FRB DMs correlate at 2.6-5 sigma with galaxies, weak lensing, CIB, CMB lensing, tSZ, X-ray clusters, SXRB and radio continuum, consistent with moderate feedback models while ruling out weak feedback at 3.5 sigma via SXRB-DM.
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4 Pith papers cite this work. Polarity classification is still indexing.
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The SFR-M_* relation develops a high-mass decline at low redshifts, driven mainly by morphological quenching from internal structure rather than environmental effects on star-forming galaxies.
Eruptive mass loss in red supergiants increases linearly with metallicity, calibrated via by-eye fits to Local Group luminosity functions, preventing initial masses above about 20 solar masses from reaching the red supergiant phase.
Simulations of an NGC 300-like galaxy find exponential distributions of feedback-driven bubble lifetimes and sizes that increase with galactocentric radius, plus matching Hα predictions.
citing papers explorer
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Backlighting the Cosmic Web with Fast Radio Bursts: An Anthology of Dispersion Measure Cross-Correlations with Large-Scale Structure and Baryon Tracers
FRB DMs correlate at 2.6-5 sigma with galaxies, weak lensing, CIB, CMB lensing, tSZ, X-ray clusters, SXRB and radio continuum, consistent with moderate feedback models while ruling out weak feedback at 3.5 sigma via SXRB-DM.
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The Evolution of the SFR-M_* relation at 0.1<z<4: Environmental and Morphological Dependencies
The SFR-M_* relation develops a high-mass decline at low redshifts, driven mainly by morphological quenching from internal structure rather than environmental effects on star-forming galaxies.
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Calibrating Eruptive Mass Loss in Red Supergiants with Local Group Data
Eruptive mass loss in red supergiants increases linearly with metallicity, calibrated via by-eye fits to Local Group luminosity functions, preventing initial masses above about 20 solar masses from reaching the red supergiant phase.
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Unmasking Stellar Feedback-Driven Bubbles: Identification and Properties Analysis
Simulations of an NGC 300-like galaxy find exponential distributions of feedback-driven bubble lifetimes and sizes that increase with galactocentric radius, plus matching Hα predictions.