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| Hauptverfasser: | , , , |
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| Format: | Preprint |
| Veröffentlicht: |
2025
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| Online-Zugang: | https://arxiv.org/abs/2506.21827 |
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| _version_ | 1866909734238420992 |
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| author | Kim, Yigon Montero-Dorta, Antonio D. Smith, Rory Shinn, Jong-Ho |
| author_facet | Kim, Yigon Montero-Dorta, Antonio D. Smith, Rory Shinn, Jong-Ho |
| contents | Context. The clustering of dark-matter halos depends primarily on halo mass. However, at fixed halo mass, numerical simulations have revealed multiple secondary dependencies. This so-called secondary halo bias has important implications for our understanding of structure formation and observational cosmology. Despite its significance, the effect has not yet been measured observationally with statistical confidence. Aims. We aim to develop the first observational method to probe halo spin bias: the secondary dependence of halo clustering on halo spin at fixed halo mass. Methods. We use a proxy for halo spin based on the coherent motion of galaxies within and around a halo. This technique is tested using the IllustrisTNG hydrodynamical simulation and subsequently applied to a group catalog from the Sloan Digital Sky Survey (SDSS). By splitting the SDSS groups according to this spin proxy and measuring the two-point correlation function of the resulting samples, the existence of halo spin bias is investigated. Results. We find consistent indications that, at fixed mass, groups with higher values of the spin proxy exhibit higher bias than those with lower spin proxy values, on scales of 5-15 ${h}^{-1}$$\mathrm{Mpc}$. The highest significance is seen for groups with halo masses ${M}_{\rm h} \gtrsim {10}^{13.2}$ ${h}^{-1}{\rm M}_\odot$, for which 85$\%$ of the sampled measurements display the expected trend. As we continue to improve the method, our results could open new avenues for studying the connection between halo spin and the large-scale structure with upcoming spectroscopic surveys. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2506_21827 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Towards an Observational Detection of Halo Spin Bias using Spin-Orbit Coherence Kim, Yigon Montero-Dorta, Antonio D. Smith, Rory Shinn, Jong-Ho Astrophysics of Galaxies Cosmology and Nongalactic Astrophysics Context. The clustering of dark-matter halos depends primarily on halo mass. However, at fixed halo mass, numerical simulations have revealed multiple secondary dependencies. This so-called secondary halo bias has important implications for our understanding of structure formation and observational cosmology. Despite its significance, the effect has not yet been measured observationally with statistical confidence. Aims. We aim to develop the first observational method to probe halo spin bias: the secondary dependence of halo clustering on halo spin at fixed halo mass. Methods. We use a proxy for halo spin based on the coherent motion of galaxies within and around a halo. This technique is tested using the IllustrisTNG hydrodynamical simulation and subsequently applied to a group catalog from the Sloan Digital Sky Survey (SDSS). By splitting the SDSS groups according to this spin proxy and measuring the two-point correlation function of the resulting samples, the existence of halo spin bias is investigated. Results. We find consistent indications that, at fixed mass, groups with higher values of the spin proxy exhibit higher bias than those with lower spin proxy values, on scales of 5-15 ${h}^{-1}$$\mathrm{Mpc}$. The highest significance is seen for groups with halo masses ${M}_{\rm h} \gtrsim {10}^{13.2}$ ${h}^{-1}{\rm M}_\odot$, for which 85$\%$ of the sampled measurements display the expected trend. As we continue to improve the method, our results could open new avenues for studying the connection between halo spin and the large-scale structure with upcoming spectroscopic surveys. |
| title | Towards an Observational Detection of Halo Spin Bias using Spin-Orbit Coherence |
| topic | Astrophysics of Galaxies Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2506.21827 |