000262303 001__ 262303
000262303 005__ 20190619220114.0
000262303 022__ $$a0035-8711
000262303 022__ $$a1365-2966
000262303 02470 $$a000449617100026$$2isi
000262303 0247_ $$a10.1093/mnras/sty1899$$2doi
000262303 037__ $$aARTICLE
000262303 245__ $$aDES Y1 Results: validating cosmological parameter estimation using simulated Dark Energy Surveys
000262303 260__ $$c2018$$aOxford$$bOXFORD UNIV PRESS
000262303 269__ $$a2018-11-01
000262303 336__ $$aJournal Articles
000262303 520__ $$aWe use mock galaxy survey simulations designed to resemble the Dark Energy Survey Year 1 (DES Y1) data to validate and inform cosmological parameter estimation. When similar analysis tools are applied to both simulations and real survey data, they provide powerful validation tests of the DES Y1 cosmological analyses presented in companion papers. We use two suites of galaxy simulations produced using different methods, which therefore provide independent tests of our cosmological parameter inference. The cosmological analysis we aim to validate is presented in DES Collaboration et al. (2017) and uses angular two-point correlation functions of galaxy number counts and weak lensing shear, as well as their cross-correlation, in multiple redshift bins. While our constraints depend on the specific set of simulated realisations available, for both suites of simulations we find that the input cosmology is consistent with the combined constraints from multiple simulated DES Y1 realizations in the Omega(m) - sigma(8) plane. For one of the suites, we are able to show with high confidence that any biases in the inferred S-8 = sigma(8)(Omega(m)/0.3)(0.5) and Omega(m) are smaller than the DES Y1 1 - sigma uncertainties. For the other suite, for which we have fewer realizations, we are unable to be this conclusive; we infer a roughly 60 per cent (70 per cent) probability that systematic bias in the recovered Omega(m) (S-8) is sub-dominant to the DES Y1 uncertainty. As cosmological analyses of this kind become increasingly more precise, validation of parameter inference using survey simulations will be essential to demonstrate robustness.
000262303 650__ $$aAstronomy & Astrophysics
000262303 650__ $$aAstronomy & Astrophysics
000262303 6531_ $$alarge-scale structure of universe
000262303 6531_ $$acosmological parameters
000262303 6531_ $$ascience verification data
000262303 6531_ $$alarge-scale structure
000262303 6531_ $$adigital sky survey
000262303 6531_ $$apower spectra
000262303 6531_ $$acosmic shear
000262303 6531_ $$agalaxy
000262303 6531_ $$amatter
000262303 6531_ $$abias
000262303 6531_ $$aalignments
000262303 6531_ $$aluminosity
000262303 700__ $$aMacCrann, N.
000262303 700__ $$aDeRose, J.
000262303 700__ $$aWechsler, R. H.
000262303 700__ $$g276121$$0250390$$aBlazek, J.
000262303 700__ $$aGaztanaga, E.
000262303 700__ $$aCrocce, M.
000262303 700__ $$aRykoff, E. S.
000262303 700__ $$aBecker, M. R.
000262303 700__ $$aJain, B.
000262303 700__ $$aKrause, E.
000262303 700__ $$aEifler, T. F.
000262303 700__ $$aGruen, D.
000262303 700__ $$aZuntz, J.
000262303 700__ $$aTroxel, M. A.
000262303 700__ $$aElvin-Poole, J.
000262303 700__ $$aPrat, J.
000262303 700__ $$aWang, M.
000262303 700__ $$aDodelson, S.
000262303 700__ $$aKravtsov, A.
000262303 700__ $$aFosalba, P.
000262303 700__ $$aBusha, M. T.
000262303 700__ $$aEvrard, A. E.
000262303 700__ $$aHuterer, D.
000262303 700__ $$aAbbott, T. M. C.
000262303 700__ $$aAbdalla, F. B.
000262303 700__ $$aAllam, S.
000262303 700__ $$aAnnis, J.
000262303 700__ $$aAvila, S.
000262303 700__ $$aBernstein, G. M.
000262303 700__ $$aBrooks, D.
000262303 700__ $$aBuckley-Geer, E.
000262303 700__ $$aBurke, D. L.
000262303 700__ $$aRosell, A. Carnero
000262303 700__ $$aKind, M. Carrasco
000262303 700__ $$aCarretero, J.
000262303 700__ $$aCastander, F. J.
000262303 700__ $$aCawthon, R.
000262303 700__ $$aCunha, C. E.
000262303 700__ $$aD'Andrea, C. B.
000262303 700__ $$ada Costa, L. N.
000262303 700__ $$aDavis, C.
000262303 700__ $$aDe Vicente, J.
000262303 700__ $$aDiehl, H. T.
000262303 700__ $$aDoel, P.
000262303 700__ $$aFrieman, J.
000262303 700__ $$aGarcia-Bellido, J.
000262303 700__ $$aGerdes, D. W.
000262303 700__ $$aGruendl, R. A.
000262303 700__ $$aGutierrez, G.
000262303 700__ $$aHartley, W. G.
000262303 700__ $$aHollowood, D.
000262303 700__ $$aHonscheid, K.
000262303 700__ $$aHoyle, B.
000262303 700__ $$aJames, D. J.
000262303 700__ $$aJeltema, T.
000262303 700__ $$aKirk, D.
000262303 700__ $$aKuehn, K.
000262303 700__ $$aKuropatkin, N.
000262303 700__ $$g274501$$0250244$$aLima, M.
000262303 700__ $$aMaia, M. A. G.
000262303 700__ $$aMarshall, J. L.
000262303 700__ $$aMenanteau, F.
000262303 700__ $$aMiquel, R.
000262303 700__ $$aPlazas, A. A.
000262303 700__ $$aRoodman, A.
000262303 700__ $$g106339$$0241512$$aSanchez, E.
000262303 700__ $$aScarpine, V.
000262303 700__ $$aSchubnell, M.
000262303 700__ $$aSevilla-Noarbe, I.
000262303 700__ $$g206098$$0244159$$aSmith, M.
000262303 700__ $$aSmith, R. C.
000262303 700__ $$aSoares-Santos, M.
000262303 700__ $$aSobreira, F.
000262303 700__ $$aSuchyta, E.
000262303 700__ $$aSwanson, M. E. C.
000262303 700__ $$aTarle, G.
000262303 700__ $$aThomas, D.
000262303 700__ $$aWalker, A. R.
000262303 700__ $$aWeller, J.
000262303 773__ $$k4$$j480$$q4614-4635$$tMonthly Notices Of The Royal Astronomical Society
000262303 8560_ $$fyves.revaz@epfl.ch
000262303 909C0 $$zPasquier, Simon$$0252365$$yApproved$$pLASTRO$$xU10933$$myves.revaz@epfl.ch
000262303 909CO $$particle$$ooai:infoscience.epfl.ch:262303$$pSB
000262303 961__ $$afantin.reichler@epfl.ch
000262303 973__ $$aEPFL$$sPUBLISHED$$rREVIEWED
000262303 980__ $$aARTICLE
000262303 980__ $$aWoS
000262303 981__ $$aoverwrite