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Author Kaeufl, H. U.; Rothermel, H.; Drapatz, S. openurl 
  Title Indication for H2O in the upper atmosphere of Mars Type Journal Article
  Year 1984 Publication Astron. Astrophys. Abbreviated Journal A&A  
  Volume 141 Issue Pages 430-432  
  Keywords atmospheric moisture, mars atmosphere, upper atmosphere, water vapor, carbon dioxide, emission spectra, nonequilibrium thermodynamics, polar regions  
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  Notes Approved no  
  Call Number Serial 452  
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Author Rothermel, H.; Käufl, H. U.; Yu, Y. openurl 
  Title A heterodyne spectrometer for astronomical measurements at 10 micrometers Type Journal Article
  Year 1983 Publication Astron. Astrophys. Abbreviated Journal A&A  
  Volume 126 Issue Pages 387-392  
  Keywords astronomical spectroscopy, infrared astronomy, infrared spectrometers, optical heterodyning, infrared telescopes, laser spectrometers, mars (planet), venus (planet)  
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  Notes Approved no  
  Call Number Serial 453  
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Author Soifer, B. T.; Pipher, J. L. url  doi
openurl 
  Title Instrumentation for infrared astronomy Type Journal Article
  Year 1978 Publication Annual Rev. Astron. Astrophys. Abbreviated Journal  
  Volume 16 Issue 1 Pages 335-369  
  Keywords infrared applications  
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  Series Volume Series Issue Edition  
  ISSN 0066-4146 ISBN Medium  
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  Notes Approved no  
  Call Number Serial 492  
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Author Hansen, Lene; Jørgensen, H.E.; Nørgaard-Nielsen, Hans Ulrik; Pedersen, Kenneth; Goudfrooij, P.; Linden-Vornle, M.J.D. openurl 
  Title ISO far-infrared observations of rich galaxy clusters III. Abell 2029, Abell 2052, Abell 2142 Type Journal Article
  Year 2000 Publication Astron. Astrophys. Abbreviated Journal A&A  
  Volume 362 Issue 1 Pages 133-137  
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  Abstract (up) 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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  Notes Approved no  
  Call Number RPLAB @ s @ Serial 456  
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Author Justtanont, K.; Decin, L.; Schöier, F. L.; Maercker, M.; Olofsson, H.; Bujarrabal, V.; Marston, A. P.; Teyssier, D.; Alcolea, J.; Cernicharo, J.; Dominik, C.; de Koter, A.; Melnick, G.; Menten, K.; Neufeld, D.; Planesas, P.; Schmidt, M.; Szczerba, R.; Waters, R.; de Graauw, Th.; Whyborn, N.; Finn, T.; Helmich, F.; Siebertz, O.; Schmülling, F.; Ossenkopf, V.; Lai, R. doi  openurl
  Title A HIFI preview of warm molecular gas around χ Cygni: first detection of H2O emission toward an S-type AGB star Type Journal Article
  Year 2010 Publication Astron. Astrophys. Abbreviated Journal  
  Volume 521 Issue Pages L6  
  Keywords HEB mixer applications, HIFI, Herschel, stars: AGB and post-AGB / circumstellar matter / stars: kinematics and dynamics / stars: individual: χ Cyg / stars: late-type / stars: mass-loss  
  Abstract (up) Aims. A set of new, sensitive, and spectrally resolved, sub-millimeter line observations are used to probe the warm circumstellar gas around the S-type AGB star χ Cyg. The observed lines involve high rotational quantum numbers, which, combined with previously obtained lower-frequency data, make it possible to study in detail the chemical and physical properties of, essentially, the entire circumstellar envelope of χ Cyg.

Methods. The data were obtained using the HIFI instrument aboard Herschel, whose high spectral resolution provides valuable information about the line profiles. Detailed, non-LTE, radiative transfer modelling, including dust radiative transfer coupled with a dynamical model, has been performed to derive the temperature, density, and velocity structure of the circumstellar envelope.

Results. We report the first detection of circumstellar H2O rotational emission lines in an S-star. Using the high-J CO lines to derive the parameters for the circumstellar envelope, we modelled both the ortho- and para-H2O lines. Our modelling results are consistent with the velocity structure expected for a dust-driven wind. The derived total H2O abundance (relative to H2) is (1.1±0.2) × 10-5, much lower than that in O-rich stars. The derived ortho-to-para ratio of 2.1±0.6 is close to the high-temperature equilibrium limit, consistent with H2O being formed in the photosphere.
 
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  Notes Approved no  
  Call Number Serial 1096  
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