Die Hard: The On-Off-Cycle of Galaxies on the Star Formation Main Sequence
arXiv:2503.20858 · doi:10.1051/0004-6361/202554805
Abstract
Our picture of galaxy evolution currently assumes that galaxies spend their life on the star formation main sequence (SFMS) until they are eventually quenched. However, recent observations show indications that the full picture might be more complicated. We reveal typical in-situ star formation histories and their relations to large-scale environment as well as gas accretion across cosmic time. We follow the evolution of central galaxies in the highest-resolution box of the Magneticum Pathfinder cosmological hydrodynamical simulations and classify their evolution scenarios with respect to the SFMS. We find that a major fraction of the galaxies undergoes long-term cycles of quenching and rejuvenation on gigayear timescales. This expands the framework of galaxy evolution from a secular evolution to a sequence of multiple active and passive phases. Only 14% of field galaxies on the SFMS at z=0 actually evolved along the scaling relation, while the bulk of star-forming galaxies in the local Universe have undergone cycles of quenching and rejuvenation. In this work we describe the statistics of these galaxy evolution modes and how this impacts their mean stellar masses, ages, and metallicities today. We further explore possible explanations and find that the geometry of gas accretion at the halo outskirts shows a strong correlation with the star formation rate (SFR) evolution, while the density parameter as a tracer of environment shows no significant correlation. A derivation of SFRs from gas accretion with simple assumptions only works in the high-z universe, where accreted gas is quickly converted into stars. We conclude that an evolution scenario consistently on the SFMS is the exception, when regarding galaxies on the SFMS at z=0. Galaxies with rejuvenation cycles can be distinguished well from SFMS-evolved galaxies, both in their halo accretion modes and in their features at z=0.
arXiv comment17 pages, 15 figures; published in A&A
References in corpus (74)
- Stellar population synthesis at the resolution of 2003
- Galactic Stellar and Substellar Initial Mass Function
- Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation
- On the variation of the Initial Mass Function
- The cosmological simulation code GADGET-2
- Coevolution (Or Not) of Supermassive Black Holes and Host Galaxies
- Cosmic Star Formation History
- Energy input from quasars regulates the growth and activity of black holes and their host galaxies
- The physical properties of star forming galaxies in the low redshift universe
- Populating a cluster of galaxies - I. Results at z=0
- Theory of Star Formation
- Cosmological SPH simulations: A hybrid multi-phase model for star formation
- Modeling feedback from stars and black holes in galaxy mergers
- The Average Star Formation Histories of Galaxies in Dark Matter Halos from z=0-8
- Star Formation in AEGIS Field Galaxies since z=1.1 : The Dominance of Gradually Declining Star Formation, and the Main Sequence of Star-Forming Galaxies
- Galaxy Bimodality due to Cold Flows and Shock Heating
- Cold streams in early massive hot haloes as the main mode of galaxy formation
- GADGET: A code for collisionless and gasdynamical cosmological simulations
- Color Separation of Galaxy Types in the Sloan Digital Sky Survey Imaging Data
- Small-Scale Challenges to the CDM Paradigm
- A Highly Consistent Framework for the Evolution of the Star-Forming "Main Sequence" from z~0-6
- The Circumgalactic Medium
- Virial shocks in galactic haloes?
