REVIEW 7 cited by
A dormant, overmassive black hole in the early Universe
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
A dormant, overmassive black hole in the early Universe
read the original abstract
Recent observations have found a large number of supermassive black holes already in place in the first few hundred million years after Big Bang. The channels of formation and growth of these early, massive black holes are not clear, with scenarios ranging from heavy seeds to light seeds experiencing bursts of high accretion rate. Here we present the detection, from the JADES survey, of broad Halpha emission in a galaxy at z=6.68, which traces a black hole with mass of ~ 4 * 10^8 Msun and accreting at a rate of only 0.02 times the Eddington limit. The host galaxy has low star formation rate (~ 1 Msun/yr, a factor of 3 below the star forming main sequence). The black hole to stellar mass ratio is ~ 0.4, i.e. about 1,000 times above the local relation, while the system is closer to the local relations in terms of dynamical mass and velocity dispersion of the host galaxy. This object is most likely the tip of the iceberg of a much larger population of dormant black holes around the epoch of reionisation. Its properties are consistent with scenarios in which short bursts of super-Eddington accretion have resulted in black hole overgrowth and massive gas expulsion from the accretion disk; in between bursts, black holes spend most of their life in a dormant state.
Forward citations
Cited by 7 Pith papers
-
(Re)solving the Complex Multiscale Morphology and V-shaped Spectral Energy Distribution of a Newly Discovered Strongly Lensed Little Red Dot in A383
Lensed LRD A383-LRD1 resolves into blue and red components ~300 pc apart whose combined light produces the canonical V-shaped SED.
-
How to raise a supermassive black hole: interpreting early JWST AGN with the AESOPICA simulations
A systematic simulation suite with a mock JWST survey shows early overmassive black holes can arise from any seed mass under fast accretion, and broad-line selection explains much of the observed overmassiveness.
-
An (in)complete NIRSpec census of Balmer absorption in Type 1 AGN -- radiation-driven outflows in little red dots, quasars and variable stars
About 44% of little red dots have hydrogen-alpha absorption from outflowing gas, implying radiatively driven outflows rather than static atmospheres.
-
Comparing gravitational wave background predictions from cosmological simulations to pulsar timing observations
FABLE simulation predictions for the nanohertz gravitational wave background are statistically consistent with NANOGrav 15-year data at 1–2.5σ tension, with physically motivated population modifications further improv...
-
A Unified Dark-Matter--Driven Relativistic Bondi Route to Black-Hole Growth from Stellar to Supermassive Scales
A relativistic self-interacting dark-matter fluid near a critical sound speed gives a universal Bondi accretion rate that can grow 10-solar-mass seed black holes into 10^9–10^10 solar-mass supermassive black holes by z≈7.
-
You can't see me: Super-Eddington growth hindering X-ray detection in high-z broad-line active galactic nuclei
High-redshift JWST broad-line AGNs may be low-mass black holes accreting far above Eddington, whose steep, over-cooled coronal spectra explain their X-ray non-detections and make them appear overmassive.
-
A Unified Dark-Matter--Driven Relativistic Bondi Route to Black-Hole Growth from Stellar to Supermassive Scales
Self-interacting dark matter with particle mass m ≳ 0.01 eV drives universal super-Eddington Bondi accretion that grows 10 solar-mass primordial black holes into 10^9-10^10 solar-mass supermassive black holes by z~7.
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.