Untitled - Laboratoire d'Astrophysique de l'Observatoire de Grenoble

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emphasis on the chemistry of planetary atmospheres, with an explicit goal to be involved in exoplanetary atmospheres by 2010. While LPG is concerned on the short term with solar system objects (mostly Titan, in relation with the Cassini-Huygens mission), LAOG (Astromol and/or FOST) will have discussions about possible common scientific goals for exoplanets in the same time frame, in preparation for Darwin. • Other space missions ? Over the long term, LAOG may also consider a greater instrumental involvement in telescopes that can only be put in space, while keeping within its scientific priorities: high-energies, and submm astronomy. The projects that one can consider would be mostly with CNES or/and ESA. In the high-energy, hard X-ray domain, the Sherpas team is already involved (for AGNs and compact binaries) in the scientific group around Simbol-X, a two-satellite proposal led by CEA Saclay (which is competing, along with Pégase, for a CNES-funded pre-Phase A study), but no instrumental development is currently foreseen at LAOG. In the 2015 timeframe, i.e., the same as Darwin, the XEUS project, successor to XMM, is the leading high-energy project within ESA. LAOG might be more involved in the project (which has strong support from space laboratories in France), but again likely not at the hardware level. In the submm domain of interest mainly for Astromol, Herschel, to be launched in 2007, will require many years of scientific exploitation. Its only currently identified long-term successor in ESPRIT, but with no date set for launch. On the other hand, there are already also here some thoughts about Antarctica (the most interesting domain is the THz range). Here again, there are no current plans for a LAOG hardware involvement, but it has to stay alert to possible evolutions. 1.7 Conclusions: A vision for the post-2010 future of LAOG By 2010, because of the important scientific results it has already obtained, and its successful bids to build new major instruments for the VLT, it can reasonably be expected that LAOG will have the following ambitious objectives for the next decade. But it has to grow again to accomplish them... • The VLT-PF and, hopefully, VITRUV will be completed and start operations at the VLT. This means that in the mean time, most of LAOG’s scientific results will be obtained with existing instruments, mostly at the VLT (with instruments it contributed to build or other Paranal instruments), and at CFH (exploitation of WIRCAM). A much better knowledge of the evolution of circumstellar disks, over a time span of ∼ 1 to ∼ 100 Myr, is expected from instruments like NAOS or AMBER. Along with work on the evolution of early solar system going on elsewhere (and at LPG in particular), the hope is that by 2010 we will know as much (or as little ?) about planet formation as we know about star formation today. Several hundreds of exoplanets, and possibly several tens of exoplanetary systems will be known, some containing Earth-like planets. Even though the VLT-PF has the main goal of imaging Jupiter-sized planets close to the host star, the recent images of the brown dwarf-exoplanet system 2M1207 demonstrate that several systems will certainly be imaged before the VLT-PF becomes available. On the other hand, studies will have matured at LAOG to contribute to building some kind of ELTs and/or single telescopes and possibly an interferometer in Antarctica, as well as contributing to the Darwin recombiner. The participation of LAOG to all these ventures will ensure activities of LAOG in the field of star and planet formation well into the next decade. But such ambitious goals require a significant increase in manpower in the coming years: 3-4 researchers for FOST, 3-5 engineers and technicians for GRIL and the Technical group. • The Herschel mission will be operational right into the present prospective, and thus, by opening a new window in the universe, will constitute the newest branch of submillimeter astronomy, with a rich harvest in spectroscopy and key results on star formation and early evolution. On the ground, IRAM telesscopes will play a pivotal role, at least until ALMA starts operations (hopefully in 2012), along with other existing (sub)millimeter telescopes elsewhere. Already a significant part of the astronomical activities related to star formation is dedicated to the search for prebiotic molecules, as part of a worldwide effort to develop exobiology. As explained in the prededing sections, the Astromol group is particularly well placed to pursue these lines of research. However, the task is daunting, and the Astromol team has to grow, and grow fast, since a few of its members will have retired by 2010. Hiring, and/or attracting at least 2-3 permanent researchers in the coming years is absolutely vital for Astromol. • A (tentative !) picture appears from combining three factors towards 2010: (i) development of exoplanet research in the FOST team; (ii) developments in the search for prebiotic molecules, and also in theoretical chemistry in the Astromol team; (iii) the planned developments in the chemistry of planetary and 38
exoplanetary atmospheres at LPG. This picture is the emergence of what might be called (in analogy with cosmology): observational exobiology, i.e. obtainining astrophysical and astrochemical diagnostics for contraining the conditions for the emergence of life in other planetary systems. This would be an extraordinary preparation for LAOG (in addition to its possible instrumental developments) and LPG to be really involved in the scientific exploitation of the Darwin mission. This could conceivably lead to create at that time a new team: S2E (Science des Exoplanètes et Exobiologie: Exoplanetary Science and Exobiology), possibly a joint venture of LAOG (researchers from FOST and Astromol ?) and LPG. (Close contacts with the CRAL group in Lyon, which is already very strong in brown dwarf and planetary atmospheres, should also be developed.) • On the high energy side, the adventure is no less exciting. As explained in the Sherpa prospective, the next decade will see the coming of age of an entirely new generation of telescopes, opening non-electromagnetic windows on the universe: gravitational waves and neutrinos. This will be the time of a radically new approach to the physics of black holes. Already the Sherpa team is exploiting data from high-energy telescopes both on the ground (HESS) and in space (X-ray and γ-ray satellites). Theoretical developments will require to explore new fields of physics and involve more and more numerical simulations. The goal of the Sherpa team is to hire 2 researchers in the coming years. What is not clear at present (but we have some time to think about it) is whether the Sherpa team will keep the close ties it has today with the rest of LAOG and still invest part of its efforts in the (more conventional ?) physics of young stars and planets: its expertise in magnetic fields and plasmas could still to be the common ground. We started this report by emphasizing the youth and fast growth of LAOG. We hope the reader is now convinced that there is currently no reason to fear a “growth crisis”, and that LAOG will be able to be up to the scientific challenges it wants to take. In total, it strongly hopes to hire or attract 7 to 9 new researchers, and 3 to 5 new engineers and technicians by 2010. Unless there is a crisis in funding (as was nearly the case in 2003), LAOG, in its local, national, and international environments, can only expect a bright long-term future. 39
Page 3: LABORATOIRE D’ASTROPHYSIQUE DE GR
Page 6 and 7: III Team ASTROMOL 41 2 Presentation
Page 8 and 9: 8.1.3 Graduate Students . . . . . .
Page 10 and 11: VI Team SHERPA 145 15 Results 147 1
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Page 17: Part II Executive Summary A 18th ce
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systems: HD 141569, HD 32297, HD 18
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C2D Spitzer/IRAC and MIPS data of s
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et al. 2002; 2003). We have found t
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Figure 6.8: Distribution of separat
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with only three known to date. Most
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300 objects, a size sufficient for
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therefore no surprise that vast eff
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data to verify the predictions we a
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Chapter 8 Appendices 8.1 Members of
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equipments for these tasks, from de
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10.1.3 Current trend of large equip
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• Improving High Angular Resoluti
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Chapter 11 Results 11.1 Towards hig
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Figure 11.2: NAOS-CONICA image of t
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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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Figure 11.7: PICNIC low noise infra
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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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164
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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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20.7 Production informatique ¡¢£
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20.10 Formation des utilisateurs La
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20.13 Darwin ¡¢£¤¥¦§¨©�
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