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

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Figure 11.10: thermal modeling of WIRCam using FEA analysis and the Ideas/TMG thermal modelling software. Left: thermal model in the steady state of the filter wheels cage and the optical barrel; right: thermal model of the cold finger which transmits the cryogenic power to the cold structure. • Devices simpler to manufacture, low cost (one single active layer) • Far higher speed (1 GHz instead of 10 kHz) • Developments supported by numerous practical applications, including commercial ones, contrary to STJ. Superconducting Single Photon Detectors (SSPD) Niobium Nitride (NbN) Superconducting Single- Photon Devices are sensitive to radiation from UV to mid-IR. In terms of speed and sensitivity, they outperform any semiconductor and superconducting photon counters. They reach Quantum Efficiency (QE) of 20-30% at wavelengths of [1.3 µm; 1.55 µm], related to intrinsic QE close to 100%. Dark counting rate is extremely low: 10 −4 counts per second and less. Measured Noise Equivalent Power (NEP) is about 5.10 −21 W/ √ Hz in a wavelength range of [0.5 µm; 1.5 µm]. NbN SSPD is practical devices for non-invasive optical analysis of CMOS circuits and can be successfully used for quantum communications and quantum cryptography. These new detectors are developed in a collaboration with the CEA Grenoble and the Laboratoire de Spectrométrie Physique de Grenoble. Some first devices have been recently produced (Figure 11.11) and are currently under performance evaluation. These detectors are particularly interesting for the Lippmann spectral detectors (see Prospective). Figure 11.11: Left: 3x3 pixel array of 30 µm x 30 µm Ta-based STJ’s. Upper middle: details of the array structure with a Scanning Electron Microscope (SEM). Lower middle: single Ta-STJ. Right Scanning Electron Microscope (SEM) photography of a SSPD meander fabricated at the CEA-Grenoble. The width of the stripes and the distance between them are 150 nm. Courtesy of CEA-Grenoble/DRFMC/LCP (Jean-Claude Villégier). 128
Chapter 12 Perspectives The instrumental research and development objectives of GRIL are described here using the same frame as for the results, distinguishing between three instrumental families. The R&D activities and instrumental realizations, although tightly linked as previously explained, are separately described only for sake of clarity. 12.1 Adaptive optics We describe below the projects that are proposed for the next ”quadrennial period”. The instruments come first since there are the ultimate goal of GRIL activities. R&D is exposed afterward. Part of the projects have already started and other are extension of previous works into a more advanced and/or more ambitious phase. From the priority already exposed, the future activities will be preferentially directed towards extreme AO systems development. 12.1.1 Instruments PRIORITIES The imminent VLT PF 2 nd generation instrument whose contract should be signed early 2006, implies an important commitment on behalf of the LAOG with an expected schedule of the commissioning in 2010-2011, i.e. after the end of the present prospective period. See the chapter 11.1.2 for the scope of this instrument. LAOG provides some of the key-persons of the project and a large part of the resources for the integration and test phase. This project is therefore a major undertaking for our laboratory with two crucial expected returns : on the scientific side, a leading role in the survey, and on the technical aspects, an additional expertise that will be essential for the extreme AO-based instrumentation of the ELT era. Studies for ELT The preparation of ELTs already require conceptual studies both on the dedicated AO systems and the instruments based on special optimization of these systems. Among the projected concepts, an extreme AO-based imager, EPICS, takes benefit of the advances that led to the conceptual definition of the VLT-PF, to reach the ultimate contrast for e.g. low-mass extra-solar planet search. A very preliminary study of this concept has started with a participation of LAOG and shows the potential interest of a 3D spectroscopic approach as we previously demonstrated with the GRaF and GRiF instruments. We wish to keep involved in the next phases and specially the optimization of this ambitious instrument. 129
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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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Untitled - Laboratoire d'Astrophysique de l'Observatoire de Grenoble

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