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| MaNGA (survey) | |
|---|---|
| Name | MaNGA |
| Acronym | MaNGA |
| Mission type | Astronomical survey |
| Operator | Sloan Digital Sky Survey Collaboration |
| Instruments | Integral Field Units on the 2.5 m Sloan Foundation Telescope |
| Wavelength | Optical |
| Survey area | Northern Hemisphere sky (SDSS footprint) |
| Start date | 2014 |
| End date | ongoing (as of 2020s) |
MaNGA (survey) is an integral-field spectroscopic survey of nearby galaxies carried out as part of the Sloan Digital Sky Survey IV project led by the Apache Point Observatory community and the Harvard & Smithsonian. The survey obtained spatially resolved spectroscopy across thousands of galaxies using fiber bundle technology mounted on the Sloan Foundation Telescope at Apache Point Observatory. MaNGA operated within a collaborative framework involving institutions such as the University of Washington, Princeton University, New Mexico State University, and the University of Oxford.
MaNGA aimed to map the internal kinematics, stellar populations, and ionized gas properties of ~10,000 galaxies drawn from the Sloan Digital Sky Survey imaging catalogs and ancillary data from the Two Micron All Sky Survey and the Wide-field Infrared Survey Explorer. The program interfaced with legacy programs including SDSS-III, BOSS, and eBOSS, and worked alongside surveys like CALIFA and SAMI to provide complementary spatially resolved spectroscopy. Leadership, funding, and technical contributions came from groups such as the National Science Foundation, the Kavli Foundation, Carnegie Institution for Science, and the Max Planck Society.
MaNGA used custom-built fiber integral field units (IFUs) feeding the BOSS spectrographs mounted on the 2.5-meter Sloan Foundation Telescope. The IFU designs included bundles of 19 to 127 fibers manufactured by teams at the University of Wisconsin–Madison and the University of Oxford instrumentation groups. Spectral coverage spanned wavelengths observed by the BOSS CCDs with spectral resolution facilitating studies similar to those enabled by the Keck Observatory instruments and the Very Large Telescope spectrographs. The survey design leveraged calibration strategies developed with input from the Space Telescope Science Institute and tested on instrumentation projects at Palomar Observatory and Kitt Peak National Observatory.
Targets were selected from the NASA-Sloan Atlas and the parent SDSS Legacy Survey to provide a flat distribution in stellar mass and a broad sampling across the Hubble sequence including ellipticals, spirals, lenticulars, and irregulars. The MaNGA sample encompassed environments traced by memberships in groups cataloged by the Yang et al. group catalog and clusters such as Coma Cluster and Virgo Cluster. Stellar mass estimates used photometry tied to calibrations from the Two Micron All Sky Survey and stellar population synthesis models developed by teams at Bruzual & Charlot and Maraston. Ancillary catalogs included cross-matches to GALEX, FIRST, NVSS, and the ROSAT X-ray catalogs to characterize star formation, active galactic nuclei (AGN), and hot gas content.
Observations were scheduled through the Apache Point Observatory queue to obtain target exposure times yielding uniform signal-to-noise ratios across effective radii, employing dithering strategies developed with instrument teams from Carnegie Mellon University and University of Tokyo. Data reduction pipelines were developed by software teams from University of Colorado Boulder and University of Portsmouth and built on algorithms previously used for SDSS spectroscopic reductions. The MaNGA Data Reduction Pipeline produced sky-subtracted, flux-calibrated datacubes; further analysis used the Data Analysis Pipeline developed by collaborators at Stanford University and the Max Planck Institute for Astronomy.
Public data releases followed the SDSS data release schedule and distributed raw frames, reduced datacubes, and value-added catalogs via the Sloan Digital Sky Survey data archive servers. Value-added products included emission-line flux maps, stellar kinematic maps, and resolved stellar population fits contributed by teams at MPIA, University of Oxford, University of Porto, and Carnegie Observatories. Data releases were accompanied by documentation authored by members of the SDSS Collaboration and were widely used in follow-up studies by groups at Harvard University, Yale University, University of California, Berkeley, and University of Michigan.
MaNGA pursued goals including mapping baryonic angular momentum, constraining inside-out quenching, characterizing radial metallicity gradients, and diagnosing feedback from star formation and AGN in relation to halo properties traced by group catalogs from Yang et al.. Key results include measurements of resolved star-formation main sequence trends reported by teams at University of St Andrews and University of Edinburgh, identification of kinematic misalignments in recent analyses by researchers at University of Tokyo, constraints on stellar initial mass function variations presented by groups at University of Cambridge and University of Oxford, and statistical studies of compact quenched cores similar to findings from HST imaging teams and follow-up IFU programs at Gemini Observatory and Subaru Telescope.
MaNGA was embedded in the Sloan Digital Sky Survey IV collaboration and collaborated with large institutions including Princeton University, New York University, University of Chicago, University of Arizona, and the University of Toronto. The survey's legacy is visible in synergies with space missions and observatories such as Hubble Space Telescope, Chandra X-ray Observatory, Spitzer Space Telescope, and ground-based arrays like ALMA and VLA. MaNGA-trained analysis tools and calibration methods influenced subsequent IFU projects and informed proposals to facilities including JWST and Euclid. The dataset continues to support work by early-career researchers and consortia at institutions like Carnegie Mellon University and University College London and feeds into theoretical comparisons with cosmological simulations run by teams at Illustris, EAGLE, and the Millennium Simulation consortium.
Category:Astronomical surveys