Future microhertz detections combined with nanohertz pulsar terms can serve as gravity echoes to measure supermassive black hole binary inspiral rates from hundreds to thousands of years in the past.
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Revisiting the Scaling Relations of Black Hole Masses and Host Galaxy Properties
28 Pith papers cite this work, alongside 1,122 external citations. Polarity classification is still indexing.
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abstract
New kinematic data and modeling efforts in the past few years have substantially expanded and revised dynamical measurements of black hole masses (Mbh) at the centers of nearby galaxies. Here we compile an updated sample of 72 black holes and their host galaxies, and present revised scaling relations between Mbh and stellar velocity dispersion (sigma), V-band luminosity (L), and bulge stellar mass (Mbulge), for different galaxy subsamples. Our best-fitting power law relations for the full galaxy sample are log(Mbh) = 8.32 + 5.64*log(sigma/200 kms), log(Mbh) = 9.23 + 1.11*log(L/10^{11} Lsun), and log(Mbh) = 8.46 + 1.05*log(Mbulge/10^{11} Msun). A log-quadratic fit to the Mbh-sigma relation with an additional term of beta_2*[log(sigma/200 kms)]^2 gives beta_2 = 1.68 +/- 1.82 and does not decrease the intrinsic scatter in Mbh. When the early- and late-type galaxies are fit separately, we obtain similar slopes of 5.20 and 5.06 for the Mbh-sigma relation but significantly different intercepts -- Mbh in early-type galaxies are about 2 times higher than in late types at a given sigma. Within early-type galaxies, our fits to Mbh(sigma) give Mbh that is about 2 times higher in galaxies with central core profiles than those with central power-law profiles. Our Mbh-L and Mbh-Mbulge relations for early-type galaxies are similar to those from earlier compilations. When the conventional quadrature method is used to determine the intrinsic scatter in Mbh, our dataset shows weak evidence for increased scatter at Mbulge < 10^{11} Msun or L_V < 10^{10.3} Lsun, while the scatter stays constant for 10^{11} < Mbulge < 10^{12.3} Msun and 10^{10.3} < L_V < 10^{11.5} Lsun. A Bayesian analysis indicates a larger sample of Mbh measurements would be needed to detect any statistically significant trend in the scatter with galaxy properties.
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Capture-driven growth model predicts M ≈ 10^5 M_⊙ × (σ/50 km s^{-1})^{2.5}, requiring the M-σ relation to flatten to 2.26 < β < 2.5 below 10^5 M_⊙.
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Morphology-dependent M_bh-σ0 relations are reported: shallow (2.5-3.1) for dust-poor S0 galaxies and steep (7.8) for massive ellipticals, using new SCOPE Bayesian regression on 137 galaxies.
Multi-epoch spectroscopy of 33 ECLEs shows coronal lines emitted at intermediate radii with log(distance)-log(black hole mass) slopes of 0.63 and 0.69 for [O III] and [Fe VII], consistent with photoionization setting the radii.
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Radiation hydro simulations produce black hole mass and viewing angle dependent bolometric correction factors (tens to thousands) and radiative efficiencies (0.001-0.1) for super-Eddington TDE flows that alleviate the missing energy problem when applied to specific events.
FIRE-3 cosmological simulations of Seyfert galaxies produce episodic AGN feedback and gas clearing but no clear anti-correlation between nuclear gas concentration and AGN luminosity, highlighting timing mismatches with observations.
The TNG SAM reproduces TNG hydro simulation gas and metal flows plus galaxy and halo properties within 30% accuracy out to z=6 via five targeted updates to the Santa Cruz SAM calibrated on stellar feedback-dominated galaxies.
Updated M_BH-R_b relation for core-Sérsic galaxies has slope 1.16 and 0.28 dex scatter; large-core galaxies drive a high-mass upturn in M_BH-σ attributed to successive dry mergers.
An obscured tidal disruption event in SDSS J010320.39+140152.5 was identified through its mid- and near-infrared dust echo peaking at 5.4e43 Lsun.
ARTEMIS and EAGLE simulations classify L* galaxies by central BH-to-stellar-mass ratio and trace how merger history drives divergence in BH growth, star formation, and morphology, offering an explanation for the observed scatter and for MW/M31 differences.
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A large collaboration compiles and compares merger rate predictions for massive black holes across multiple galaxy formation models to forecast LISA detections and quantify uncertainties.
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.
Optical imaging and BAGPIPES SED fitting of eight FXTs yields candidate hosts consistent with WD-IMBH TDEs or BNS mergers for most events, with one reclassified as a Galactic flare and evidence for diverse origins.
Spectroscopic analysis of dual nuclei shows SMBH masses higher in galaxy mergers than single nuclei at fixed stellar mass.
50 constrained simulations of Coma cluster analogues reproduce the observed radial X-ray surface brightness and Compton-y profiles within the scatter expected from environment and assembly history.
Simulations forecast 21-51% probability of resolving individual SMBH binaries with PTAs in 0-10 years, with localization areas containing ~190k early-type galaxies on average and a ranking method that excludes roughly half the candidates when galaxy properties are available.
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.
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