Abstract

Very compact objects probe extreme gravitational fields and may be the key to understand outstanding puzzles in fundamental physics. These include the nature of dark matter, the fate of spacetime singularities, or the loss of unitarity in Hawking evaporation. The standard astrophysical description of collapsing objects tells us that massive, dark and compact objects are black holes. Any observation suggesting otherwise would be an indication of beyond-the-standard-model physics. Null results strengthen and quantify the Kerr black hole paradigm. The advent of gravitational-wave astronomy and precise measurements with very long baseline interferometry allow one to finally probe into such foundational issues. We overview the physics of exotic dark compact objects and their observational status, including the observational evidence for black holes with current and future experiments.

Highlights

  • The discovery of the electron and the known neutrality of matter led in 1904 to J

  • Together with observations of phenomena so powerful that could only be explained via massive compact objects, the theoretical understanding of black holes (BHs) turned them into undisputed kings of the cosmos

  • It is tacitly assumed that such “quantum gravity effects” are relevant only near the Planck scale: at lengths P ∼ G /c3 ∼ 10−35 m, the Schwarzschild radius is of the order of the Compton wavelength of the BH and the notion of a classical system is lost

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Summary

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The crushing of matter to infinite density by infinite tidal gravitation forces is a phenomenon with which one cannot live comfortably. From a purely philosophical standpoint it is difficult to believe that physical singularities are a fundamental and unavoidable feature of our universe [...] one is inclined to discard or modify that theory rather than accept the suggestion that the singularity occurs in nature. No testimony is sufficient to establish a miracle, unless the testimony be of such a kind, that its falsehood would be more miraculous than the fact which it endeavors to establish

Introduction
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Black holes: kings of the cosmos?
Problems on the horizon
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Quantifying the evidence for black holes
The dark matter connection
Taxonomy of compact objects: a lesson from particle physics
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The small -limit
Structure of stationary compact objects
Anatomy of compact objects
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Quantifying the shades of dark objects: the closeness parameter
Quantifying the softness of dark objects: the curvature parameter
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Geodesic motion and associated scales
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Photon spheres
Escape trajectories and shadows
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The role of the spin
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Multipolar structure
ECO taxonomy: from DM to quantum gravity
A compass to navigate the ECO atlas
Self-gravitating fundamental fields
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Perfect fluids
Anisotropic stars
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Quasiblack holes
Wormholes
P where
Dark stars
Gravastars
Fuzzballs and collapsed polymers
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Dynamics of compact objects
Quasinormal modes
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Gravitational-wave echoes
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A black-hole representation and the transfer function
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A Dyson-series representation
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Echo modeling
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Echoes: a historical perspective
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QNMs of spinning Kerr-like ECOs
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Echoes from spinning ECOs
The stability problem
The ergoregion instability
Nonlinear instabilities I: long-lived modes and their backreaction
Binary systems
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Tidal heating
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Tidal deformability and Love numbers
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Accretion and drag in inspirals around and inside DM objects
GW emission from ECOs orbiting or within neutron stars
Formation and evolution
Observational evidence for horizons
Tidal disruption events and EM counterparts
Equilibrium between ECOs and their environment
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Bounds with shadows
Tests with accretion disks
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Signatures in the mass-spin distribution of dark compact objects
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Projected constraints with EMRIs
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Tidal deformability
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Resonance excitation
5.10 QNM tests
5.11 Inspiral-merger-ringdown consistency
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5.12 Tests with GW echoes
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5.13 Stochastic background
5.14 Motion within ECOs
Discussion and observational bounds
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Findings
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Full Text
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