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

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Part I Foreword: Presentation of the Report The welcome web page of the LAOG as of October 6, 2005 13
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 15: Chapter 1 The last Visiting Committ
Page 19 and 20: 1.1 Presentation of LAOG 1.1.1 A yo
Page 21 and 22: Figure 1.2: Old LAOG organigram (20
Page 23 and 24: Figure 1.4: The current repartition
Page 25 and 26: Permanent staff: 7. PhDs completed:
Page 27 and 28: - First fringes in the H band with
Page 29 and 30: clearly in its goals to have scient
Page 31 and 32: organization of astronomy events li
Page 33 and 34: • Contract-related funding. These
Page 35 and 36: in relation with planet formation.
Page 37 and 38: BASECOL database hosted in Meudon t
Page 39: exoplanetary atmospheres at LPG. Th
Page 43 and 44: Chapter 2 Presentation and Scientif
Page 45 and 46: supported by PCMI and PNPS, and mem
Page 47 and 48: (PV) are also involved in several h
Page 49 and 50: Chapter 3 Results 3.1 Overview In t
Page 51 and 52: et al. 2002, 2003). When CO disappe
Page 53 and 54: 3.2.4 The outflows of protostars As
Page 55 and 56: Since X-rays mainly come from flare
Page 57 and 58: • Monitoring of the error propaga
Page 59 and 60: Rate coefficient (cm 3 s -1 ) 1e-10
Page 61 and 62: Differential Cross Section (Å 2 sr
Page 63 and 64:
Figure 3.7: Detection of HDO in the
Page 65 and 66:
Chapter 4 Perspectives 4.1 Overview
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in the midplane of young disks surr
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more difficult (iv) The region wher
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• 12D-Surface of NH3 with H2 •
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for doing that, but we are limited
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• Determination of the gas-to-dus
Page 79 and 80:
Chapter 6 Introduction of the team
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the central star. They regulate the
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disks. At these wavelength, the bul
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Wind and disk interaction in MWC 29
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6.3.3 The physics and origins of ma
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Figure 6.5: Observation and model o
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Multiplicity of protostars Followin
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masses up to 10 solar masses for a
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Figure 6.9: Top panels: DENIS disco
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process by comparing its outcome fo
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With this new tool at hands, search
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Chapter 7 Future Research Direction
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at LAOG (in collaboration with Gene
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8.1.3 Graduate Students Completed P
Page 107 and 108:
Part V TEAM GRIL The first fringes
Page 109 and 110:
Chapter 9 Presentation of the team
Page 111 and 112:
Chapter 10 Scientific rationale 10.
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The first and last items are a defi
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Figure 10.1: The logical link betwe
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Figure 11.1: NAOS-CONICA installed
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Figure 11.3: Left: the first 52-act
Page 121 and 122:
Figure 11.4: Left: the AMBER instru
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Figure 11.6: Left: Integrated optic
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Figure 11.8: Left panel: Process fl
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Figure 11.9: Left View of the WIRCa
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Chapter 12 Perspectives The instrum
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12.1.2 R&D activities PRIORITIES Fo
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laboratories of OSUG, a collaborati
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collaborations. Moreover, part of o
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Chapter 13 Recruitment plan GRIL ne
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Chapter 14 Appendix 14.1 Staff 14.1
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• Tantalum superconducting tunnel
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• I3 IInternational Integrating I
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Part VI TEAM SHERPA The two-flow pa
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Chapter 15 Results 15.1 History and
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Figure 15.1: A standard accretion d
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mechanics community, for non-rotati
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to be produced in the relativistic
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Figure 15.3: The spectrum of cosmic
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Ferreira, in collaboration with Ron
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• “Particle Transport in Tangle
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controls the level of the anomalous
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Part VII APPENDICES 163
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Chapter 17 Appendix 1: General orga
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Chapter 18 Appendix 2: LAOG Technic
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Chapter 19 Appendix 3: Internationa
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19.2 Organisation de colloques, wor
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(2003-présent): Membre du CNAP, se
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Membre du conseil scientifique du L
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• LESIA (Observatoire de Paris-Me
Page 179 and 180:
20.9 Groupes de Recherche et Dével
Page 181 and 182:
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Page 183:
20.15 Prospective Le centre Mariott
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Untitled - Laboratoire d'Astrophysique de l'Observatoire de Grenoble

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