JWST and ALMA data provide the earliest direct evidence of ram-pressure stripping in a post-starburst galaxy at z=3.06, implying the process can quench star formation in nascent groups at z>3.
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FIRE-2 simulations show per-galaxy tidal disruption rates peak near z=2.5 at 4e-4 per year, correlate with SFR and central density, and remain high in satellite galaxies at early times.
Central black holes in ASTRID and TNG300 follow a tight, redshift-invariant M_BH–M_⋆ relation from z=2 to 0.5; departures mark merger-driven high-mass quenchers, tidally stripped overmassive satellites, and undermassive wanderers.
Derives GR jump conditions and self-similar shock solutions for SIS collapse to BH, showing shocks up to 0.4c, accretion suppressed by factor 5-7, and shock energy release ~10% of enclosed rest mass.
DESI DR1 yields 314k high-mass and 9.6k dwarf AGN, extending the M_BH-M_star relation to log M_star ~7.8 and suggesting two evolutionary pathways for galaxies and black holes.
Two FRBs in the CHIME/FRB catalog look microlensed by black holes of roughly 550 and 2000 solar masses, presented as IMBH candidates.
Low-luminosity AGN exhibit structure function slopes rising from 0.1 to 0.3 with black hole mass, no breaks on decadal scales, amplitude anticorrelated with luminosity and positively correlated with mass.
Machine learning on cosmological simulations achieves 91-94% accuracy classifying over-massive versus under-massive SMBH growth regimes from LSST photometry, with 83-89% cross-simulation transfer accuracy driven primarily by host galaxy colors.
Five LRDs at z≈2 yield number density ≈7×10^{-6} cMpc^{-3}, confirming a decline from the z≈5 peak but gentler than prior photometric estimates.
Black hole occupation fraction rises with stellar mass but its normalization, shape, and redshift trend depend strongly on BH mass threshold, central vs satellite galaxies, simulation box, resolution, and sampled population in the FEGA25 model.
JWST data on LRDs and LBDs show AGN-like excitation, strong Lyα with broad components, and X-ray weakness, implying clumpy or equatorial geometries around growing black holes rather than complete gas envelopes.
Lenient heavy-seed models in BRAHMA simulations produce black hole merger rates above 100 per year and near-unity occupation fractions down to low-mass galaxies, while strict models yield only about 1 merger per year and occupation fractions below 10 percent for galaxies under 10^8 solar masses.
Semi-analytical models show AGN disks produce repeated BBH mergers with a high-mass tail beyond the pair-instability gap, more efficiently at low viscosity, with spin and mass-ratio signatures that can match events like GW190521.
Simulations show heavy-seed formation with BH-BH mergers or Bondi accretion under weak feedback can assemble 10^6-10^7 solar mass black holes at z greater than or equal to 9.
A multiphase ISM grain-size model with low supernova dust yield reproduces observed dust-to-stellar mass ratios and UV luminosity functions at z=7-12 by letting small grains seed rapid metal accretion.
LILA can detect IMBH binaries at redshifts 20-30, IMRIs, and provide months-to-years early warnings with high-SNR events for gravity tests.
Super-Eddington accretion boosts predicted LISA detections of high-redshift black hole binaries to ~64 per year while dropping ET detections to ~4 per year, compared to ~32 and ~64 under Eddington-limited growth.
Dark matter clustering, possibly via self-interaction, may help stellar-remnant black holes reach over 10^7 solar masses by z=10.
Simulations and analytic modeling predict that the supermassive black hole to stellar mass ratio peaks at several percent around redshift 7-10 before declining toward the present day.
Simulations indicate LISA could statistically distinguish CDM from SIDM (constant 1 cm²/g cross-section) with at least ~70 high-SNR massive black hole merger detections.
A review chapter summarizing theoretical 21-cm signatures from Cosmic Dawn and Reionization and their detectability with SKA-Low.
A review summarizing detection methods, population statistics, and coevolution of supermassive black holes with host galaxies from early universe observations and simulations.
citing papers explorer
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A Post-starburst Galaxy Undergoing Ram-pressure Stripping at Redshift 3.06
JWST and ALMA data provide the earliest direct evidence of ram-pressure stripping in a post-starburst galaxy at z=3.06, implying the process can quench star formation in nascent groups at z>3.
-
TDEs on FIRE: Illuminating the Cosmic Evolution of Tidal Disruption Rates
FIRE-2 simulations show per-galaxy tidal disruption rates peak near z=2.5 at 4e-4 per year, correlate with SFR and central density, and remain high in satellite galaxies at early times.
-
Tracing black hole and galaxy growth across environments since cosmic noon
Central black holes in ASTRID and TNG300 follow a tight, redshift-invariant M_BH–M_⋆ relation from z=2 to 0.5; departures mark merger-driven high-mass quenchers, tidally stripped overmassive satellites, and undermassive wanderers.
-
General Relativistic Shock Wave Solutions with Black Hole Formation: The Singular Isothermal Sphere Case
Derives GR jump conditions and self-similar shock solutions for SIS collapse to BH, showing shocks up to 0.4c, accretion suppressed by factor 5-7, and shock energy release ~10% of enclosed rest mass.
