Astronomy and Astrophysics – Astronomy
Scientific paper
May 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...19513801p&link_type=abstract
American Astronomical Society, 195th AAS Meeting, #138.01; Bulletin of the American Astronomical Society, Vol. 32, p.885
Astronomy and Astrophysics
Astronomy
2
Scientific paper
The time required to obtain an observation of an astronomical source depends upon the characteristics of that source, the characteristics of the detector, the brightness of the background, the desired signal-to-noise ration, and the angle subtended by a detector pixel (the pixel scale). In addition, if the observation is not of a single source, but is a survey of many sources, then the field of view of the detector is also important. For background-limited observations, which is expected to be the typical case for NGST, the source characteristic of importance is the solid angle of the source image. The detector characteristic of importance is the dark current. An optimal pixel scale exists that minimizes the time required to obtain the observations. That optimal scale depends upon the above variables. The Design Reference Mission (DRM), prepared by the Ad Hoc Science Working Group, embodies the key science goals for NGST. An approximately equal amount of single-target and survey observations and a range of target sizes comprise the DRM. Therefore, no single pixel scale is optimal for all observations. We present the functional dependance of the optimal scale upon the relevant variables. We also present the results of parametric variations of the NGST Yardstick design which determine for each instrument module the optimal pixel scale that minimizes the time required to complete the Design Reference Mission.
Petro Larry
Stockman Hervey S.
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