ISO Images from the 14th February Press Conference
The most recent ISO images can be found in the ISO Science Results Gallery
- Saturn (SWS, FP) showing the prescence of molecular Hydrogen
- Saturn (LWS, FP) with the prescence of Deuterated Molecular Hydrogen (HD)
- Saturn (LWS, Grating) with detection of PH3 and NH3
- Interstellar Cirrus (LWS, Grating) with prescence of CII
- GL2591 (SWS spectra) with detection of H2O Ice, CO2 Ice, silicate
- S106, Cirrus, NGC7027 and Antennae with detection at 158 microns of CII
- S106 (LWS Grating) with OI, OII, CII
- NGC7027 & NGC6543 spectra (PHT-S)
- NGC7027 & NGC6543 (SWS Grating - Full scan) with prescence of hydro-carbons
- NGC6543 (SWS Grating - Full scan) with detection of neon, sulphur, argon and hydrogen
- NGC6543 (SWS FP) with detailed sulphur line
- NGC6543 (SWS FP)
with details on the neon line
- The Planetary Nebulae NGC7027 (LWS Grating) overlaid on an HST visible image
- The Supernova Remnant MSH 11-54 (PHT image)
- The 'Whirlpool' Galaxy (M51) (CAM map) at a wavelength of 15 microns
- The 'Whirlpool' Galaxy (M51) (CAM map) at a wavelength of 7 microns
- NGC6946 (PHT map)
at a wavelength of 60 microns
- NGC6946 (SWS spectrum)
, showing molecular hydrogen emission
- Antennae colliding galaxies (PHT Spectral energy distribution overlaid on a visible image
- Antennae colliding galaxies(LWS spectra)
- Antennae colliding galaxies (CAM image)
at a wavelength of 15 microns
- Antennae colliding galaxies (CAM image + CVF spectra)
- NGC6090 spectral energy distribution (PHT)
- Arp220 (CAM image) at 15 microns with 1.5" Pixel field of view
- Our galaxy (view by IRAS) with an example of slew path for Serendipity Mode (PHT)
- Our galaxy (View by IRAS) with initial data for serendipity Mode(PHT)
- The galactic plane (IRAS) Slews from PHT
- The galactic plane (IRAS) cuts across galactic plane for PHT
- The galactic plane (IRAS) cuts through cirrus (PHT)
Acknowledgements
The ISO success could not have been possible without the dedication,
professionalism and inspiration of countless individuals over a period
stretching back nearly 20 years.
Overall management was carried out by the ESA Project Team, located at ESTEC.
The satellite was built by an industrial
consortium, led by Aerospatiale (F) as prime contractor, and including 35
companies at its peak. Each instrument was built by a consortium of institutes
and industries, led by a Principal Investigator, Catherine Cesarsky (CEA,
Saclay, F) for ISOCAM, Peter Clegg (QMW, London, UK) for the Long Wavelength
Spectrometer, Thijs de Graauw, (SRON, Groningen, NL) for the Short Wavelength
Spectrometer and Dietrich Lemke (MPIA, Heidelberg, D) for ISOPHOT. A full
description of the participants in the ISO Programme is given in issue
number 84 of the ESA Bulletin.
