ESA Science & Technology - Publication Archive
Joint Jupiter Science Definition Team
NASA/ESA Study Team
The Europa Jupiter System Mission (EJSM) is a joint endeavour by ESA and NASA.
This Joint Summary Report (JSR) is intended to provide a high-level description of the following: the science rationale and goals; the mission concept; the NASA and ESA responsibilities and interdependencies; the role of other space agencies; and the costs, schedule, and management approach. The JSR also describes the membership and roles of the JSDT and the engineering study teams that supported them and provides a guide to the extensive documentation that has been developed for the mission concept.
Joint Titan Saturn System Mission Science Definition Team,
ESA Study Team,
NASA Study Team
The Titan Saturn System Mission (TSSM) is a joint endeavour by ESA and NASA.
This Joint Summary Report (JSR) is intended to provide a high level description of the science rationale and goals; the mission concept; the NASA and ESA responsibilities and interdependencies; the role of other space agencies; and the costs, schedule and management approach. It also describes the membership and roles of the JSDT and the engineering study teams that supported them and a guide to the extensive documentation that has been developed for the mission concept.
The Mid-Infrared Instrument (MIRI) is a multipurpose imager, coronagraph, and spectrometer for the James Webb Space Telescope. It provides wavelength coverage from 5 through 28 microns and is an integral contributor to all four of JWST's primary science themes. MIRI is being developed as a partnership between NASA and ESA, with JPL providing the Focal Plane System (FPS, consisting of the detectors, control electronics, and flight software) and the cooler, and a consortium of European astronomical institutes providing the optical bench and structure. The flight FPS is being prepared for delivery to the European Consortium for its integration into the optical bench, while the cooler is nearing its Critical Design Review. We describe the capabilities of the FPS and cooler, present test results and the predicted sensitivity performance of the FPS, and update the current status of each these systems. The research described in this poster was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.
The recycling of matter between the interstellar medium (ISM) and stars are key evolutionary drivers of a galaxy's baryonic matter. The Spitzer and JWST/MIRI wavelengths provide a sensitive probe of circumstellar and interstellar dust and hence, allow us to study the physical processes of the ISM, the formation of new stars and the injection of mass by evolved stars and their relationships on the galaxy-wide scale. We have performed a uniform and unbiased imaging survey of the Large Magellanic Cloud (LMC, 7x7 degrees), using the IRAC (3.6, 4.5, 5.8 and 8 microns) and MIPS (24, 70, and 160 microns) instruments on board the Spitzer Space Telescope (Spitzer) in order to survey the agents of a galaxy's evolution (SAGE): the ISM, young stellar objects (YSOs) and dusty evolved stars (Meixner et al. 2006). Initial results from SAGE have revealed >1000 new YSOs (Whitney et al. 2008), a detailed map of the dust and ISM mass (Bernard et al. 2008) and estimates of the dusty mass-loss return (Srinivsan et al., submitted) of the 30,000 dusty evolved stars (Blum et al. 2006). Here we describe how the powerful capabilities of the JWST MIRI can be used to followup these new discoveries of SAGE-LMC and also how SAGE-like studies can be extended to nearby galaxies.
The SAGE Project is supported by NASA/Spitzer grant 1275598 and MIRI science team work is supported by NASA NAG5-12595.
More than 25 spacecraft from the United States and the Soviet Union visited Venus in the 20th century, but in spite of the many successful measurements they made, a great number of fundamental problems in the physics of the planet remained unsolved [Taylor, 2006; Titov et al., 2006]. In particular, a systematic and long-term survey of the atmosphere was missing, and most aspects of atmospheric behavior remained puzzling. After the Magellan radar mapping mission ended in 1994, there followed a hiatus of more than a decade in Venus research, until the European Space Agency took up the challenge and sent its own spacecraft to our planetary neighbor. The goal of this mission, Venus Express, is to carry out a global, long-term remote and in situ investigation of the atmosphere, the plasma environment, and some aspects of the surface of Venus from orbit [Titov et al., 2001; Svedhem et al., 2007].
Venus Express continues and extends the investigations of earlier missions by providing detailed monitoring of processes and phenomena in the atmosphere and near-space environment of Venus. Radio, solar, and stellar occultation, together with thermal emission spectroscopy, sound the atmospheric structure in the altitude range from 150 to 40 km with vertical resolution of few hundred meters, revealing strong temperature variations driven by radiation and dynamical processes.
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Presentation of the IXO mission concept at the IXO Coordination Group meeting on 20 November 2008.
- IXO mission requirements
- IXO mission analysis
- IXO configuration
- IXO instrument module
- IXO service module
- IXO mirror assembly
- Hubble Status
- The Hubble Cache
- Footprint Finder
- HLA ACS Grism Data
- Scisoft 7.2