In TNG100-1, close pericentric passages enhance central sSFR by 1.6x, peaking ~0.1 Gyr later, with about 70% of the boost attributed to increased star formation efficiency rather than increased gas supply.
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7 Pith papers cite this work, alongside 76 external citations. Polarity classification is still indexing.
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In simulated major galaxy pairs, central kiloparsec star formation enhancement is mostly fuel-driven and suppression is mostly efficiency-driven, with the secondary galaxy more centrally concentrated than the primary.
New CO survey of 62 CALIFA galaxies shows median molecular gas depletion times rising from 2.1 Gyr on the main sequence to 128 Gyr in red galaxies, with SFE declining systematically below the SFMS independent of CO-to-H2 conversion factor choice.
Simulations show observationally selected protocluster candidates at z ≳ 5 include significant interlopers, undergo 2-6 major mergers, and exhibit stronger clustering than observed, requiring total galaxy mass within 10 cMpc for reliable progenitor identification.
Galaxies' recent star-formation histories vary strongly across the sSFR-M* plane, and the evolution of the star-forming sequence results from changing contributions of increasing, constant, and declining star-formation populations.
In TNG50, the resolved star-forming main sequence has slope 0.30, much shallower than observed, while the resolved mass-metallicity relation matches data; both can be described by a leaky-box model that prefers low net outflows.
In FIRE-2 simulations, the torque from major companion galaxies correlates with elevated star formation, but the majority of starbursts in Milky Way-mass galaxies are not triggered by galaxy interactions.
citing papers explorer
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Interacting galaxies in the IllustrisTNG simulations -- VIII: Pericentric star formation rate enhancements are driven both by increased fuelling and efficiency
In TNG100-1, close pericentric passages enhance central sSFR by 1.6x, peaking ~0.1 Gyr later, with about 70% of the boost attributed to increased star formation efficiency rather than increased gas supply.
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Spatially resolved star formation and fuelling in galaxy interactions
In simulated major galaxy pairs, central kiloparsec star formation enhancement is mostly fuel-driven and suppression is mostly efficiency-driven, with the secondary galaxy more centrally concentrated than the primary.
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The EDGE-CALIFA Survey: Star Formation Efficiency and Galaxy Quenching across 62 Main Sequence, Green Valley, and Red Galaxies
New CO survey of 62 CALIFA galaxies shows median molecular gas depletion times rising from 2.1 Gyr on the main sequence to 128 Gyr in red galaxies, with SFE declining systematically below the SFMS independent of CO-to-H2 conversion factor choice.
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On the later evolution of observationally selected protocluster candidates at $z\,{\gtrsim}\,5$
Simulations show observationally selected protocluster candidates at z ≳ 5 include significant interlopers, undergo 2-6 major mergers, and exhibit stronger clustering than observed, requiring total galaxy mass within 10 cMpc for reliable progenitor identification.
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Deep Extragalactic VIsible Legacy Survey (DEVILS): The sSFR-M$_{\star}$plane part I: The recent SFH of galaxies and movement through the plane
Galaxies' recent star-formation histories vary strongly across the sSFR-M* plane, and the evolution of the star-forming sequence results from changing contributions of increasing, constant, and declining star-formation populations.
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Star Formation Rates, Metallicities, and Stellar Masses on kpc-scales in TNG50
In TNG50, the resolved star-forming main sequence has slope 0.30, much shallower than observed, while the resolved mass-metallicity relation matches data; both can be described by a leaky-box model that prefers low net outflows.
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The Effect of Galaxy Interactions on Starbursts in Milky Way-Mass Galaxies in FIRE Simulations
In FIRE-2 simulations, the torque from major companion galaxies correlates with elevated star formation, but the majority of starbursts in Milky Way-mass galaxies are not triggered by galaxy interactions.