-
A New Record Census of Dwarf AGN and a Bimodal $M_{\rm BH}$-$M_{\star}$ Scaling Relation with DESI DR1
DESI DR1 yields 314k high-mass and 9.6k dwarf AGN, extending the M_BH-M_star relation to log M_star ~7.8 and suggesting two evolutionary pathways for galaxies and black holes.
-
Evidence for Intermediate-Mass Black Holes From Microlensing Signatures in CHIME/FRB catalog 2
Two FRBs in the CHIME/FRB catalog look microlensed by black holes of roughly 550 and 2000 solar masses, presented as IMBH candidates.
-
Optical Variability Structure Function of Low-Luminosity AGN using ATLAS Lightcurves
Low-luminosity AGN exhibit structure function slopes rising from 0.1 to 0.3 with black hole mass, no breaks on decadal scales, amplitude anticorrelated with luminosity and positively correlated with mass.
-
Classifying Supermassive Black Hole Growth Regimes to Observables Across Cosmological Simulations with Forecasts for LSST
Machine learning on cosmological simulations achieves 91-94% accuracy classifying over-massive versus under-massive SMBH growth regimes from LSST photometry, with 83-89% cross-simulation transfer accuracy driven primarily by host galaxy colors.
-
Little Red Dots at z~2 in EIGER reveal a gentle decline with respect to their peak number density at z~5
Five LRDs at z≈2 yield number density ≈7×10^{-6} cMpc^{-3}, confirming a decline from the z≈5 peak but gentler than prior photometric estimates.
-
Black Hole Occupation Fraction: Dependence on Black Hole Mass Threshold, Environment, Resolution and Redshift
Black hole occupation fraction rises with stellar mass but its normalization, shape, and redshift trend depend strongly on BH mass threshold, central vs satellite galaxies, simulation box, resolution, and sampled population in the FEGA25 model.
-
Little Red and Blue Dots: AGN-excited narrow lines, Lyman-$\alpha$ emission, and resemblance to standard quasars
JWST data on LRDs and LBDs show AGN-like excitation, strong Lyα with broad components, and X-ray weakness, implying clumpy or equatorial geometries around growing black holes rather than complete gas envelopes.
-
Supermassive Black Hole Assembly from Heavy Seeds with Dynamical Friction in the BRAHMA Simulations: Implications for JWST, LISA, and the Local Universe
Lenient heavy-seed models in BRAHMA simulations produce black hole merger rates above 100 per year and near-unity occupation fractions down to low-mass galaxies, while strict models yield only about 1 merger per year and occupation fractions below 10 percent for galaxies under 10^8 solar masses.
-
AGN-driven BBH mergers: Black hole populations and hierarchical growth across the AGN parameter space
Semi-analytical models show AGN disks produce repeated BBH mergers with a high-mass tail beyond the pair-instability gap, more efficiently at low viscosity, with spin and mass-ratio signatures that can match events like GW190521.
-
Learning the Universe at High Redshifts: Impact of Accretion Modeling on Early Black Hole Growth
Simulations show heavy-seed formation with BH-BH mergers or Bondi accretion under weak feedback can assemble 10^6-10^7 solar mass black holes at z greater than or equal to 9.
-
Grain-size evolution and rapid dust growth in high-redshift galaxies
A multiphase ISM grain-size model with low supernova dust yield reproduces observed dust-to-stellar mass ratios and UV luminosity functions at z=7-12 by letting small grains seed rapid metal accretion.
-
Black Hole Binary Detection Landscape for the Laser Interferometer Lunar Antenna (LILA): Signal-to-Noise Calculations & Science Cases
LILA can detect IMBH binaries at redshifts 20-30, IMRIs, and provide months-to-years early warnings with high-SNR events for gravity tests.
-
Gravitational Waves from the Cosmic Dawn: Tracing Cosmic Black Hole Binaries with ET, LGWA and LISA
Super-Eddington accretion boosts predicted LISA detections of high-redshift black hole binaries to ~64 per year while dropping ET detections to ~4 per year, compared to ~32 and ~64 under Eddington-limited growth.
-
Dark Matter and the Early Formation of Supermassive Black Holes
Dark matter clustering, possibly via self-interaction, may help stellar-remnant black holes reach over 10^7 solar masses by z=10.
-
Redshift Evolution of the Ratio of Supermassive Black Hole Mass to Stellar Mass
Simulations and analytic modeling predict that the supermassive black hole to stellar mass ratio peaks at several percent around redshift 7-10 before declining toward the present day.
-
Probing the Nature of Dark Matter Self-Interactions Through Observations of Massive Black Hole Mergers
Simulations indicate LISA could statistically distinguish CDM from SIDM (constant 1 cm²/g cross-section) with at least ~70 high-SNR massive black hole merger detections.
-
High-Redshift Signatures from the Cosmic Dawn and the Epoch of Reionization
A review chapter summarizing theoretical 21-cm signatures from Cosmic Dawn and Reionization and their detectability with SKA-Low.
-
Massive black holes and their galaxies
A review summarizing detection methods, population statistics, and coevolution of supermassive black holes with host galaxies from early universe observations and simulations.