A data compression and optimal galaxy weights scheme for Dark Energy Spectroscopic Instrument and weak lensing datasets

Combining different observational probes, such as galaxy clustering and weak lensing, is a promising technique for unveiling the physics of the Universe with upcoming dark energy experiments. The galaxy redshift sample from the Dark Energy Spectroscopic Instrument (DESI) will have a significant overlap with major ongoing imaging surveys specifically designed for weak lensing measurements: the Kilo-Degree Survey (KiDS), the Dark Energy Survey (DES) and the Hyper Suprime-Cam (HSC) survey. In this work we analyse simulated redshift and lensing catalogues to establish a new strategy for combining high-quality cosmological imaging and spectroscopic data, in view of the first-year data assembly analysis of DESI. In a test case fitting for a reduced parameter set, we employ an optimal data compression scheme able to identify those aspects of the data that are most sensitive to the cosmological information, and amplify them with respect to other aspects of the data. We find this optimal compression approach is able to preserve all the information related to the growth of structure; we also extend this scheme to derive weights to be applied to individual galaxies, and show that these produce near-optimal results.Comment: 14 pages, 12 Figures, DESI collaboration articl

Measurement of the inclusive charmless semileptonic branching ratio of B mesons and determination of vertical bar V-ub vertical bar

We report a measurement of the inclusive charmless semileptonic branching fraction of B mesons in a sample of 89x10(6) B(b) over bar events recorded with the BABAR detector at the Y(4S) resonance. Events are selected by fully reconstructing the decay of one B meson and identifying a charged lepton from the decay of the other B meson. The number of signal events is extracted from the mass distribution of the hadronic system accompanying the lepton and is used to determine the ratio of branching fractions B((B) over bar --> X(u)l (v) over bar)/B((B) over bar --> Xl (v) over bar) = [2.06 +/- 0.25(stat) +/- 0.23(syst) +/- 0.36(theo)] x 10(-2). Using the measured branching fraction for inclusive semileptonic B decays, we find B((B) over bar --> X(u)l (V) over bar) = [2.24+/-0.27(stat) +/- 0.26(syst) +/- 0.39(theo)] x 10(-3) and derive the Cabibbo-Kobayashi-Maskawa matrix element parallel toV(ub)parallel to = [4.62 +/- 0.28(stat) +/- 0.27(syst) +/- 0.48(theo)] x 10(-3)