First spectroscopic variability in a z~7 LRD shows rapid changes in both narrow and broad line regions, implying direct ionization from the central source to surrounding nebular gas.
2025a, MNRAS[arXiv:2501.13082]
13 Pith papers cite this work, alongside 7 external citations. Polarity classification is still indexing.
13
Pith papers citing it
7
external citations · external index
fields
astro-ph.GA 13representative citing papers
LRD host galaxies show average metallicity 0.08 Z_sun with narrow stable range, challenging pristine-gas formation models while ruling out typical local AGN.
Defines a sample of ~1300 SDSS quasars as Local Red Dots matching LRD photometric colors at z~0.4-0.8, with a V-shaped subset showing Balmer absorption and [NeV] emission, and SEDs modeled as reddened AGN plus host galaxy that match LRD stacks.
Derives idealized P-L-T relation from hydrostatic envelope model for LRDs and uses sparse data to obtain preliminary H0 = 120.7 with large errors as proof-of-concept.
The survey identifies 27 low-redshift LRDs with compact morphology, V-shaped continua, broad Balmer lines with extreme decrements, and ubiquitous outflows, matching high-z counterparts and yielding a number density lower limit of 7.5e-10 cMpc^-3.
A theoretical model of a magnetized black hole envelope is developed to explain the broad emission lines and X-ray faintness observed in little red dots using co-rotating plasma clumps and limited X-ray sources.
X-ray non-detection of little red dots requires both Compton-thick gas columns (~1e25 cm^-2) and intrinsically weak X-ray emission with bolometric correction k_bol,X ≳ 30.
Coevolving super-Eddington black holes and nuclear starbursts in high-redshift halos naturally generate the V-shaped UV-to-optical spectra and weak high-energy emission of little red dots.
A source 660 million years after the Big Bang is interpreted as a black hole star with a dust-free dense gas atmosphere, implying Little Red Dots have black hole masses overestimated by orders of magnitude.
Using JWST photometry of ~17,000 galaxies, the median Balmer break strength decreases from 1.5 to 1.1 (flux ratio) from z~3.5 to z~10, driven by stellar population age, with rare extremely strong breaks at both epochs tracing distinct populations.
Compact nuclear starbursts in metal-poor dwarfs produce AGN-like mid-IR colors without accretion, as revealed by JWST observations of two such galaxies.
Number density of LRDs with L_bol ≳ 3×10^44 erg s^{-1} shows no evolution at z>2 and is ~350 times higher than model predictions at cosmic noon.
citing papers explorer
-
The GlimmIr: Spectroscopic Variability in a z~7 LRD Indicates Rapid Changes in Both the Narrow and Broad Line Regions
First spectroscopic variability in a z~7 LRD shows rapid changes in both narrow and broad line regions, implying direct ionization from the central source to surrounding nebular gas.
-
The metallicities of little red dot host galaxies: LRDs are metal poor, but not pristine
LRD host galaxies show average metallicity 0.08 Z_sun with narrow stable range, challenging pristine-gas formation models while ruling out typical local AGN.
-
A Population of Little Red Dot-like Quasars in SDSS
Defines a sample of ~1300 SDSS quasars as Local Red Dots matching LRD photometric colors at z~0.4-0.8, with a V-shaped subset showing Balmer absorption and [NeV] emission, and SEDs modeled as reddened AGN plus host galaxy that match LRD stacks.
-
Little red dots as a cosmological probe: constraining $H_0$ with quasi-periodic pulsations
Derives idealized P-L-T relation from hydrostatic envelope model for LRDs and uses sparse data to obtain preliminary H0 = 120.7 with large errors as proof-of-concept.
-
(LRDs)$^2$: The Low-ReDshift Little Red Dots Survey. II. DESI DR1 Sample
The survey identifies 27 low-redshift LRDs with compact morphology, V-shaped continua, broad Balmer lines with extreme decrements, and ubiquitous outflows, matching high-z counterparts and yielding a number density lower limit of 7.5e-10 cMpc^-3.
-
A Magnetized Black Hole Envelope Model for Little Red Dots
A theoretical model of a magnetized black hole envelope is developed to explain the broad emission lines and X-ray faintness observed in little red dots using co-rotating plasma clumps and limited X-ray sources.
-
Quenching of X-ray emission in little red dots by both Compton-thick gas and high accretion rates
X-ray non-detection of little red dots requires both Compton-thick gas columns (~1e25 cm^-2) and intrinsically weak X-ray emission with bolometric correction k_bol,X ≳ 30.
-
Spectral Uniformity of Little Red Dots: A Natural Outcome of Coevolving Seed Black Holes and Nascent Starbursts
Coevolving super-Eddington black holes and nuclear starbursts in high-redshift halos naturally generate the V-shaped UV-to-optical spectra and weak high-energy emission of little red dots.
-
A "Black Hole Star" Reveals the Remarkable Gas-Enshrouded Hearts of the Little Red Dots
A source 660 million years after the Big Bang is interpreted as a black hole star with a dust-free dense gas atmosphere, implying Little Red Dots have black hole masses overestimated by orders of magnitude.
-
Tracing the Evolution of the Balmer Break from Cosmic Dawn to Cosmic Noon with JWST
Using JWST photometry of ~17,000 galaxies, the median Balmer break strength decreases from 1.5 to 1.1 (flux ratio) from z~3.5 to z~10, driven by stellar population age, with rare extremely strong breaks at both epochs tracing distinct populations.
-
JWST Reveals Compact Nuclear Starbursts Masquerading as AGNs in Metal-Poor Dwarfs: Where Are the Accreting Intermediate-Mass Black Holes?
Compact nuclear starbursts in metal-poor dwarfs produce AGN-like mid-IR colors without accretion, as revealed by JWST observations of two such galaxies.
-
No evolution in the number density of little red dots from cosmic dawn to cosmic noon
Number density of LRDs with L_bol ≳ 3×10^44 erg s^{-1} shows no evolution at z>2 and is ~350 times higher than model predictions at cosmic noon.
- Super-Eddington accretion of black holes in early nuclear bursts gives birth to Little Red Dots