Renbin Yan, Kevin Bundy, David R. Law, Matthew A. Bershady, Brett Andrews, Brian Cherinka, Aleksandar M. Diamond-Stanic, Niv Drory, Nicholas MacDonald, José R. Sánchez-Gallego, Daniel Thomas, David A. Wake, Anne Marie Weijmans, Kyle B. Westfall, Kai Zhang, Alfonso Aragón-Salamanca, Francesco Belfiore, Dmitry Bizyaev, Guillermo A. Blanc, Michael R. BlantonJoel Brownstein, Michele Cappellari, Richard D'Souza, Eric Emsellem, Hai Fu, Patrick Gaulme, Mark T. Graham, Daniel Goddard, James E. Gunn, Paul Harding, Amy Jones, Karen Kinemuchi, Cheng Li, Hongyu Li, Roberto Maiolino, Shude Mao, Claudia Maraston, Karen Masters, Michael R. Merrifield, Daniel Oravetz, Kaike Pan, John K. Parejko, Sebastian F. Sanchez, David Schlegel, Audrey Simmons, Karun Thanjavur, Jeremy Tinker, Christy Tremonti, Remco Van Den Bosch, Zheng Zheng

Research output: Contribution to journalArticlepeer-review

213 Scopus citations


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 Å. 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 (R e) while maximizing spatial resolution. About two-thirds of the sample is covered out to 1.5R e (Primary sample), and one-third of the sample is covered to 2.5R e (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 Å pixel for spectra stacked between 1R e and 1.5R e. 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.

Original languageEnglish
Article number197
JournalAstronomical Journal
Issue number6
StatePublished - Dec 2016

Bibliographical note

Funding Information:
K.B. is supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. M.A.B. acknowledges support by grant NSF/AST 1517007. A.W. acknowledges support of a Leverhulme Trust Early Career Fellowship. A.D. acknowledges support from the Grainger Foundation. D.B. acknowledges support by grant RSF 14-50-00043. M.C. acknowledges support from a Royal Society University Research Fellowship.

Publisher Copyright:
© 2016. The American Astronomical Society. All rights reserved.


  • galaxies: evolution
  • galaxies: general
  • surveys
  • techniques: imaging spectroscopy

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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