Hydrodynamic simulations show that dark matter heating strongly suppresses the circumgalactic medium column densities of neutral hydrogen and metal ions in dwarf galaxies, offering a new observational probe.
The physical origin of long gas depletion times in galaxies
7 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
abstract
We present a model that explains why galaxies form stars on a time scale significantly longer than the time scales of processes governing the evolution of interstellar gas. We show that gas evolves from a non-star-forming to a star-forming state on a relatively short time scale and thus the rate of this evolution does not limit the star formation rate. Instead, the star formation rate is limited because only a small fraction of star-forming gas is converted into stars before star-forming regions are dispersed by feedback and dynamical processes. Thus, gas cycles into and out of star-forming state multiple times, which results in a long time scale on which galaxies convert gas into stars. Our model does not rely on the assumption of equilibrium and can be used to interpret trends of depletion times with the properties of observed galaxies and the parameters of star formation and feedback recipes in simulations. In particular, the model explains how feedback self-regulates the star formation rate in simulations and makes it insensitive to the local star formation efficiency. We illustrate our model using the results of an isolated $L_*$-sized galaxy simulation that reproduces the observed Kennicutt-Schmidt relation for both molecular and atomic gas. Interestingly, the relation for molecular gas is almost linear on kiloparsec scales, although a nonlinear relation is adopted in simulation cells. We discuss how a linear relation emerges from non-self-similar scaling of the gas density PDF with the average gas surface density.
years
2026 7representative citing papers
Simulations with realistic patchy reionization show that the diversity of ultra-faint dwarf galaxies is primarily controlled by the halo mass at the moment of reionization.
In simulated high-redshift galaxies, stellar mass is smooth while young-star light (Halpha, FUV, optical) is clumpy on 0.1-1 kpc scales, with clumpiness tracking bursty star formation and feedback strength.
Sites of stripped-envelope supernovae have about eight times higher star formation efficiency than sites of hydrogen-rich supernovae, measured at cloud-scale resolution via VLT/MUSE and ALMA.
ReaxFF molecular dynamics and supporting lab measurements show interstellar dust grains can accrete gas-phase metals with sticking coefficients above 0.2, growing significantly within 100 Myr.
Polarization observations reveal scale-dependent differences in magnetic field morphology between molecular clouds and clumps, a velocity-dispersion correlation, and unreliable field-strength estimates that contradict flux conservation.
PSD modeling of SFR scatter at six timescales shows dominant variability on 10-30 Myr scales, stronger in lower-mass galaxies at z=3-8.
citing papers explorer
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Using the Circumgalactic Medium of Dwarf Galaxies as a Calorimetric Dark Matter Detector
Hydrodynamic simulations show that dark matter heating strongly suppresses the circumgalactic medium column densities of neutral hydrogen and metal ions in dwarf galaxies, offering a new observational probe.
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RIGEL: Ultra-faint dwarf galaxy diversity shaped by inhomogeneous cosmic reionization
Simulations with realistic patchy reionization show that the diversity of ultra-faint dwarf galaxies is primarily controlled by the halo mass at the moment of reionization.
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The THESAN-ZOOM project: clumpiness of high-redshift galaxies and its connection to bursty star formation
In simulated high-redshift galaxies, stellar mass is smooth while young-star light (Halpha, FUV, optical) is clumpy on 0.1-1 kpc scales, with clumpiness tracking bursty star formation and feedback strength.
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The efficient star-forming regions of stripped-envelope supernovae
Sites of stripped-envelope supernovae have about eight times higher star formation efficiency than sites of hydrogen-rich supernovae, measured at cloud-scale resolution via VLT/MUSE and ALMA.
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Efficient Interstellar Grain Growth from High Sticking Coefficients on Amorphous Carbon Dust
ReaxFF molecular dynamics and supporting lab measurements show interstellar dust grains can accrete gas-phase metals with sticking coefficients above 0.2, growing significantly within 100 Myr.
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Characterising magnetic fields at the onset of star cluster formation: From giant molecular clouds to infrared dark clumps
Polarization observations reveal scale-dependent differences in magnetic field morphology between molecular clouds and clumps, a velocity-dispersion correlation, and unreliable field-strength estimates that contradict flux conservation.
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Star-formation variability on the star-forming main sequence during the Epoch of Reionization
PSD modeling of SFR scatter at six timescales shows dominant variability on 10-30 Myr scales, stronger in lower-mass galaxies at z=3-8.