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The impact of quenching on galaxy profiles in the SIMBA simulation

dc.contributor.authorDave, Romeel
dc.contributor.authorAppleby, Sarah
dc.contributor.authorKraljic, Katarina
dc.date.accessioned2021-02-08T12:26:18Z
dc.date.available2021-02-08T12:26:18Z
dc.date.issued2020
dc.identifier.citationDave, R. et al. (2020). The impact of quenching on galaxy profiles in the SIMBA simulation. Monthly Notices of the Royal Astronomical Society, 494(4), 6053–6071en_US
dc.identifier.issn1365-2966
dc.identifier.urihttps://doi.org/10.1093/mnras/staa1169
dc.identifier.urihttp://hdl.handle.net/10566/5863
dc.description.abstractWe study specific star formation rate (sSFR) and gas profiles of star-forming (SF) and green valley (GV) galaxies in the SIMBA cosmological hydrodynamic simulation. SF galaxy half-light radii (Rhalf) at z = 0 and their evolution (∝(1 + z)−0.78) agree with observations. Passive galaxy Rhalf agree with observations at high redshift, but by z = 0 are too large, owing to numerical heating. We compare SIMBAz = 0 sSFR radial profiles for SF and GV galaxies to observations. SIMBA shows strong central depressions in star formation rate (SFR), sSFR, and gas fraction in GV galaxies and massive SF systems, qualitatively as observed, owing to black hole X-ray feedback, which pushes central gas outwards.en_US
dc.language.isoenen_US
dc.publisherOxford University Pressen_US
dc.subjectGalaxies: evolutionen_US
dc.subjectGalaxies: formationen_US
dc.subjectGalaxies: jetsen_US
dc.subjectGalaxies: spiralen_US
dc.subjectGalaxies: structureen_US
dc.titleThe impact of quenching on galaxy profiles in the SIMBA simulationen_US
dc.typeArticleen_US


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