INTRODUCTION - Intro on BH-XRBs (quiescence + outburst, typical binary properties,...) We only consider those dynamical BHs with a constrain on both of the masses (i.e. BH mass and mass ratio from blackCAT). We remove from the sample those systems with an intermediate mass donor: SAX J1819.3-2525 (Md ≈ 4.0 M⊙), GRO J1655-40 (Md ≈ 2.5 M⊙), 4U 1543-475 (Md ≈ 2.3 M⊙), as GCs are typically much older. It has long ben recognised that globular clusters (GCs) are factories of stellar exotica such as X-ray binaries (XRBs; see e.g. and ). Despite the total mass of GCs accounting for only 0.1% of the mass of the Galaxy (), GCs produce XRBs 100 times more efficiently than the Galactic field via the dynamical formation channel [...]. All the XRBs found so far in Galactic GCs harbour a neutron star (NS). There is evidence for the presence of two BHs in M22 () and one in M62 (), and there is another BH candidate in an extra-Galactic GC (). However, these candidates lack a dynamical confirmation of the nature of the accreting source. More indirect evidence comes from the study of the radial distribution of different types of stars in a GC. attribute the lack of mass segregation in the GC NGC 6101 to the presence of a sub-population of BHs. Preliminary studies based on encounter-rate calculations and time-scale arguments suggested that BHs would tend to form a subsystem segregated to the center of the cluster via the process of mass segregation. Subsequent scatterings would eject such BHs from the cluster. With the advent of detailed N-body and Monte Carlo simulations of the dynamical evolution of a GC, it has become clear that up to hundreds [...] BHs can be retained in a GC, depending on the initial cluster properties [...] and on the size of the natal kick (NK) BHs receive at birth (see e.g. ; [...]). If (some) BHs are retained, they can potentially form a binary system with a stellar companion via 3-body dynamical interactions. For instance, if the BH passes by a binary formed by two stars, the gravitational interaction between the three bodies can lead to the exchange of the lightest component in the binary with the BH. Such binary can then undergo subsequent scatterings which build up its peculiar velocity with respect to the average motion of the stars in the cluster. If at the same point such a velocity is larger that the GC escape velocity, the binary escapes. The topic of binaries formed by a BH and a stellar component in GCs has been covered previously by and . [...]. Up to date, the population of field BH transients (BHTs) amounts to 19 objects (). Their scale height above the Galactic plane is remarkably similar to the scale height of NS-XRBs (). A large fraction (30%) of the BHTs are located at a large distance z from the Galactic plane (z ≳ 1 kpc). One way of explaining this offset, is to launch the binary out of the birth-plane as a consequence of the NK to the BH. An alternative way to explain such high-z systems is through formation and consequence ejection of the BHT (or of the progenitor of the BHT) from GCs, whose typical scale height is ≈1 kpc. A possible globular cluster origin for BH-XRBs was already suggested by for the source XTE J1118. The eccentricity of the orbit around the Galactic centre as well as the velocity components, makes the kinematics of this systems similar to that of halo stars. Furthermore, X-ray spectral fitting suggests a low metallicity for the reflector medium, also consistent with an halo object . In this Paper, we analyse the data resulting from 2000 GC models simulated with the MOCCA code and look for escaping binaries containing a BH and a low-mass stellar companion. After accounting for the binary evolution and Galactic orbit of such escaping binaries, we compare their orbital, kinematic, and accretion properties with those of the observed BHTs. MOCCA DATABASE 1973 models. OBSERVATIONS - orbital period and component masses distribution - age and metallicity constraints on the donor There’s evidence for super-solar metallicity in the optical spectra of a few donors in BHTs: V404 Cyg ; V4641 Sgr ; XTE J1118+480 and ; GRO J1655-40 and ; A0620-00 . In all of these cases but one, a solar metallicity was assumed for the donor star as binaries containing a BH are widespreadly thought of having formed in the Galactic thin disc where most of the massive stars reside. The donor chemical enhancement in heavy elements is explained via pollution of its atmosphere from the the ejecta material of the SN that formed the BH. An origin in a globular cluster has not been contemplated so far, except for the binary XTE J1118-480. assumes different metallicity for the companion star, either solar or less than solar (typical of a thick disc and of the halo). For the three different metallicities, the donor is required to accrete a different amount of mass for pollution to cause the observed abundances. Neither of the models was preferred by their results. New spectroscopic data allowed the same authors to revisit the chemical enrichment study to find that a halo or thick disc initial metallicity for the companion star produce worse fits than a solar metallicity, in disagreement with the finding on the metallicity of the reflector medium by . If the system was born in the Galactic plane, a NK is required to launch the system into the current halo-type orbit. The spatial distribution of BHTs We take the dynamical BHs in X-ray transients from the _BlackCAT_ catalogue of , considering only those ones with a confirmed distance, i.e. we exclude SWIFT J1357.2-0933 (d > 2.29 kpc), 1H 1659-487 (d > 6 kpc) and GS 1354-64 (d ≈ 25 kpc). cumulative plot of z-distribution The spatial distribution of globular clusters