally, it provides extra support to the disc forming paradigm presented by Pichon et al (2011) as it extends it by characterizing the geometry of secondary infall at high redshift. |
| first_indexed | 2024-03-07T04:56:52Z |
| format | Journal article |
| id | oxford-uuid:d6e4ffec-b9b3-4f65-ba18-ba74fbac46ed |
| institution | University of Oxford |
| last_indexed | 2024-03-07T04:56:52Z |
| publishDate | 2012 |
| publisher | Oxford University Press |
| record_format | dspace |
| spelling | oxford-uuid:d6e4ffec-b9b3-4f65-ba18-ba74fbac46ed2022-03-27T08:37:06ZConnecting the cosmic web to the spin of dark halos: implications for galaxy formationJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:d6e4ffec-b9b3-4f65-ba18-ba74fbac46edSymplectic Elements at OxfordOxford University Press2012Codis, SPichon, CDevriendt, JSlyz, APogosyan, DDubois, YSousbie, TWe investigate the alignment of the spin of dark matter halos relative (i) to the surrounding large-scale filamentary structure, and (ii) to the tidal tensor eigenvectors using the Horizon 4pi dark matter simulation which resolves over 43 million dark matter halos at redshift zero. We detect a clear mass transition: the spin of dark matter halos above a critical mass tends to be perpendicular to the closest filament, and aligned with the intermediate axis of the tidal tensor, whereas the spin of low-mass halos is more likely to be aligned with the closest filament. Furthermore, this critical mass of 5 10^12 is redshift-dependent and scales as (1+z)^-2.5. We propose an interpretation of this signal in terms of large-scale cosmic flows. In this picture, most low-mass halos are formed through the winding of flows embedded in misaligned walls; hence they acquire a spin parallel to the axis of the resulting filaments forming at the intersection of these walls. On the other hand, more massive halos are typically the products of later mergers along such filaments, and thus they acquire a spin perpendicular to this direction when their orbital angular momentum is converted into spin. We show that this scenario is consistent with both the measured excess probabilities of alignment w.r.t. the eigen-directions of the tidal tensor, and halo merger histories. On a more qualitative level, it also seems compatible with 3D visualization of the structure of the cosmic web as traced by "smoothed" dark matter simulations or gas tracer particles. Finally, it provides extra support to the disc forming paradigm presented by Pichon et al (2011) as it extends it by characterizing the geometry of secondary infall at high redshift. |
| spellingShingle | Codis, S Pichon, C Devriendt, J Slyz, A Pogosyan, D Dubois, Y Sousbie, T Connecting the cosmic web to the spin of dark halos: implications for galaxy formation |
| title | Connecting the cosmic web to the spin of dark halos: implications for
galaxy formation |
| title_full | Connecting the cosmic web to the spin of dark halos: implications for
galaxy formation |
| title_fullStr | Connecting the cosmic web to the spin of dark halos: implications for
galaxy formation |
| title_full_unstemmed | Connecting the cosmic web to the spin of dark halos: implications for
galaxy formation |
| title_short | Connecting the cosmic web to the spin of dark halos: implications for
galaxy formation |
| title_sort | connecting the cosmic web to the spin of dark halos implications for galaxy formation |
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