Note on the Cardoso-Pani-Rico parametrization to test the Kerr black hole hypothesis

Bambi, Cosimo

doi:10.1103/physrevd.90.047503

Cited by 26 publications

(27 citation statements)

References 60 publications

(58 reference statements)

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“…It is compared with a set of models in which the spacetime geometry is described by the Cardoso-Pani-Rico metric with only one non-vanishing deformation parameter, namely  is more difficult to constrain from the line profile alone. A similar conclusion is found by Bambi (2014a). It is evident that iron lines are more capable of constraining deformation parameters when the inclination of the reference model i′ is large, since this maximizes light bending effects.…”

Section: Simulationssupporting

confidence: 83%

“…However, the usual problem with such a test is often strong degeneracy among system parameters, in particular between the parameter measuring deviation from Kerr geometry, and the spin and the inclination angle. The thermal spectrum of thin disks has a simple shape and therefore it is fundamentally more challenging to break such a degeneracy (Bambi 2014a;Kong et al 2014). The iron line profile is potentially more powerful.…”

Section: Introductionmentioning

confidence: 99%

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Testing the Kerr Nature of Black Hole Candidates Using Iron Line Spectra in the CPR Framework

Jiang

Bambi

Steiner

2015

ApJ

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The iron Kα line commonly observed in the X-ray spectrum of both stellar-mass and supermassive black hole (BH) candidates originates from X-ray fluorescence of the inner accretion disk. Accordingly, it can be used to map the spacetime geometry around these objects. In this paper, we extend previous work using the iron Kα line to test the Kerr BH hypothesis. We adopt the Cardoso-Pani-Rico parametrization and we test the possibility of constraining possible deviations from the Kerr solution that can be obtained from observations across the range of BH spins and inclination angles. We confirm previous claims that the iron Kα line is potentially a quite powerful probe for testing the Kerr metric given sufficiently high quality data and with systematics under control, especially in the case of fast-rotating BHs and high inclination angles since both conditions serve to maximize relativistic effects. We find that some geometric perturbations from Kerr geometry manifest more strongly in the iron line profile than others. While the perturbation parameter t 3  can be well constrained by the iron line profile, an orthogonal data set is necessary to constrain departures from Kerr geometry in .

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Section: Simulationssupporting

confidence: 83%

Section: Introductionmentioning

confidence: 99%

Testing the Kerr Nature of Black Hole Candidates Using Iron Line Spectra in the CPR Framework

Jiang

Bambi

Steiner

2015

ApJ

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“…Another approach is the study of the thermal component of the spectrum from stellar-mass BHs using the so-called continuum-fitting method [475,483,484], which can provide information about the ISCO location and hence the BH spin [484]. The method can be also used to test the spacetime geometry [476,[480][481][482][485][486][487][488] but is limited by the fact that deviations from the Kerr geometry are typically degenerate with the ISCO properties, e.g. with the spin of the object [473,489].…”

Section: Tests With Accretion Disksmentioning

confidence: 99%

Testing the nature of dark compact objects: a status report

2019

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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 gravitationalwave 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.

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“…has continuous derivatives up to second order at the point r = 1. By direct integration in (4) and then in (3), we obtain…”

Section: A Family Of Compact Black Holesmentioning

confidence: 99%

“…Namely, are they black holes, wormholes, naked singularities, or maybe boson stars? In any of these cases, the observations of bound orbits in the centers of galaxies play a key role for this question [4,5,6,7,8,9,10]). In this paper, we study some properties of bound orbits near black holes in the model of a static, self-gravitating, spherically symmetric scalar field.…”

Section: Introductionmentioning

confidence: 99%

Bound orbits near black holes with scalar hair

Potashov

Tchemarina

Tsirulev

2019

J. Phys.: Conf. Ser.

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We consider spherically symmetric black holes with minimally coupled scalar fields and concentrate our attention on asymptotically flat self-gravitating configurations having the event horizons located at radii much smaller than 2m. We think of such configurations as rigorous mathematical models of the gravitating objects, surrounded by dark matter, in the centres of normal galaxies. It turns out that the radius of the event horizon of a scalar field black hole always less than the Schwarzschild radius of vacuum black hole of the same mass and can be arbitrary close to zero. In astronomical observations, a key role in distinguishing between black holes, wormholes, and naked singularities plays measuring parameters of bound quasiperiodic orbits, in particular, the shape of an orbit and the angle of precession of its pericentre. We consider a typical two-parameter family of compact scalar field black holes and compute numerically the shapes of some bound orbits. We find that a key feature of bound orbits around a compact black hole is that the angle between closest pericentre points is either negative or, at least, less than that for the Schwarzschild black hole of the same mass.

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Note on the Cardoso-Pani-Rico parametrization to test the Kerr black hole hypothesis

Cited by 26 publications

References 60 publications

Testing the Kerr Nature of Black Hole Candidates Using Iron Line Spectra in the CPR Framework

Testing the Kerr Nature of Black Hole Candidates Using Iron Line Spectra in the CPR Framework

Testing the nature of dark compact objects: a status report

Bound orbits near black holes with scalar hair

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