학술논문
Dark Energy Survey Year 3 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing
Document Type
Working Paper
Author
DES Collaboration; Abbott, T. M. C.; Aguena, M.; Alarcon, A.; Allam, S.; Alves, O.; Amon, A.; Andrade-Oliveira, F.; Annis, J.; Avila, S.; Bacon, D.; Baxter, E.; Bechtol, K.; Becker, M. R.; Bernstein, G. M.; Bhargava, S.; Birrer, S.; Blazek, J.; Brandao-Souza, A.; Bridle, S. L.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Camacho, H.; Campos, A.; Rosell, A. Carnero; Kind, M. Carrasco; Carretero, J.; Castander, F. J.; Cawthon, R.; Chang, C.; Chen, A.; Chen, R.; Choi, A.; Conselice, C.; Cordero, J.; Costanzi, M.; Crocce, M.; da Costa, L. N.; Pereira, M. E. da Silva; Davis, C.; Davis, T. M.; De Vicente, J.; DeRose, J.; Desai, S.; Di Valentino, E.; Diehl, H. T.; Dietrich, J. P.; Dodelson, S.; Doel, P.; Doux, C.; Drlica-Wagner, A.; Eckert, K.; Eifler, T. F.; Elsner, F.; Elvin-Poole, J.; Everett, S.; Evrard, A. E.; Fang, X.; Farahi, A.; Fernandez, E.; Ferrero, I.; Ferté, A.; Fosalba, P.; Friedrich, O.; Frieman, J.; García-Bellido, J.; Gatti, M.; Gaztanaga, E.; Gerdes, D. W.; Giannantonio, T.; Giannini, G.; Gruen, D.; Gruendl, R. A.; Gschwend, J.; Gutierrez, G.; Harrison, I.; Hartley, W. G.; Herner, K.; Hinton, S. R.; Hollowood, D. L.; Honscheid, K.; Hoyle, B.; Huff, E. M.; Huterer, D.; Jain, B.; James, D. J.; Jarvis, M.; Jeffrey, N.; Jeltema, T.; Kovacs, A.; Krause, E.; Kron, R.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Leget, P. -F.; Lemos, P.; Liddle, A. R.; Lidman, C.; Lima, M.; Lin, H.; MacCrann, N.; Maia, M. A. G.; Marshall, J. L.; Martini, P.; McCullough, J.; Melchior, P.; Mena-Fernández, J.; Menanteau, F.; Miquel, R.; Mohr, J. J.; Morgan, R.; Muir, J.; Myles, J.; Nadathur, S.; Navarro-Alsina, A.; Nichol, R. C.; Ogando, R. L. C.; Omori, Y.; Palmese, A.; Pandey, S.; Park, Y.; Paz-Chinchón, F.; Petravick, D.; Pieres, A.; Malagón, A. A. Plazas; Porredon, A.; Prat, J.; Raveri, M.; Rodriguez-Monroy, M.; Rollins, R. P.; Romer, A. K.; Roodman, A.; Rosenfeld, R.; Ross, A. J.; Rykoff, E. S.; Samuroff, S.; Sánchez, C.; Sanchez, E.; Sanchez, J.; Cid, D. Sanchez; Scarpine, V.; Schubnell, M.; Scolnic, D.; Secco, L. F.; Serrano, S.; Sevilla-Noarbe, I.; Sheldon, E.; Shin, T.; Smith, M.; Soares-Santos, M.; Suchyta, E.; Swanson, M. E. C.; Tabbutt, M.; Tarle, G.; Thomas, D.; To, C.; Troja, A.; Troxel, M. A.; Tucker, D. L.; Tutusaus, I.; Varga, T. N.; Walker, A. R.; Weaverdyck, N.; Wechsler, R.; Weller, J.; Yanny, B.; Yin, B.; Zhang, Y.; Zuntz, J.
Source
Subject
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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)
Comment: See https://www.darkenergysurvey.org/des-year-3-cosmology-results-papers/ for the full DES Y3 3x2pt cosmology release. Matches version accepted in PRD
Comment: See https://www.darkenergysurvey.org/des-year-3-cosmology-results-papers/ for the full DES Y3 3x2pt cosmology release. Matches version accepted in PRD