Max Planck Institute for Astronomy - Annual Report 2007

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92 IV. Instrumental Developments and Projects IV.1 Instruments for the LBT Lucifer i/ii: Two Multi-Mode Instruments for the Near Infrared The first of two identical infrared instruments, Lucifer I and II, will be delivered mid 2009 to the Large Binocular Telescope (LBT) near Tucson. The complex systems consist in each case of a highly resolving infrared camera, a long-slit spectrograph, and a multi-object spectrograph– they will be the central infrared devices on the LBT. The first tests of the entire system were performed at the end of 2007 after Lucifer I’s assembly at the MPIA. Simultaneously, at the MPI for Extraterrestrial Physics the unit for multi-object spectroscopy (Mos) was produced and tested. At the end of 2007 it was installed at the MPIA in Lucifer I. Essentially the Mos unit consists of a cryogenic mask changer: A robot system enables longslit or Mos masks to be exchanged out of a loader. The loaders can be exchanged during the day without having to warm the cryostats. The second Lucifer instrument should follow in about one year. Fig. IV.1.1: Both LBT individual telescopes will be equipped with an IR camera spectrograph. LUCIFER - I / II Instrument Concept Lucifer (LBT NIR Spectrograph Utility with Camera and Integral Field Unit for Extragalactic Research) is a spectrograph with camera designed for use at the LBT in the near infrared (wavelength range of 0.9 to 2.5 micrometers). A consortium of five Institutes (State Observatory Heidelberg, MPIA, MPI for Extraterrestrial Physics, Astronomical Institute of the Ruhr-Universität Bochum, and the University of Applied Sciences for Technology and Design Mannheim) built two identical versions of this instrument. Lucifer I/II will be the LBT’s workhorse in the near infrared. It will be able to deliver infrared images and spectra both with seeing and diffraction limited angular resolution. An overview of the various observation modes is provided in Tables IV.1.1 and IV.1.2. The instrument will work at temperatures of less than 70 K. Essentially, the following observation possibilities are available: • seeing-limited imaging • diffraction-limited imaging with a field of vision of 0.5 0.5 square arc minutes • long-slit spectroscopy (seeing- and diffraction-limited) • multi-object spectroscopy (Mos) with slit mask
mode seeing limited diffrectionlimited camera N 3.75 N 1.8 N 30 FOV 434 434 0.5 3 0.5 f Coll 1500 mm 1500 mm 1500 mm f Cam 375 mm 1800 mm 3000 mm f eff 30 940 mm 14 850 mm 247 540 mm scale 120 mas/pxl 250 mas/pxl 15 mas/pxl pupil diameter 102 mm 102 mm 102 mm spaltlänge 4 4 0.5 R lim 10 000 500 FSR (K) 0.22 µm 0.46 µm Table. IV.1.1: Instrumental parameters of the diffraction-limited and seeing-limited observing modes. The switch between direct imaging and spectroscopy takes place by swiveling the lattice unit (exchanging a flat mirror with a grating) and changing the focal mask (from field-limited mask to long-slit or multiple-slit mask). This swap of focal masks takes place via a complicated cryogenic robot system which was developed at the MPI for Extraterrestrial Physics. A special observing mode – not shown in Table IV.1.2 – is still in the preparatory phase: To support the search for extrasolar planets, an optical system is being integrated in the filter discs delivering four parallel images with the f/30 camera that have slightly different narrow-band filters at and near the methane absorption wavelength of Fig. IV.1.2: The optical concept of the camera and of the spectrograph. entry window filter wheel detector fold mirror 2 collimator L2 focal plane parameter camera spectroscopy scale FOV resolution scale FOV resolution scale FOV resolution Table. IV.1.2: The available observing modes. 1.6 µm. Thus differential images can be created which facilitate the search for planets in the immediate vicinity of bright stars, particularly where there are high levels of methane in the planetary atmospheres. The optical components required for this are currently being built at the Institute for Applied Optics and Fine Mechanics in Jena. Technical Details 0.25 /pxl 434 acquisition mode only narrow band filter 0.12 /pxl 434 wide and narrow band filter 0.015 /pxl 0.530.5 FOV limited by isoplanatism IV.1 Instruments for the LBT 93 0.25 /pxl 334 500 – 5000 acquisition mode total band zJHK longslit and MOS 0.12 /pxl 433 1000 – 10 000 longslit and Mos 0.015 /pxl 0.530.5 4000 – 40 000 longslit The Optical System The optical concept is represented in Fig. IV.1.2: To permit cold field boundary masks, long slit and Mos masks to be swiveled in, the focal plane of the telescope is located in the cryogenic region (behind the entry window). The entry window itself is an AR coated quartz window which is inclined by 15 degrees against the optical axis. The reflected optical fraction of the incoming light is collimator L1 camera collimator L3 fold mirror 2 grate/mirror
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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. General I.1 Scienti
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8 I. General Planet and Star Format
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10 I. General plementary. Ground-ba
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12 I. General High-fidelity imagers
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14 I. General Fig. I.6: Foreseen de
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16 I. General I.3 National and Inte
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18 I. General Edinburgh, University
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20 II. Highlights II.1 Youngest Ext
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22 II. Highlights radial velocity [
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24 II. Highlights II.2 A Search for
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26 II. Highlights F 1 [5] -2 0 2 4
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28 II. Highlights Number of Planets
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30 II. Highlights z [AU] z [AU] 1 0
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32 II. Highlights t =0 T orb t =1 T
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34 II. Highlights II.4 An Exoplanet
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36 II. Highlights F / F 12m 4 3 2
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38 II. Highlights the planet disapp
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40 II. Highlights The Hercules Dwar
Page 44 and 45: 42 II. Highlights on the giant bran
Page 46 and 47: 44 II. Highlights II.6 Black Hole A
Page 48 and 49: 46 II. Highlights F [10 -23 W cm -
Page 50 and 51: 48 II. Highlights Flux [10 -23 W cm
Page 52 and 53: 50 II. Highlights Fig. II.7.2: A 22
Page 54 and 55: 52 II. Highlights i [mag] i [mag] 1
Page 56 and 57: 54 II. Highlights Follow-up Observa
Page 58 and 59: 56 II. Highlights II.8 Unique Galay
Page 60 and 61: 58 II. Highlights NGC5055 (M63) NGC
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Page 66 and 67: 64 III. Selected Research Areas III
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Page 120 and 121: 118 V. People and Events Dr. Gerner
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Page 126 and 127: 124 V. People and Events Ludwig-Bie
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Page 138 and 139: 136 Staff Directors: Henning, Rix (
Page 140 and 141: 138 Staff / Calar Alto / Department
Page 142 and 143: 140 Teaching Activities / Service i
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142 Further Activities / Compatibil
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144 Cooperation with Industrial Com
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146 Conferences StageS workshop, MP
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148 Conferences Ralf Launhardt: Wor
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150 Conferences Anna Pasquali: ASU
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152 Publications Apai, D., A. Bik,
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154 Publications Chen, X. P., R. La
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156 Publications of an unusual dwar
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158 Publications Moreau, J. A. Peac
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160 Publications Pontoppidan, K. M.
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162 Publications Garching-Bonn Deep
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164 Publications Zirm, A. W., A. va
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166 Publications Linz, H., R. Klein
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168 Publications Güdel, M.: The su
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A656 Eppelheim Patrick- Henry- Sied
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Max Planck Institute for Astronomy - Annual Report 2007

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