F. R. Ferraro, E. Vesperini, B. Lanzoni, D. Romano, L. Origlia, C. Pallanca, C. Fanelli, F. Calura, E. Dalessandro, D. Massari, G. Zullo, M. Cadelano

The discovery of the complex stellar populations hosted in two massive stellar systems in the Galactic bulge, namely Terzan5 and Liller 1, posed intriguing questions about their origin. Despite their globular cluster appearance, they host sub-populations with significantly different ages (several Gyrs) and metallicities (about 1 dex) tracing a chemical abundance pattern that is consistent only with that observed in the bulge. These surprising properties can be naturally explained in the context of a self-enrichment scenario, opening the possibility that they could be the remnants of primordial massive structures that contributed to the bulge formation (the so-called Bulge Fossil Fragments, BFFs) capable of retaining supernova ejecta within their potential well. In this paper we present a first attempt to quantify the expected contribution of BFFs to the gravitational wave emission. In particular, by adopting Terzan5 as prototype of BFF, using its chemical evolutionary model, and following a scaling relation derived for globular clusters, we present a first-guess estimate of the number of binary black hole (BH) mergers expected in this stellar system. Within the adopted simplifying assumptions and the uncertainties about the initial conditions of the proto-Terzan 5 system, we find that several hundreds of binary BH mergers are expected, a number that is between 15 and 250 times larger than that produced by a typical globular cluster. Hence, this study identifies in the BFF family a new population of stellar systems potentially able to produce a significant number of gravitational wave emitters, that has not been considered in any previous investigation. Moreover we speculate that they could also be the natural place where BHs with masses above 60 Msun and even intermediate-mass BHs can form via repeated dynamical interactions.