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Full-Text Articles in Physical Sciences and Mathematics
Comptel Observations Of Cosmic Gamma‐Ray Bursts, C Winkler, K Bennett, H Bloemen, H Deboer, W Collmar, A Connors, R Diehl, L O. Hanlon, J W. Den Herder, W Hermsen, L Kuiper, R M. Kippen, G G. Lichti, J Lockwood, Mark L. Mcconnell, D Morris, James M. Ryan, V Schonfelder, G Stacy, H Steinle, A W. Strong, B Swanenburg, B G. Taylor, M Varendorff, C De Vries, O R. Williams, M Busetta
Comptel Observations Of Cosmic Gamma‐Ray Bursts, C Winkler, K Bennett, H Bloemen, H Deboer, W Collmar, A Connors, R Diehl, L O. Hanlon, J W. Den Herder, W Hermsen, L Kuiper, R M. Kippen, G G. Lichti, J Lockwood, Mark L. Mcconnell, D Morris, James M. Ryan, V Schonfelder, G Stacy, H Steinle, A W. Strong, B Swanenburg, B G. Taylor, M Varendorff, C De Vries, O R. Williams, M Busetta
Space Science Center
The imaging γ‐ray telescope COMPTEL on board NASA’s Compton Gamma‐Ray Observatory (GRO) has observed many cosmic gamma‐ray bursts during the early mission phase of GRO. COMPTEL records time‐resolved burst spectra over 0.1 MeV to 10 MeV energies, and, for the first time, produces direct single‐telescope gamma‐ray images (0.8–30 MeV) of cosmic gamma‐ray bursts occurring in its 1 sr field of field.
Comptel Images Locations Of Gamma‐Ray Bursts, M Varendorff, K Bennett, H Deboer, M Busetta, H Bloemen, W Collmar, A Connors, R Diehl, J W. Den Herder, W Hermsen, R M. Kippen, L Kuiper, G G. Lichti, J Lockwood, Mark L. Mcconnell, D Morris, R Much, James M. Ryan, V Schonfelder, G Stacy, H Steinle, A W. Strong, B Swanenburg, C De Vries, C Winkler
Comptel Images Locations Of Gamma‐Ray Bursts, M Varendorff, K Bennett, H Deboer, M Busetta, H Bloemen, W Collmar, A Connors, R Diehl, J W. Den Herder, W Hermsen, R M. Kippen, L Kuiper, G G. Lichti, J Lockwood, Mark L. Mcconnell, D Morris, R Much, James M. Ryan, V Schonfelder, G Stacy, H Steinle, A W. Strong, B Swanenburg, C De Vries, C Winkler
Space Science Center
The γ‐ray telescope COMPTEL onboard GRO has so far located 6 gamma‐ray bursts which occurred in its ∼1 sr field of view. The positions of the sources were derived by the maximum‐entropy method. Systematic and statistical uncertainties for the four strongest bursts are approximately 1° to 2° and can be reduced in future analysis.