Constraining ultralight bosonic dark matter with Keck observations of S2’s orbit and kinematics
Constraining ultralight bosonic dark matter with Keck observations of S2’s orbit and kinematics
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DOI：
10.1103/physrevd.106.103024
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发表时间：
2022-05
影响因子：
5
通讯作者：
G. Yuan;Z. Shen;Y. S. Tsai;Q. Yuan;Yizhou Fan
中科院分区：
文献类型：
--
作者：
G. Yuan;Z. Shen;Y. S. Tsai;Q. Yuan;Yizhou Fan
超轻玻色子暗物质有望在银河系中心的超大质量黑洞（SMBH）周围形成云。随着SMBH周围恒星运动学观测精度的提高，这种暗物质云的微小影响，包括其引力扰动和与普通物质的直接耦合可能是可检测的。在这项工作中，我们使用Sgr~A* 周围的S2星星的精确轨道测量来寻找标量云的可能证据。我们求解了一阶后牛顿方程，同时考虑了标量云的扩展质量分布和通过Higgs门或光子门相互作用产生的附加耦合引起的频移。此外，我们还研究了气体和恒星残余物的天体物理幂律分量的影响。我们发现S2星星的天体测量和光谱数据与Sgr~A* 的点状质量的假设是一致的。因此，我们得到的新的相互作用和扩展质量的耦合的上限，有和没有从天体物理组件的贡献。在标量质量窗口为3.2 × 10 - 19 ~ 1.6 × 10 - 18 eV之间，Higgs/光子耦合的极限和标量云的扩展质量是最严格的.
Ultralight bosonic dark matter is expected to be able to form a cloud surrounding the supermassive black hole (SMBH) in the Galactic center. With increasing precision of the observations of the stellar kinematics around the SMBH, tiny effects from such a dark matter cloud, including its gravitational perturbation and the direct coupling with the ordinary matter may be detectable. In this work, we search for possible evidence of the scalar cloud using accurate orbital measurements of the S2 star around Sgr~A*. We solve the first order Post-Newtonian equation, considering simultaneously the extended mass distribution of the scalar cloud and the frequency shift induced by the additional coupling via Higgs portal or photon portal interaction. Furthermore, we also investigate the impact of an astrophysical power-law component from the gas and stellar remnants. We find that the astrometric and spectroscopic data of the S2 star are well consistent with the scenario of a point-like mass of Sgr~A*. We thus derive upper limits of the coupling of the new interaction and the extended mass, with and without the contribution from the astrophysical component. The limits of the Higgs/photon coupling and the extended mass of the scalar cloud are the most stringent ones for the scalar mass window between $3.2\times 10^{-19}$~eV and $1.6\times 10^{-18}$~eV.