Nidever, David L.Olsen, Knut A. G.Walker, Alistair RVivas, Anna KatherinaBlum, Robert D.Kaleida, CatherineChoi, YumiConn, BlairGruendl, R.ABell, Eric FBesla, GurtinaMunoz, Ricardo R2021-09-160004-6256http://hdl.handle.net/1885/247938The Large and Small Magellanic Clouds are unique local laboratories for studying the formation and evolution of small galaxies in exquisite detail. The Survey of the MAgellanic Stellar History (SMASH) is an NOAO community Dark Energy Camera (DECam) survey of the Clouds mapping 480 deg2 (distributed over ~2400 square degrees at ~20% filling factor) to ~24th mag in ugriz. The primary goals of SMASH are to identify low surface brightness stellar populations associated with the stellar halos and tidal debris of the Clouds, and to derive spatially resolved star formation histories. Here, we present a summary of the survey, its data reduction, and a description of the first public Data Release (DR1). The SMASH DECam data have been reduced with a combination of the NOAO Community Pipeline, the PHOTRED automated point-spread-function photometry pipeline, and custom calibration software. The astrometric precision is ~15 mas and the accuracy is ~2 mas with respect to the Gaia reference frame. The photometric precision is ~0.5%–0.7% in griz and ~1% in u with a calibration accuracy of ~1.3% in all bands. The median 5σ point source depths in ugriz are 23.9, 24.8, 24.5, 24.2, and 23.5 mag. The SMASH data have already been used to discover the Hydra II Milky Way satellite, the SMASH 1 old globular cluster likely associated with the LMC, and extended stellar populations around the LMC out to R ~ 18.4 kpc. SMASH DR1 contains measurements of ~100 million objects distributed in 61 fields. A prototype version of the NOAO Data Lab provides data access and exploration tools.D.L.N. was supported by a McLaughlin Fellowship while at the University of Michigan. Y.C. acknowledges support from NSF grant AST 1655677. B.C.C. acknowledges the support of the Australian Research Council through Discovery project DP150100862. E.F.B. acknowledges support from NSF grants AST 1008342 and 1655677. E.W.O. was partially supported by NSF grant AST 1313006. T.d.B. acknowledges financial support from the ERC under Grant Agreement n. 308024. M.-R.C. acknowledges support by the German Academic Exchange Service (DAAD), from the UK’s Science and Technology Facility Council (grant number ST/M001008/1), and from the the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 682115). S.J. is supported by the Netherlands Organization for Scientific Research (NWO) Veni grant 639.041.131. S.R.M. acknowledges partial support from NSF grant AST 1312863. D.M.-D. acknowledges support by Sonderforschungsbereich (SFB) 881 “The Milky Way System” of the German Research Foundation (DFB), subproject A2. R.R.M. acknowledges partial support from CONICYT Anillo project ACT-1122 and project BASAL PFB-06. G.S.S. is supported by grants from NASA. Based on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory (NOAO Prop. ID: 2013A-0411 and 2013B-0440; PI: Nidever), which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation.application/pdfen-AU© 2017. The American Astronomical Societygalaxies: dwarfgalaxies: individual (Large Magellanic Cloud, Small Magellanic Cloud)Local GroupMagellanic Cloudssurveys201710.3847/1538-3881/aa8d1c2020-11-23