CHANDRA/VLA Follow-up of TeV J2032+4131, the Only Unidentified TeV Gamma-ray Source

Details CHANDRA/VLA Follow-up of TeV J2032+4131, the Only Unidentified TeV Gamma-ray Source CHANDRA/VLA Follow-up of TeV J2032+4131, the Only Unidentified TeV Gamma-ray Source

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003head....7.1022b&link_type=abstract

American Astronomical Society, HEAD meeting #7, #10.22; Bulletin of the American Astronomical Society, Vol. 35, p.863

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Scientific paper

The HEGRA Cherenkov telescope array group recently reported a steady and extended unidentified TeV gamma-ray source lying at the outskirts of Cygnus OB2. This is the most massive stellar association known in the Galaxy, estimated to contain ˜2600 OB type members alone. It has been previously argued that the large scale shocks and turbulence in such associations may play a role in accelerating Galactic cosmic rays. Indeed, Cyg OB2 also coincides with the MeV-GeV range unidentified EGRET source, 3EG 2033+4118. We report on the near-simultaneous follow-up observations of the extended TeV source region with the CHANDRA X-ray Observatory and the Very Large Array (VLA) radio telescope obtained in order to explore this possibility. Analysis of the CO, HI, and IRAS 100 micron emissions shows that the TeV source region coincides with an outlying sub-group of powerful OB stars which have evacuated or destroyed much of the ambient atomic, molecular and dust material, and which may be related to the very high-energy emissions. An interesting SNR-like structure is also revealed near the TeV source region in the CO, HI and radio emission maps. Applying a numerical simulation which accurately tracks the radio to gamma-ray emission from primary hadrons as well as primary and secondary e+/-, we find that the broadband spectrum of the TeV source region favors a predominantly nucleonic - rather than electronic - origin of the high-energy flux, though deeper X-ray and radio observations are needed to confirm this. A very reasonable, ˜0.1 conversion efficiency of Cyg OB2's extreme stellar wind mechanical luminosity to nucleonic acceleration to PeV (1015 eV) energies is sufficient to explain the multifrequency emissions.
This research was supported by NASA & other contracts & grants

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