Donald E. Jennings

Exploration of the Solar System by Infrared Remote Sensing

Introduction 1. Foundation of radiation theory 2. Radiative transfer 3. Interaction of radiation with matter 4. The emerging radiation field 5. Instruments to measure the radiation field 6. The measured radiation field 7. Retrieval of physical parameters from measurement 8. Interpretation of results Closing remarks Appendices References Tables Index.

Absolute line strengths in ν 4 , 12 CH 4 : a dual-beam diode laser spectrometer with sweep integration

A tunable diode laser spectrometer with several unique features has been developed for use in the middle IR. The all-reflective optical system has a dual-beam configuration before the dispersive mode selector to eliminate transit-angle errors at the calibration etalon. By maintaining separated beams through the mode selector, beam combiner losses are avoided. Averaging successive sweeps of the current-modulated laser permits stable reproducible spectral integrations, eliminating etalon thermal errors and producing high photometric sensitivity. Line strengths have been measured using this instrument for eleven transitions in nu(4) of (12)CH(4). These include R0 and R1 and nine P-branch transitions in the 1202-1263-cm(-1) range. Techniques for measuring strengths with a diode laser are discussed.

Cassini infrared Fourier spectroscopic investigation

The composite infrared spectrometer (CIRS) is a remote sensing instrument to be flown on the Cassini orbiter. CIRS will retrieve vertical profiles of temperature and gas composition for the atmospheres of Titan and Saturn, from deep in their tropospheres to high in their stratospheres. CIRS will also retrieve information on the thermal properties and composition of Saturns rings and Saturnian satellites. CIRS consists of a pair of Fourier Transform Spectrometers (FTSs) which together cover the spectral range from 10-1400 cm-1 with a spectral resolution up to 0.5 cm-1. The two interferometers share a 50 cm beryllium Cassegrain telescope. The far-infrared FTS is a polarizing interferometer covering the 10-600 cm-1 range with a pair of thermopile detectors, and a 3.9 mrad field of view. The mid-infrared FTS is a conventional Michelson interferometer covering 200-1400 cm-1 in two spectral bandpasses: 600-1100 cm- 1100-1400 cm(superscript -1 with a 1 by 10 photovoltaic HgCdTe array. Each pixel of the arrays has an approximate 0.3 mrad field of view. The HgCdTe arrays are cooled to approximately 80K with a passive radiative cooler.

The v = 1 ← 0 quadrupole spectrum of N2

Abstract Transitions in the O and S branches of the v = 1 ← 0 band of molecular 14 N 2 have been recorded in the laboratory using the 1-m Fourier transform spectrometer located at Kitt Peak. Analysis of the line position data has led to improved values for the Dunham coefficients of N 2 . Furthermore, an analysis of the linewidths and peak heights have yielded values of γ L = (0.0345 ± 0.0029) cm −1 /atm for the self-broadening coefficient of N 2 and ( ∂Q ∂r )r e = (0.933 ± 0.039)ea 0 for the derivative of the molecular quadrupole moment.

Ralph: A Visible/Infrared Imager for the New Horizons Pluto/Kuiper Belt Mission

The New Horizons instrument named Ralph is a visible/near infrared multi-spectral imager and a short wavelength infrared spectral imager. It is one of the core instruments on New Horizons, NASA’s first mission to the Pluto/Charon system and the Kuiper Belt. Ralph combines panchromatic and color imaging capabilities with SWIR imaging spectroscopy. Its primary purpose is to map the surface geology and composition of these objects, but it will also be used for atmospheric studies and to map the surface temperature. It is a compact, low-mass (10.5 kg) power efficient (7.1 W peak), and robust instrument with good sensitivity and excellent imaging characteristics. Other than a door opened once in flight, it has no moving parts. These characteristics and its high degree of redundancy make Ralph ideally suited to this long-duration flyby reconnaissance mission.

