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Kaeufl, H. U., Rothermel, H., & Drapatz, S. (1984). Indication for H2O in the upper atmosphere of Mars. A&A, 141, 430–432.
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Rothermel, H., Käufl, H. U., & Yu, Y. (1983). A heterodyne spectrometer for astronomical measurements at 10 micrometers. A&A, 126, 387–392.
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Soifer, B. T., & Pipher, J. L. (1978). Instrumentation for infrared astronomy. Annual Rev. Astron. Astrophys., 16(1), 335–369.
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Käufl, H. U., Rothermal, H., & Drapatz, S. (1984). Investigation of the Martian atmosphere by 10 micron heterodyne spectroscopy. A&A, 136, 319–325.
Keywords: astronomical spectroscopy, atmospheric composition, infrared astronomy, mars atmosphere, spectral line width, carbon dioxide concentration, nonequilibrium thermodynamics, optical heterodyning, planetary radiation, mars, atmosphere, spectroscopy, atmosphere, carbon dioxide, altitude, kinetics, rotation, thermal properties, temperature, emissions, intensity, models, data, spectra
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Rothermel, H., Käufl, H. U., Schrey, U., & Drapatz, S. (1988). Thermal structure of the Martian mesosphere. A&A, 196, 296–300.
Keywords: atmospheric temperature, carbon dioxide, infrared spectroscopy, mars atmosphere, mesosphere, emission spectra, line spectra, spatial resolution, mars, atmosphere, mesosphere, structure, thermal properties, spectra, spectroscopy, earth-based observations, temperature, patterns, infrared, polar regions, wavelengths, equipment, procedure, carbon dioxide, emissions
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Chen, P. S. (2001). Infrared properties of barium stars. A&A, 372(1), 245–248.
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Hartogh, P., Crovisier, J., de Val-Borro, M., Bockelée-Morvan, D., Biver, N., Lis, D. C., et al. (2010). HIFI observations of water in the atmosphere of comet C/2008 Q3 (Garradd). Astron. Astrophys., 518, L150 (1 to 5).
Abstract: High-resolution far-infrared and sub-millimetre spectroscopy of water lines is an important tool to understand the physical and chemical properties of cometary atmospheres. We present observations of several rotational ortho- and para-water transitions in comet C/2008 Q3 (Garradd) performed with HIFI on Herschel. These observations have provided the first detection of the 212–101 (1669 GHz) ortho and 111–000 (1113 GHz) para transitions of water in a cometary spectrum. In addition, the ground-state transition 110–101 at 557 GHz is detected and mapped. By detecting several water lines quasi-simultaneously and mapping their emission we can constrain the excitation parameters in the coma. Synthetic line profiles are computed using excitation models which include excitation by collisions, solar infrared radiation, and radiation trapping. We obtain the gas kinetic temperature, constrain the electron density profile, and estimate the coma expansion velocity by analyzing the map and line shapes. We derive water production rates of 1.7–2.8 × 1028 s-1 over the range rh = 1.83–1.85 AU.
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Johnson, M. A., Betz, A. L., McLaren, R. A., Townes, C. H., & Sutton, E. C. (1976). Nonthermal 10 micron CO2 emission lines in the atmospheres of Mars and Venus. A&A, 208, 145.
Keywords: carbon dioxide, emission spectra, infrared spectra, mars atmosphere, nonthermal radiation, optical heterodyning, planetary radiation, venus atmosphere, absorption spectra, energy transfer, line spectra, molecular absorption, molecular collisions, near infrared radiation, solar flux
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Hansen, L., Jørgensen, H. E., Nørgaard-Nielsen, H. U., Pedersen, K., Goudfrooij, P., & Linden-Vornle, M. J. D. (2000). ISO far-infrared observations of rich galaxy clusters III. Abell 2029, Abell 2052, Abell 2142. A&A, 362(1), 133–137.
Abstract: A sample of five rich galaxy clusters has been mapped by ISO at 60 μm, 100 μm, 135 μm, and 200 μm using the PHT-C camera. In previous papers Abell 2670 and Sersic 159-03 were discussed. Here we present the results for Abell 2029, Abell 2052, and Abell 2142. The conclusion of the survey is that the relatively small fields (approximate to 60 square are minutes) are structured with filaments or superpositions of point sources. In some cases point sources (approximate to 0.1 Jy) can be identified with cluster galaxies. An attempt to demonstrate infrared emission from dust in the cooling flows (due to star formation) was inconclusive.
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Pineda, J. L., Langer, W. D., Velusamy, T., & Goldsmith, P. F. (2013). A Herschel [C ii] Galactic plane survey. I. The global distribution of ISM gas components. Astron. Astrophys., 554, A103.
Abstract: Context. The [C ii] 158 μm line is an important tool for understanding the life cycle of interstellar matter. Ionized carbon is present in a variety of phases of the interstellar medium (ISM), including the diffuse ionized medium, warm and cold atomic clouds, clouds in transition from atomic to molecular, and dense and warm photon dominated regions.
Aims. Velocity-resolved observations of [C ii] are the most powerful technique available to disentangle the emission produced by these components. These observations can also be used to trace CO-dark H2 gas and determine the total mass of the ISM.
Methods. The Galactic Observations of Terahertz C+ (GOT C+) project surveys the [C ii] 158 μm line over the entire Galactic disk with velocity-resolved observations using the Herschel/HIFI instrument. We present the first longitude-velocity maps of the [C ii] emission for Galactic latitudes b = 0°, ±0.5°, and ±1.0°. We combine these maps with those of H i, 12CO, and 13CO to separate the different phases of the ISM and study their properties and distribution in the Galactic plane.
Results. [C ii] emission is mostly associated with spiral arms, mainly emerging from Galactocentric distances between 4 and 10 kpc. It traces the envelopes of evolved clouds as well as clouds that are in the transition between atomic and molecular. We estimate that most of the observed [C ii] emission is produced by dense photon dominated regions (~47%), with smaller contributions from CO-dark H2 gas (~28%), cold atomic gas (~21%), and ionized gas (~4%). Atomic gas inside the Solar radius is mostly in the form of cold neutral medium (CNM), while the warm neutral medium gas dominates the outer galaxy. The average fraction of CNM relative to total atomic gas is ~43%. We find that the warm and diffuse CO-dark H2 is distributed over a larger range of Galactocentric distances (4–11 kpc) than the cold and dense H2 gas traced by 12CO and 13CO (4–8 kpc). The fraction of CO-dark H2 to total H2 increases with Galactocentric distance, ranging from ~20% at 4 kpc to ~80% at 10 kpc. On average, CO-dark H2 accounts for ~30% of the molecular mass of the Milky Way. When the CO-dark H2 component is included, the radial distribution of the CO-to-H2 conversion factor is steeper than that when only molecular gas traced by CO is considered. Most of the observed [C ii] emission emerging from dense photon dominated regions is associated with modest far-ultraviolet fields in the range χ0 â‰<192> 1 – 30.
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