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

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– Ceccarelli Cecilia (AT) – Delfosse Xavier (AA) – Ferreira Jonathan (MC) – Malbet Fabien (CR) – Ménard François (CR) – Delboulbé Alain (IE) – Preis Olivier (IE) – Stadler Eric (IR) • Nominated members – Chelli Alain (AT) – Beust Hervé (AA) – Lefloch Bertrand (CR) – Bouillet Françoise (IE) – Freautrier Philippe (IR) – Kern Pierre (IR) 17.2 Management tools and quality control In order to project an attractive image of its activities, LAOG has invested in refurbishing its web site: http://www-laog.obs.ujf-grenoble.fr through which all the main documents can be accessed, either publicly or internally. The activities of the teams are publicly available and regularly presented. A highlight window in the home page allows to directly browse through recent major results of LAOG, several of which having been the subject of press releases by our agencies (mainly CNRS and ESO). Also available via the LAOG web page is Symastro, an internal management system through which various documents (including instrumental projects), reports, minutes of meetings, electronic forms (orders, missions), etc., can be accessed using quality-control rules. Among the new documents is the “Règlement Intérieur” (LAOG by-laws), which regulates many aspects of the everyday life at LAOG (safety recommendations, working hours, composition of internal councils, etc.). 166
Chapter 18 Appendix 2: LAOG Technical group & facilities 18.1 Introduction The organization LAOG technical group is driven by the necessity to support efficiently the activity of the astrophysical teams, mainly dedicated on three points: • general support to the laboratory (computing support); • R&D actions dedicated to the preparation of future operations; • direct involvements in the realization of large instruments dedicated to large international facilities and agencies (VLT-ESO, ESA, CNES, CFHT). The main drivers are the critical astrophysical requirements, which are mostly related to High Angular Resolution (HAR) observations for the two last above items. 18.2 Teams The composition of the technical group aimes at having the full range of required specialties for all design studies of very specific instrument dedicated to HAR observations, either through adaptive optics or interferometry (mechanics, optics, electronics, instrument control, system engineering, project management, and software development). An important part of the staff, 21 engineers and technicians, has a strong expertise for the design of the instruments main critical aspects. The technical group is thus organized into 5 teams (see organigram in Figure 1.3 ) 1. Instrumentation, including optics, tests and system expertise 2. Electronics, including design, cabling, and system expertise 3. Mechanics, with strong expertise in CAO, detailed design, finite element analysis, MEMS/MOEMS design 4. General support to the computing LAOG facilities 5. Software developments for all instrumental projects. 167
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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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Part I Foreword: Presentation of th
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Part II Executive Summary A 18th ce
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of CNRS for technicians and enginee
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Figure 1.3: New LAOG organigram (20
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heart attack. Manuel went back to t
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Figure 1.6: PhD student repartition
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• LAOG researchers (and publishin
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and published 95 papers in four yea
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• National astronomy programs. 4
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1.5 From dreams to reality: Human r
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and accretion disks with heavy nume
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emphasis on the chemistry of planet
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Part III TEAM ASTROMOL Sub-arcsecon
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• we develop quantum and classica
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Table shows not only the volume of
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• Herschel-HIFI: Astromol is invo
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particular, we calculated a 9D H2O-
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• The hot corinos. More spectacul
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the massive deeply embedded protost
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tens of visual magnitudes, hence pr
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quantum VCC-IOS approximation may f
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Rate constant (cm 3 s -1 ) 1e-09 1e
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• One of us (PV) is strongly invo
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sublimation of water ice trapped ei
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If the chemistry in the first phase
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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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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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Page 182 and 183: 20.13 Darwin ¡¢£¤¥¦§¨©�
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Untitled - Laboratoire d'Astrophysique de l'Observatoire de Grenoble

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