|
|
| IBIS: the Gamma-Ray Imager Onboard Integral |
|
| Publication date: 01 Jun 1999 |
|
|
| Integral - the current status |
|
| Publication date: 01 Jun 1999 |
|
|
| JEM-X: the X-ray Monitor on Integral |
|
| Publication date: 01 Jun 1999 |
|
|
| OMC: AN Optical Monitoring Camera for Integral |
| Proceedings of the 3rd Integral Workshop, Taormina 1998 |
| Publication date: 01 Jun 1999 |
|
|
| The Integral Science Data Centre |
| Proceedings of the 3rd INTEGRAL Workshop, Taormina 1998 |
| Publication date: 01 Jan 1999 |
|
|
| INTEGRAL: The Current Status |
| The International Gamma-Ray Astrophysics Laboratory (INTEGRAL) is dedicated to the fine spectroscopy (Delta-E: 2 keV FWHM @ 1.3 MeV) and fine imaging (angular resolution: 12 arcmin FWHM) of celestial gamma-ray sources in the energy range 15 keV to 10 MeV with concurrent source monitoring in the X-ray (3 - 35 keV) and optical (V, 550 nm) range. The mission is conceived as an observatory led by ESA with contributions from Russia and NASA. The INTEGRAL observatory will provide to the science community at large an unprecedented combination of imaging and spectroscopy over a wide range of energies. Most of the observing time will be open to the scientific community. This paper summarises the key scientific goals of the mission, the current development status of the payload and spacecraft and it will give an overview of the science ground segment including data centre, science operations and the key elements of the observing programme |
| Publication date: 01 Sep 1998 |
|
|
| The INTEGRAL Core Observing Programme |
| The Core Programme of the INTEGRAL mission is defined as the portion of the scientific programme covering the guaranteed time observations for the INTEGRAL Science Working Team. This paper describes the current status of the Core Programme preparations and summarizes the key elements of the observing programme.
Letters & Communications, 1999 |
| Publication date: 01 Sep 1998 |
|
|
| 'Integral' - A Challenging Scientific Mission |
| The spectroscopic study of atomic and molecular lines in the infrared, optical and ultraviolet regions of the electromagnetic spectrum has provided us with knowledge and understanding of the physics of normal stars. Spectrallines in the gamma-ray region are produced by new and different processes. These include radioactivity, nuclear excitation, electron- positron annihilation and radiation in the vicinity of magnetic fields. Gamma-ray lines are indicators of all these processes and have now been observed at astrophysical sites.They provide powerful diagnostics for the high-energy processes occurring in some of the most violent and exotic objects in the Universe.
The key features of the Integral satellite will allow us to study in great detail these, and other sites of key interest in today's astrophysical research, with high sensitivity combined with very good energy resolution and very good imaging capabilities (in order to avoid source confusion) using two main instruments, an 'Imager' and a 'Spectrometer'.
|
| Publication date: 01 Aug 1994 |
|
|
| COMPTEL observations of Ti-44 gamma-ray line emission from CAS A |
| The Compton Telescope (COMPTEL) telescope aboard the Compton Gamma-Ray Observatory (CGRO) is capable of imaging gamma-ray line sources in the MeV region with a sensitivity of the order 10-5 photons/(cm²s). During two observations periods in July 1992 and February 1993 the Galactic plane in the region of the young supernova remnant Cas A was observed, showing evidence for line emission at 1.16 MeV from the decay of 44Ti at a significance level of approximately 4 sigma. This is the first time a supernova remnant has been detected in the gamma-ray line from 44Ti decay. Adopting a distance of 2.8 kpc to the Cas A remnant, the measured line flux (7.0 +/- 1.7) x 10-5 photons/(cm²s), can be translated into a 44Ti mass ejected during the Cas A supernova explosion, between (1.4 +/- 0.4) x 10-4 solar mass and (3.2 +/- 0.8) x 10-4 solar mass, depending on the precise value of the 44Ti mean life time and on the precise date of the event. Implications of this result for supernova nucleosynthesis models are discussed. |
| Publication date: 15 Apr 1994 |
|
|
