Expected Sensitivity of the Nuclear Compton Telescope to Gamma-Ray Line Emission

Details Expected Sensitivity of the Nuclear Compton Telescope to Gamma-Ray Line Emission Expected Sensitivity of the Nuclear Compton Telescope to Gamma-Ray Line Emission

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008head...10.2812c&link_type=abstract

American Astronomical Society, HEAD meeting #10, #28.12

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The Nuclear Compton Telescope (NCT) is a balloon-borne soft gamma-ray (0.2-10 MeV) telescope designed to study astrophysical sources of nuclear line emission and gamma-ray polarization. NCT consists of twelve 3D position-sensitive germanium strip detectors. The ultra-compact design and new technologies allow NCT to achieve high efficiency with excellent spectral resolution and background reduction. We are currently preparing for a conventional balloon flight ( 36 hr) of the NCT instrument from New Mexico in September 2008 and a long-duration balloon flight (LDBF) ( 20 days) from Australia in December 2009. Here we focus on the LDBF in 2009. Our source and background simulations are performed using the Monte Carlo simulation package MGGPOD, and events are reconstructed using the Medium Energy Gamma-ray Astronomy library (MEGAlib). We use the same tools that were successfully used for background simulations of the 2005 prototype flight (see J. Bowen, this conference). Sensitivity is optimized using standard cuts such as photon energy, angular resolution measure (ARM), and event quality factor. In this work, we present realistic line sensitivities for NCT for the LDBF in 2009.

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