- Substructures in hydrodynamical cluster simulations
- A General Theory of Turbulence-Regulated Star Formation, From Spirals to ULIRGs
- The Star-formation Mass Sequence out to z=2.5
- Gas-regulation of galaxies: the evolution of the cosmic sSFR, the metallicity-mass-SFR relation and the stellar content of haloes
- On the Star Formation Rates in Molecular Clouds
- Chemical enrichment in cosmological, smoothed particle hydrodynamics simulations
- The bimodal galaxy color distribution: dependence on luminosity and environment
- Slow Star Formation in Dense Gas: Evidence and Implications
- The Impact of cold gas accretion above a mass floor on galaxy scaling relations
- Mass, Metal, and Energy Feedback in Cosmological Simulations
- A Universal, Local Star Formation Law in Galactic Clouds, Nearby Galaxies, High-Redshift Disks, and Starbursts
- The Star Formation Rate and Gas Surface Density Relation in the Milky Way: Implications for Extragalactic Studies
- Structure and star formation in galaxies out to z=3: evidence for surface density dependent evolution and upsizing
- The Evolution of the Star-forming Interstellar Medium across Cosmic Time
- Cosmological simulations of black hole growth: AGN luminosities and downsizing
- The UV-optical Galaxy Color-Magnitude Diagram I: Basic Properties
- Chemical enrichment of galaxy clusters from hydrodynamical simulations
- The Confinement of Star-Forming Galaxies into a Main Sequence through Episodes of Gas Compaction, Depletion, and Replenishment
- Turbulent gas motions in galaxy cluster simulations: The role of SPH viscosity
- The Main Sequence of star-forming galaxies across cosmic times
- GALEX UV Color-Magnitude Relations and Evidence for Recent Star Formation in Early-type Galaxies
- A Model of Supernovae Feedback in Galaxy Formation
- The star-formation activity of IllustrisTNG galaxies: main sequence, UVJ diagram, quenched fractions, and systematics
- Simulating the effect of AGN feedback on the metal enrichment of galaxy clusters
- Connecting Angular Momentum and Galactic Dynamics: The complex Interplay between Spin, Mass, and Morphology
- The Hydrangea simulations: galaxy formation in and around massive clusters
- The Star Formation Main Sequence in the Hubble Space Telescope Frontier Fields
- Gravitational Quenching in Massive Galaxies and Clusters by Clumpy Accretion
- Fuel Efficient Galaxies: Sustaining Star Formation with Stellar Mass Loss
- Thermal Conduction in Simulated Galaxy Clusters
- Main sequence of star forming galaxies beyond the Herschel confusion limit
- Rise and Fall of Radio Halos in Simulated Merging Galaxy Clusters
- The VLA-COSMOS 3 GHz Large Project: Evolution of specific star formation rates out to
- Galactic outflow rates in the EAGLE simulations
- The Star Formation Efficiency per Free Fall Time in Nearby Galaxies
- Cooling and heating the ICM in hydrodynamical simulations
- Gone after one orbit: How cluster environments quench galaxies
- Kinematics of Simulated Galaxies I: Connecting Dynamical and Morphological Properties of Early-Type Galaxies at Different Redshifts
- The SAMI Galaxy Survey: comparing 3D spectroscopic observations with galaxies from cosmological hydrodynamical simulations
- Timing the earliest quenching events with a robust sample of massive quiescent galaxies at 2 < z < 5
- Galaxy mergers can rapidly shut down star formation
- Rejuvenation in quiescent galaxies in LEGA-C
- GOODS-ALMA 2.0: Starbursts in the main sequence reveal compact star formation regulating galaxy evolution prequenching
- The Morphology-Density-Relation: Impact on the Satellite Fraction
- Accreted or Not Accreted? The Fraction of Accreted Mass in Galaxies from Simulations and Observations
- Massive quiescent galaxies at : a comparison of selection, stellar population and structural properties with simulation predictions
- Galaxy Lookback Evolution Models -- a Comparison with Magneticum Cosmological Simulations and Observations
- A simple spectroscopic technique to identify rejuvenating galaxies
- Galaxy shapes in Magneticum. I. Connecting stellar and dark matter shapes to dynamical and morphological galaxy properties and the large-scale structure
- How the cool-core population transitions from galaxy groups to massive clusters: A comparison of the largest Magneticum simulation with eROSITA, XMM-Newton, Chandra and LOFAR observations
- Go with the Flow: The Self-Similar and Non-Linear Behaviour of Large-Scale In- and Outflows and the Impact of Accretion Shocks from Galaxies to Galaxy Clusters