The Near Infrared Camera and Multi-Object Spectrometer, A Status Report

Details The Near Infrared Camera and Multi-Object Spectrometer, A Status Report The Near Infrared Camera and Multi-Object Spectrometer, A Status Report

Dec 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...187.0406s&link_type=abstract

American Astronomical Society, 187th AAS Meeting, #04.06; Bulletin of the American Astronomical Society, Vol. 27, p.1289

Physics

Optics

Scientific paper

The development of the Near Infrared Camera and Multi-Object Spectrometer (NICMOS), a second-generation instrument to be installed on the Hubble Space Telescope (HST) during the February 13, 1997 on-orbit servicing mission, is nearing completion. The current status of that development effort from the purview of anticipated scientific capabilities, instrumental performance, and on-orbit operating considerations are reported here. NICMOS will provide infrared imaging and spectroscopic observations of astronomical targets between 0.8-2.5 microns. NICMOS is an HST Axial Replacement Instrument, containing three cameras designed for simultaneous operation. The NICMOS optics will present the detectors with three adjacent, but not spatially contiguous Fields-of-View of different image scales. NICMOS will employ three low noise, high Quantum Efficiency, HgCdTe 256x256 Focal Plane Arrays in a passive dewar using solid N2 as a coolant. Thermoelectric cooling will prolong the nominal mission lifetime to approximately 4.6 years. Each camera carries a complement of 19 of these optical elements, selected through three independent Filter Wheel Mechanisms. Grism spectroscopy, in the widest field camera (number 3) will provide a multi-object spectrographic capability with a resolution of 200. A 0.3 arc-second radius occulting spot, and optimized cold mask, in the intermediate resolution camera (number 2) provides a coronographic imaging capability. The NICMOS Fore-Optics Assembly will fully correct the spherically aberrated HST input beam. NICMOS will achieve diffraction limited performance in the high resolution camera (number 1) to 1.0 microns, and in camera 2 to 1.75 microns. An internal Field-Offset Mechanism will allow NICMOS to observe background fields and in parallel with other HST instruments without the necessity of re-pointing the spacecraft. Support for this work was provided by NASA through contract number NAS5-31289.

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