KSP: Large Magellanic Cloud Survey

Abstract

The Large Magellanic Cloud (LMC) is a unique galaxy hosting extraordinary objects, including the star-forming region 30 Doradus (the most active starforming region in the local group of galaxies), the super star cluster R136 (an exceptional cluster with a large concentration of very massive O and Wolf-Rayet stars), supernova SN1987A (the closest supernova in modern times), and the puzzling 30 Dor C superbubble (a rare superbubble with non-thermal emission). As a satellite of the Milky Way, it is one of the nearest star-forming galaxies, and a very active one; it has one-tenth of the star formation rate of the Milky Way, distributed in only about two percent of its volume. This activity is attested by more than 60 supernova remnants (SNRs), dozens to hundreds of HII regions, and bubbles and shells observed at various wavelengths, all of which promise fruitful gamma-ray observations. The LMC is seen nearly face-on at high Galactic latitude, and hence source confusion, line of sight crowding, and interstellar absorption do not hamper these studies, in contrast to the case for the plane of our Galaxy. It is therefore a unique place to obtain a significantly-resolved global view of a star-forming galaxy at very high energies. In addition, the distance to the LMC is known to the few percent level, thus allowing precise luminosity measurements to be made, something which is often very difficult for Galactic sources. The current Fermi-LAT and H.E.S.S. instruments have opened the way for a study of the LMC by CTA. Observations with these telescopes have revealed a small number of sources, some of uncertain nature. With CTA, we would have a unique opportunity to further and deeper explore the entire LMC. With its unprecedented sensitivity and angular resolution, CTA will