Stellar streams are a consequence of the tidal forces produced by a host galaxy on its satellites (i.e. globular clusters and dwarf spheroidals). As the self-gravity of stellar streams is almost negligible, they constitute excellent probes of the gravitational potential of the host galaxy. For this reason, some Milky Way stellar streams have been used …

As part of a work carried out on Magellanic Clouds (MCs) stellar clusters (SCs), we present results in age, metallicity and reddening for Bruck 50, NGC 176, SL 164 and SL 396, applying different methods (equivalent widths, template matching and spectral synthesis) from the SC integrated spectrum. These interesting SCs are useful on determining parameter …

Membership of stars in clusters is very crucial in parameter determination and studies of clusters. We compare results obtained using supervised and unsupervised methods with Gaia DR2 and EDR3 data. We shall provide insights in to what are the suitable methods to be used and compare results using Gaussian Mixture Models and DBScan as well …

The ongoing interaction with the Large Magellanic Cloud (LMC) is revolutionizing our view of the dynamical state of the Milky Way. The perturbations caused by the LMC open new avenues to test the nature of dark matter. Using results from high-resolution N-body simulations, I will describe the two main perturbations caused by the LMC: the …

The analysis of the internal structure of star clusters can provide us important information about their formation and dynamic evolution. Using data from the VISCACHA survey, we studied the spatial distribution of the stars in clusters located at the peripheries of the Large Magellanic Cloud and the Small Magellanic Cloud. We characterized their internal structure …

We present the results of the chemical analysis of 6 star clusters in the inner region of the Small Magellanic Cloud (SMC). We used near infrared spectra obtained with GMOS (GEMINI-S) in the region of Calcium Triplet (CaT) lines of red giant stars belonging to the star clusters and their surrounding fields. We measured radial …

Bulge Globular Cluster have always ben a challange for the determination of their distance and reddening. This is because they are affected by high differential reddening and strong field contamination. In addition, in most of the cases only the RGB is observed since SGB and MS are too faint. However, thank to the advent of …