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tokens: We thank Iftach Sadeh for the assistance in using the ANNz2 software, and for its continuous development, as well as Jonn Soo for very useful suggestions regarding the practicalities of the code. Ben Hoyle is acknowledged for enlightening discussions on machine-learning photo-z estima- tion. We also thank an anonymous referee for very useful comments and sugges- tions that allowed us to improve this paper. 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. OmegaCEN and the KiDS production team acknowledge support by NOVA and NWO-M grants. 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). GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalog is based on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being ob- tained by a number of independent survey programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT, and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO, and the participating institutions. The GAMA website is http://www.gama-survey.org/ . 2dFLenS is based on data acquired through the Australian Astronomical Obser- vatory, under programme A/2014B/008. It would not have been possible without the dedicated work of the staff of the AAO in the development and support of the 2dF-AAOmega system, and the running of the AAT. Funding for SDSS-III was provided by the Alfred P. Sloan Foundation, the Partic- ipating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/ . SDSS-III is managed by the Astrophysical Research Consortium for the Par- ticipating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Labora- tory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de As- trofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Van- derbilt University, University of Virginia, University of Washington, and Yale University. MBi is supported by the Netherlands Organization for Scientific Research, NWO, through grant number 614.001.451, and by the Polish National Science Center under contract UMO-2012/07/D/ST9/02785. MBi and HHo acknowledge support from the European Research Council FP7 grant number 279396. HHo acknowledges support from Vici grant 639.043.512, financed by the NWO. CB acknowledges the support of the Australian Research Council through the award of a Future Fellowship. JTAdJ is supported by the Netherlands Organisation for Scientific Research (NWO) through grant 621.016.402. HHi is supported by an Emmy Noether grant (No. Hi 1495/2-1) of the Deutsche Forschungs- gemeinschaft. MBr acknowledges financial contribution from the agreement ASI/INAF I/023/12/1. CH acknowledges support from the ERC under grant number 647112. KK acknowledges support by the Alexander von Humboldt Foundation. DP acknowledges the support of the Australian Research Council through the award of a Future Fellowship. GVK acknowledges financial support from the Netherlands Research School for Astronomy (NOVA) and Target. Tar- get 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. This work has made use of TOPCAT ( Taylor 2005 ) and STILTS ( Taylor 2006 ) software, as well as of PYTHON ( www.python.org ), including the packages N UM PY ( van der Walt et al. 2011 ), S CI PY ( Jones et al. 2001 ), and MATPLOTIB ( Hunter 2007 ).