Abstract
Massive star-forming regions assemble a large number of young stars with remnants of stellar evolution and a very dense environment. Therefore, particles accelerated in supernova remnants and pulsar wind nebulae encounter optimal conditions for interacting with target material and photon fields, and thus produce gamma-ray emission. However, observations are challenging because multiple phenomena may appear entangled within the resolution of current gamma-ray telescopes. We report on MAGIC observations aimed to understand the nature of the emission from the star-forming region W51 and the unidentified source HESSJ1857+026. While gamma-ray emission from W51 is dominated by the interaction of the supernova remnant W51C with dense molecular clouds, HESSJ1857+026 is associated to the pulsar wind nebula from PSRJ1856+0245. However, an additional source is resolved north of HESSJ1857+026, with sufficient separation to determine that it cannot be powered by the same pulsar. We search for multiwavelength data to determine the origin of the new source.
Highlights
MAGIC are two imaging atmospheric Cherenkov telescopes characterized by its ∼50 GeV threshold, the lowest achieved in ground-based stereo observations of veryhigh-energy (VHE) gamma rays
The science cases for MAGIC include the observation of Galactic sources of VHE gamma rays: to resolve the multiple components that may overlap along the line of sight; to understand the physical processes that produce the observed gamma-ray emission; and to assess the contribution that these sources may have to the Galactic cosmic rays
We suggest that possible origins of the gamma-ray emission from MAGIC J1857.6+0297 are: a pulsar wind nebula (PWN) whose progenitor star created a cavity in the cloud prior to its explosion [26]; or particle acceleration
Summary
MAGIC are two imaging atmospheric Cherenkov telescopes characterized by its ∼50 GeV threshold, the lowest achieved in ground-based stereo observations of veryhigh-energy (VHE) gamma rays. The science cases for MAGIC include the observation of Galactic sources of VHE gamma rays: to resolve the multiple components that may overlap along the line of sight; to understand the physical processes that produce the observed gamma-ray emission; and to assess the contribution that these sources may have to the Galactic cosmic rays. In this contribution, we discuss the particular cases of W51 [2] and HESSJ1857+026 [3]. The configuration and performance of the telescopes at that time is described in [4]
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