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

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Among the various areas of expertise, very specific competences are available at LAOG, mainly related to micro-technologies. One concerns fiber optics and integrated optics conditioning, testing and operation for interferometry. The other one concerns adaptive optics mirror design and building. An important part of the software development activity, oriented towards interferometry users, is related to the JMMC (Jean-Marie Mariotti Center, see GRIL chapter and next Appendix). 18.3 Equipment The LAOG building contains specific facilities for technical developments and instrument integration activities. • Machine shop with required machining and metrology tools. • Working stations for CAO (mechanical design and finite element analysis together with related printing capabilities, thermal simulation, electronic design, optical design). • An optical lab dedicated to all Interferometry / Integrated Optics developments. It includes: – facilities for guided optics characterization and connectorization. – An anti-vibration bench devoted to interferometric measurements related to the image reconstruction issues connected to the VITRUV developments, – An anti-vibration bench devoted to interferometric measurements related to thermal IR wave guide characterization. • A small clean room for detector integrations, and micro-optics mounting. • An optical lab for adaptive optics developments, mainly for various Micro Deformable Mirrors characterization. • An electronic lab with all required tools • A 200 m 2 , 8-m high integration hall with related facilities (handling, fluid distribution capabilities, control rooms) • Vacuum room with all related equipment, including Helium leak detector • Specific metrology equipments for component and instrument qualification (Wavefront Sensor , electronic auto pointing collimators, optical and mechanical displacement sensors) • Specific sources and detectors for near and thermal infrared operations, and photometric characterization. Oncoming activities will require a significant evolution of the existing technical support. Due to the increasing range of activities but also to professional evolutions, it is already necessary to hire new engineers and technicians, specialists of adaptive optics system, of mechanical design and of software development. It is also mandatory to improve the LAOG experimental integration facilities, especially to be able to achieve the VLT-PF and possibly VITRUV, integration phases in state-of-the-art conditions. One of the major foreseen improvements is the environmental control of the integration hall and of the optical lab. The strong constrains that apply to these sophisticated instruments are a major issue in order to meet the expected severe requirements. 168
Chapter 19 Appendix 3: International and Local & National responsibilities of LAOG members 19.1 Responsabilités individuelles internationales 19.1.1 Astromol Ceccarelli Cecilia Co-Astronomer du Consortium Heterodyne Instrument for the Far Infrared (HIFI), a bord du satellite ESA Herschel Space Observatory (HSO) (2000-2006) Coordinator du Group “HSO-HIFI Star Formation” (2001-2006) PI du Key Program HSO-HIFI “Line Surveys of Star Forming Regions” (2005-2006) Task Manager de “Chemistry in Star Formation” du resau EC FP6 “The Molecular Universe” (2005-2006) Kahane Claudine Présidente de la commission d’évaluation de lÕenseignement de la Physique dans les Universites belges francophones (jan 2003 - mai 2003). Montmerle Thierry Membre du Comité des Programmes des satellites XMM (ESA, 2005) et Chandra (NASA, 2002-2003) Membre du Comité des Programmes de l’ESO, Président du Panel ”Star Formation” (2002-2005) Valiron Pierre Membre de l’Advisory Board de la revue Chemical Physics (-2006) 19.1.2 FOST Jean-Charles Augereau: - membres des groupes scientifiques des instruments VLT/PF et VLTI/ApreS-MIDI Jérôme Bouvier: (2000-2004): CEE FP5 RTN (Clusters): Grenoble + 6 CEE institutes, co-PI (2002-2003): Key Program CFHT, 2002-2003 CFHT12K/MEGACAM, PI (2005-2006): ECO-NET 2005 : Grenoble-Tashkent-Moscou, PI (2001-2002): Membre extérieur du TAC du Telescopio Nazionale Galileo, Italie (2001): Membre Steering Committee CFHT-WIRCAM (2004): Membre du Groupe Scientifique CFHT-ESPADONS Catherine Dougados: (2005-2008): CEE FP6 RTN (JETSET): Grenoble + 10 CEE institutes, co-PI, Membre du comité exécutif de JETSET (resp. du training et du suivi des étudiants) Gilles Duvert: 169
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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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Chapter 11 Results 11.1 Towards hig
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