E-resources
-
Friedrich, O; Andrade-Oliveira, F; Camacho, H; Alves, O; Rosenfeld, R; Sanchez, J; Fang, X; Eifler, T F; Krause, E; Chang, C; Omori, Y; Amon, A; Baxter, E; Elvin-Poole, J; Huterer, D; Porredon, A; Prat, J; Terra, V; Troja, A; Alarcon, A; Bechtol, K; Bernstein, G M; Buchs, R; Campos, A; Carnero Rosell, A; Carrasco Kind, M; Cawthon, R; Cordero, J; Crocce, M; DeRose, J; Diehl, H T; Dodelson, S; Doux, C; Drlica-Wagner, A; Everett, S; Fosalba, P; Gatti, M; Giannini, G; Gruen, D; Gruendl, R A; Harrison, I; Hartley, W G; Jain, B; Jarvis, M; MacCrann, N; McCullough, J; Muir, J; Myles, J; Pandey, S; Raveri, M; Roodman, A; Rodriguez-Monroy, M; Rykoff, E S; Samuroff, S; Sánchez, C; Secco, L F; Sevilla-Noarbe, I; Troxel, M A; Weaverdyck, N; Yanny, B; Aguena, M; Avila, S; Bacon, D; Bertin, E; Brooks, D; Burke, D L; Costanzi, M; Pereira, M E S; De Vicente, J; Desai, S; Evrard, A E; Ferrero, I; García-Bellido, J; Gaztanaga, E; Gerdes, D W; Giannantonio, T; Gschwend, J; Hinton, S R; Hollowood, D L; Honscheid, K; James, D J; Kuehn, K; Lahav, O; Maia, M A G; Menanteau, F; Miquel, R; Morgan, R; Palmese, A; Paz-Chinchón, F; Plazas, A A; Sanchez, E; Scarpine, V; Serrano, S; Smith, M; Suchyta, E; Tarle, G; Thomas, D; To, C; Varga, T N; Weller, J
Monthly notices of the Royal Astronomical Society, 12/2021, Volume: 508, Issue: 3Journal Article
ABSTRACT We describe and test the fiducial covariance matrix model for the combined two-point function analysis of the Dark Energy Survey Year 3 (DES-Y3) data set. Using a variety of new ansatzes for covariance modelling and testing, we validate the assumptions and approximations of this model. These include the assumption of Gaussian likelihood, the trispectrum contribution to the covariance, the impact of evaluating the model at a wrong set of parameters, the impact of masking and survey geometry, deviations from Poissonian shot noise, galaxy weighting schemes, and other sub-dominant effects. We find that our covariance model is robust and that its approximations have little impact on goodness of fit and parameter estimation. The largest impact on best-fitting figure-of-merit arises from the so-called fsky approximation for dealing with finite survey area, which on average increases the χ2 between maximum posterior model and measurement by $3.7{{\ \rm per\ cent}}$ (Δχ2 ≈ 18.9). Standard methods to go beyond this approximation fail for DES-Y3, but we derive an approximate scheme to deal with these features. For parameter estimation, our ignorance of the exact parameters at which to evaluate our covariance model causes the dominant effect. We find that it increases the scatter of maximum posterior values for Ωm and σ8 by about $3{{\ \rm per\ cent}}$ and for the dark energy equation-of-state parameter by about $5{{\ \rm per\ cent}}$.
Author
Shelf entry
Permalink
- URL:
Impact factor
Access to the JCR database is permitted only to users from Slovenia. Your current IP address is not on the list of IP addresses with access permission, and authentication with the relevant AAI accout is required.
Year | Impact factor | Edition | Category | Classification | ||||
---|---|---|---|---|---|---|---|---|
JCR | SNIP | JCR | SNIP | JCR | SNIP | JCR | SNIP |
Select the library membership card:
If the library membership card is not in the list,
add a new one.
DRS, in which the journal is indexed
Database name | Field | Year |
---|
Links to authors' personal bibliographies | Links to information on researchers in the SICRIS system |
---|
Source: Personal bibliographies
and: SICRIS
The material is available in full text. If you wish to order the material anyway, click the Continue button.