SDSS-IV MaNGA: Evidence for Enriched Accretion onto Satellite Galaxies in Dense Environments
We investigate the environmental dependence of the local gas-phase metallicity in a sample of star-forming galaxies from the MaNGA survey. Satellite galaxies with stellar masses in the range are found to be ∼0.05 dex higher in metallicity than centrals of similar stellar mass. Within the low-mass sa...
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| Veröffentlicht in: | The Astrophysical journal 2019-10, Vol.884 (2), p.156 |
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| creator | Schaefer, Adam L. Tremonti, Christy Pace, Zachary Belfiore, Francesco Argudo-Fernandez, Maria Bershady, Matthew A. Drory, Niv Jones, Amy Maiolino, Roberto Stark, David Wake, David Yan, Renbin |
| description | We investigate the environmental dependence of the local gas-phase metallicity in a sample of star-forming galaxies from the MaNGA survey. Satellite galaxies with stellar masses in the range are found to be ∼0.05 dex higher in metallicity than centrals of similar stellar mass. Within the low-mass satellite population, we find that the interstellar medium (ISM) metallicity depends most strongly on the stellar mass of the galaxy that is central to the halo, though there is no obvious difference in the metallicity gradients. At fixed total stellar mass, the satellites of high-mass (M* > 1010.5 M ) centrals are ∼0.1 dex more metal-rich than the satellites of low-mass (M* < 1010 M ) centrals, controlling for local stellar mass surface density and gas fraction. Fitting a gas regulator model to the spaxel data, we are able to account for variations in the local gas fraction, stellar mass surface density, and local escape velocity-dependent outflows. We find that the best explanation for the metallicity differences is the variation in the average metallicity of accreted gas between different environments that depends on the stellar mass of the dominant galaxies in each halo. This is interpreted as evidence for the exchange of enriched gas between galaxies in dense environments that is predicted by recent simulations. |
| doi_str_mv | 10.3847/1538-4357/ab43ca |
| format | Article |
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Satellite galaxies with stellar masses in the range are found to be ∼0.05 dex higher in metallicity than centrals of similar stellar mass. Within the low-mass satellite population, we find that the interstellar medium (ISM) metallicity depends most strongly on the stellar mass of the galaxy that is central to the halo, though there is no obvious difference in the metallicity gradients. At fixed total stellar mass, the satellites of high-mass (M* > 1010.5 M ) centrals are ∼0.1 dex more metal-rich than the satellites of low-mass (M* < 1010 M ) centrals, controlling for local stellar mass surface density and gas fraction. Fitting a gas regulator model to the spaxel data, we are able to account for variations in the local gas fraction, stellar mass surface density, and local escape velocity-dependent outflows. We find that the best explanation for the metallicity differences is the variation in the average metallicity of accreted gas between different environments that depends on the stellar mass of the dominant galaxies in each halo. This is interpreted as evidence for the exchange of enriched gas between galaxies in dense environments that is predicted by recent simulations.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/ab43ca</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Astrophysics ; Computer simulation ; Density ; Deposition ; Escape velocity ; Galactic abundances ; Galaxies ; Galaxy accretion ; Galaxy environments ; Galaxy evolution ; Intergalactic abundances ; Intergalactic gas ; Interstellar matter ; Interstellar medium ; Metallicity ; Satellites ; Scaling relations ; Spectroscopy ; Star formation ; Stars & galaxies ; Stellar mass</subject><ispartof>The Astrophysical journal, 2019-10, Vol.884 (2), p.156</ispartof><rights>2019. The American Astronomical Society. 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We find that the best explanation for the metallicity differences is the variation in the average metallicity of accreted gas between different environments that depends on the stellar mass of the dominant galaxies in each halo. 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Tremonti, Christy ; Pace, Zachary ; Belfiore, Francesco ; Argudo-Fernandez, Maria ; Bershady, Matthew A. ; Drory, Niv ; Jones, Amy ; Maiolino, Roberto ; Stark, David ; Wake, David ; Yan, Renbin</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c380t-87a2070182d9c7030adc9af2eff3c7b6d1e4a1935e2f2a42821c2740017967fb3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2019</creationdate><topic>Astrophysics</topic><topic>Computer simulation</topic><topic>Density</topic><topic>Deposition</topic><topic>Escape velocity</topic><topic>Galactic abundances</topic><topic>Galaxies</topic><topic>Galaxy accretion</topic><topic>Galaxy environments</topic><topic>Galaxy evolution</topic><topic>Intergalactic abundances</topic><topic>Intergalactic gas</topic><topic>Interstellar matter</topic><topic>Interstellar medium</topic><topic>Metallicity</topic><topic>Satellites</topic><topic>Scaling relations</topic><topic>Spectroscopy</topic><topic>Star formation</topic><topic>Stars & galaxies</topic><topic>Stellar mass</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Schaefer, Adam L.</creatorcontrib><creatorcontrib>Tremonti, Christy</creatorcontrib><creatorcontrib>Pace, Zachary</creatorcontrib><creatorcontrib>Belfiore, Francesco</creatorcontrib><creatorcontrib>Argudo-Fernandez, Maria</creatorcontrib><creatorcontrib>Bershady, Matthew A.</creatorcontrib><creatorcontrib>Drory, Niv</creatorcontrib><creatorcontrib>Jones, Amy</creatorcontrib><creatorcontrib>Maiolino, Roberto</creatorcontrib><creatorcontrib>Stark, David</creatorcontrib><creatorcontrib>Wake, David</creatorcontrib><creatorcontrib>Yan, Renbin</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Schaefer, Adam L.</au><au>Tremonti, Christy</au><au>Pace, Zachary</au><au>Belfiore, Francesco</au><au>Argudo-Fernandez, Maria</au><au>Bershady, Matthew A.</au><au>Drory, Niv</au><au>Jones, Amy</au><au>Maiolino, Roberto</au><au>Stark, David</au><au>Wake, David</au><au>Yan, Renbin</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>SDSS-IV MaNGA: Evidence for Enriched Accretion onto Satellite Galaxies in Dense Environments</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. 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| subjects | Astrophysics Computer simulation Density Deposition Escape velocity Galactic abundances Galaxies Galaxy accretion Galaxy environments Galaxy evolution Intergalactic abundances Intergalactic gas Interstellar matter Interstellar medium Metallicity Satellites Scaling relations Spectroscopy Star formation Stars & galaxies Stellar mass |
| title | SDSS-IV MaNGA: Evidence for Enriched Accretion onto Satellite Galaxies in Dense Environments |
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