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A diode-laser based ultrahigh resolution IR heterodyne spectrometer for laboratory and field use has been developed for operation between 7.5 and 8.5 microm. The local oscillator is a PbSe tunable diode laser kept continuously at operating temperatures of 12-60 K using a closed-cycle cooler. The laser output frequency is controlled and stabilized using a high-precision diode current supply, constant temperature controller, and a shock isolator mounted between the refrigerator cold tip and the diode mount. The system largely employs reflecting optics to minimize losses from internal reflection and absorption and to eliminate chromatic effects. Spectral analysis of the diode-laser output between 0 and 1 GHz reveals excess noise at many diode current settings, which limits the IR spectral regions over which useful heterodyne operation can be achieved. Observations have been made of atmospheric N(2)O, O(3), and CH(4) between 1170 and 1200 cm(-1) using both a single-frequency swept IF channel and a 64-channel rf spectral line receiver with a total IF coverage of 1600 MHz.

The sensitivity of an ideal heterodyne spectrometer approaches the quantum detection limit provided the local oscillator power is sufficiently large and the shot noise dominates all other sources of noise. The postintegration minimum-detectable-number of photons/sec for an ideal heterodyne system is (B/tau)((1/2)), where B is the IF bandwidth, and tau is the integration time. For astronomical observations, however, a number of factors (Delta(i)) tend to degrade the sensitivity, a fact that becomes significant particularly when the laser power is insufficient. A discussion and an evaluation of the degradation in sensitivity are given for a heterodyne spectrometer employing a HgCdTe photodiode mixer and tunable diode lasers. The minimum detectable source brightness is considered as a function of the mixer parameters, transmission coefficient of the beam splitter, and local oscillator emission powers. The degradation in the minimum detectable line source brightness that results from the bandwidth being a fraction of the line width is evaluated and plotted as a function of the wavelength and bandwidth for various temperature to mass ratios. It is shown that the minimum achievable degradation [pi(i)(Delta(i))] in the sensitivity of a practical astronomical heterodyne spectrometer is ~30. Estimates of SNR's with which ir line emission from astronomical sources of interest may be detected are given.

The performance of an upconversion system is examined for observation of astronomical sources in the low to middle ir spectral range. Theoretical values for the performance parmeters of an upconversion system for astronomical observations are evaluated in terms of the conversion efficiencies, spectral resolution, field of view minimum detectable source brightness, and source flux. Experimental results of blackbody measurements and molecular absorption spectrum measurements using a lithium niobate upconverter with an argon-ion laser as the pump are presented. Estimates are given of the expected optimum sensitivity of an upconversion device that may be built with presently available components.