Annual Report 2011 Max Planck Institute for Astronomy

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74 IV. Instrumental Developments and Projects Credit: W. Gässler Credit: W. Gässler Fig. IV.2.2: The swing arms mounted on the LBT. They are retracted in their park position at the inner windbrace. Fig. IV.2.3: The dichroic in its test mount. The reflection and transmission of the unit was measured and verified. year the laser system will be installed at the telescope followed by the wavefront sensor in summer of the year after. Finally, in 2014, argos is supposed to be handed over to the user community. Involved at MPIA: Wolfgang Gässler (Co-I), Thomas Blümchen, Jose Borelli, Martin Kulas, Michael Lehmitz, Diethard Peter. Partners (local representatives only): Wolfgang Gässler (MPIA), Sebastian Rabien (MPE), Simone Esposito (INAF-OAA), Michael Loyd-Hardt (UA), Andreas Quirrenbach (LSW), Jesper Storm (AIP), Richard Green (LBTO), Udo Beckmann (MPIfR)
IV.3 MatiSSe – Interferometric Imaging in the Mid-Infrared MatiSSe – the Multi Aperture Mid-Infrared SpectroScopic Experiment – is one of two second generation instruments which had been selected by eSo for the VLTI at Paranal. Thus MatiSSe is in a sense the successor of Midi, the Mid-Infrared Interferometric Instrument, which has been built at MPIA and which is working on Paranal since 2003. Matisse will combine the beams of up to four of the 8 m UTs (Unit Telescopes) or of up to four of the 1.8 m ATs (Auxiliary Telescopes) and thus will be able to measure in “closure phase mode”, i.e. it offers an efficient capability for image reconstruction with a spatial resolution of up to 7 milliarcsec. The instrument will work at three wavelength bands: L (3.2 – 3.9 μm), M (4.5 – 5 μm), and N (8 – 13 μm), where the L and M band observations are performed simultaneously to the N band. With the three different spectroscopic resolutions in the range of R 30 – 1500 it will provide the basis for a fundamental analysis of the composition of gas and dust grains in various astrophysical environments. Key science programs for the ATs cover for example the formation and evolution of planetary systems, the birth of massive stars as well as the observation of the highcontrast environment of hot and evolved stars. With the UTs selected astrophysical programs such as the study of Active Galactic Nuclei and Extrasolar Planets shall be possible. Matisse is developed and built by a collaboration of the Observatoire de la Cote d’Azure, the MPIA, the MPI for Radio Astronomy in Bonn and two institutions (astron/Dwingeloo and Leiden University) from the Netherlands. In this consortium MPIA is responsible for the cryogenics system, the entire control electronics, and the instrument control software. After the successful Preliminary Design Review (PDR) in December 2010 the year 2011 was dominated by the preparations for the first part of the Final Design Fig. IV.3.1: Pulse tube cooler PTC 410 from Cryomech. The two copper plates mark the two stages. Fig. IV.3.2: Head of Pulse tube cooler with damping system on test set-up. Review (FDR) in September 2011, where the cryogenic system and the design of the optics were reviewed by eso. For the development of the cryostats several tests Table. IV.3.1: The characteristic parameters of Matisse. Number of beams/ telescopes 4 (2 or 3 possible) Field of view 2 arcsec Spectral resolution L/M N Low 20 R 40 20 R 40 Medium 200 R 400 200 R 400 High 750 R 1250 Spatial resolution 0.007 arcsec 0.02 arcsec had to be performed. By using an auxiliary cryostat we specified the characteristics of the selected Pulse Tube Cooler PT410 from Cryomech (Fig. IV.3.1). With using such a device the induced vibrations are typically factors of 10–50 lower than with normal Closed Cycle Coolers of similar cooling power. Besides the vibrations inside and outside of the test cryostat we also tested for the minimum temperatures to be reached with this kind of cooler at its first and second stage and for the temperature variations caused by the cooler when connected to a dummy cold optical bench (first stage) and a dummy detector (second stage). Here the copper braid used for this connection had to be opti- Credit: U. Graser Credit: U. Graser 75
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Contents Preface ..................
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6 I. General Credit: MPIA / AMQ I.
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8 I. General lows us to understand
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10 I. General Credit: CAHA I.2 Obse
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12 I. General in December 2009, the
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14 I. General Credit: eSo/l. calça
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16 I. General Point source sensitiv
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18 I. General I.3 National and Inte
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Page 96 and 97: 94 V.3 Honors and Awards Ernst Patz
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128 Publications Hansen, S. H., A.
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132 Publications Notices of the Roy
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134 Publications Riechers, D. A., F
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144 Publications Astrophysics of Pl
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Annual Report 2011 Max Planck Institute for Astronomy

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