Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 501, Issue 1, Pages 948-953Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/staa3785
Keywords
ISM: general; galaxies: general; galaxies: ISM; galaxies: spiral; galaxies: statistics; galaxies: structure
Categories
Funding
- CONACYT [CB-285080, FC-2016-01-1916]
- Alfred P. Sloan Foundation
- U.S. Department of Energy Office of Science
- (UNAM) project [PAPIIT-DGAPA-IN100519]
- Brazilian Participation Group
- Carnegie Institution for Science
- Carnegie Mellon University
- Chilean Participation Group
- French Participation Group
- Harvard-Smithsonian Center for Astrophysics
- Instituto de Astrofisica de Canarias
- Johns Hopkins University
- Kavli Institute for the Physics and Mathematics of the Universe (IPMU) / University of Tokyo
- Lawrence Berkeley National Laboratory
- Leibniz Institut fur Astrophysik Potsdam (AIP)
- Max-Planck-Institut fur Astronomie (MPIA Heidelberg)
- Max-Planck-Institut fur Astrophysik (MPA Garching)
- Max-Planck-Institut fur Extraterrestrische Physik (MPE)
- National Astronomical Observatories of China
- New Mexico State University
- New York University
- University of Notre Dame
- Observatario Nacional / MCTI
- Ohio State University
- Pennsylvania State University
- Shanghai Astronomical Observatory
- United Kingdom Participation Group
- Universidad Nacional Autonoma de Mexico
- University of Arizona
- University of Colorado Boulder
- University of Oxford
- University of Portsmouth
- University of Utah
- University of Virginia
- University of Washington
- University of Wisconsin
- Vanderbilt University
- Yale University
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Gas-phase abundance gradients in galaxies have been found to vary systematically with galaxy size and mass, with smaller galaxies displaying flatter gradients than larger galaxies at a given stellar mass above 10^10 solar masses. This mass-size behavior cannot be explained by instrumental effects, and is not simply a reflection of known trends between gradients and morphology. Further investigation is needed to establish a firm physical interpretation for this pattern.
Gas-phase abundances and abundance gradients provide much information on past stellar generations, and are powerful probes of how galaxies evolve. Gas abundance gradients in galaxies have been studied as functions of galaxies' mass and size individually, but have largely not been considered across the galaxy mass-size plane. Thus, we investigate gas-phase abundance gradients across this plane, using a sample of over 1000 galaxies selected from the MApping Nearby Galaxies at APO (MaNGA) spectroscopic survey. We find that gradients vary systematically such that above 10(10) M-circle dot, smaller galaxies display flatter gradients than larger galaxies at a given stellar mass. This mass-size behaviour cannot be explained by instrumental effects, nor is it simply a reflection of known trends between gradients and morphology. We explore multiple possibilities for a physical origin for this pattern, though further work is needed to establish a firm physical interpretation.
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