Max Planck Institute for Astronomy - Annual Report 2005

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14 I. General Point Source sensitivity (1 h , 5s) [Jy] 1 0.01 10 –4 10 –6 10 –8 10 –10 LAICA CHEOPS LINC-NIRVANA Ω 2000 MIDI LUCIFER APRÈS–MIDI DARWIN (est.) JWST MIRI HERSCHEL– PACS 1 10 100 Wavelength [mm] Fig. I.7: The Institute's major instruments. Left: sensitivity as a function of wavelength; right: spatial resolution as a function of the field of view. cision-optical hearts of miri and nirSpec the MPIA is also closely cooperating with Carl Zeiss Optronics, Oberkochen. The MPIA has been representing Germany since 1998 within the Darwin Science Advisory Team. Darwin is a space interferometer to be launched by the European Space Agency eSa not before 2015. In the plan it will comprise up to eight telescopes orbiting the Sun at the Lagrangian point L2, at 1.5 million kilometer distance from Earth. This observatory will be used for imaging and spectroscopy of extrasolar planets in the mid-infrared range. At present, the Institute is carrying out preparatory technology studies. MPIA also contributes to eSa's Gaia project, a space observatory scheduled for launch between 2010 and 2012. Spatial Resolution [milli-arsec] 1 10 100 1000 10 4 10 5 APRÈS–MIDI MIDI DARWIN PLANET FINDER JWST MIRI HERSCHEL PACS LINC-NIRVANA CONICA/ LUCIFER Ω 2000 LAICA 1� 10� 100� 1000� 10000� Field of view Gaia will be the successor to the hipparcoS astrometry satellite, exceeding the latter’s sensitivity by several orders of magnitude. With this the satellite will measure positions, magnitudes and radial velocities of one billion stars plus numerous galaxies, quasars and asteroids. The telescope will provide photometric data in 15 spectral bands as well as spectra in a selected spectral range. Unlike hipparcoS, however, Gaia needs not be provided with an input catalogue, but will measure systematically all accessible objects. An automatic object classification will thus be of major importance for data analysis. At present, concepts for coping with this demanding task are being developed at the MPIA (supported by a grant from DLR). Figure I.7 gives an overview of the major instruments which are already working or are about to be put into operation. Sensitivity is shown as a function of wavelength (left), and spatial resolution as a function of the size of the field of view (right). PRIME
I.3 National and International Cooperations Its location in Heidelberg embeds the MPIA into an exceptionally active astronomical environment. Cooperation with the department Kosmophysik of the MPI für Kernphysik and with the institutes of the Center for Astronomy Heidelberg (ZAH), established on January 1 st 2005, are manifold (the ZAH consists of the Landessternwarte, the Astronomische Rechen- Institut, and the Institut für Theoretische Astrophysik der Universität). At present, this is particularly true for the long-standing DFG-Sonderforschungsbereich No. 439, »Galaxies in the Young Universe«, in which all Heidelberg institutes named above are participating. There is also a close cooperation within the »International Max Planck Research School« (IMPRS) for Astronomy and Cosmic Physics (see I.4). In addition, MPIA supports the University of Heidelberg in its activities for the Excellence Initiative. Nationally, cooperation with the MPI für extraterrestrische Physik in Garching and the MPI für Radioastronomie in Bonn as well as with numerous German institutes is extensive. An overview is given in Fig. I.8. The establishment of the German Center for Interferometry (Frontiers of Interferometry in Germany, or frinGe for short), located at MPIA, also emphasizes the Institute’s leading role in Germany in this trend-setting astronomical technique. The goal is to coordinate efforts made by German institutes in this field and to request the interests of German community in the European Interferometric Initiative. Another specific goal is the preparation of the next generation of interferometric instruments. This includes the preparation of second generation VLTI-instruments such as matiSSe (the former apréS-miDi) – an imaging interferometer consisting of four telescopes – and Gravity. Further tasks are: participation in the definition of new imaging capabilities of the VLT interferometer, and participation in preparing the Darwin space mission. frinGe, together with other interferometric centers in Europe, was partaking in the establishment of the European Interferometry Initiative. The long-term perspective is to establish a European interferometric center for the optical and infrared wavelength region. Apart from MPIA, the following institutes are participating in frinGe: the Astrophysikalische Institut Potsdam, the Astrophysikalische Institut der Universität Jena, the Kiepenheuer-Insitut für Sonnenphysik in Freiburg, the MPI für extraterrestrische Physik in Garching, the MPI für Radioastronomie in Bonn, the Universität Hamburg, and the I. Physikalische Institut der Universität zu Köln. MPIA is participating in a number of EU-networks and worldwide collaborations, in part as project leads. These include: Bochum Köln Bonn Kaiserslautern Darmstadt Mannheim Heidelberg Hamburg Braunschweig Tautenburg Dresden Jena Chemnitz Tübingen Donaueschingen Garching Freiburg München Potsdam Fig. I.8: Distribution of German partner institutes of MPIA OpticOn:. A network of all operators of major telescopes in Europe, financed by the European Union. Its one main goal is to optimize use of the scientific-technical infrastructure in order to increase scientific results and reduce costs. opticons other main goal is to coordinate technology development for the next generation ground-based telescopes. Within opticon, the Calar Alto Observatory with its 2.2m and 3.5m telescopes is participating in the comet program that includes a total of 20 European telescopes. Observing teams from every country of the EU and associated countries that have been allocated observing time at the telescopes by the caha Program Committee get free access as well as scientific and technical support in the realization of their observations. For this service, caha is compensated financially from opticon. The matiSSe study at MPIA mentioned above is supported by opticon and the European Interferometry Initiative (EII), as is the software work on image reconstruction for Linc-nirvana (Chapter IV.4). opticon is also supporting a so-called Joint Research Activity (JRA) of MPIA with the Osservatorio Astrofisico di Arceti and the University of Durham and other partners. Within JRA a prototype of a multiple-field-of-view 15
Page 1 and 2: Max Planck Institute for Astronomy
Page 3 and 4: Max Planck Institute for Astronomy
Page 5: Contents Preface ..................
Page 8 and 9: 6 I. General I.1 Scientific Goals U
Page 10 and 11: 8 I. General massive protostars and
Page 12 and 13: 10 I. General achieve higher angula
Page 14 and 15: 12 I. General The institute is co-l
Page 18 and 19: 16 I. General Edinburgh Groningen D
Page 20 and 21: 18 II. Highlights II.1 Light Echoes
Page 22 and 23: 20 II. Highlights 10 arcsec Fig. II
Page 24 and 25: 22 II. Highlights AB Dor C AB Dor A
Page 26 and 27: 24 II. Highlights II.3 The First He
Page 28 and 29: 26 II. Highlights II.4 Planetesimal
Page 30 and 31: 28 II. Highlights azimuthal directi
Page 32 and 33: 30 II. Highlights ticles fall faste
Page 34 and 35: 32 II. Highlights ANTU Seyfert 2 ga
Page 36 and 37: 34 II. Highlights cretion disk, one
Page 38 and 39: 36 II. Highlights 8.5 �m 2.3 ly 0
Page 40 and 41: 38 II. Highlights II.6 Massive Star
Page 42 and 43: 40 II. Highlights log M� /pc2 �
Page 44 and 45: 42 II. Highlights II.7 Observations
Page 46 and 47: 44 II. Highlights log IR luminosity
Page 48 and 49: 46 II.8 Dynamics, