Scientific/Technical Abstract:

CASIMIR will be a sensitive submillimeter and far-infrared heterodyne receiver for SOFIA. The receiver will use sensitive superconducting mixers, including both tunnel junction (SIS) and hot electron bolometers (HEB). The double-sideband receiver noise temperatures are projected to be 4-10 times the quantum limit. The local oscillators will be continuously tunable, and will consist of Gunn oscillators or HEMT power amplifiers followed by frequency multipliers.

Our goal is to cover the 500-2100 GHz frequency range in seven bands: SIS mixers in four bands up to 1200 GHz, and HEB mixers in three bands covering 1200-2100 GHz. Up to four of these frequency bands could be selected for use on a given flight; if necessary, the selection of frequency bands could be changed between flights. The HEB mixers will not be available at first light on SOFIA. The receiver will have an intermediate-frequency (IF) bandwidth of 4 GHz, which will be processed by a high resolution backend spectrometer (most likely an acousto-optic spectrometer with 1 MHz resolution), as well as a low resolution (30 MHz) analog correlator.

This instrument will be used to study a wide range of astrophysical problems ranging from the evolution of galaxies to the birth and death of stars.

CASIMIR Performance Summary – Instrument sensitivity and resolution summary is provided to permit estimating feasibility of scientific investigations.

Download Performance Summary

Get Acrobat Reader

All sensitivity and resolution data are preliminary, and based on anticipated performance of the observatory and the instrument. Actual performance of the SOFIA telescope and instrument combination will be established after flight operations begin. Telescope performance is expected to be upgraded during the first two years, and instrument performance may be upgraded, or additional modes or capabilities may be added.

Performance estimates given here are based on data supplied by the instrument team. Further details and updates may be obtained from the instrument team via the contact information given above.

Further References:

top of page