TY - JOUR
T1 - SMASH
T2 - Survey of the MAgellanic Stellar History
AU - Nidever, David L.
AU - Olsen, Knut
AU - Walker, Alistair R.
AU - Vivas, A. Katherina
AU - Blum, Robert D.
AU - Kaleida, Catherine
AU - Choi, Yumi
AU - Conn, Blair C.
AU - Gruendl, Robert A.
AU - Bell, Eric F.
AU - Besla, Gurtina
AU - Munoz, Ricardo R.
AU - Gallart, Carme
AU - Martin, Nicolas F.
AU - Olszewski, Edward W.
AU - Saha, Abhijit
AU - Monachesi, Antonela
AU - Monelli, Matteo
AU - De Boer, Thomas J.L.
AU - Johnson, L. Clifton
AU - Zaritsky, Dennis
AU - Stringfellow, Guy S.
AU - Van Der Marel, Roeland P.
AU - Cioni, Maria Rosa L.
AU - Jin, Shoko
AU - Majewski, Steven R.
AU - Martinez-Delgado, David
AU - Monteagudo, Lara
AU - Noël, Noelia E.D.
AU - Bernard, Edouard J.
AU - Kunder, Andrea
AU - Chu, You Hua
AU - Bell, Cameron P.M.
AU - Santana, Felipe
AU - Frechem, Joshua
AU - Medina, Gustavo E.
AU - Parkash, Vaishali
AU - Navarrete, J. C.Serón
AU - Hayes, Christian
N1 - Funding Information:
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. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. This project used data obtained with the Dark Energy Camera (DECam), which was constructed by the Dark Energy Survey (DES) collaboration. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvi-mento Cientfico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Enérgeticas, Med-ioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, the Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa. int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC;https://www.cosmos.esa.int/web/gaia/ dpac/consortium). Funding for DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.
Funding Information:
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
Publisher Copyright:
© 2017. The American Astronomical Society. All rights reserved..
PY - 2017/11
Y1 - 2017/11
N2 - The 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.
AB - The 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.
KW - Local Group
KW - Magellanic Clouds
KW - galaxies: dwarf
KW - galaxies: individual (Large Magellanic Cloud, Small Magellanic Cloud)
KW - surveys
UR - http://www.scopus.com/inward/record.url?scp=85034590762&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85034590762&partnerID=8YFLogxK
U2 - 10.3847/1538-3881/aa8d1c
DO - 10.3847/1538-3881/aa8d1c
M3 - Article
AN - SCOPUS:85034590762
SN - 0004-6256
VL - 154
JO - Astronomical Journal
JF - Astronomical Journal
IS - 5
M1 - 199
ER -