Contributors to the March Issue/Notes

Notes by Robert A. Oberfell, John Power, John D. O\u27Neill, Arthur M. Diamond, Theodore M. Ryan, C. G. Remmo, and Francis J. Paulson

Contributors to the March Issue/Notes

Notes by Robert A. Oberfell, John Power, John D. O\u27Neill, Arthur M. Diamond, Theodore M. Ryan, C. G. Remmo, and Francis J. Paulson

Current Law Review Digest Series

Series by David S. Landis, John D. O\u27Neill, Arthur A. May, Arthur M. Diamond, Norbert S. Wleklinski, and Francis J. Paulson

Current Law Review Digest Series

Series by David S. Landis, John D. O\u27Neill, Arthur A. May, Arthur M. Diamond, Norbert S. Wleklinski, and Francis J. Paulson

The TIGRE gamma-ray telescope

TIGRE is an advanced telescope for gamma-ray astronomy with a few arcmin resolution. From 0.3 to 10 MeV it is a Compton telescope. Above 1 MeV, its multi-layers of double sided silicon strip detectors allow for Compton recoil electron tracking and the unique determination for incident photon direction. From 10 to 100 MeV the tracking feature is utilized for gamma-ray pair event reconstruction. Here we present TIGRE energy resolutions, background simulations and the development of the electronics readout system

Minute-of-Arc Resolution Gamma ray Imaging Experiment—MARGIE

MARGIE (Minute-of-Arc Resolution Gamma-ray Imaging Experiment) is a large area(∼104 cm2), wide field-of-view (∼1 sr), hard X-ray/gamma-ray (∼20–600 keV) coded-mask imaging telescope capable of performing a sensitive survey of both steady and transient cosmic sources. MARGIE has been selected for a NASA mission-concept study for an Ultra Long Duration (100 day) Balloon flight. We describe our program to develop the instrument based on new detector technology of either cadmium zinc telluride (CZT) semiconductors or pixellated cesium iodide (CsI) scintillators viewed by fast-timing bi-directional charge-coupled devices (CCDs). The primary scientific objectives are to image faint Gamma-Ray Bursts (GRBs) in near-real-time at the low intensity (high-redshift) end of the logN-logS distribution, thereby extending the sensitivity of present observations, and to perform a wide field survey of the Galactic plane