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

Yan, Renbin and Bundy, Kevin and Law, David R. and Bershady, Matthew A. and Andrews, Brett and Cherinka, Brian and Diamond-Stanic, Aleksandar M. and Drory, Niv and MacDonald, Nicholas and Sánchez-Gallego, José R. and Thomas, Daniel and Wake, David A. and Weijmans, Anne-Marie and Westfall, Kyle B. and Zhang, Kai and Aragón-Salamanca, Alfonso and Belfiore, Francesco and Bizyaev, Dmitry and Blanc, Guillermo A. and Blanton, Michael R. and Brownstein, Joel and Cappellari, Michele and D’Souza, Richard and Emsellem, Eric and Fu, Hai and Gaulme, Patrick and Graham, Mark T. and Goddard, Daniel and Gunn, James E. and Harding, Paul and Jones, Amy and Kinemuchi, Karen and Li, Cheng and Li, Hongyu and Maiolino, Roberto and Mao, Shude and Maraston, Claudia and Masters, Karen and Merrifield, Michael R. and Oravetz, Daniel and Pan, Kaike and Parejko, John K. and Sanchez, Sebastian F. and Schlegel, David and Simmons, Audrey and Thanjavur, Karun and Tinker, Jeremy and Tremonti, Christy and van den Bosch, Remco and Zheng, Zheng (2016) SDSS-IV MaNGA IFS galaxy survey—survey design, execution, and initial data quality. The Astronomical Journal, 152 (6). 197/1-197/32. ISSN 1538-3881

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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 (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 Å 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.

Item Type: Article
Keywords: galaxies: evolution; galaxies: general; surveys; techniques: imaging spectroscopy
Schools/Departments: University of Nottingham, UK > Faculty of Science > School of Physics and Astronomy
Identification Number:
Depositing User: Aragon-salamanca, Alfonso
Date Deposited: 11 Jan 2017 09:01
Last Modified: 04 May 2020 18:19

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