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

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on PUEO at CFHT. The IFS experts (A. Chalabaev and E. le Coarer) have recently contributed to the studies of the spectroscopic option for the VLT-PF instrument and are now studying the best possible integral field spectrograph designs for ELT’s. MCAO and GLAO studies In the frame of our collaboration with ONERA, a study has been initiated on the determination of the sky coverage for Multi Conjugate Adaptive Optics (MCAO). An optimized algorithm has been developed to improve previous sky coverage estimates, by more accurately accounting for instrumental and observational parameters such as the wavefront sensor concepts (star or layer oriented), the guide stars relative positions in the field and the guide star magnitude histogram. This work was conducted by A. Blanc on a 2-years contract financed by ESO. Another critical point for the conception of the next generation large field adaptive optics systems is the optimization of the wavefront sensing approaches. As part of these efforts, a ONERA-funded PhD thesis has been started in 2003 to address this question for the particular case of Ground Layer Adaptive Optics (GLAO) systems (co-directors: by T. Fusco and J.-L. Beuzit). 11.2 Bringing optical interferometry into mainstream astronomy The LAOG interferometric activities aims at bringing optical interferometry into mainstream astronomy. To fulfill this goal LAOG is carrying a multiple front effort going from instrumental research and development, instrument design and construction to real data analysis and interpretation. Optical interferometry has been developed in LAOG since 1995 through the participation to the Very Large Telescope Interferometer run by ESO and national actions on GI2T and FLUOR. Then LAOG has started an R&D activity in integrated optics in 1996 and has participated in 1998 to the VLTI/AMBER instrument. 11.2.1 The classical approach: AMBER AMBER is the three-telescope beam combiner for the VLTI operating in the J, H, and K bands and equipped with a spectrograph whose spectral resolution can reach 10000. It has been manufactured by a European consortium including the Observatoire de la Côte d’Azur, the Université de Nice, the Observatory of Arcetri (Italy), the Max-Planck Institute for Radioastronomie in Bonn (Germany) and the LAOG. This instrument has involved a major part of the LAOG resources during 6 years, for its design, its manufacturing and its integration. LAOG was in charge of the instrumental control device (resp. E. Le Coarer ), of the data reduction software (resp. G. Duvert), and of the assembly, integration and tests (resp. K. Perraut). The laboratory is also responsible of the leadership of the scientific group (F. Malbet, Project scientist) and the co-management of the projet (resp. P. Puget then P. Kern). Challenges The main challenges of AMBER consists mainly in the original design of such an instrument. The main idea was to merge the French expertise in interferometry both in high precision (FLUOR experiment) and spectro-interferometry (GI2T experiment). The AMBER concept is directly inherited from these two experiments using part of their technology: optical fibers, dispersed fringes,... In addition, we have developed a new way to process the signal with a very strong emphasis on internal calibration of all the instrument from the entrance to the pixels. It has produced a new data reduction algorithm based on carrying waves that we have called ”Pixel-to-Visibilities” processing. This processing relies on a full calibration of the internal effects to produce a matrix of the instrumental transfer function. The complex visibility is therefore a direct product from this matrix to the flux detected on the pixels. Current status AMBER has already produced a full hand of scientific results on the luminous blue variable Eta Carinae (Petrov et al. 2005, ESO conference), the evolved binary system Gamma Velorum (Petrov et al. 2005, ESO conference), the Be star HD 50013, the young stellar system MWC 297 (Malbet et al. 2005, ESO 120
Figure 11.4: Left: the AMBER instrument in the VLTI focal laboratory at the ESO Paranal VLT observatory. Right: first AMBER observations with the three Unit Telescopes on 70 Aql with the medium spectral resolution in K band. From ESO Press Release 07/04. conference) and some progress in the qualification of the instrument for exoplanet detection. The result on MWC 297 is developed in the FOST part. AMBER expected on-sky performances in terms of limited magnitude, spectral resolution and dynamic range have no equivalent. This translates into mandatory requirements for the VLTI in terms of dynamical cophasing and throughput that have not yet been met. Informations gathered during AMBER commissioning periods have been a key point to reveal current VLTI weaknesses (various sources of vibration, degradation on PSF in the delay-lines tunnel, etc. yielding low instrumental contrast). Much is expected from the VLTI recovery plan under progress in order for AMBER to reach its final performances. The instrument has been offered to the European astronomical community for the first time for the period P76 (starting 1st Oct 2005) and proposed again for P77. The commissioning period is still continuing with long periods of waiting for improvement of the performance of the VLTI subsystems. The VLTI is in 2005 following a recovery plan that should in principle help to eventually reach the AMBER ultimate performances. Most of the remaining actions for LAOG people are now commissioning runs, data reduction, support to the astronomical community for preparing observations and optimally using the AMBER ability, science planning for the Guaranteed Time Observations (GTO) and publication. Several PhD students have taken part to this project: P. Mège at the concept study, C. Gil during integration in Grenoble, E. Tatulli and F. Millour for the data reduction algorithms. A CNRS postdoc has been hired to focus on the astrophysical interpretation of commissioning data: W.-J. De Wit. This instrument is being used by member of the FOST team and SHERPA team. An internet web site is being hosted by LAOG at the following address: amber.obs.ujf-grenoble.fr. Fabien Malbet is the main responsible for this activity at LAOG. 121
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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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-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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20.10 Formation des utilisateurs La
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Untitled - Laboratoire d'Astrophysique de l'Observatoire de Grenoble

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