Astrometric Detection of Intermediate-Mass Black Holes At the Galactic Centre

Abstract

We assess the astrometric detectability of intermediate-mass black holes populating the inner parsec of the Milky Way Galaxy. The presence of these objects induces dynamical effects on Sgr A* and the star S2, which could be detected by next generation astrometric instruments that enable micro-arcsecond astrometry. An allowed population of ten $10^4{M}_{\odot }$ IMBHs within one parsec induces an angular shift of about 65 $\mu$as yr${}^{-1}$ on the position of Sgr A*, corresponding to a perpendicular velocity component magnitude of 1.6 km s${}^{-1}$. It also induces changes in the orbit of S2 that surpass those induced by general relativity but lie within observational constraints, generating a mean angular shift in periapse and apoapse of 62 $\mu$as and 970 $\mu$as respectively.

arXiv comment10 pages, 16 figures, 4 tables

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• On Detecting Nearby Nano-Hertz Gravitational Wave Sources via Pulsar Timing Arrays
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• Intermediate-mass black hole binary parameter estimation with next-generation ground-based detector networks
• Trigonometric parallax and proper motion of Sagittarius A* measured by VERA using the new broad-band back-end system OCTAVE-DAS
• Electromagnetic signatures of black hole clusters in the center of super-Eddington galaxies
• Detectability of dark matter density distribution via gravitational waves from binary black holes in the Galactic center
• Resonant Dynamical Friction in Nuclear Star Clusters: Rapid Alignment of an Intermediate-mass Black Hole with a Stellar Disk