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|Title:||The first and second data releases of the Kilo-Degree Survey||Authors:||de Jong, Jelte T. A.
Verdoes Kleijn, Gijs A.
Boxhoorn, Danny R.
LA BARBERA, Francesco
McFarland, John P.
NAPOLITANO, NICOLA ROSARIO
Valentijn, Edwin A.
Begeman, Kor G.
PUDDU, Emanuella Anna
van Uitert, Edo
Eriksen, Martin B.
Kitching, Thomas D.
Koopmans, Léon V. E.
Sutherland, Will J.
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||582||First Page:||1||Abstract:||Context. The Kilo-Degree Survey (KiDS) is an optical wide-field imaging survey carried out with the VLT Survey Telescope and the OmegaCAM camera. KiDS will image 1500 square degrees in four filters (ugri), and together with its near-infrared counterpart VIKING will produce deep photometry in nine bands. Designed for weak lensing shape and photometric redshift measurements, its core science driver is mapping the large-scale matter distribution in the Universe back to a redshift of ~0.5. Secondary science cases include galaxy evolution, Milky Way structure, and the detection of high-redshift clusters and quasars. <BR /> Aims: KiDS is an ESO Public Survey and dedicated to serving the astronomical community with high-quality data products derived from the survey data. Public data releases, the first two of which are presented here, are crucial for enabling independent confirmation of the survey's scientific value. The achieved data quality and initial scientific utilization are reviewed in order to validate the survey data. <BR /> Methods: A dedicated pipeline and data management system based on Astro-WISE, combined with newly developed masking and source classification tools, is used for the production of the data products described here. Science projects based on these data products and preliminary results are outlined. <BR /> Results: For 148 survey tiles (≈160 sq.deg.) stacked ugri images have been released, accompanied by weight maps, masks, source lists, and a multi-band source catalogue. Limiting magnitudes are typically 24.3, 25.1, 24.9, 23.8 (5σ in a 2'' aperture) in ugri, respectively, and the typical r-band PSF size is less than 0.7''. The photometry prior to global homogenization is stable at the ~2% (4%) level in gri (u) with some outliers due to non-photometric conditions, while the astrometry shows a typical 2D rms of 0.03''. Early scientific results include the detection of nine high-z QSOs, fifteen candidate strong gravitational lenses, high-quality photometric redshifts and structural parameters for hundreds of thousands of galaxies.||Acknowledgments:||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. The KiDS production team acknowledge support by NWO-M grants. OmegaCEN is financially supported by NOVA and Target. Members of INAF-OAPD and INAF-OACN also acknowledge the support from the Department of Physics Astronomy of the University of Padova, and of the Department of Physics of Univ. Federico II (Naples). Target is supported by Samenwerkingsverband Noord Nederland, European fund for regional development, Dutch Ministry of economic affairs, Pieken in de Delta, Provinces of Groningen and Drenthe. Target operates under the auspices of Sensor Universe. This work has made use of Astro-WISE, which is an on-going project which started from an EU FP5 RTD programme funded by the EC Action “Enhancing Access to Research Infrastructures”. J.d.J., E.M.H. and N.I. are supported by NWO grant 614.061.610. M.R. acknowledges support from the Italian MIUR 20102011 through the PRIN “The dark Universe and the cosmic evolution of baryons: from current surveys to Euclid”. A.C. and C.H. acknowledge support from the European Research Council under the EC FP7 grant number 240185. H.H.i. is supported by the DFG Emmy Noether grant Hi 1495/2-1. G.L. wishes to acknowledge partial support from the Italian MIUR through the PRIN “Cosmology with Euclid”. M.P. acknowledges financial support from PRIN-INAF 2014. C.T. has received funding from the European Union Seventh Framework Programme (FP7/20072013) under grant agreement no. 267251 “Astronomy Fellowships in Italy” (AstroFIt). J.H. is funded by NSERC. B.J. acknowledges support by an STFC Ernest Rutherford Fellowship, grant reference ST/J004421/1. H.H. and M.B.E. acknowledge support from the European Research Council FP7 grant number 279396. L.V.E.K. is supported in part through an NWO-VICI career grant (project number 639.043.308). M.V. is funded by grant 614.001.103 from the Netherlands Organisation for Scientific Research (NWO) and from the European Research Council under FP7 grant number 279396. This work was supported by the Deutsche Forschungsgemeinschaft via the project TR33 “The Dark Universe”.||URI:||http://hdl.handle.net/20.500.12386/23579||URL:||https://www.aanda.org/articles/aa/abs/2015/10/aa26601-15/aa26601-15.html||ISSN:||0004-6361||DOI:||10.1051/0004-6361/201526601||Bibcode ADS:||2015A&A...582A..62D||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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