Resumen:

Gamma-ray bursts (GRBs) have traditionally been categorized based on their durations. However, the emergence of extended emission (EE) GRBs, characterized by durations higher than 2 seconds and properties similar to short GRBs, challenges conventional classification methods. In this talk, we delve into GRB classification, focusing on a non-supervised machine-learning technique (t-distributed stochastic neighbor embedding, t-SNE) for classification and the identification of extended emission in GRBs. Furthermore, we introduce an innovative tool, ClassipyGRB, designed for astronomers whose research centers on GRBs. This versatile Python3 module enhances the exploration of GRBs by offering interactive visualizations of their light curves and highlighting shared attributes. With ClassipyGRB, astronomers can swiftly compare events, identifying resemblances and exploring their high-frequency characteristics. This tool uses the power of proximity analysis, enabling rapid identification of similar GRBs within seconds.

Resumen:

NGC 2071 is a star-forming region positionally correlated with three unidentified $\gamma$-ray sources detected by the \textit{Fermi} satellite telescope. According to preliminary models, T-Tauri stars could produce $\gamma$-ray emission under specific conditions. We performed a spectral and temporal analysis of the \textit{Fermi} data to determine whether the detected emission was caused by flares occurring in T-Tauri stars. We found that the $\gamma$-ray source can only be detected in the first two years of observations at energies above 100~GeV. In addition, a variability analysis reveals that the expected frequency of events is compatible with flare activity with a minimum X-ray energy of $5 \times 10^{37}~\text{erg}$. These observational results impose, for the first time, a substantial constraint on the energetic of flares in T-Tauri stars that could explain the origin of unknown $\gamma$-ray sources in star-forming regions.

Resumen:

In recent years, massive stellar clusters have received renewed attention as possible contributors to the Galactic component of cosmic rays. The collective action of stellar winds forms superbubbles, which are large, multi-parsec structures. The interacting stellar winds supply large amounts of kinetic energy that could be used to accelerate cosmic rays up to very high energies. The particles interact with the surrounding material producing gamma rays. In this work we study the particle acceleration and interactions in super bubbles produced by the collective interactions of massive young stars. We model the gamma-ray emission expected from these interactions and constrain the production of cosmic rays. We also analyze the observability of the modeled sources by gamma-ray observatories.