The 12 micron band of ethane - High-resolution laboratory analysis with candidate lines for infrared heterodyne searches

Attention is given to the results of a laboratory study of the v9 band of ethane at 12 microns, using both high resolution Fourier transform and diode laser absorption spectroscopy. The analysis to which about 2000 transitions in this band have been subjected includes the normal rotational terms as well as the higher order effects of l-doubling, l-resonance, internal rotation, and a Coriolis resonance with the 3v4 state. A model is presented for the v9 band which is able to reproduce the observed features to an accuracy of better than 0.001/cm, and a list has been compiled for v9 transitions, occurring near C-14O2 laser lines, that are good candidates for laser heterodyne searches.

Earth-Based Observations of the Galileo Probe Entry Site

Earth-based observations of Jupiter indicate that the Galileo probe probably entered Jupiters atmosphere just inside a region that has less cloud cover and drier conditions than more than 99 percent of the rest of the planet. The visual appearance of the clouds at the site was generally dark at longer wavelengths. The tropospheric and stratospheric temperature fields have a strong longitudinal wave structure that is expected to manifest itself in the vertical temperature profile.

Raman spectroscopy of gases with a Fourier transform spectrometer: the spectrum of D2

A high-resolution Fourier transform spectrometer (FTS) has been used to record spontaneous incoherent laser Raman spectra of gases. The resolution, sensitivity, calibration accuracy, and spectral coverage achieved in these spectra demonstrate the viability of the FTS for Raman spectroscopy. Measurements from a spectrum of D2 containing both υ = 0−0 and υ = 1−0 transitions were fitted to the Dunham expansion of the vibration–rotation energy levels. The coefficients are (in cm−1) Y10 = 2993.6060 (67), Y01 = 30.4401(89), Y11 = −1.0538(17), Y02 = −0.011590(41), Y12 = 2.02(80) × 10−4, and Y03 = 5.83(11) × 10−6. Errors in parentheses are one standard deviation.

New Horizons: Anticipated Scientific Investigations at the Pluto System

The New Horizons spacecraft will achieve a wide range of measurement objectives at the Pluto system, including color and panchromatic maps, 1.25–2.50 micron spectral images for studying surface compositions, and measurements of Pluto’s atmosphere (temperatures, composition, hazes, and the escape rate). Additional measurement objectives include topography, surface temperatures, and the solar wind interaction. The fulfillment of these measurement objectives will broaden our understanding of the Pluto system, such as the origin of the Pluto system, the processes operating on the surface, the volatile transport cycle, and the energetics and chemistry of the atmosphere. The mission, payload, and strawman observing sequences have been designed to achieve the NASA-specified measurement objectives and maximize the science return. The planned observations at the Pluto system will extend our knowledge of other objects formed by giant impact (such as the Earth–moon), other objects formed in the outer solar system (such as comets and other icy dwarf planets), other bodies with surfaces in vapor-pressure equilibrium (such as Triton and Mars), and other bodies with N2:CH4 atmospheres (such as Titan, Triton, and the early Earth).

Diode laser spectra of the torsional splittings in the ν9 band of ethane: Torsion‐vibration‐rotation interactions and the barrier to internal rotation

Diode laser spectra of most of the Q branches of the ν9 band of ethane from RQ8–PQ15 have been recorded. The Q branches RQ0–RQ4 were deconvoluted to yield an effective resolution of (0.5–1.0)×10−3 cm−1 FWHM. Torsional splittings were observed for most lines. In contrast to predictions based on first order theory, the splittings which range from (2–53)×10−3 cm−1, have a marked J and K dependence. A second order theory of torsion‐vibration‐rotation interaction between ν9 and 3ν4 is developed, which fits the splittings with an rms error of 0.0006 cm−1, using only three adjustable parameters: the barrier to internal rotation in ν9, the energy difference between ν9 and 3ν4, and an effective coupling constant. The barrier to internal rotation in ν9 is found to be 1123±10 cm−1.