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sublimation of water ice trapped either in comets or meteorites or, more in general, in the planetesimals which formed the Earth. A key parameter in these theories is the HDO/H2O ratio: in oceans it is ten times larger than the cosmic D/H elemental ratio, close to that of comets, and hundred times smaller than that observed in solar type protostars (§3.2.2). A big unanswered question is: what is the HDO/H2O in proto-planetary disks, which contain the material from which planetesimals, meteorites and comets are formed? Astromol has reported the first detection of HDO in a proto-planetary disk (Fig. 3.7: Ceccarelli et al. 2005), from which a HDO/H2O ratio (∼ 1%) slightly lower than in protostars has been estimated. Indeed, the big contribution of these observations is that HDO in the measured quantities should have not been detected, because H2O and HDO are believed to be almost totally frozen onto the grain mantles (at least in the region probed by the observations)! Since HDO has been observed, something is reinjecting water molecules from the grain mantles. Soon after the HDO detection, Astromol showed that grain mantle photo-desorption from the Interstellar UV field can indeed keep the observed water column density in the gas phase (Dominik, Ceccarelli, Hollenbach, Kaufman 2005, ApJL submitted). • The discovery of a small warm disk in a low mass binary system. By using Adaptive Optics (AO) aided 2µm observations at Keck, we revealed the presence of a small ( ∼ < 5 AU), warm (∼ 400 K) and dense ( ∼ > 10 7 cm −3 disk surrounding the more massive companion of the binary system forming T Tau S (Duchene et al. 2005). The observations detected the CO lines (from J=9 to J=20) in absorption against the source continuum, a technique already used by other authors for studying a (very) few other disk sources. The originality and importance of our observations is that, thanks to the coupling with the AO, we could study a close binary system and demonstrate that the disk of (at least) one of the two protostars is probably truncated because of the presence of the other protostar. We plan to carry out similar studies in a larger sample of sources, with the scope to understand how, indeed, the presence of a companion affects the circumstellar disks of the two composing protostars. More in general, the CO absorption technique is extremely powerful in characterizing the physical conditions of the gas in the warm layers of the protoplanetary disks, much more efficient than the mm/submm observations, which only provide one CO J level at once. 64
Chapter 4 Perspectives 4.1 Overview Astrochemistry is going to be the keyword of our research in the incoming years. Astrochemistry in its two major aspects: the molecular composition of the extra-terrestrial matter (§4.2.1) and the basic physical processes (§4.2.2) that govern it. In a more general context, our activity will expand to “touch” the new emerging research field of Exobiology, meant as the general study of life in the Universe. On this, our contribution will evidently be on the Astrochemistry side. The major new challenge that the Astromol team will face is the study of the molecular complexity in the interstellar space, and the basic processes linked to it: molecule identification, formation, and evolution, with emphasis on during the star formation process, from the pre-collapse to the proto-planetary disk phase. This study will require substantial observational and theoretical progresses, and, consequently, a coordinated effort at the French, European and world level. Two new instruments, involving world wide consortia, will allow those major observational leaps and are at the 2007-2010 horizon: Herschel and ALMA (§4.3). Besides, a large European coordinated effort is on progress to exploit at best the potentialities of both instruments: the EC FP6 network “The Molecular Universe” (§4.4). Astromol is heavily involved in those three large international projects, and our activity in the next 2007-2010 will be scientifically and practically dominated by that. Indeed, the Astromol scientific involvement in these three large projects is heavy, ambitious and important at the same time. It will require a substantial enlargement of the group to fulfill the engagements and, most important, to fully exploit all the potentiality of this involvement, which should allow to keep a leading position of Astromol in the relevant studies (§4.6). 4.2 Scientific goals In the last four years, substantial progresses have been obtained in our understanding of how stars, notably solar type stars, form. New signatures and processes of the early formation of solar type stars have been discovered: e.g. the extreme molecular deuteration, which accompanies the freezeout of the heavy-bearing molecules, and the birth of hot corinos in the interiors of the envelopes. However, many questions remain open. Here we mention what we consider some major open questions which Astromol can help to answer in the next years to come. From a chemical point of view, it is totally unclear what is the ultimate molecular complexity reached during the proto-stellar phase. Do pre-biotic or even biotic molecules form? In what quantity? How? From a chemical and evolutionary point of view, it is even less clear what is the fate of these and any other molecules formed during the protostellar phase. Do they survive the proto-planetary disk phase? Are they incorporated into the forming and/or formed planets, via for example bombardment by comets and asteroids? In what quantity? How? 65
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LABORATOIRE D’ASTROPHYSIQUE DE GR
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III Team ASTROMOL 41 2 Presentation
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8.1.3 Graduate Students . . . . . .
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VI Team SHERPA 145 15 Results 147 1
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on PUEO at CFHT. The IFS experts (A
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Figure 11.5: Image of the binary st
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have taken responsibilities: A. Che
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Figure 11.10: thermal modeling of W
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Figure 12.1: All the GRIL projects
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12.2 Optical interferometry As for
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the VLTI. CHARA is equipped with an
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• ANR Alterdetect, with IMEP : si
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Mixed GRIL-other team profiles 1. A
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Name Grade Comm. Project Berger Jea
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• First fringes in the H band wit
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Table 15.1: List of the permanent S
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15.4 Transport phenomena in accreti
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Figure 15.2: Spectral energy distri
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states, combining a still powerful
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Excitation of turbulence by Cosmic
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Table 15.2: Former PhD students of
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Chapter 16 Perspectives The distinc
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Ray background. The second project
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- Ceccarelli Cecilia (AT) - Delfoss
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Among the various areas of expertis
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-responsable du groupe ”logiciel
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Chef de l’ Equipe ASTROMOL du LAO
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jury de concours: 1 concours IR CNR
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Chapter 20 Appendix 4: The Jean Mar
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20.10 Formation des utilisateurs La
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