期刊
ASTROPHYSICAL JOURNAL
卷 897, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/ab94af
关键词
Galaxy abundances; Galaxy evolution; Galaxy chemical evolution; Interstellar medium; Interstellar emissions
资金
- National Key R&D Program of China [2017YFA0402600]
- B-type Strategic Priority Program of the Chinese Academy of Sciences [XDB41000000]
- National Natural Science Foundation of China (NSFC) [11421303, 11973038]
- CAS-TWAS President's Fellowship
- China Scholarship Council [201906340095]
- Alfred P. Sloan Foundation
- U.S. Department of Energy Office of Science
- Center for High-Performance Computing at the University of Utah
- Brazilian Participation Group
- Carnegie Institution for Science
- Carnegie Mellon University
- Chilean Participation Group
- French Participation Group
- Harvard-Smithsonian Center for Astrophysics
- Instituto de Astrofsica de Canarias
- The Johns Hopkins University
- Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo
- Lawrence Berkeley National Laboratory
- Leibniz Institut fr Astrophysik Potsdam (AIP)
- Max-Planck-Institut fr Astronomie (MPIA Heidelberg)
- Max-Planck-Institut fr Astrophysik (MPA Garching)
- Max-PlanckInstitut fr Extraterrestrische Physik (MPE)
- National Astronomcal Observatory of China
- New Mexico State University
- New York University
- University of Notre Dame
- Observatao Nacional/MCTI
- The 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
We study the relations between gas-phase metallicity (Z), local stellar mass surface density (sigma(*)), and the local star formation surface density (sigma(SFR)) in a sample of 1120 star-forming galaxies from the MaNGA survey. At fixed sigma(*)the local metallicity increases as sigma(SFR)decreases or vice versa for metallicity calibrators of N2 and O3N2. Alternatively, at fixed sigma(SFR)metallicity increases as sigma(*)increases, but in the high mass region, the trend is flatter. However, the dependence of metallicity on sigma(SFR)nearly disappears for N2O2 and N2S2 calibrators. We investigate the local metallicity against sigma(SFR)with different metallicity calibrators and find negative/positive correlations depending on the choice of the calibrator. We demonstrate that the O32 ratio (or ionization parameter) is probably dependent on star formation rate at fixed local stellar mass surface density. Additionally, the shape of sigma(*)-Z-sigma(SFR)(fundamental metallicity relation; FMR) depends on metallicity calibrator and stellar mass range. Due to the large discrepancy between the empirical fitting-based (N2, O3N2) electronic temperature metallicity and the photoionization model-dependent (N2O2, N2S2) metallicity calibrations, we conclude that the selection of metallicity calibration affects the existence of FMR on sigma(SFR).
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