Revisiting stellar orbits and the Sgr 
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 quadrupole moment

Alush, Yael; Stone, Nicholas C.

doi:10.1103/physrevd.106.123023

Phys. Rev. D

2022

DOI: 10.1103/physrevd.106.123023

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Revisiting stellar orbits and the Sgr A* quadrupole moment

Yael Alush

Nicholas C. Stone²

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Cited by 3 publications

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Dark matter reconstruction from stellar orbits in the Galactic centre

Lechien,

Heißel,

Grover

et al. 2024

A&A

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Current constraints on distributed matter in the innermost Galactic centre (such as a cluster of faint stars and stellar remnants, dark matter, or a combination thereof) based on the orbital dynamics of the visible stars closest to the central black hole typically assume simple functional forms for the distributions. We aim to take a general model-agnostic approach in which the form of the distribution is not constrained by prior assumptions on the physical composition of the matter. This approach yields unbiased, entirely observation-driven fits for the matter distribution and places constraints on our ability to discriminate between different density profiles (and consequently between physical compositions) of the distributed matter. We constructed a spherical shell model with the flexibility to fit a wide variety of physically reasonable density profiles by modelling the distribution as a series of concentric mass shells. We tested this approach in an analysis of mock observations of the star S2. For a sufficiently large and precise data set, we find that it is possible to discriminate among several physically motivated density profiles. However, for data coming from current and expected next generation observational instruments, the potential for profile distinction will remain limited by the precision of the instruments. Future observations will still be able to constrain the overall enclosed distributed mass within the apocentre of the probing orbit in an unbiased manner. We interpret this in the theoretical context of constraining the secular versus non-secular orbital dynamics. Our results show that while stellar data over multiple orbits of currently known stars will eventually yield model-agnostic constraints for the overall amount of distributed matter within the probe's apocentre in the innermost Galactic centre, an unbiased model distinction made by determining the radial density profile of the distribution is, in principle, out of the measurement accuracy of the current and next-generation instruments. Constraints on dark matter models will therefore remain subject to model assumptions and will not be able to significantly downsize the zoo of candidate models.

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Dark matter reconstruction from stellar orbits in the Galactic centre

Lechien,

Heißel,

Grover

et al. 2024

A&A

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Improvement of graviton mass constraints using GRAVITY’s detection of Schwarzschild precession in the orbit of S2 star around the Galactic Center

Jovanović,

Borka Jovanović,

Borka

et al. 2024

Phys. Rev. D

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Is It Possible to Measure the Lense–Thirring Orbital Shifts of the Short-period S Star S4716 Orbiting Sgr A*?

Iorio

2023

ApJ

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The maximal values of the general relativistic Lense–Thirring (LT) orbital shifts ΔI LT, ΔΩLT, and Δω LT of the inclination I, the longitude of the ascending node Ω, and the perinigricon ω, respectively, of the recently discovered star S4716, which has the shortest orbital period P b = 4.02 yr of all the S stars that orbit the supermassive black hole (SMBH) in Sgr A*, are of the order of ≃5–16 arcseconds per revolution ″ rev − 1 . Given the current error σ ω = 0.°02 in determining ω, which is the most accurate orbital parameter of S4716 among all those affected by the SMBH's gravitomagnetic field through its angular momentum J •, about 48 yr would be needed to reduce σ ω to ≃10% of the cumulative LT perinigricon shift over the same time span. Measuring ΔI LT and ΔΩLT to the same level of accuracy would take much longer. Instead, after just 16 yr, a percent measurement of the larger gravitoelectric (GE) Schwarzschild-like perinigricon shift Δω GE, which depends only on the SMBH's mass M •, would be possible. On the other hand, the uncertainties in the physical and orbital parameters entering Δω GE would cause a huge systematic bias of Δω LT itself. The SMBH's quadrupole mass moment Q 2 • induces orbital shifts as little as ≃0.01–0.05″ rev−1.

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Revisiting stellar orbits and the Sgr A* quadrupole moment

Cited by 3 publications

References 59 publications

Dark matter reconstruction from stellar orbits in the Galactic centre

Dark matter reconstruction from stellar orbits in the Galactic centre

Improvement of graviton mass constraints using GRAVITY’s detection of Schwarzschild precession in the orbit of S2 star around the Galactic Center

Is It Possible to Measure the Lense–Thirring Orbital Shifts of the Short-period S Star S4716 Orbiting Sgr A*?

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