Microlensing surveys constrain fast and slow compact objects at masses and densities differing by orders of magnitude from dark matter limits due to speed-mass degeneracy in Einstein crossing times.
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Scaling monopoles generate PBHs via stochastic overdensities and GWs with correlated spectra, potentially with magnetically charged PBHs as a signature if the scaling ends via gauge boson mass.
Tensor perturbations from first-order phase transitions and domain wall annihilation induce curvature fluctuations at second order that form primordial black holes, allowing asteroid-mass PBHs to comprise all dark matter for specific parameter ranges with associated gravitational wave peaks in LISA,
Collapsing Z_N domain walls trap baryons into dense baryoids, yielding a dark matter-baryon energy density ratio of approximately (N-1):1 after the QCD phase transition.
G objects are modeled as primordial black hole-neutron star remnants whose population simultaneously accounts for the Galactic Center pulsar deficit.
Re-analysis of Subaru HSC data shows that twelve previously claimed planetary-mass primordial black hole candidates are actually misidentified variable stars.
Blue-tilted running spectrum with α_s ≈ 0.02 and β_s ≈ 0.02 resolves JWST early galaxy tension at 1σ in joint CMB analysis.
CMB data limits the s-wave annihilation cross section of thermal dark matter particles to ≲ 10^{-30} cm³/s scaled by PBH fraction and mass for PBHs heavier than ~10^{-10} solar masses.
The paper reviews primordial black hole formation during the cosmic QCD phase transition in a microscopical model and explores how beyond-Standard-Model physics affects the equation of state and PBH probability distributions as dark matter candidates.
Stellar microlensing surveys exclude compact objects between 10^{-11} and 10^4 solar masses from making up all dark matter under standard assumptions.