{"work":{"id":"fabf5f21-456d-434b-abb8-0bb3dccfaab9","openalex_id":null,"doi":null,"arxiv_id":"2105.13549","raw_key":null,"title":"Dark Energy Survey Year 3 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing","authors":null,"authors_text":"DES Collaboration: T. M. C. Abbott, M. Aguena, A. Alarcon, S. Allam, O. Alves, A. Amon","year":2021,"venue":"astro-ph.CO","abstract":"We present the first cosmology results from large-scale structure in the Dark Energy Survey (DES) spanning 5000 deg$^2$. We perform an analysis combining three two-point correlation functions (3$\\times$2pt): (i) cosmic shear using 100 million source galaxies, (ii) galaxy clustering, and (iii) the cross-correlation of source galaxy shear with lens galaxy positions. The analysis was designed to mitigate confirmation or observer bias; we describe specific changes made to the lens galaxy sample following unblinding of the results. We model the data within the flat $\\Lambda$CDM and $w$CDM cosmological models. We find consistent cosmological results between the three two-point correlation functions; their combination yields clustering amplitude $S_8=0.776^{+0.017}_{-0.017}$ and matter density $\\Omega_{\\mathrm{m}} = 0.339^{+0.032}_{-0.031}$ in $\\Lambda$CDM, mean with 68% confidence limits; $S_8=0.775^{+0.026}_{-0.024}$, $\\Omega_{\\mathrm{m}} = 0.352^{+0.035}_{-0.041}$, and dark energy equation-of-state parameter $w=-0.98^{+0.32}_{-0.20}$ in $w$CDM. This combination of DES data is consistent with the prediction of the model favored by the Planck 2018 cosmic microwave background (CMB) primary anisotropy data, which is quantified with a probability-to-exceed $p=0.13$ to $0.48$. When combining DES 3$\\times$2pt data with available baryon acoustic oscillation, redshift-space distortion, and type Ia supernovae data, we find $p=0.34$. Combining all of these data sets with Planck CMB lensing yields joint parameter constraints of $S_8 = 0.812^{+0.008}_{-0.008}$, $\\Omega_{\\mathrm{m}} = 0.306^{+0.004}_{-0.005}$, $h=0.680^{+0.004}_{-0.003}$, and $\\sum m_{\\nu}<0.13 \\;\\mathrm{eV\\; (95\\% \\;CL)}$ in $\\Lambda$CDM; $S_8 = 0.812^{+0.008}_{-0.008}$, $\\Omega_{\\mathrm{m}} = 0.302^{+0.006}_{-0.006}$, $h=0.687^{+0.006}_{-0.007}$, and $w=-1.031^{+0.030}_{-0.027}$ in $w$CDM. (abridged)","external_url":"https://arxiv.org/abs/2105.13549","cited_by_count":null,"metadata_source":"pith","metadata_fetched_at":"2026-05-25T08:05:30.372224+00:00","pith_arxiv_id":"2105.13549","created_at":"2026-05-11T09:56:03.254130+00:00","updated_at":"2026-06-05T21:23:00.469572+00:00","title_quality_ok":true,"display_title":"Dark Energy Survey Year 3 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing","render_title":"Dark Energy Survey Year 3 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing"},"hub":{"state":{"work_id":"fabf5f21-456d-434b-abb8-0bb3dccfaab9","tier":"hub","tier_reason":"10+ Pith inbound or 1,000+ external citations","pith_inbound_count":31,"external_cited_by_count":null,"distinct_field_count":3,"first_pith_cited_at":"2022-04-11T17:58:33+00:00","last_pith_cited_at":"2026-05-21T15:14:45+00:00","author_build_status":"not_needed","summary_status":"needed","contexts_status":"needed","graph_status":"needed","ask_index_status":"not_needed","reader_status":"not_needed","recognition_status":"not_needed","updated_at":"2026-06-06T14:51:00.786048+00:00","tier_text":"hub"},"tier":"hub","role_counts":[{"context_role":"background","n":12},{"context_role":"dataset","n":3},{"context_role":"method","n":3}],"polarity_counts":[{"context_polarity":"background","n":12},{"context_polarity":"use_dataset","n":3},{"context_polarity":"use_method","n":3}],"runs":{},"summary":{},"graph":{},"authors":[]}}