# Browsing by Author "Bacon, D"

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Item Open Access Dark Energy Survey Year 1 Results: Cosmological Constraints from Cluster Abundances and Weak LensingAbbott, TMC; Aguena, M; Alarcon, A; Allam, S; Allen, S; Annis, J; Avila, S; Bacon, D; Bechtol, K; Bermeo, A; Bernstein, GM; Bertin, E; Bhargava, S; Bocquet, S; Brooks, D; Brout, D; Buckley-Geer, E; Burke, DL; Carnero Rosell, A; Carrasco Kind, M; Carretero, J; Castander, FJ; Cawthon, R; Chang, C; Chen, X; Choi, A; Costanzi, M; Crocce, M; da Costa, LN; Davis, TM; De Vicente, J; DeRose, J; Desai, S; Diehl, HT; Dietrich, JP; Dodelson, S; Doel, P; Drlica-Wagner, A; Eckert, K; Eifler, TF; Elvin-Poole, J; Estrada, J; Everett, S; Evrard, AE; Farahi, A; Ferrero, I; Flaugher, B; Fosalba, P; Frieman, J; García-Bellido, J; Gatti, M; Gaztanaga, E; Gerdes, DW; Giannantonio, T; Giles, P; Grandis, S; Gruen, D; Gruendl, RA; Gschwend, J; Gutierrez, G; Hartley, WG; Hinton, SR; Hollowood, DL; Honscheid, K; Hoyle, B; Huterer, D; James, DJ; Jarvis, M; Jeltema, T; Johnson, MWG; Johnson, MD; Kent, S; Krause, E; Kron, R; Kuehn, K; Kuropatkin, N; Lahav, O; Li, TS; Lidman, C; Lima, M; Lin, H; MacCrann, N; Maia, MAG; Mantz, A; Marshall, JL; Martini, P; Mayers, J; Melchior, P; Mena-Fernández, J; Menanteau, F; Miquel, R; Mohr, JJ; Nichol, RC; Nord, B; Ogando, RLC; Palmese, A; Paz-Chinchón, F; Plazas, AA; Prat, J; Rau, MM; Romer, AK; Roodman, A; Rooney, P; Rozo, E; Rykoff, ES; Sako, M; Samuroff, S; Sánchez, C; Sanchez, E; Saro, A; Scarpine, V; Schubnell, M; Scolnic, D; Serrano, S; Sevilla-Noarbe, I; Sheldon, E; Smith, J Allyn; Smith, M; Suchyta, E; Swanson, MEC; Tarle, G; Thomas, D; To, C; Troxel, MA; Tucker, DL; Varga, TN; von der Linden, A; Walker, AR; Wechsler, RH; Weller, J; Wilkinson, RD; Wu, H; Yanny, B; Zhang, Y; Zhang, Z; Zuntz, J; Collaboration, DESWe perform a joint analysis of the counts and weak lensing signal of redMaPPer clusters selected from the Dark Energy Survey (DES) Year 1 dataset. Our analysis uses the same shear and source photometric redshifts estimates as were used in the DES combined probes analysis. Our analysis results in surprisingly low values for $S_8 =\sigma_8(\Omega_{\rm m}/0.3)^{0.5}= 0.65\pm 0.04$, driven by a low matter density parameter, $\Omega_{\rm m}=0.179^{+0.031}_{-0.038}$, with $\sigma_8-\Omega_{\rm m}$ posteriors in $2.4\sigma$ tension with the DES Y1 3x2pt results, and in $5.6\sigma$ with the Planck CMB analysis. These results include the impact of post-unblinding changes to the analysis, which did not improve the level of consistency with other data sets compared to the results obtained at the unblinding. The fact that multiple cosmological probes (supernovae, baryon acoustic oscillations, cosmic shear, galaxy clustering and CMB anisotropies), and other galaxy cluster analyses all favor significantly higher matter densities suggests the presence of systematic errors in the data or an incomplete modeling of the relevant physics. Cross checks with X-ray and microwave data, as well as independent constraints on the observable--mass relation from SZ selected clusters, suggest that the discrepancy resides in our modeling of the weak lensing signal rather than the cluster abundance. Repeating our analysis using a higher richness threshold ($\lambda \ge 30$) significantly reduces the tension with other probes, and points to one or more richness-dependent effects not captured by our model.Item Open Access Dark Energy Survey Year 3 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing(arXiv e-prints, 2021-05) Collaboration, DES; Abbott, TMC; Aguena, M; Alarcon, A; Allam, S; Alves, O; Amon, A; Andrade-Oliveira, F; Annis, J; Avila, S; Bacon, D; Baxter, E; Bechtol, K; Becker, MR; Bernstein, GM; Bhargava, S; Birrer, S; Blazek, J; Brandao-Souza, A; Bridle, SL; Brooks, D; Buckley-Geer, E; Burke, DL; Camacho, H; Campos, A; Carnero Rosell, A; Carrasco Kind, M; Carretero, J; Castander, FJ; Cawthon, R; Chang, C; Chen, A; Chen, R; Choi, A; Conselice, C; Cordero, J; Costanzi, M; Crocce, M; da Costa, LN; da Silva Pereira, ME; Davis, C; Davis, TM; De Vicente, J; DeRose, J; Desai, S; Di