Data-driven analysis of Dark Matter Self-Annihilation signal from some of the prospective astrophysical sources.

	With the growing interest in indirect detection for dark matter (DM) signature, our work aims to investigate the signal originating from the self-annihilation of DM candidates. The methods for targeting the DM signal are two-fold, on one hand, we explore the gamma rays resulting from DM particles. On the other hand, we focus on complementary radio properties. Such analysis is challenging because of astrophysical emissions of various nature. For finding the DM signals, we performed the analysis of gamma-ray data from DM rich Ultra-Faint Dwarf galaxies (UFDs), including Triangulum-II and Tucana-II, detected by the Fermi Large Area Telescope (Fermi-LAT). For Triangulum-II, the nondetection of DM annihilation signals provided limits on the theoretical models that are in good agreement with similar analyses performed by many international research groups. In the case of Tucana-II, we observed a faint emission from its location and our analysis at best hints that such emission might be related to the DM annihilation signal. We have also examined the electromagnetic radiation over a wide range, from gammaray down to radio frequencies appearing from the low surface brightness galaxies (LSBs) and a class of newly discovered UFDs. For radio emission, we investigated the data detected by the very large area (VLA) and Giant Metrewave Radio Telescope (GMRT). From our study, we found that for DM annihilation radio limits could be competitive with gamma-rays. Moreover, we also check whether the forthcoming mission like Cherenkov Telescope Array (CTA) and Square Kilometer Array (SKA) will be able to detect any positive gamma-ray or radio emission from them.