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SDSS-IV MaNGA IFS galaxy survey-survey design, execution, and initial data quality

Research output: Contribution to journalArticle

  • 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
  • David A. Wake
  • Anne-Marie Weijmans
  • Kyle B. Westfall
  • Kai Zhang
  • Alfonso Aragón-Salamanca
  • Francesco Belfiore
  • Dmitry Bizyaev
  • Guillermo A. Blanc
  • Michael R. Blanton
  • Joel 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
  • 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
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 (IFS) for 10K nearby galaxies at a spectral resolution of R~2000 from 3,622-10,354A. 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 2/3 of the sample is covered out to 1.5Re (Primary sample), and 1/3 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 ~73 per 1.4A pixel for spectra stacked between 1-1.5 Re. 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
JournalThe Astronomical Journal
Volume152
Issue number6
DOIs
Publication statusPublished - 29 Nov 2016

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