Speaker
Description
Estimating the spin of SgrA$^*$ is one of the current challenges we face in understanding the center of our Galaxy. In the present work, we show that detecting the gravitational waves (GWs) emitted by a brown dwarf inspiraling around SgrA$^*$ will allow us to measure the mass and the spin of SgrA$^*$ with unprecedented accuracy. Such systems are known as extremely large mass-ratio inspirals (XMRIs) and are expected to be abundant and loud sources in our galactic center. We consider XMRIs with a fixed orbital inclination and two scenarios for SgrA$^*$'s spin ($s$): A highly spinning scenario where $s$=0.9 and a low spinning scenario where $s$=0.1. For both cases, we obtain the number of circular and eccentric XMRIs expected to be detected by space-borne GW detectors like LISA and TianQin. We later perform a Fisher matrix analysis to show that by detecting a single XMRI the mass of SgrA$^*$ can be determined with an accuracy ranging from 0.017 and 0.06 solar masses, while the spin can be measured with an accuracy between 1.7$\times$10$^{-7}$ and 7.5$\times$10$^{-4}$.
