DESI DR2 quasar sample yields bias b_Q(z=2.48)=3.61 that evolves as b(z)=0.230[(1+z)^2-6.565]+2.394, consistent with constant ~10^12 M_sun halo mass and weak luminosity dependence at fixed redshift.
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Energy input from quasars regulates the growth and activity of black holes and their host galaxies
31 Pith papers cite this work, alongside 2,928 external citations. Polarity classification is still indexing.
31
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2,928
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abstract
In the early Universe, while galaxies were still forming, black holes as massive as a billion solar masses powered quasars. Supermassive black holes are found at the centers of most galaxies today, where their masses are related to the velocity dispersions of stars in their host galaxies and hence to the mass of the central bulge of the galaxy. This suggests a link between the growth of the black holes and the host galaxies, which has indeed been assumed for a number of years. But the origin of the observed relation between black hole mass and stellar velocity dispersion, and its connection with the evolution of galaxies have remained unclear. Here we report simulations that simultaneously follow star formation and the growth of black holes during galaxy-galaxy collisions. We find that in addition to generating a burst of star formation, a merger leads to strong inflows that feed gas to the supermassive black hole and thereby power the quasar. The energy released by the quasar expels enough gas to quench both star formation and further black hole growth. This determines the lifetime of the quasar phase (approaching 100 million years) and explains the relationship between the black hole mass and the stellar velocity dispersion.
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JWST data on 3C305 shows the compact radio jet efficiently drives kiloparsec-scale multiphase outflows via shocks, with high coupling to the observed gas kinetic power and radiative losses.
JWST spectra of six z=5-9 galaxies show low-ionization covering fractions of 0.2-0.9 and diverse kinematics including blueshifted outflows, indicating heterogeneous multiphase ISM.
Calypso is a parameter-conditioned stochastic surrogate model for circumbinary accretion flows using PCA and multivariate Gaussian modeling, released as open-source software with a closed-form likelihood for parameter inference from time series.
A score-based diffusion generative model on deep infrared galaxy photometry yields a star formation rate density peaking at z=1.3 and shows distinct non-parametric star formation histories plus AGN activity peaking during the quenching transition of massive galaxies.
Confirmation of 77 new heavily reddened quasars at 1.5 < z < 3.9 with high luminosities and extinctions, showing they are deficient in hot and warm dust relative to blue quasars and supporting a blow-out feedback phase.
Machine learning on simulated images identifies that flux eruption events cause more diffuse, polarized, lower-flux millimeter emission with decreased Q-U loop rotation rate, achieving ~80% accuracy with random forests on summary statistics.
Slim-disk self-shadowing plus accretion-rate-dependent BLR density enhancement explains the observed offsets of high-Eddington AGNs below the canonical R-L relation.
tSZ cross-correlations with large-scale structure tracers prefer low S8 and strong baryonic feedback, yielding S8 = 0.72 and low group baryon fraction in FLAMINGO simulations.
JWST observations of ERQs show stratified gas kinematics via deblended optical emission lines, with UV lines dominated by scattered light and optical lines mixing scattered and obscured emission.
New spectroscopy and simulations of Arp 143 suggest it formed via head-on collision between S0 and Sc galaxies following a flyby.
Line ratio diagnostics in NGC 1068 indicate AGN outflows are shock-accelerated, with outflowing gas dust-free and 19-110 times denser than disk gas.
Radiation hydrodynamic simulations of wind-reprocessed TDEs reveal a ~3-week offset between optical/UV and bolometric light curve peaks due to the buildup time of the reprocessing layer.
In TNG50, compact dwarf satellites (log M_star 8.4-9.2) form via DM-rich gas inflows in low-merger environments, tidal stripping for DM-poor cases, and ram-pressure starbursts for some metal-rich ones.
Chaotic Cold Accretion reproduces the observed near-linear black hole mass-bolometric luminosity scaling (slope 0.91) in z>2 quasars while Bondi accretion underpredicts by ~2 dex.
Horizon-AGN shows galaxy and black hole merger rates both rise with stellar mass and fall with redshift, peaking near z=2-3, establishing a direct evolutionary link from galaxy interactions to black hole coalescences.
JWST spectroscopy reveals radio jets in nearby AGN drive multiphase ISM turbulence and shock-dominated H2 excitation both along and perpendicular to the jet direction.
Five new HI 21-cm absorption detections in LERGs and HERGs at z<0.5 reveal disturbed gas kinematics with velocity offsets over 350 km/s and a 3% detection rate consistent with lower-redshift samples.
Multi-phase molecular gas in IRAS20551-4250 is dominated by cold CO, shows UV-heated warm H2, tidal features from a merger, and no molecular outflows, consistent with ongoing star formation.
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.
Disc galaxies inhibit supermassive black hole growth by preserving rotational support in central gas, while mergers in ellipticals disrupt this support and enable rapid accretion.
VLBI imaging detects a compact radio source with Tb > 10^7 K and flat spectrum in the northern core of UGC 2369S, confirming a buried low-luminosity AGN.
Higher Eddington ratio AGN exhibit increased [O III] outflow incidence and reduced obscuration, supporting radiative feedback as the regulator.
Morphological merger fractions exceed close-pair fractions across 0.2<z<0.9 in DEVILS, with minimal sample overlap, attributed to different merger stages and timescales.
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