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tokens: ) suggest that these events, and hence IMBHs, are not equally distributed amongst galaxies but rather they find that the Milky Way is expected to underproduce these events by a factor of 10 2 compared to compact blue galaxies. This means the number of lower mass IMBHs in the Milky Way could be as low as 10 2 . As these young clusters evaporate, if they evaporate, their IMBHs would be left with at most only the few stars within the IMBHs sphere of influence. If there are such low-mass IMBHs threading their way through the Milky Way then Gaia may provide a unique opportunity to spot them. As Gaia (de Bruijne 2012 ) observes a billion or so stars in the Milky Way, making very high-precision measurements of the peculiar motion of the stars, it should observe some systems for which their motions can only be explained with the addition of an IMBH. However, if there are in fact only 10 2 such IMBHs in the Milky Way, and Gaia is only sampling 1 out of every 10 2 stars in the Milky Way, we would expect to detect on order of 1 of these objects. Of course, as with the rest of this letter, caution must be taken when considering such a low number of statistics. The spatial distribution of these systems should not deviate much from their initial distribution, at least not as a result of dynamical friction since for the 10 3 M case dynamical friction should only result in an inward migration of the black hole of 40pc, and only 0.4kpc even for a 10 5 M black hole in 13Gyr (assuming a value of 6 for the Coulomb logarithm). Additionally, the all-sky, X-ray survey provided by eROSITA (Merloni etal. 2016 ), with an anticipated launch data in 2016, will likely provide many more IMBH candidates with its sensitivity and long expected exposure time. 4.3 IMBHs in relation to other black holes Finally, in Table 1 we compile the number and total mass of different types of massive objects [stars, stellar mass black holes (StMBHs), IMBHs and SMBHs] in both our Galaxy and within a sphere with a radius of 100Mpc. Here, we outline how we arrived at these values: in the Milky Way there is one observed SMBH, Sgr A*, with a mass of 4.110 6 M (Ghez etal. 2008 ). Caramete Biermann ( 2010 ) estimate a total number of SMBHs within 100Mpc with masses 10 7 M to be about 2.410 4 and from the mass density provided therein, we estimate a total mass of 2.810 11 M within the same volume. We must be careful to note that while the number of SMBHs within 100Mpc may be larger due to excluding the SMBHs with masses 10 7 , Caramete Biermann ( 2010 ) claim that the total mass is barely dependent on the cutoff due to a flattening of the integral mass function at lower mass. Table 1. The estimated number and total mass of SMBHs, IMBHs, StMBHs and Stars within the Milky Way (left two columns) and within 100Mpc (right two columns). In this work, we have calculated the values for the number of IMBHs within 100Mpc and within the Milky Way. In order to estimate the total mass of the IMBHs, we used