Poster abstract details

M87 is an Active Galactic Nucleus (AGN) in the center of a large elliptical galaxy located about 55 million light years away in the Virgo Cluster. Over the past years M87 has been detected up to TeV (10^{12}eV) energies. Up to now only one subclass of AGNs is suspected to emit radiation in the TeV range - the so called Blazars. A Blazar is an AGN with one of its relativistic jets pointing right in the direction of the observer. The particles in the jet are relativistic, what leads to an increase in the observed luminosity and a shift of the whole Blazar spectrum to higher (even TeV) energies. This process is called 'Relativistic Beaming'. Contrary to the most TeV-AGNs it seems that M87 is not a Blazar. The pivotal question is whether the TeV emission of M87 is produced in the vicinity of the central Supermassive Black Hole (SMBH) or in one of the knots in the jet of M87. Many authors favor the core of M87 as production site of its TeV emission. That raises the question if radiation in this energy range would even be able to escape the inner region of M87. AGNs are assumed to contain several low-energetic radiation fields especially near its center. This low-energetic radiation could lead to an attenuation or even to an annihilation of TeV radiation that might be produced near the core. Probably the most important source is the accretion flow surrounding the SMBH. We try to calculate the strength of attenuation of TeV photons from the jet by low-energy photons from the accretion flow, assuming that the flow is a Radiatively Inefficient Accretion Flow (RIAF).