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|Title:||Gravitational lensing analysis of the Kilo-Degree Survey||Authors:||Kuijken, Konrad
de Jong, Jelte T. A.
van Uitert, Edo
Conti, Ian Fenech
LA BARBERA, Francesco
NAPOLITANO, NICOLA ROSARIO
Verdoes Kleijn, Gijs
van Waerbeke, Ludovic
|Issue Date:||2015||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||454||Issue:||4||First Page:||3500||Abstract:||The Kilo-Degree Survey (KiDS) is a multi-band imaging survey designed for cosmological studies from weak lensing and photometric redshifts. It uses the European Southern Observatory VLT Survey Telescope with its wide-field camera OmegaCAM. KiDS images are taken in four filters similar to the Sloan Digital Sky Survey ugri bands. The best seeing time is reserved for deep r-band observations. The median 5σ limiting AB magnitude is 24.9 and the median seeing is below 0.7 arcsec. Initial KiDS observations have concentrated on the Galaxy and Mass Assembly (GAMA) regions near the celestial equator, where extensive, highly complete redshift catalogues are available. A total of 109 survey tiles, 1 square degree each, form the basis of the first set of lensing analyses of halo properties of GAMA galaxies. Nine galaxies per square arcminute enter the lensing analysis, for an effective inverse shear variance of 69 arcmin<SUP>-2</SUP>. Accounting for the shape measurement weight, the median redshift of the sources is 0.53. KiDS data processing follows two parallel tracks, one optimized for weak lensing measurement and one for accurate matched-aperture photometry (for photometric redshifts). This technical paper describes the lensing and photometric redshift measurements (including a detailed description of the Gaussian aperture and photometry pipeline), summarizes the data quality and presents extensive tests for systematic errors that might affect the lensing analyses. We also provide first demonstrations of the suitability of the data for cosmological measurements, and describe our blinding procedure for preventing confirmation bias in the scientific analyses. The KiDS catalogues presented in this paper are released to the community through http://kids.strw.leidenuniv.nl.||Acknowledgments:||We are grateful to Matthias Bartelmann for being our external blinder, revealing which of the four catalogues analysed was the true unblinded catalogue at the end of this study, to Giovanni Covone and Mattia Vaccari for providing the VOICE data, to all the members of the KiDS weak lensing team who supported this work, and to the GAMA team for their spectroscopic catalogues. We also thank Mike Jarvis and Martin Kilbinger for corr2 and athena , the correlation function measurement software used in this analysis. We acknowledge support from the European Research Council under FP7 grant numbers 279396 (MV, MC, CS, RH, ME, HHo) and 240185 (AC and CH). EvU acknowledges support from an STFC Ernest Rutherford Research Grant, grant reference ST/L00285X/1. RN and EvU acknowledge support from the German Federal Ministry for Economic Affairs and Energy (BMWi) provided via DLR under project no. 50QE1103. HHi is supported by the DFG Emmy Noether grant Hi 1495/2-1. JHD and LvW are funded by the NSERC of Canada, and LvW by CIfAR. TDK is supported by a Royal Society URF. CB acknowledges the support of the Australian Research Council through the award of a Future Fellowship. This work is supported by the Netherlands Organisation for Scientific Research (NWO) through grants 614.001.103 and 614.061.610, by the Dutch Research School for Astronomy (NOVA), and by the Deutsche Forschungsgemeinschaft in the framework of the TR33 ‘The Dark Universe’. This work is based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 177.A-3016, 177.A-3017 and 177.A-3018, and on data products produced by Target/OmegaCEN, INAF-OACN, INAF-OAPD and the KiDS production team, on behalf of the KiDS consortium. Author Contributions: All authors contributed to the development and writing of this paper. The authorship list is given in three groups: the lead authors (KK, CH, HHi, RN, TE, JdJ, MV), followed by two alphabetical groups. The first alphabetical group includes those who are key contributors to both the scientific analysis and the data products. The second group covers those who have either made a significant contribution to the data products or to the scientific analysis.||URI:||http://hdl.handle.net/20.500.12386/23578||URL:||https://academic.oup.com/mnras/article/454/4/3500/993789||ISSN:||0035-8711||DOI:||10.1093/mnras/stv2140||Bibcode ADS:||2015MNRAS.454.3500K||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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