Addressing the Challenges in NextGen Decision Making

DTFAWA-10-X-80005, Annex 9NASA provided a broad overview of flight crew decision making and training challenges expected to result from the implementation of NextGen automation, including decision support automation. Recommendations included the following human factors recommendations and caveats for the design of future flight deck systems: - Pilots Need Accurate Mental Models of Automated Systems - Systems Awareness Is Key to Situation Awareness - Changes Must Be Highlighted - CRM \u2018Monitor and Challenge\u2019 Philosophy for Flight Crew Must Also Apply to Flight Deck Automatio

Proceedings : Outer Planet Probe Technology Workshop, May 21-23, 1974, Sections I through IV.

Photocopy. Springfield, Va. : National Technical Information Service, 1974. -- 28 cm."Prepared under contract no. NAS2-7541.""NASA CR 137543."Includes bibliographical references.Mode of access: Internet

Optics studies of the planned SOFIA instrument SPICA/LISA

The proposed Spectral-Photometric Far-Infrared Camera (SPICA) will use the 2.5m SOFIA telescope to image astronomical objects at wavelengths between 20 and 220 mm. A low-resolution spectrometer channel will record simultaneously individual diffraction limited spectra from several tens to several hundreds of spatial positions on the sky. For both observing modes large format far-infrared arrays will be required. Their physical size would be in the range of 40 × 40 mm2 to 120 × 120 mm2. This extended geometry and the large fields-of-view are the major design drivers for the instrument optics. A concept study with a common collimator and three individual imagers showed that geometrical aberrations remain small compared to diffraction effects, even when standard manufacturing and alignment tolerances are included. An additional study also taking diffraction effects into account, showed the feasibility of a 40 - 70 mm spectrometer using a 64 × 64 element array and an image slicer to image a 26 × 46 square arcseconds sky field at a spectral resolution of ~30. The overall transmission of the spectrometer will be at the order of 20%. While the camera will study the morphology of objects, namely of their coldest matter components at 10 to 20 K, the spectrometer will determine the spectral energy distribution as well as broad band spectral features in galactic and extragalactic objects at the highest sensitivity