Abstract
We study the internal gradients of stellar population propertieswithin 1.5 Re for a representative sample of 721 galaxies, with stellar masses ranging between 109M⊙ and 1011.5M⊙ from the SDSS-IV MaNGA Integral-Field-Unit survey. Through the use of our full spectral fitting code FIREFLY, we derive light- and mass-weighted stellar population properties and their radial gradients, as well as full star formation and metal enrichment histories. We also quantify the impact that different stellar population models and full spectral fitting routines have on the derived stellar population properties and the radial gradient measurements. In our analysis, we find that age gradients tend to be shallow for both early-type and late-type galaxies. Mass-weighted age gradients of early-types arepositive (~0.09 dex/Re) pointing to 'outside- in' progression of star formation, while late-type galaxies have negative light-weighted age gradients (~-0.11 dex/Re), suggesting an 'inside-out' formation of discs. We detect negative metallicity gradients in both early- and late-type galaxies, but these are significantly steeper in late-types, suggesting that the radial dependence of chemical enrichment processes and the effect of gas inflow and metal transport are far more pronounced in discs. Metallicity gradients of both morphological classes correlate with galaxy mass, with negative metallicity gradients becoming steeper with increasing galaxy mass. The correlation with mass is stronger for late-type galaxies, with a slope of d(∇[Z/H])/d(logM) ~ -0.2 ± 0.05, compared to d(∇[Z/H])/d(logM) ~ -0.05 ± 0.05 for early-types. This result suggests that the merger history plays a relatively small role in shaping metallicity gradients of galaxies.
| Original language | English |
|---|---|
| Pages (from-to) | 4731-4758 |
| Number of pages | 28 |
| Journal | Monthly Notices of the Royal Astronomical Society |
| Volume | 466 |
| Issue number | 4 |
| DOIs | |
| State | Published - 2017 |
Bibliographical note
Funding Information:The authors would like to thank Alfonso Aragon-Salamanca and Matthew Withers for fruitful discussions. DG is supported by an STFC PhD studentship. MAB acknowledges NSF AST-1517006. AW acknowledges support from a Leverhulme Early Career Fellowship. DB is supported by grant RSCF-14-22-00041. RR thanks CNPq and Fapergs for financial support. RM acknowledges support by the Science and Technology Facilities Council (STFC) and the ERCAdvanced Grant 695671 'QUENCH'.Numerical computations were done on the Sciama High Performance Compute (HPC) cluster, which is supported by the Institute of Cosmology of Gravitation, SEPNet and the University of Portsmouth. Funding for the SDSS IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org. SDSSIV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofísica 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 fór Astrophysik Potsdam (AIP), Max-Planck-Institut fór Astronomie (MPIA Heidelberg), Max-Planck-Institut fór Astrophysik (MPA Garching), Max-Planck-Institut fór Extraterrestrische Physik (MPE), National Astronomical Observatory of China, New Mexico State University, New York University, University of Notre Dame, Observatório Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University ofVirginia, University ofWashington, University ofWisconsin, Vanderbilt University and Yale University. All data taken as part of SDSS-IV are scheduled to be released to the community in fully reduced form at regular intervals through dedicated data releases. The first MaNGA data release was part of the SDSS data release 13 (release date 2016 July 31).
Funding Information:
The authors would like to thank Alfonso Aragon-Salamanca and Matthew Withers for fruitful discussions. DG is supported by an STFC PhD studentship. MAB acknowledges NSF AST-1517006. AW acknowledges support from a Leverhulme Early Career Fellowship. DB is supported by grant RSCF-14-22-00041. RR thanks CNPq and Fapergs for financial support. RM acknowledges support by the Science and Technology Facilities Council (STFC) and the ERCAdvanced Grant 695671 'QUENCH'.Numerical computations were done on the Sciama High Performance Compute (HPC) cluster, which is supported by the Institute of Cosmology of Gravitation, SEPNet and the University of Portsmouth. Funding for the SDSS IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org. SDSSIV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrof?sica 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 f?r Astrophysik Potsdam (AIP), Max-Planck-Institut f?r Astronomie (MPIA Heidelberg), Max-Planck-Institut f?r Astrophysik (MPA Garching), Max-Planck-Institut f?r Extraterrestrische Physik (MPE), National Astronomical Observatory of China, New Mexico State University, New York University, University of Notre Dame, Observat?rio Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Aut?noma de M?xico, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University ofVirginia, University ofWashington, University ofWisconsin, Vanderbilt University and Yale University. All data taken as part of SDSS-IV are scheduled to be released to the community in fully reduced form at regular intervals through dedicated data releases. The first MaNGA data release was part of the SDSS data release 13 (release date 2016 July 31).
Publisher Copyright:
© 2016 The Authors.
Keywords
- CD
- Galaxies: elliptical and lenticular
- Galaxies: evolution
- Galaxies: formation
- Galaxies: spiral
- Galaxies: star formation
- Galaxies: stellar content
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science