Learn More
We have analysed the ISO-SWS spectrum of Jupiter in the 12–16 µm range, where several hydrocarbons exhibit rovibrational bands. Using temperature information from the methane and hydrogen emissions, we derive the mixing ratios (q) of acetylene and ethane at two independent pressure levels. For acetylene, we find q = (8.9 +1.1 −0.6) × 10 −7 at 0.3 mbar and q(More)
We present mid-infrared ISO-SWS observations of the fine-structure emissions and the recombination lines Brα and Brβ, in a sample of 112 Galactic H II regions and 37 nearby extra-galactic H II regions in the LMC, SMC, and M33. We selected our sources from archival ISO-SWS data as those showing prominent [Ne II]12.8µm or [Ne III]15.6µm emissions. The(More)
We report new observations of the far infrared and submillimeter water vapor emission of NML Cygnus based on data gathered with the Infrared Space Observatory and the Submillimeter Wave Astronomy Satellite. We compare the emission from NML Cyg to that previously published for VY CMa and W Hya in an attempt to establish the validity of recently proposed(More)
We report the first detection of thermal water vapour emission from a circumstellar outflow. We have observed four far-infrared rotational emission lines of water vapour and one water absorption feature toward the evolved star W Hydrae, using the Short Wavelength Spectrometer (SWS) of the Infrared Space Observatory (ISO). Three of the emission lines were(More)
Observations with the Short Wavelength Spectrometer (SWS) onboard the Infrared Space Observatory (ISO) have led to the first unambiguous detection of HD in the atmospheres of Uranus and Neptune, from its R(2) rotational line at 37.7 µm. Using S(0) and S(1) quadrupolar lines of H 2 at 28.2 and 17.0 µm as atmospheric thermometers, we derive D/H ra
The atmospheres of the giant planets are reducing, being mainly composed of hydrogen, helium and methane. But the rings and icy satellites that surround these planets, together with the flux of interplanetary dust, could act as important sources of oxygen, which would be delivered to the atmospheres mainly in the form of water ice or silicate dust. Here we(More)
The detection of circumstellar water vapour around the ageing carbon star IRC +10216 challenged the current understanding of chemistry in old stars, because water was predicted to be almost absent in carbon-rich stars. Several explanations for the water were postulated, including the vaporization of icy bodies (comets or dwarf planets) in orbit around the(More)
In this paper, the feasibility of on-board data reduc-tion/compression concept described in [1] is evaluated for infrared images taken from space observatories. The method described in [1], which was initially designed and developed for the PACS (Photodetector Array Camera and Spectrometer) instrument [10], makes use of on-board integration to achieve(More)
We present a 2.4–45 m spectrum of the center of our Galaxy obtained with the Short Wavelength Spectrometer (SWS) on board ISO. The wide range of ionic fine structure lines observed yields an average effective temperature for the ionizing stars of 35000 K, with a small contribution of significantly hotter stars, consistent with ageing of an active period of(More)