Yan,Renbin1; Bundy,Kevin2; Law,David R.3; Bershady,Matthew A.4; Andrews,Brett5; Cherinka,Brian6; Diamond-Stanic,Aleksandar M.4; Drory,Niv7; MacDonald,Nicholas8; Sánchez-Gallego,José R.8; Thomas,Daniel9; Wake,David A.10; Weijmans,Anne-Marie11; Westfall,Kyle B.9; Zhang,Kai1; Aragón-Salamanca,Alfonso12; Belfiore,Francesco13,14; Bizyaev,Dmitry15,16; Blanc,Guillermo A.17,18; Blanton,Michael R.19; Brownstein,Joel20; Cappellari,Michele21; D’Souza,Richard22; Emsellem,Eric23,24,25; Fu,Hai26; Gaulme,Patrick15; Graham,Mark T.21; Goddard,Daniel9; Gunn,James E.27; Harding,Paul28; Jones,Amy22; Kinemuchi,Karen15; Li,Cheng29,30; Li,Hongyu31,32; Maiolino,Roberto13,14; Mao,Shude30,31,33; Maraston,Claudia9; Masters,Karen9; Merrifield,Michael R.12; Oravetz,Daniel15; Pan,Kaike15; Parejko,John K.8; Sanchez,Sebastian F.34; Schlegel,David35; Simmons,Audrey15; Thanjavur,Karun36; Tinker,Jeremy19; Tremonti,Christy4; van den Bosch,Remco37; Zheng,Zheng31
Source PublicationThe Astronomical Journal
AbstractABSTRACT The MaNGA Survey (Mapping Nearby Galaxies at Apache Point Observatory) is one of three core programs in the Sloan Digital Sky Survey IV. It is obtaining integral field spectroscopy for 10,000?nearby galaxies at a spectral resolution of R?~?2000 from 3622 to 10354 ?. The design of the survey is driven by a set of science requirements on the precision of estimates of the following properties: star formation rate surface density, gas metallicity, stellar population age, metallicity, and abundance ratio, and their gradients; stellar and gas kinematics; and enclosed gravitational mass as a function of radius. We describe how these science requirements set the depth of the observations and dictate sample selection. The majority of targeted galaxies are selected to ensure uniform spatial coverage in units of effective radius (Re) while maximizing spatial resolution. About two-thirds of the sample is covered out to 1.5Re (Primary sample), and one-third?of the sample is covered to 2.5Re (Secondary sample). We describe the survey execution with details that would be useful in the design of similar future surveys. We also present statistics on the achieved data quality, specifically?the point-spread function, sampling uniformity, spectral resolution, sky subtraction, and flux calibration. For our Primary sample, the median r-band signal-to-noise ratio is ~70 per 1.4 ? pixel for spectra stacked between 1Re and 1.5Re. Measurements of various galaxy properties from the first-year data show that we are meeting or exceeding the defined requirements for the majority of our science goals.
Keywordgalaxies: evolution galaxies: general surveys techniques: imaging spectroscopy
WOS IDIOP:0004-6256-152-6-197
PublisherThe American Astronomical Society
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Document Type期刊论文
Affiliation1.Department of Physics and Astronomy, University of Kentucky, 505 Rose Street, Lexington, KY 40506-0057, USA;
2.Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
3.Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
4.Department of Astronomy, University of Winsconsin-Madison, 475 N. Charter Street, Madison, WI 53706-1582, USA
5.Department of Physics and Astronomy and Pittsburgh Particle Physics, Astrophysics and Cosmology Center (PITT PACC), University of Pittsburgh, 3941 OHara Street, Pittsburgh, PA 15260, USA
6.Department of Physics and Astronomy, Johns Hopkins University, Bloomberg Center, 3400 N. Charles Street, Baltimore, MD 21218, USA
7.McDonald Observatory, University of Texas at Austin, 1 University Station, Austin, TX 78712-0259, USA
8.Department of Astronomy, Box 351580, University of Washington, Seattle, WA 98195, USA
9.Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth, UK
10.10Department of Physical Sciences, The Open University, Milton Keynes, MK7 6AA, UK
11.11School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK
12.12School of Physics and Astronomy, University of Nottingham, University Park, Nottingham NG7 2RD, UK
13.13Cavendish Laboratory, University of Cambridge, 19 J. J. Thomson Avenue, Cambridge CB3 0HE, UK
14.14Kavli Institute for Cosmology, University of Cambridge, Madingley Road, CB3 0HA Cambridge, UK
15.15Apache Point Observatory and New Mexico State University, P.O. Box 59, Sunspot, NM 88349, USA
16.16Sternberg Astronomical Institute, Moscow State University, Universitetskij pr. 13, Moscow, Russia
17.17Departamento de Astronoma, Universidad de Chile, Camino el Observatorio 1515, Las Condes, Santiago, Chile
18.18Centro de Astrofsica y Tecnologas Afines (CATA), Camino del Observatorio 1515, Las Condes, Santiago, Chile
19.19Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, NY 10003, USA
20.20Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA
21.21Sub-Department of Astrophysics, Department of Physics, University of Oxford, DenysWilkinson Building, Keble Road, Oxford OX1 3RH, UK
22.22Max Plank Institute for Astrophysics, Munich, D-85741, Garching, Germany
23.23European Southern Observatory, Karl-Schwarzschild-Strasse?2, D-85748 Garching, Germany
24.24Université Lyon 1, Observatoire de Lyon, Centre de Recherche Astrophysique de Lyon, 9 avenue Charles André, F-69561 Saint Genis Laval Cedex, France
25.25Ecole Normale Supérieure de Lyon, 9 avenue Charles André, F-69230 Saint-Genis Laval, France
26.26Department of Physics and Astronomy, 203 Van Allen Hall,?University of Iowa, Iowa City, IA 52242-1479, USA
27.27Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
28.28Department of Astronomy, Case Western Reserve University, Cleveland, OH 44106, USA
29.29Shanghai Astronomical Observatory, Nandan Road 80, Shanghai 200030, China
30.30Department of Physics and Tsinghua Center for Astrophysics, Tsinghua University, Beijing 100086, China
31.31National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, China
32.32University of Chinese Academy of Sciences, Beijing 100049, China
33.33Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester M13 9PL, UK
34.34Instituto de Astronomia, Universidad Nacional Autonoma deMexico, A.P. 70-264, 04510 Mexico D.F., Mexico
35.35Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720-8160, USA
36.36Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P5C2, Canada
37.37Max Planck Institute for Astronomy, K?nigstuhl 17, D-69117 Heidelberg, Germany
Recommended Citation
GB/T 7714
Yan,Renbin,Bundy,Kevin,Law,David R.,等. SDSS-IV MaNGA IFS GALAXY SURVEY—SURVEY DESIGN, EXECUTION, AND INITIAL DATA QUALITY[J]. The Astronomical Journal,2016,152(6).
APA Yan,Renbin.,Bundy,Kevin.,Law,David R..,Bershady,Matthew A..,Andrews,Brett.,...&Zheng,Zheng.(2016).SDSS-IV MaNGA IFS GALAXY SURVEY—SURVEY DESIGN, EXECUTION, AND INITIAL DATA QUALITY.The Astronomical Journal,152(6).
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