Ultraviolet imager for the International Solar Terrestrial Physics Mission

Torr, D. G.

doi:10.1117/12.149175

Cited by 4 publications

(3 citation statements)

References 3 publications

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“…All these scientific requirements strongly limit the possible optical designs, and, in particular, none of those commonly found in the literature [5][6][7][8] can be considered without significant modifications. In the following, a brief description of the historical evolution of the camera optical design is given, from the initial three-mirror configuration, to the final and simpler two-mirror one.…”

Section: Wide Angle Camera Optical Designmentioning

confidence: 99%

Optical design of the Wide Angle Camera for the Rosetta mission

Naletto¹,

Deppo²,

Pelizzo³

et al. 2002

Appl. Opt.

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The final optical design of the Wide Angle Camera for the Rosetta mission to the P/Wirtanen comet is described. This camera is an F/5.6 telescope with a rather large 12 degrees x 12 degrees field of view. To satisfy the scientific requirements for spatial resolution, contrast capability, and spectral coverage, a two-mirror, off-axis, and unobstructed optical design, believed to be novel, has been adopted. This configuration has been simulated with a ray-tracing code, showing that theoretically more than 80% of the collimated beam energy falls within a single pixel (20" x 20") over the whole camera field of view and that the possible contrast ratio is smaller than 1/1000. Moreover, this novel optical design is rather simple from a mechanical point of view and is compact and relatively easy to align. All these characteristics make this type of camera rather flexible and also suitable for other space missions with similar performance requirements.

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Section: Wide Angle Camera Optical Designmentioning

confidence: 99%

Optical design of the Wide Angle Camera for the Rosetta mission

Naletto¹,

Deppo²,

Pelizzo³

et al. 2002

Appl. Opt.

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“…The detector represents an evolution of the intensified-CCD detectors that we have used in other instruments (Torr and Devlin, 1982;Torr et al, 1986). It is described in more detail by Torr et al (1993) and comprises several key elements. The first of these is a proximity focused image intensifier with chevron microchannel plates.…”

Section: Detector Systemmentioning

confidence: 99%

“…This was followed by a test program to build multilayer transmission filters intended to be forerunners of those needed here (Zukic et al, 1990b). The basic design of the filters used in this instrument (Torr et al, 1993;Zukic et al, 1993) are a combination of reflective and transmissive elements, as summarized in Table 2.4.2. An important additional element in the rejection of long wavelength light, is the use of a 'solar blind' CsI photocathode.…”

mentioning

confidence: 99%

A far ultraviolet imager for the International Solar-Terrestrial Physics Mission

et al. 1995

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The aurorae are the result of collisions with the atmosphere of energetic particles that have their origin in the solar wind, and reach the atmosphere after having undergone varying degrees of acceleration and redistribution within the Earth's magnetosphere. The global scale phenomenon represented by the aurorae therefore contains considerable information concerning the solar-terrestrial connection. For example, by correctly measuring specific auroral emissions, and with the aid of comprehensive models of the region, we can infer the total energy flux entering the atmosphere and the average energy of the particles causing these emissions. Furthermore, from these auroral emissions we can determine the ionospheric conductances that are part of the closing of the magnetospheric currents through the ionosphere, and from these we can in turn obtain the electric potentials and convective patterns that are an essential element to our understanding of the global magnetosphereionosphere-thermosphere-mesosphere. Simultaneously acquired images of the auroral oval and polar cap not only yield the temporal and spatial morphology from which we can infer activity indices, but in conjunction with simultaneous measurements made on spacecraft at other locations within the magnetosphere, allow us to map the various parts of the oval back to their source regions in the magnetosphere. This paper describes the Ultraviolet Imager for the Global Geospace Sciences portion of the International Solar-Terrestrial Physics program. The instrument operates in the far ultraviolet (FUV) and is capable of imaging the auroral oval regardless of whether it is sunlit or in darkness. The instrument has an 8 ~ circular field of view and is located on a despun platform which

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