LAUSR

The detection of the gravitational waves (GWs) emitted in the capture process of a compact object by a massive black hole (MBH) is known as an extreme-mass ratio inspiral (EMRI) and represents a unique probe of gravity in the strong regime and is one of the main targets of LISA. The possibility of observing a compact-object EMRI at the Galactic Centre (GC) when LISA is taking data is very low. However, the capture of a brown dwarf (BD), an X-MRI, is more frequent because these objects are much more abundant and can plunge without being tidally disrupted. An X-MRI covers some $\sim 10^8$ cycles before merger, and hence stay on band for millions of years. About $2\times 10^6$ yrs before merger they have a signal-to-noise ratio (SNR) at the GC of 10, $10^4$ yrs several thousands, and $10^3$ yrs before the merger a few $10^4$. Based on these values, this kind of EMRIs are also detectable at neighbour MBHs, albeit with fainter SNRs. We calculate the event rate of X-MRIs at the GC taking into account the asymmetry of pro- and retrograde orbits on the location of the last stable orbit. We estimate that at any given moment, and using a conservative approach, there are of the order of $\gtrsim\,20$ sources in band. From these, $\gtrsim\,5$ are highly eccentric and are located at lower frequencies, and about $\gtrsim\,15$ are circular and are at higher frequencies. Due to their proximity, X-MRIs represent a unique probe of gravity in the strong regime. The mass ratio for a X-MRI at the GC is $q \sim 10^8$, i.e., three orders of magnitude larger than stellar-mass black hole EMRIs. Since backreaction depends on $q$, the orbit follows closer a standard geodesic, which means that approximations work better in the calculation of the orbit. X-MRIs can be sufficiently loud so as to track the systematic growth of their SNR, which can be high enough to bury that of MBH binaries.