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

Abstract

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.

Frequency Shift of Photons in the Spacetime of Deformed RN BH

“…This information is encoded in the frequency shift of these photons, denoted as z dRN 1,2 in Equation (55), which is directly observable. Consequently, by performing a statistical fit [49,[51][52][53] or solving an inverse problem, as demonstrated in [54], the set of spacetime parameters M, Q, , Λ can be estimated. In other words, Equation ( 55) enables the extraction of the spacetime properties characterized by the black hole mass M, electric charge Q, deformation , and cosmological constant Λ through the measurement of frequency shifts in the photons, z dRN 1,2 .…”

A general relativistic mass-to-distance ratio for a set of megamaser AGN black holes

“…the redshift of the emitted photons (Banerjee et al 2022). In Nucamendi et al (2021) and Villalobos-Ramírez et al (2022) the authors use the mentioned model considering the Schwarzschild metric to estimate the BH parameters and quantify the corresponding gravitational redshift in the megamaser galaxy NGC 4258 and the gigamaser of TXS 2226-184, respectively; the latter being the first BH mass estimation using gigamaser observations. Following this general relativistic approach, in this work we fit the mass-to-distance ratio 𝑀/𝐷 and the recession velocity of the BHs hosted at the center of the galaxies NGC 5765b, NGC 6323, UGC 3789, CGCGC 074-064, ESO 558-G009, NGC 2960, NGC 6264, NGC 4388, J0437+2456 and NGC 2273 using the observations of the megamaser positions in the sky as well as their frequency shifts.…”