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

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of CNRS for technicians and engineers) to LAOG’s Technical Director P. Kern (2004; the second such award after E. Le Coarer in 1999), and the “Palmes Académiques” (a Ministry of Education award for professional excellence) to LAOG’s Head of Administration F. Bouillet (2004). In addition, LAOG has had until recently the highest concentration of “Institut Universitaire de France” professors (G. Pelletier as senior member, J.-L. Monin and G. Henri as junior members). We thereore believe that LAOG is poised for a bright future and exciting science. As the present report aims at showing, there is no “growth crisis” at LAOG, because of continuous and sometimes radical adaptation to a constantly changing and challenging environment. We are convinced that this “Spirit of LAOG”, felt across all personnel categories, has been one of the strongest assets of this laboratory since its creation. 1.1.2 Evolutions: scientific strategy and team synergy Major evolutions have taken place at LAOG since 2002, with the aim of better fulfilling its major scientific goals and of making them more prominent and visible to the community and funding agencies, while accommodating an ever-growing population. In short, LAOG switched from a research structure of nine small thematic teams (sometimes as small as three individuals), supported by a technical group, and a theoretical team, to a simpler, more visible structure of four large teams. This evolution took place in two steps. • Following the recommendation of the previous Evaluation Committee in 2002 to look for a way to regroup the existing small scientific teams, and strongly encouraged by the new Director, the LAOG researchers, after many constructive internal discussions, decided to create two new “topical” teams, named “Astromol” and “FOST”, while keeping the theoretical group (Sherpas) intact. (See details below.) • After some time, it was however realized that instrumental research activities, central to the building of new instruments for large telescopes in relation to the scientific goals of LAOG, were not adequately taken into account. Technological developments are traditionnally strong at LAOG, and were conducted both by researchers and high-level engineers on a project-by-project basis. It was thus decided in mid-2004 to create a new, transverse group, the “GRIL”, where researchers and engineers would exchange ideas and work together globally, both as an official recognition of instrumental developments as a genuine research activity, and as a strategic and advisory group to the Director while keeping the scientific goals of LAOG in mind. In this team, most of the researchers also belong to one of the topical teams –in practice today the FOST team. Last but not least, the existence of such a team provides a correct, visible framework for PhD students working on instrumental topics. Figure 1.2 and Figure 1.3 display for comparison the previous organigram (2002) and the new organigram (2005), which will be discussed in more detail below. As a result, LAOG today is structured in four roughly balanced research teams (totalling 44 permanent staff), three topical and one instrumental, and in a technical group which is responsible for conducting the building of instruments after approval by GRIL (and of course after having been selected by external agencies). Figure 1.4 displays their respective sizes. To understand these evolutions, and before proceeding to describe the teams in more detail in the next section, it is appropriate to start with the main scientific axes developed over the years since the creation of LAOG a little more than a decade ago. These can be summarized as follows: • Origins: the physics of low-mass star formation and early evolution, and the path to planet formation; • High energies and astrophysical plasmas: the accretion-ejection phenomenon and its implications for astroparticle physics; • Instrumental research: high angular resolution and high dynamic range instruments for large telescopes. As schematically illustrated by Figure 1.5, these three scientific axes are strongly interrelated: the study of the conditions for star and planet formation (disks and jets from young stars and protostars; exoplanets), a 20
Figure 1.2: Old LAOG organigram (2002). The scientific activities were divided in nine teams, while a separate “Project group” included all the engineers and technicians. 21
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
Page 13: Part I Foreword: Presentation of th
Page 17: Part II Executive Summary A 18th ce
Page 22 and 23: Figure 1.3: New LAOG organigram (20
Page 24 and 25: heart attack. Manuel went back to t
Page 26 and 27: Figure 1.6: PhD student repartition
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Page 34 and 35: 1.5 From dreams to reality: Human r
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Page 41: Part III TEAM ASTROMOL Sub-arcsecon
Page 44 and 45: • we develop quantum and classica
Page 46 and 47: Table shows not only the volume of
Page 48 and 49: • Herschel-HIFI: Astromol is invo
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Page 52 and 53: • The hot corinos. More spectacul
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Page 60 and 61: Rate constant (cm 3 s -1 ) 1e-09 1e
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Page 68 and 69: 4.2.2 Molecular Physics The theoret
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Source Herschel Time Astromol Class
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several important studies that anti
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Chapter 5 Selected Publications •
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Part IV TEAM FOST The first image o
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393254 (5MJup at 55 AU) & AB Pic (1
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2.2 µ m 0.5" 11.7 µ m Figure 6.1:
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Figure 6.3: Contribution of heating
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such mid-term (several weeks) magne
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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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108
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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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144
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146
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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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Untitled - Laboratoire d'Astrophysique de l'Observatoire de Grenoble

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