Paper: 2019ApJ...882...62N (acknowledgments)
We are thankful for fruitful discussions and comments provided by Simone Ferraro and Emmanuel Schaan. The Hyper Suprime-Cam (HSC) Collaboration includes the astronomical communities of Japan and Taiwan and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. The Pan-STARRS1 Surveys (PS1), which are used for the photometry and astrometry calibration, have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, Johns Hopkins University, Durham University, the University of Edinburgh, Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE). This paper makes use of software developed for the Large Synoptic Survey Telescope. We thank the LSST Project for making their code available as free software at http://dm.lsst.org . This work is based in part on data collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by the Subaru Telescope and Astronomy Data Center at the National Astronomical Observatory of Japan. The P olarbear project is funded by the National Science Foundation under grant Nos. AST-0618398 and AST-1212230. The James Ax Observatory operates in the Parque Astronómico Atacama in Northern Chile under the auspices of the Comisión Nacional de Investigación Científica y Tecnológica de Chile (CONICYT). The James Ax Observatory would not be possible without the support of CONICYT in Chile. All silicon-wafer-based technology for P olarbear was fabricated at the UCB Nanolab. This research used resources of the Central Computing System, owned and operated by the Computing Research Center at KEK, the HPCI system (Project ID:hp150132), and the National Energy Research Scientific Computing Center (NERSC), a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under contract No. DE-AC02-05CH11231. This work was supported in part by the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and MEXT Grant-in-Aid for Scientific Research on Innovative Areas (JP15H05887, JP15H05891, JP15H05892, JP15H05893). In Japan, this work was supported by MEXT KAKENHI grant Nos. 21111002 and JP18H05539, JSPS KAKENHI grant Nos. JP26220709, JP24111715, JP26800125, and the JSPS Core-to-Core Program. In Italy, this work was supported by the RADIOFOREGROUNDS grant of the European Union’s Horizon 2020 research and innovation program (COMPET-05-2015, grant agreement No. 687312), as well as by the INDARK INFN Initiative and the COSMOS network of the Italian Space Agency (cosmosnet.it). Support from the Ax Center for Experimental Cosmology is gratefully acknowledged. The KEK authors acknowledge support from KEK Cryogenics Science Center. The APC group acknowledges travel support from Labex UNIVEARTHS. The Melbourne group acknowledges support from the University of Melbourne and an Australian Research Council's Future Fellowship (FT150100074). Y.C. acknowledges the support from JSPS KAKENHI grant Nos. 18K13558 and 18H04347. T.N. acknowledges the support from the Ministry of Science and Technology (MOST), Taiwan, R.O.C., through the MOST research project grants (No. 107-2112-M-002-002-MY3). H.M. acknowledges the support from JSPS KAKENHI grant No. JP18H04350. M.O. acknowledges the support from JSPS KAKENHI grant No. JP18K03693. R.T. acknowledges the support from Grant-in-Aid for Scientific Research from the JSPS Promotion of Science (17H01131). Numerical computations were in part carried out on Cray XC50 at the Center for Computational Astrophysics, National Astronomical Observatory of Japan. A.K. acknowledges the support by the JSPS Leading Initiative for Excellent Young Researchers (LEADER) and by JSPS KAKENHI grant No. JP16K21744. M.A. acknowledges support from CONICYT UC Berkeley-Chile Seed grant (CLAS fund) No. 77047, Fondecyt project 1130777 and 1171811, the DFI postgraduate scholarship program, and the DFI Postgraduate Competitive Fund for Support in the Attendance to Scientific Events. G.F. acknowledges support from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013)/ERC grant agreement No. 616170. F.M. acknowledges the support by the JSPS Fellowship (grant No. JP17F17025). J.S.S. is supported by the NSF Graduate Research Fellowship.