Ellipticities of Galaxy Cluster Halos from Halo-Shear-Shear Correlations
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arXiv
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| Format: | Preprint |
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2024
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| _version_ | 1866910804090028032 |
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| author | Liu, Zhenjie Zhang, Jun Liu, Cong Li, Hekun |
| author_facet | Liu, Zhenjie Zhang, Jun Liu, Cong Li, Hekun |
| contents | We report the first detection of the halo ellipticities of galaxy clusters by applying the halo-shear-shear correlations (HSSC), without the necessity of major axis determination. We use the Fourier\_Quad shear catalog based on the Hyper Suprime-Cam Survey and the group catalog from the DESI Legacy Surveys for the measurement of group/cluster lensing and HSSC. Our analysis includes the off-centering effects. We obtain the average projected ellipticity of dark matter halos with mass $13.5 < {\rm log} (M_G h/ M_\odot) < 14.5$ within 1.3 virial radius to be $0.48^{+0.12}_{-0.19}$. We divide the sample into two groups based on mass and redshift, and we find that halos with higher mass tend to exhibit increased ellipticity. We also reveal that high-richness halos have larger ellipticities, confirming the physical picture from numerical simulation that high-richiness halos have a dynamical youth and more active mass accretion phase. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2408_07373 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Ellipticities of Galaxy Cluster Halos from Halo-Shear-Shear Correlations Liu, Zhenjie Zhang, Jun Liu, Cong Li, Hekun Cosmology and Nongalactic Astrophysics We report the first detection of the halo ellipticities of galaxy clusters by applying the halo-shear-shear correlations (HSSC), without the necessity of major axis determination. We use the Fourier\_Quad shear catalog based on the Hyper Suprime-Cam Survey and the group catalog from the DESI Legacy Surveys for the measurement of group/cluster lensing and HSSC. Our analysis includes the off-centering effects. We obtain the average projected ellipticity of dark matter halos with mass $13.5 < {\rm log} (M_G h/ M_\odot) < 14.5$ within 1.3 virial radius to be $0.48^{+0.12}_{-0.19}$. We divide the sample into two groups based on mass and redshift, and we find that halos with higher mass tend to exhibit increased ellipticity. We also reveal that high-richness halos have larger ellipticities, confirming the physical picture from numerical simulation that high-richiness halos have a dynamical youth and more active mass accretion phase. |
| title | Ellipticities of Galaxy Cluster Halos from Halo-Shear-Shear Correlations |
| topic | Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2408.07373 |