Development and field tests of a narrowband all-reflective spatial heterodyne spectrometer.

We describe the design, development, and performance of a narrowband, all-reflective, unaliased spatial heterodyne spectrometer (SHS) that has been tested in observations at the focus of the 1.6 m main telescope of the McMath-Pierce solar telescope on Kitt Peak. The all-reflective SHS described herein is a highly robust common-path Fourier transform spectrometer without moving parts that, over a limited spectral region, combines the large field of view and high resolving power characteristic of interference spectrometers but at substantially reduced instrument size and optical tolerances. The self-scanned region of wavelength space and resolving power of the SHS are determined by the beam size, the diffraction grating groove density, the number of detector elements, and the fixed orientation of a set of pilot mirrors. The results presented here represent the first successful implementation of this reflective SHS design for field use. We discuss concepts behind the unaliased reflective SHS design and report the performance of the instrument when used to observe terrestrial airglow and absorption features, the solar spectrum, and the Jovian spectrum near λ=6300 Å, at the achieved resolving power (R=λ/δλ) of R>100,000. The results confirm that reflective SHS instruments can deliver effective interferometric performance in the visible to the far-ultraviolet wavelengths with commercial optics of moderate surface quality.

Far-ultraviolet imaging spectroscopy of Io's atmosphere with HST/STIS.

Well-resolved far-ultraviolet spectroscopic images of O I, S I, and previously undetected H ILyman-alpha emission from Io were obtained with the Hubble space telescope imaging spectrograph (STIS). Detected O I and S I lines (1250 to 1500 angstroms) have bright equatorial spots (up to 2.5 kilorayleighs) that shift position with jovian magnetic field orientation; limb glow that is brighter on the hemisphere facing the jovian magnetic equator; and faint diffuse emission extending to approximately 20 Io radii. All O I and S I features brightened by approximately 50 percent in the last two images, concurrently with a ground-based observation of increased iogenic [O I] 6300-angstrom emission. The H ILyman-alpha emission, consisting of a small, approximately 2-kilorayleigh patch near each pole, has a different morphology and time variation.

Fabry-Perot CCD annular-summing spectroscopy: study and implementation for aeronomy applications.

The technique of Fabry-Perot CCD annular-summing spectroscopy, with particular emphasis on applications in aeronomy, is discussed. Parameter choices for optimizing performance by the use of a standard format CCD array are detailed. Spectral calibration methods, techniques for determining the ring pattern center, and effects imposed by limited radial resolution caused by superpixel size, variable by on-chip binning, are demonstrated. The technique is carefully evaluated experimentally relative to the conventional scanning Fabry-Perot that uses a photomultiplier detector. We evaluate three extreme examples typical of aeronomical spectroscopy using calculated signal-to-noise ratios. Predicted sensitivity gains of 10-30 are typical. Of the cases considered, the largest savings in integration time are estimated for the day sky thermospheric O(1)D case, in which the bright sky background dominates the CCD read noise. For profile measurements of faint night sky emission lines, such as exospheric hydrogen Balmer-α, long integration times are required to achieve useful signal-to-noise ratios. In such cases, CCD read noise is largely overcome. Predictions of a factor of 10-15 savings in integration time for night sky Balmer-α observations are supported by field tests. Bright, isolated night sky lines such as thermospheric O(1)D require shorter integration times, and more modest gains dependent on signal level are predicted. For such cases it appears from estimate results that the Fabry-Perot CCD annular-summing technique with a conventional rectangular format may be outperformed by a factor of 2-5 by special CCD formats or by unusual optical coupling configurations that reduce the importance of read noise, based on the ideal transmission for any additional optics used in these configurations.

High spectral resolution lidar to measure optical scattering properties of atmospheric aerosols. 1: theory and instrumentation.

A high spectral resolution lidar technique to measure optical scattering properties of atmospheric aerosols is described. Light backscattered by the atmosphere from a narrowband optically pumped oscillator-amplifier dye laser is separated into its Doppler broadened molecular and elastically scattered aerosol components by a two-channel Fabry-Perot polyetalon interferometer. Aerosol optical properties, such as the backscatter ratio, optical depth, extinction cross section, scattering cross section, and the backscatter phase function, are derived from the two-channel measurements.

High spectral resolution lidar to measure optical scattering properties of atmospheric aerosols. 2: calibration and data analysis.

The high spectral resolution lidar (HSRL) measures optical properties of atmospheric aerosols by interferometrically separating the elastic aerosol backscatter from the Doppler broadened molecular contribution. Calibration and data analysis procedures developed for the HSRL are described. Data obtained during flight evaluation testing of the HSRL system are presented with estimates of uncertainties due to instrument calibration. HSRL measurements of the aerosol scattering cross section are compared with in situ integrating nephelometer measurements.

All-reflection Michelson interferometer: analysis and test for far ir Fourier spectroscopy.

The beam splitter of the all-reflection Michelson interferometer consists of a combination of three parallel diffraction gratings. This paper extends the analysis of the instrument to include the effects of lateral errors in the grating adjustment (i.e., displacements parallel to the grating faces and perpendicular to the grooves). Such errors are shown to introduce a phase shift independent of wavenumber and proportional to grating order number. Tests of an instrument designed for Fourier transform spectroscopy in the 500-1000-microm spectral range are reported and shown to be in agreement with the analysis. For wavenumbers which pass through the instrument in 2 or more orders, cross-order interference effects are expected to occur which cause rapid variations in the efficiency vs wavenumber curve. This possibility should be eliminated in the design of a practical instrument. The resolution of the test instrument (1.6 cm(-1)) was insufficient to reveal this effect.

New fourier transform all-reflection interferometer.

This paper describes the design and tests of an all-reflection two-beam interferometer. The interferometer consists of three reflecting diffraction gratings and two collimating mirrors. The use of only reflection optics eliminates the need for a transmitting beam splitter and compensation plate thus permitting the possibility of using the interferometer in the vacuum ultraviolet. This instrument can be used as a Fourier transform spectrometer. Obtaining the spectrum of the incident light from the interferogram is not so straightforward as with a Michelson interferometer. The method of Fourier inversion is described, and examples of interferograms taken with the instrument and the spectra obtained from the interferograms are presented. The interferometer has been tested in the visible and in the near ultraviolet at 2537 A.

Fabry-perot spectrometer adjustment for the compensation of Doppler shift from rapidly rotating and rapidly flowing sources.

The Doppler shift of light from a rapidly rotating or rapidly flowing source limits the spectroscopic resolution with which it can be studied using Fabry-Perot spectrometers that have the usual axial fringe adjustment. Because of the angular dependence of the wavenumber transmitted by the Fabry-Perot, the entrance aperture can be positioned off-axis at an angle chosen such that the wavenumber shift across the entrance aperture matches the shift presented by the source, thereby compensating for the Doppler effect. The principle can be extended to the Michelson interferometer for Fourier transform spectroscopy when the Michelson is used without field compensation. High resolution spectra obtained with a PEPSIOS spectrometer using the entire disk of Jupiter, a rapidly rotating planet, are presented as an example.

Precision mapping of pairs of uncoated optical flats.

The essential features of apparatus suitable for routine mapping of pairs of wedged uncoated optical flats are described. In this method the aperture of the pair of flats is scanned in a regular pattern, and information about the spacing uniformity is derived from the interference of light reflected from the flat surfaces. Accuracies within about lambda/500 are obtained.