[PDF] Top 20 Dark Energy Survey year 1 results: measurement of the galaxy angular power spectrum

... from the so-called Y1 Gold catalogue (Drlica-Wagner et ...from the data reduction performed by the Dark Energy Survey Data Management (DESDM) system on DECam ...images. ... See full document

... at the locations of galaxy clusters detected by DES, SPT, and ...Comparison of the amplitudes of the mock tSZ profiles of clusters detected in the different ... See full document

... for the full photometric redshift distributions, we find that for our ...bin, the non-linear linear alignment model predicts at most an ∼4 per cent contamination of the tangential shear ... See full document

... by the Na- tional Science Foundation under grant numbers AST-1138766 and ...AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015- 71825, ... See full document

... constructing the lensing potential and deflection ...in the CMB lensing community, but seldom constructed and visualized using measurements of galaxy lensing except in some theoretical studies ... See full document

... Furthermore, the resultant χ 2 and p.t.e. values indicate that the model is a good description of the ...in the rightmost columns of Table II . This measurement rejects ... See full document

... Validation of assumptions using synthetic data In order to verify that our results are robust to modeling assumptions and approximations, we compare the inferred values of the extension ... See full document

... from the PRIMUS DR1 data set (Coil et ...obtain the best fit of the six basic templates to each of the highest quality PRIsm MUlti-Object Survey (PRIMUS) objects (quality ... See full document

... Our results are shown in the upper panels of ...and the residual shifts in the mean z A after the calibration are summarized in the first row of Tables 1 ... See full document

... < 1 per ...with the mass profile model and systematic corrections. This way the estimated statistical uncertainty of the boost factors is propagated self-consistently into their ... See full document

... upon the DES five year ...increase the galaxy BAO measurements to redshifts z∼ 1, only to be surpassed by new spectroscopic surveys such as DESI (DESI Collaboration 2016a , b ) and ... See full document

... In the past decade, a separate technique of determining redshifts has been studied, starting most prominently with Schneider et ...). The technique, sometimes called the cross-correlation ... See full document

... is the assumption of a fiducial cosmology in converting the galaxy angular positions and redshifts observed in a galaxy redshift survey (such as BOSS) into the ... See full document

... measure the clustering of the galaxies and their correlations with the CMB lensing maps in position ...to the galaxy density ...to the CMB lensing map in order to cut off ... See full document

... report the results of several searches of the DES SV and Y1 imaging data for strong gravitational lens ...combination of techniques. We searched the positions of ... See full document

... We perform a joint analysis of intrinsic alignments and cosmology using tomographic weak lensing, galaxy clustering, and galaxy–galaxy lensing measurements from Year 1 Y1 of the Dark Ene[r] ... See full document

... Most of the above void finders have either been applied to simulations, or galaxy survey data with spectroscopic redshifts (spec-z), where the precise positions of tracers are ... See full document

... that the χ 2 is sensitive to the inclusion of the shot-noise correction applied to the covariance detailed in ...for the fiducial analysis in each of the 5 redshift ... See full document

... cosmological results from a combined analysis of galaxy clustering and weak gravitational lensing, using 1321 deg 2 of griz imaging data from the first year of the ... See full document

... i Shear measurement systematics Section 4.1, ii Source photometric redshift uncertainties Section 4.3, iii Source sample dilution by cluster members Section 4.2, Section 5.3.1, iv Cluste[r] ... See full document