Pinpointing the TeV Gamma-ray Emission Region in M87 Using TeV and 43 GHz Radio Observations

Details Pinpointing the TeV Gamma-ray Emission Region in M87 Using TeV and 43 GHz Radio Observations Pinpointing the TeV Gamma-ray Emission Region in M87 Using TeV and 43 GHz Radio Observations

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.3006b&link_type=abstract

American Astronomical Society, HEAD meeting #11, #30.06; Bulletin of the American Astronomical Society, Vol. 41, p.702

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The giant radio galaxy M87 is located at a distance of 16.7 Mpc and harbors a supermassive black hole (6 billion solar masses) in its center. M87 was the first radio galaxy known to emit TeV gamma-rays. The structure of its relativistic plasma jet, which is not pointing towards our line of sight, is spatially resolved in X-ray (Chandra), optical and radio observations. In spring 2008, the three TeV observatories VERITAS, MAGIC and H.E.S.S. coordinated their observations in a joint campaign with a total observation time of approx. 120 hours. During the same time M87 was intensively monitored by the VLBA at 43 GHz with a spatial resolution of 30x60 Schwarzschild radii, starting to resolve the jet collimation region. In February, strong and rapid day-scale TeV flares were detected. The VLBA observations showed that the radio flux
density of the unresolved core began to rise at the time of the TeV flares and eventually reached levels above any previously seen at these frequencies. New jet components appeared during the flare. The temporal coincidence of the TeV and radio flares indicates that they are related and provides the first experimental evidence that the TeV radiation originates from the close vicinity of the radio core, thought to be coincident with the central black hole. The recent results and an outlook will be presented.

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