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. 

Infrared Space Observatory Short-Wavelength Spectrometer 300... 

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. °... 

P/Hartley 2 observed with the Infrared Space Observatory. In Thermal Emission Spectroscopy and Analysis of Dust, Disks, and Regoliths, ASP Conference 196, eds. Sitko, M. L., Sprague, A. L. and Lynch, D. K., San Francisco Astronomical Society of the Pacific, pp. 109-117. 

Supermolecular absorption determines significant features of the atmospheres of the planets and their large moons, such as the vertical temperature profile and the high-altitude haze distribution, and offers opportunities for the determination of abundance ratios of helium and hydrogen, ortho- and para-H2, etc. [390, 396]. In certain spectral bands the spectra may sometimes be obtained by Earth-based observations. More commonly, the spectra will be obtained in space missions, such as IRIS of Voyager I and II future missions (Infrared Space Observatory) will doubtlessly enhance the available information significantly. 

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. 

The composition of dust constituents and ices in disks are studied by ground-based and space-borne infrared spectroscopy, and by observing various vibrational bands in absorption (when a disk is seen edge-on) or emission (when a disk is seen face-on). The results from the Infrared Space Observatory and Spitzer Space... 

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

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... 

Spectroscopic observations of Jupiter and Saturn made with the Infrared Space Observatory are consistent with other estimates of protosolar D/H (see Robert et al. 2000 and references therein), as is the D/H value determined by the Galileo atmospheric entry probe mass spectrometer (26 7 ppm Mahaffy et al. 1998). This result is expected as the jovian planets are thought to have formed by quantitative capture of gas from the solar nebula. On the other hand, the outer solar system planets Uranus and Neptune appear to be significantly enriched in D/H by factors of -3 compared to the protosolar value (Feuchtgruber et al. 1999). This enrichment is interpreted to reflect the mixing of material from the more D-rich icy cores of these planets, which constitutes a significant fraction of their mass (as opposed to the jovian case where the planetary mass is dominated by the gaseous envelope). 

Earlier in 2013, as a response to the call for White Papers for the definition of the L2 and L3 missions in the ESA Science Programme, and following the steps of the 2006 proposal a new sub-arcsecond far-infrared space observatory was presented. This White Paper was the result of an European collaboration lead by Ivison, Helmich and Sauvage. 

R. Genzel, C.J. Cesarsky, Extragalactic results from the infrared space observatory. Annu. Rev. 

M. Sauvage, R. J. Ivison, F. Helmich, Sub-arcsecond far-infrared space observatory a science imperative (2013). submitted in response to the European Space Agency s caU for Science White Papers for the L2 and L3 L-class missions... 

The raw materials of organic compounds—hydrogen, carbon, nitrogen, and oxygen atoms—are present in these clouds, as are molecules and molecular fragments containing these atoms. Radioastronomy, which can be done from Earth s surface, and data from a satellite (the Infrared Space Observatory) have provided the evidence. 

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... 

Gibb EL, Whittet DCB, Boogert ACA, Tielens AGGM (2004) Interstellar ice the infrared space observatory legacy. Astrophys J 151 35... 

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