Toward the Gravitational Redshift Detection in NGC 4258 and the Estimation of Its Black Hole Mass-to-distance Ratio

Nucamendi, Ulises; Herrera–Aguilar, Alfredo; Lizardo-Castro, Raúl; López-Cruz, Omar

doi:10.3847/2041-8213/ac151b

Cited by 13 publications

(18 citation statements)

References 34 publications

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“…This expression depends on both the mass and the spin parameters, implying the fact that the gravitational redshift is generated by the black hole mass (given by the first two items when the spin vanishes) and its rotation (the third term). This quantity generalizes the gravitational redshift formula for the Schwarzschild black hole given in [21] and reproduces it when the rotation parameter is trivial.…”

Section: The Dragging Effect On the Light Bending Parameter And The R...supporting

confidence: 71%

“…The total frequency shifts (34)-( 35) for large orbits of the emitter M , ã << 1 read which reduce to those for the Schwarzschild black hole for ã = 0 [21], as it should be.…”

Section: Boosting the Black Hole With Respect To A Distant Observermentioning

confidence: 77%

“…where we should recall that 0 ≤ ϕ ≤ 2π. Note that this equation plausibly reduces to relation (5) for ϕ = ±π/2 and to (21) for ϕ = 0, as it should be. This formula for the light bending parameter is quite remarkable since it unifies the two expressions we had for this quantity when considering the motion of a particle on either side of the line of sight.…”

Section: Dependency Of the Redshift On The Azimuthal Anglementioning

confidence: 90%

“…Thus, this formalism allows one to compute the values of the Kerr black hole parameters on the basis of the directly measured observational quantities: the total redshifts and blueshifts of the emitted photons and the positions of their source, in contrast to the commonly used radial velocities, which are coordinate dependent observables. Moreover, a simplified version of this formalism for static (Schwarzschild) black holes has been already applied to the accretion disk with water masers that orbit circularly and equatorially around a supermassive black hole hosted at the center of the active galactic nucleus of NGC 4258 [21]. In the aforementioned study, the massto-distance ratio was estimated and the gravitational redshift of the closest maser to the black hole was quantified using this general relativistic method.…”

Section: A Brief Overview Of the Gr Formalismmentioning

confidence: 99%

“…Astronomers usually call this motion systemic when referring to orbiting the black hole particles lying close to the line of sight, where the radial component of the rotational velocity vanishes. Now, by considering the peculiar redshift, the total redshift becomes [21]…”

Section: Boosting the Black Hole With Respect To A Distant Observermentioning

confidence: 99%

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Mass and spin of Kerr black holes in terms of observational quantities: The dragging effect on the redshift

Banerjee,

Herrera-Aguilar,

Momennia

et al. 2022

Preprint

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In this work, we elaborate on the development of a general relativistic formalism that allows one to analytically express the mass and spin parameters of the Kerr black hole in terms of observational data: the total redshift and blueshift of photons emitted by geodesic massive particles revolving the black hole and their orbital parameters. Thus, we present concise closed formulas for the mass and spin parameters of the Kerr black hole in terms of few directly observed quantities in the case of equatorial circular orbits either when the black hole is static or is moving with respect to a distant observer. Furthermore, we incorporate the gravitational dragging effect generated by the rotating nature of the Kerr black hole into the analysis and elucidate its non-trivial contribution to the expression for the light bending parameter and the frequency shifts of photons emitted by orbiting particles that renders simple symmetric expressions for the kinematic redshift and blueshift. We also incorporate the dependency of the frequency shift on the azimuthal angle, a fact that allows one to express the total redshift/blueshift along any point of the orbit of the revolving particle for the cases when the black hole is both static or moving with respect to us. These formulas allow one to compute the Kerr black hole parameters by applying this general relativistic formalism to astrophysical systems like the megamaser accretion disks orbiting supermassive black holes at the core of active galactic nuclei. Our results open a new window to implement parameter estimation studies to constrain black hole variables, and they can be generalized to black hole solutions beyond Einstein gravity.

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Section: The Dragging Effect On the Light Bending Parameter And The R...supporting

confidence: 71%

“…The total frequency shifts (34)-( 35) for large orbits of the emitter M , ã << 1 read which reduce to those for the Schwarzschild black hole for ã = 0 [21], as it should be.…”

Section: Boosting the Black Hole With Respect To A Distant Observermentioning

confidence: 77%

Section: Dependency Of the Redshift On The Azimuthal Anglementioning

confidence: 90%

Section: A Brief Overview Of the Gr Formalismmentioning

confidence: 99%

Section: Boosting the Black Hole With Respect To A Distant Observermentioning

confidence: 99%

See 3 more Smart Citations

Mass and spin of Kerr black holes in terms of observational quantities: The dragging effect on the redshift

Banerjee,

Herrera-Aguilar,

Momennia

et al. 2022

Preprint

Self Cite

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A general relativistic estimation of the black hole mass-to-distance ratio at the core of TXS 2226–184

Villalobos-Ramírez

Gallardo-Rivera

Herrera–Aguilar

et al. 2022

A&A

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In this work we make use of a general relativistic method to estimate the mass-to-distance ratio M/D = 3.54−0.18+0.20 × 104 M⊙ Mpc−1 of the black hole hosted at the core of the active galactic nucleus of TXS 2226–184, along with its right ascension offset and the recession redshift (velocity) of the galaxy. Our statistical fit is based on the frequency shift of photons emitted by water masers and their orbital positions when circularly revolving around the black hole center within the accretion disk of the active galactic nucleus. By taking a previously reported distance to the galaxy into account, we compare the result of the black hole mass fit to an estimate based on a mass-luminosity correlation. We find that the black hole mass at the core of TXS 2226–184 obtained with the aid of the statistical fit using the general relativistic method, M = 3.67−0.18+0.20 × 106 M⊙, is approximately 0.6 times the black hole mass, MBH = 6.24−2.27+3.63 × 106 M⊙, which was computed with the mass–luminosity correlation.

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Estimating the mass-to-distance ratio for a set of megamaser AGN black holes by employing a general relativistic method

González-Juárez,

Momennia,

Villalobos-Ramírez

et al. 2024

A&A

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Motivated by the recent achievements of a full general relativistic method in determining black hole (BH) parameters, we continue to estimate the mass-to-distance ratio of the supermassive BHs hosted at the core of the active galactic nuclei (AGNs) of the megamaser galaxies NGC 1320, NGC 1194, NGC 5495, and Mrk 1029. Our aim is to study the properties of super massive BHs at the centers of the selected AGNs by using a full general relativistic method that allows us to address the potential detection of relativistic effects within such astrophysical systems. In order to perform statistical estimations with publicly available observational data, we used a general relativistic model that describes BH rotation curves and further employed a Bayesian fitting method. We estimated the mass-to-distance ratio of the aforementioned BHs, their position and the recessional redshifts of the host galaxies produced by both peculiar motion and cosmological expansion of the Universe. Finally, we calculated the gravitational redshift of the closest maser to the BH for each AGN. This gravitational redshift is a general relativistic effect produced by the gravitational field of the BH properly included in the modelling.

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Toward the Gravitational Redshift Detection in NGC 4258 and the Estimation of Its Black Hole Mass-to-distance Ratio

Cited by 13 publications

References 34 publications

Mass and spin of Kerr black holes in terms of observational quantities: The dragging effect on the redshift

Mass and spin of Kerr black holes in terms of observational quantities: The dragging effect on the redshift

A general relativistic estimation of the black hole mass-to-distance ratio at the core of TXS 2226–184

Estimating the mass-to-distance ratio for a set of megamaser AGN black holes by employing a general relativistic method

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