Valentino, E; Diehl, HT; Dietrich, JP; Dodelson, S; Doel, P; Doux, C; Drlica-Wagner, A; Eckert, K; Eifler, TF; Elsner, F; Elvin-Poole, J; Everett, S; Evrard, AE; Fang, X; Farahi, A; Fernandez, E; Ferrero, I; Ferté, A; Fosalba, P; Friedrich, O; Frieman, J; García-Bellido, J; Gatti, M; Gaztanaga, E; Gerdes, DW; Giannantonio, T; Giannini, G; Gruen, D; Gruendl, RA; Gschwend, J; Gutierrez, G; Harrison, I; Hartley, WG; Herner, K; Hinton, SR; Hollowood, DL; Honscheid, K; Hoyle, B; Huff, EM; Huterer, D; Jain, B; James, DJ; Jarvis, M; Jeffrey, N; Jeltema, T; Kovacs, A; Krause, E; Kron, R; Kuehn, K; Kuropatkin, N; Lahav, O; Leget, P-F; Lemos, P; Liddle, AR; Lidman, C; Lima, M; Lin, H; MacCrann, N; Maia, MAG; Marshall, JL; Martini, P; McCullough, J; Melchior, P; Mena-Fernández, J; Menanteau, F; Miquel, R; Mohr, JJ; Morgan, R; Muir, J; Myles, J; Nadathur, S; Navarro-Alsina, A; Nichol, RC; Ogando, RLC; Omori, Y; Palmese, A; Pandey, S; Park, Y; Paz-Chinchón, F; Petravick, D; Pieres, A; Plazas Malagón, AA; Porredon, A; Prat, J; Raveri, M; Rodriguez-Monroy, M; Rollins, RP; Romer, AK; Roodman, A; Rosenfeld, R; Ross, AJ; Rykoff, ES; Samuroff, S; Sánchez, C; Sanchez, E; Sanchez, J; Sanchez Cid, D; Scarpine, V; Schubnell, M; Scolnic, D; Secco, LF; Serrano, S; Sevilla-Noarbe, I; Sheldon, E; Shin, T; Smith, M; Soares-Santos, M; Suchyta, E; Swanson, MEC; Tabbutt, M; Tarle, G; Thomas, D; To, C; Troja, A; Troxel, MA; Tucker, DL; Tutusaus, I; Varga, TN; Walker, AR; Weaverdyck, N; Weller, J; Yanny, B; Yin, B; Zhang, Y; Zuntz, JWe 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)Item Open Access The Dark Energy Survey Supernova Program: Cosmological biases from supernova photometric classificationVincenzi, M; Sullivan, M; Möller, A; Armstrong, P; Bassett, BA; Brout, D; Carollo, D; Carr, A; Davis, TM; Frohmaier, C; Galbany, L; Glazebrook, K; Graur, O; Kelsey, L; Kessler, R; Kovacs, E; Lewis, GF; Lidman, C; Malik, U; Nichol, RC; Popovic, B; Sako, M; Scolnic, D; Smith, M; Taylor, G; Tucker, BE; Wiseman, P; Aguena, M; Allam, S; Annis, J; Asorey, J; Bacon, D; Bertin, E; Brooks, D; Burke, DL; Rosell, A Carnero; Carretero, J; Castander, FJ; Costanzi, M; Costa, LN da; Pereira, MES; Vicente, J De; Desai, S; Diehl, HT; Doel, P; Everett, S; Ferrero, I; Flaugher, B; Fosalba, P; Frieman, J; García-Bellido, J; Gerdes, DW; Gruen, D; Gutierrez, G; Hinton, SR; Hollowood, DL; Honscheid, K; James, DJ; Kuehn, K; Kuropatkin, N; Lahav, O; Li, TS; Lima, M; Maia, MAG; Marshall, JL; Miquel, R; Morgan, R; Ogando, RLC; Palmese, A; Paz-Chinchón, F; Pieres, A; Malagón, AA Plazas; Reil, K; Roodman, A; Sanchez, E; Schubnell, M; Serrano, S; Sevilla-Noarbe, I; Suchyta, E; Tarle, G; To, C; Varga, TN; Weller, J; Wilkinson, RDCosmological analyses of samples of photometrically-identified Type Ia supernovae (SNe Ia) depend on understanding the effects of 'contamination' from core-collapse and peculiar SN Ia events. We employ a rigorous analysis on state-of-the-art simulations of photometrically identified SN Ia samples and determine cosmological biases due to such 'non-Ia' contamination in the Dark Energy Survey (DES) 5-year SN sample. As part of the analysis, we test on our DES simulations the performance of SuperNNova, a photometric SN classifier based on recurrent neural networks. Depending on the choice of non-Ia SN models in both the simulated data sample and training sample, contamination ranges from 0.8-3.5 %, with the efficiency of the classification from 97.7-99.5 %. Using the Bayesian Estimation Applied to Multiple Species (BEAMS) framework and its extension 'BEAMS with Bias Correction' (BBC), we produce a redshift-binned Hubble diagram marginalised over contamination and corrected for selection effects and we use it to constrain the dark energy equation-of-state, $w$. Assuming a flat universe with Gaussian $\Omega_M$ prior of $0.311\pm0.010$, we show that biases on $w$ are $<0.008$ when using SuperNNova and accounting for a wide range of non-Ia SN models in the simulations. Systematic uncertainties associated with contamination are estimated to be at most $\sigma_{w, \mathrm{syst}}=0.004$. This compares to an expected statistical uncertainty of $\sigma_{w,\mathrm{stat}}=0.039$ for the DES-SN sample, thus showing that contamination is not a limiting uncertainty in our analysis. We also measure biases due to contamination on $w_0$ and $w_a$ (assuming a flat universe), and find these to be $<$0.009 in $w_0$ and $<$0.108 in $w_a$, hence 5 to 10 times smaller than the statistical uncertainties expected from the DES-SN sample.