Max Planck Institute for Astronomy - Annual Report 2005

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100 IV. Instrumental Development allows the observer to synthesize panoramic images with full, 23-meter spatial resolution. During 2005, Linc-nirvana passed its final design review, and is now well into the construction, integration, and testing phase. Highlights of the past year include completion of the large optical bench, receipt of the innovative hybrid cooling system, and the start of full-scale lab testing and verification of individual components. The optical bench (Fig. IV.4.1) presented a particularly interesting design challenge. The focal plane of the LBT lies approximately 2.5 meters above the instrument platform. The optical bench must provide a lightweight, stiff, vibration-damping reference surface that can carry the substantial mass of the various Linc-nirvana subsystems. The solution adopted was a monolithic carbon fiber and aluminum honeycomb table supported by fourteen hollow carbon fiber legs. The large steel base ring interfaces to the telescope and absorbs flexures due to different telescope orientations and dimensional changes due to temperature variation. With the bench now in place, the Linc-nirvana team has begun testing individual subsystems as they are delivered from our academic and industrial partners. One such subsystem is the ambient temperature fore-optics, consisting of two groups of three lenses for each side of the interferometer. Designing, constructing, and particularly, aligning these optics presents a serious challenge: not only must the lenses deliver diffraction-limited image quality over the wavelength range 0.6 to 2.5 µm, but also the two optical paths must be exactly matched to ensure maximum interferometric performance. During 2005 and the first part of 2006, the Linc-nirvana team tested Fig. IV.4.2: (Left) One of the warm fore-optics lens assemblies. (Right) Aligning and testing the complete fore-optics on a large optical bench. and characterized the warm fore-optics. When properly aligned, the lens groups exceed optical performance specifications. Completing the Linc-nirvana instrument will involve carrying these successful component tests forward into integration of sub-systems. For example, the warm fore-optics must now be integrated and tested with the large optical bench and other items currently being tested at the component level. Once the subsystems are complete, the team will begin testing and optimizing the performance of the instrument as a whole. The assembly, integration, and testing phase of Lincnirvana is now well underway. In the meantime, installation and commissioning efforts continue in Arizona on the telescope itself. With continued good progress on both fronts, the instrument will arrive at the LBT soon after completion of both adaptive secondary mirrors in Fall, 2008. At that point, the Large Binocular Telescope and Linc-nirvana can begin functioning as a Fizeau interferometer, delivering to MPIA astronomers unique observational capability. A detailed description of Linc-nirvana can be found in the MPIA Annual Report 2004, p. 75 – 86. (H. Baumeister, J. Berwein, P. Bizenberger, A. Böhm, J.L. Borelli, F. Briegel, F. De Bonis, M. Dörsam, S. Egner, R. Friedlein, W. Gässler, B. Grimm, S. Hanke, T. Herbst (PI), F. Kittmann, M. Kürster (PM), L. Labadie, W. Laun, U. Mall, L. Mohr, N. Münch, V. Naranjo, A. Pavlov, D. Reinmann, H.-W. Rix, R. Soci, E. Schinnerer, C. Storz, V. Volchkov. Collaborating Institute: inaf, I. Physikalisches Institut der Universität Köln, MPI für Radioastronomie, Bonn)
IV.5 LucifEr I / II – Spectrographs for the LBT LucifEr is a pair of multi-mode imagers and spectrographs for the Large Binocular Telescope (LBT). LucifEr is being built by a consortium of five institutes: the MPIA, Landessternwarte Heidelberg, MPE Garching, Ruhr- Universität Bochum, and Fachhochschule Mannheim. Fig. IV.5.1: LucifEr I and II in the dust-free experimental hall at MPIA. In the center, the assembled cryostat of LucifEr I is seen during the first cooling tests. Partly obscured behind it and in the foreground are parts of the second cryostat. Fig. IV.5.2: The Mos unit during the tests at MPE in Garching before installation into the cryostat. The worm drive with the two mask magazines in the foreground, while the exchange robot and locking device appear to the left and right, respectively. Since the end of 2005, tests have also been conducted in the original cryostat at cryogenic temperatures. IV.5 LucifEr I / II – Spectrographs for the LBT 101 The assembly of the two infrared camera/spectrograph-systems LucifEr I and II is making progress: in the year under report, both cryostats were completed, tested and delivered to the MPIA. One cryostat was subsequently transported to the Max Planck Institute for Extraterrestrial Physics in Garching for integration of the cryogenic multi-object spectroscopy unit (Fig. IV.5.2). Two auxiliary cryostats for changing the mask magazines were completed at MPE, allowing the team to test and optimize the process of magazine changing. LucifEr I is presently being integrated at the MPIA. The cold structure has been installed and tested at cryogenic temperatures. All opto-mechanical components will follow. In September 2005, the telescope simulator was delivered and set up in the experimental hall. Flexure tests will be carried out with this device to verify functional performance for varying telescope positions. During spring and summer 2006, integration of LucifEr I will be completed. Delivery is planned for spring 2007. LucifEr II will follow about one year later. (Bernhard Grimm, Werner Laun, Rainer Lenzen, Ralf-Rainer Rohloff. in cooperation with: Landessternwarte Heidelberg, MPI for Extraterrestrische Physik, Garching, Astronomisches Institut der Ruhr-Universität Bochum, Fachhochschule für Technik und Gestaltung, Mannheim)
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Max Planck Institute for Astronomy
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Max Planck Institute for Astronomy
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Contents Preface ..................
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6 I. General I.1 Scientific Goals U
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8 I. General massive protostars and
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10 I. General achieve higher angula
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12 I. General The institute is co-l
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14 I. General Point Source sensitiv
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16 I. General Edinburgh Groningen D
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18 II. Highlights II.1 Light Echoes
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20 II. Highlights 10 arcsec Fig. II
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22 II. Highlights AB Dor C AB Dor A
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24 II. Highlights II.3 The First He
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26 II. Highlights II.4 Planetesimal
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28 II. Highlights azimuthal directi
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30 II. Highlights ticles fall faste
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32 II. Highlights ANTU Seyfert 2 ga
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34 II. Highlights cretion disk, one
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36 II. Highlights 8.5 �m 2.3 ly 0
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38 II. Highlights II.6 Massive Star
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40 II. Highlights log M� /pc2 �
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42 II. Highlights II.7 Observations
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44 II. Highlights log IR luminosity
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46 II.8 Dynamics, Dust, and Young S
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48 II. Highlights and we see a temp
Page 52 and 53: 50 III. Selected Research Areas III
Page 54 and 55: 52 III. Scientific Work Fig. III.1.
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Page 90 and 91: 88 IV. Instrumental Development All
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Page 146 and 147: 144 Staff Directors: Henning (Actin
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150 Conferences Conferences and Mee
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152 Conferences D. Lemke: JWST-miri
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154 Conferences/Service in Comitees
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156 Publications Szalay, I. Szapudi
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158 Publications Hamilton, C. M., W
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160 Publications Brinkmann, D. G. Y
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162 Publications Zheng, X. Z., F. H
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164 Publications of the wheel mecha
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166 Publications ASP Conf. Ser. 331
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The Max Planck Society The Max Plan
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