S301 and friends: Measuring the spin of Sgr A*
Abstract
The discovery of S301 (GRAVITY Collaboration et al., 2026) with pericenter distance rp= 280rg and eccentricity e=0.9825, opens the prospect of measuring the spin parameter of Sgr A* through Lense--Thirring (LT) nodal precession. A major obstacle is Newtonian confusion: any non-spherical extended mass distribution can also induce nodal precession. We aim to separate the LT spin signal of S301 from the Newtonian nodal precession. We compare the secular Newtonian torque exerted by a disk or flattened mass distribution on the orbits of S301 and of the apocenter-matched reference stars S2, S55, and S38, using analytic estimates validated by numerical orbit-averaged torque calculations. For a disk or flattened distribution extending beyond the stellar pericenters, the secular Newtonian torque on a highly eccentric orbit is controlled mainly by the apocenter, whereas the LT signal is controlled mainly by the pericenter. Thus stars with apocenters comparable to S301's but much larger pericenters, in particular S2, but also S55, and S38, experience comparable Newtonian torques while having ~ 30 times smaller LT signals (for S2). Their measured precessions, or upper limits on them, can therefore calibrate the mass and orientation of the Newtonian background for subtraction from S301's precession. The Schwarzschild apsidal advance of S301 further rotates the orbit's pericenter relative to any disk, producing a systematic time dependence in the Newtonian contribution, while the LT signal remains fixed by the spin vector. Granularity of the perturber population sets a stochastic floor on this subtraction, which orbit- and star-averaging suppress. With continued GRAVITY+ astrometry and Extremely Large Telescope (ELT) spectroscopy, the in-plane spin projection may be within near-term reach; the full spin vector requires a much longer-term accumulation of the LT apsidal signal.
Related
- Probing departures from Schwarzschild geometry with the S301 star and kilometre-baseline interferometry
- Probing Dark matter-Baryon Interaction with S301--the Fastest Known Star in the Milky Way
- A New Window for Testing the PPN in the Strong-Field Regime: Stellar Rotation of S301
- Catching Up with the Fastest Star in the Galaxy: A Two-Passage GRAVITY+ Campaign to Detect S301's Schwarzschild Precession
- Measuring the Milky Way potential with the phase snail shape curves
BibTeX
@misc{piran2026s301,
title = {{S301 and friends: Measuring the spin of Sgr A*}},
author = {T. Piran and P. Amaro-Seoane and B. Aytac and G. Bourdarot and A. Burkert and D. Calderon and J. Cuadra and F. Eisenhauer and R. Genzel and S. Gillessen and S. Joharle and F. Mang and T. Ott and D. C. Ribeiro and M. Sadun Bordoni and R. Sari},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2607.24931},
eprint = {2607.24931},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2607.24931},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - S301 and friends: Measuring the spin of Sgr A*
AU - T. Piran
AU - P. Amaro-Seoane
AU - B. Aytac
AU - G. Bourdarot
AU - A. Burkert
AU - D. Calderon
AU - J. Cuadra
AU - F. Eisenhauer
AU - R. Genzel
AU - S. Gillessen
AU - S. Joharle
AU - F. Mang
AU - T. Ott
AU - D. C. Ribeiro
AU - M. Sadun Bordoni
AU - R. Sari
PY - 2026
DA - 2026/10/24
PB - arXiv
DO - 10.48550/arxiv.2607.24931
UR - https://arxiv.org/abs/2607.24931
AB - The discovery of S301 (GRAVITY Collaboration et al., 2026) with pericenter distance rp= 280rg and eccentricity e=0.9825, opens the prospect of measuring the spin parameter of Sgr A* through Lense--Thirring (LT) nodal precession. A major obstacle is Newtonian confusion: any non-spherical extended mass distribution can also induce nodal precession. We aim to separate the LT spin signal of S301 from the Newtonian nodal precession. We compare the secular Newtonian torque exerted by a disk or flattened mass distribution on the orbits of S301 and of the apocenter-matched reference stars S2, S55, and S38, using analytic estimates validated by numerical orbit-averaged torque calculations. For a disk or flattened distribution extending beyond the stellar pericenters, the secular Newtonian torque on a highly eccentric orbit is controlled mainly by the apocenter, whereas the LT signal is controlled mainly by the pericenter. Thus stars with apocenters comparable to S301's but much larger pericenters, in particular S2, but also S55, and S38, experience comparable Newtonian torques while having ~ 30 times smaller LT signals (for S2). Their measured precessions, or upper limits on them, can therefore calibrate the mass and orientation of the Newtonian background for subtraction from S301's precession. The Schwarzschild apsidal advance of S301 further rotates the orbit's pericenter relative to any disk, producing a systematic time dependence in the Newtonian contribution, while the LT signal remains fixed by the spin vector. Granularity of the perturber population sets a stochastic floor on this subtraction, which orbit- and star-averaging suppress. With continued GRAVITY+ astrometry and Extremely Large Telescope (ELT) spectroscopy, the in-plane spin projection may be within near-term reach; the full spin vector requires a much longer-term accumulation of the LT apsidal signal.
ER -