The variable spectrum of Sagittarius A*

I will report on new simultaneous observations and modeling of the millimeter, near-infrared, and X-ray flare emission of the source Sagittarius A* (SgrA*) associated with the super-massive (4x10$^6 solar masses) black hole at the Galactic center.
The observations have been carried out using the NACO adaptive optics (AO) instrument at the European Southern Observatory's Very Large Telescope and the ACIS-I instrument aboard the Chandra X-ray Observatory, the LABOCA bolometer at the Atacama Pathfinder Experiment (APEX), and the CARMA mm telescope array at Cedar Flat, California.
The data suggests that adiabatically expanding source components either have a bulk motion greater than 0.01c  or the expanding material contributes to a corona or disk, confined to the immediate surroundings of SgrA*.
We find that the flaring state can be explained with a Synchrotron Self-Compton model involving up-scattered sub-millimeter photons from a compact source component.
~