Microquasars are X-ray binary systems harboring black holes that can enter into outburst, during which they become extremely bright, exhibiting relativistic-speed matter ejections. Although we have a rough understanding of what occurs during the outburst cycle, typically between 1 keV and 100 (…)
High energy emission from galactic microquasars
Floriane Cangemi
Microquasars are X-ray binary systems harboring black holes that can enter into outburst, during which they become extremely bright, exhibiting relativistic-speed matter ejections. Although we have a rough understanding of what occurs during the outburst cycle, typically between 1 keV and 100 keV, what happens at energies beyond 200 keV is much less clear. A non-thermal component is sometimes detected beyond 200 keV for some of these sources. The origin of this component is not yet established and is a subject of debate. In this presentation, I will present the results of analyses from the INTEGRAL satellite beyond 200 keV for different sources where this component is detected. I will discuss the spectral and polarimetric characteristics of this component and explore their implications for the nature of the emission process responsible for this component.
