Recommended Priorities for NASA's Gamma Ray Astronomy Program 1996-2010: Report of the Gamma Ray Astronomy Program Working GroupNational Aeronautics and Space Administration, Goddard Space Flight Center, 1997 - Electronic government information - 48 pages |
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Common terms and phrases
acceleration accretion angular resolution arcmin arcsec arcsecond array astrophysics balloon program BATSE black holes blazars capabilities CdZnTe CGRO Cherenkov cm² cm2 s¹ COMPTEL Compton scattering Compton telescope cosmic rays counterparts detection detectors diffuse EGRET electron energy range energy resolution error boxes field-of-view flares flux sensitivity focusing future missions galactic plane galaxy gamma gamma-ray astronomy gamma-ray bursts gamma-ray emission gamma-ray line gamma-ray sources gamma-ray telescopes GRAPWG ground-based halo halo models hard X-ray hard X-ray band high-energy gamma-ray imaging important improvement instruments INTEGRAL interactions launch line emission low-energy measurements ments MeV range microstrip MIDEX mission concepts models NASA neutron stars nonthermal novae nucleosynthesis objects Observatory optical orders of magnitude OSSE particle photons positron pulsars radiation radio require RXTE searches Seyfert sion SMEX solar spacecraft spectra spectroscopy spectrum supernova remnants tion Type II supernovae unidentified X-ray and gamma-ray
Popular passages
Page 6 - MeV line have revealed a broad, patchy longitude distribution that is very different from that of the 0.511 MeV line which is strongly peaked at the galactic center.
Page 7 - In addition to the galactic longitude and latitude distribution of the 1.809 MeV line emission, information on the origin of the 26Al can also be obtained from studies of the shape of the line.
Page 12 - Very little is known about this portion of the jet. Yet it is precisely the region where the most important physics occurs: the formation of the jet, the acceleration of the energetic particles, the collimation of the flow into a narrow cone, and the acceleration of the flow to Lorentz factors...
Page 7 - MeV, consistent with the de-excitation of excited states in 12C and 16O produced by accelerated particle interactions. Moreover, the intensity of these lines is roughly two orders of magnitude greater than that expected from irradiation by low-energy cosmic rays with energy density equal to that of the local galactic cosmic rays.
Page 14 - There is strong statistical evidence that some of the EGRET unidentified sources in the galactic plane are supernova remnants. Unfortunately, the identifications are somewhat ambiguous, and improved angular resolution is needed to confirm them.
Page 13 - The low-energy portion of the cosmic diffuse spectrum (10 keV to 60 keV) is characterized by a bremsstrahlung spectral form that can be approximated by a power-law segment of energy index -0.4. The energy spectrum transitions to a power law of index -1.6 above 60 keV.
Page 20 - B development stage. The two main instruments onboard are a spectrometer which employs high-spectral-resolution germanium detectors and an imager which employs high-spatial-resolution arrays of cadmium telluride and cesium iodide detectors.
Page 8 - The gamma-ray emission from molecular clouds arises from the same cosmic-ray interactions with matter which produce the general galactic diffuse emission. Molecular clouds provide a means to study these processes and the galactic cosmic rays in localized regions of the galaxy.
Page 14 - Many of the highlatitude unidentified sources show spectral and time variations similar to those of the identified gamma-ray emitting blazars. It is reasonable to anticipate that those sources are similar to the previously identified blazars.
Page 12 - In a few well-monitored objects, there is a close association between flares seen at millimeter to optical wavelengths and high gamma-ray states (eg, PKS 0528+134 and 3C-279) and between UV to X-ray and very high-energy gamma-ray emission (eg, Mkn 421).