Globular clusters ( GCs ) have long been recognized as being amongst the oldest objects in the Galaxy . As such , they have the potential of playing a pivotal role in deciphering the Milky Way ’ s early history . Here we present the first spectroscopic study of the low-mass system ESO452-SC11 using the AAOmega multifibre spectrograph at medium resolution . Given the stellar sparsity of this object and the high degree of foreground contamination due to its location toward the Galactic bulge , very few details are known for this cluster – there is no consensus , for instance , about its age , metallicity , or its association with the disk or bulge . We identify five member candidates based on common radial velocity , calcium-triplet metallicity , and position within the GC . Using spectral synthesis , the measurement of accurate Fe-abundances from Fe-lines , and abundances of several \alpha - , Fe-peak , and neutron-capture elements ( Si , Ca , Ti , Cr , Co , Ni , Sr , and Eu ) is carried out , albeit with large uncertainties . We find that two of the five cluster candidates are likely non-members , as they have deviating iron abundances and [ \alpha /Fe ] ratios . The cluster mean heliocentric velocity is 19 \pm 2 km s ^ { -1 } with a velocity dispersion of 2.8 \pm 3.4 km s ^ { -1 } , a low value in line with its sparse nature and low mass . The mean Fe-abundance from spectral fitting is -0.88 \pm 0.03 dex , where the spread is driven by observational errors . Furthermore , the \alpha -elements of the GC candidates are marginally lower than expected for the bulge at similar metallicities . As spectra of hundreds of stars were collected in a 2-degree field centered on ESO452-SC11 , a detailed abundance study of the surrounding field was also enabled . The majority of the non-members have slightly higher [ \alpha /Fe ] ratios , in line with the typical nearby bulge population . A subset of the spectra with measured Fe-peak abundance ratios shows a large scatter around solar values , albeit with large uncertainties . Furthermore , our study provides the first systematic measurements of strontium abundances in a Galactic bulge GC . Here , the Eu and Sr abundances of the GC candidates are broadly consistent with a disk or bulge association . Recent proper motions and our orbital calculations place ESO452 on an elliptical orbit in the central 3 kpc of the Milky Way , establishing a firm connection with the bulge . Finally , while the radial velocities and preferential position of a dozen of stars outside the GC radius appear to imply the presence of extra-tidal stars , their significantly different chemical composition refutes this hypothesis .