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Stars are born and die in clouds of gasoline and mud, opaque to such a lot kinds of radiation, yet obvious within the infrared. Requiring complicated detectors, area missions and cooled telescopes, infrared astronomy is the final department of this self-discipline to return of age. After a truly profitable sky survey played within the eighties by means of the IRAS satellite tv for pc, the Infrared area Observatory, within the nineties, introduced amazing advances within the realizing of the methods giving upward push to robust infrared emission through a good number of celestial resources.
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Stars are born and die in clouds of gasoline and mud, opaque to so much forms of radiation, yet obvious within the infrared. Requiring complicated detectors, area missions and cooled telescopes, infrared astronomy is the final department of this self-discipline to return of age. After a truly winning sky survey played within the eighties via the IRAS satellite tv for pc, the Infrared house Observatory, within the nineties, introduced awesome advances within the realizing of the techniques giving upward push to strong infrared emission by way of an excellent number of celestial resources.
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352, 587. Tielens, A. G. G. , McKee, C. , Seab, C. , and Hollenbach, D. : 1994, Astrophys. J. 431, 321. Tielens, A. G. G. , Waters, L. B. F. , Molster, F. : 1997, Astrophys. Space Sci. 255, 415. Uchida, K. , Forrest, W. , Watson, D. : 2004, Astrophys. J. Suppl. 154, 439. , Waters, L. B. F. , Dullemond, C. , Tielens, A. G. G. : 2004, Astron. Astrophys. 418, 177. , Waters, L. B. F. , de Graauw, M. : 1996, Astron. Astrophys. 315, L245. Waters, L. B. F. , Molster, F. , van Loon, J. : 1998, Nature 391, 868.
Line identiﬁcation are given in the zoom to the central position in the top-left panel. The CO data, including the LWS/FP data, have been presented and analyzed by Sempere et al. (2000). of H2 O. Figure 6 shows a selection of the observed lines together with the lowresolution spectrum of Orion. Water lines with upper energy levels below ∼1500 K have been detected by ISO towards Orion IRc2. Nevertheless, the spatial/spectral resolution of these thermal water IR lines is not enough to resolve the complexity of the observed regions.
2001b, 2004). The low-resolution spectrum obtained with the LWS, together with the available data from the LWS/FP, have been analyzed by Goicoechea et al. (2004; see Figure 21 for a comparison of the grating spectrum of Sgr B2(M) and Arp220). The dust emission could be ﬁtted with a Tdust 30–40 K with a peak opacity at 80 μm of 5. A detailed view of the absorption lines found in SgrB2 in the 40–200 μm range is shown in Figure 3, while those of water vapor are shown in Figure 8. 5 μm, all water lines have the same proﬁle and are centered at Sgr B2(M) velocities.