|Authors:||A.E. Piatti 1,2, N. Hwang 3, A.A. Cole 4, M.S. Angelo 5, B. Emptage 4|
|Affiliations:||(1) Consejo Nacional de Investigaciones Científicas y Técnicas, Buenos Aires, Argentina; (2) Observatorio Astronómico de Córdoba, Córdoba, Argentina; (3) Korea Astronomy and Space Science Institute, Daejeon, Korea; (4) School of Natural Sciences, University of Tasmania, Hobart, Australia; (5) Laboratório Nacional de Astrofísica, Itajubá, Brazil|
|Accepted by:||Monthly Notices of the Royal Astronomical Society|
We present results obtained from spectroscopic observations of red giants located in the fields of the Large Magellanic Cloud (LMC) globular clusters (GCs) NGC 1928 and NGC 1939. We used the GMOS and AAOmega+2dF spectrographs to obtain spectra centred on the Ca II triplet, from which we derived individual radial velocities (RVs) and metallicities. From cluster members we derived mean RVs of RV NGC 1928 = 249.58$\pm$4.65 km/s and RV NGC 1939 = 258.85$\pm$2.08 km/s, and mean metallicities of [Fe/H] NGC 1928 = −1.30$\pm$0.15 dex and [Fe/H] NGC 1939 = −2.00$\pm$0.15 dex. We found that both GCs have RVs and positions consistent with being part of the LMC disc, so that we rule out any possible origin but that in the same galaxy. By computing the best solution of a disc that fully contains each GC, we obtained circular velocities for the 15 known LMC GCs. We found that 11/15 of the GCs share the LMC rotation derived from HST and Gaia DR2 proper motions. This outcome reveals that the LMC disc existed since the very early epoch of the galaxy formation and experienced the steep relatively fast chemical enrichment shown by its GC metallicities. The four remaining GCs turned out to have circular velocities not compatible with an in situ cluster formation, but rather with being stripped from the SMC.