ISO, Infrared Space Observatory

On the last three decades, several space experiments with parts at very low temperatures have been flown. Among these, we mention IRAS (Infrared Astronomical Satellite) launched in 1983 (see Fig. 14.1), COBE (Cosmic Background Explorer) launched in 1989, ISO (Infrared Space Observatory) launched in 1995 and Astro-E (X-ray Observatory), launched in 2000 with instrumentation at 65 mK [35], Some cryogenic space missions are in the preparation or in final phase in Europe, USA and Japan. For example, ESA is going to fly Planck (for the mapping of the cosmic background radiation) and Herschel (called before FIRST Far Infrared and Submillimetre Telescope ) [36], These missions will carry experiments at 0.1 and 0.3 K respectively. 

NASA has formally invited its European counterpart to work on a continuation of the HST and the ESA has accepted. This in no way compromises its own cryostatic project, FIRST (the Far InfraRed Space Telescope). Designed to supersede the highly successful ISO (Infrared Space Observatory), this new space observatory will probe the Universe in the far infrared and submillimetre ranges. It should be recalled that the ESA contributed some 15% of the costs... 

The second interesting feature of this isotope is that minuscule grains of silicon carbide extracted from meteorites have been found to be very rich in calcium-44, as mentioned earlier. They have been identified with presolar grains that condensed in the ejecta of supernovas during their first few years of expansion. Could it be that supernovas have been throwing sand in our eyes Data gathered by the ISO (Infrared Space Observatory), yet another experiment with strong participation by the French CEA, clearly demonstrates that new dust condensed inside the Cas A remnant very soon after explosion of the supernova that caused it. °... 

ISO Infrared Space Observatory, an ESA-led infrared space telescope that carried out targeted observations. ISO had both imaging and spectroscopic modes. 

FIGURE 2 The infrared spectrum of M82 by D. Lutz et at PAH. polycyclic aromatic hydrocarbons ISO, Infrared Space Observatory. 

Models of irradiated disks predict four chemically distinct zones (see Fig. 4.1). (I) Zone of ices in the cold mid-plane opaque to incoming radiation. Chemistry in this region is dominated by cold gas-phase and grain-surface reactions. Here Infrared Space Observatory (ISO) and Spitzer observations confirmed the existence of ices, various silicates and PAHs (polycyclic aromatic hydrocarbons e.g. van den Ancker et al. 2000 van Dishoeck 2004 Bouwman et al. 2008). (II) Zone of molecules, a warm molecular layer adjacent to the mid-plane, dominated by ultraviolet/X-ray-driven photochemistry (III) the heavily irradiated zone of radicals, a hot dilute disk atmosphere deficient in molecules and (IV) the inner zone, inside of the ice line where terrestrial planets form. 

A solar system origin could explain the anomalously high abundance of nanodiamonds relative to other types of presolar grains in meteorites (Hoppe and Zinner, 2000). The recent detection by the Infrared Space Observatory (ISO) of nanodiamonds formed in situ within the accretion disks of young stars confirms that nanodiamonds could indeed have formed in the inner solar system (Van Kerckhoven et al., 2002). 

Infrared Space Observatory Education and Public Outreach, European Space Agency (ESA), URL http //www.iso.vilspa.esa.es and URL http //sci.esa.int... 

The atmospheric transmission becomes very poor past 10 pm, with the increased attenuation of the mid and far infrared radiation by molecules in the atmospheres, most notably water vapour H2O and carbon dioxide CO2. Therefore the information has been acquired using space borne or airborne telescopes such as the ESA mission Infrared Space Observatory (ISO http //sci.esa.int/iso) and... 

Several Fabry-Perot interferometers can also be operated in series. Each etalon is adjusted by piezo electric crystals to peak at the same wavenumber but at different orders. Up to three Eabry-Perot interferometers have been scanned together (Hegyi etal., 1972 Kumcz etal., 1977). Several Fabry-Perot interferometers were flown in November 1995 as part of the Short- and Long-Wave Spectrometers on the Infrared Space Observatory (ISO). A more detailed description of these instmments is given at the end of the next section (5.7). 

Fig. 5.7.5 Optical train of the Long-Wave Spectrometer of the Infrared Space Observatory (ISO). Mirrors 1,2, and 6 are folding mirrors. Mirror 2 is at the focal point of the telescope, mirror 3 collimates the beam for the benefit of the Fabry-Perot et ons. The etalons are mounted on a rotating wheel together with a transparent opening and an opaque disk (Clegg, 1992 Clegg et al, 1996).

Fig. 6.3.4 The 5 /u,m spectrum of Jupiter recorded by IRIS (Hand et al., 1979) and by the Infrared Space Observatory (Fig. 2 of Encrenaz et al., 1996). To facilitate comparison, the ISO spectrum (which is the spectrum with the higher resolution) is plotted with increasing wavenumbers, (a) Voyager IRIS and (b) ISO spectrum.

Much higher spectral resolution ( 0.5 cm ) was obtained by the Infrared Space Observatory (ISO) in 1997 (see Coustenis etal., 1997 Coustenis Taylor, 1999). A disk-average spectrum of Titan by the Short-Wavelength Spectrometer (SWS) of... 

Water has been first detected with the Infrared Space Observatory (ISO) in the atmosphere of Titan. The Infrared Space Observatory (ISO) was launched by the ESA Ariane in November 1995 and was the first true orbiting infrared observatory for a detailed investigation of the universe in the infrared. It was equipped with a 60 cm diameter telescope which was cooled by superfluid liquid helium to temperatures of 2-A K. Observations were made from 2.5 microns to 240 microns with a spatial resolution ranging from 1.5 arcseconds to 90 arcsec (at the longer wavelengths). 

This has been investigated with the ISO satellite, Infrared Space Observatory. 

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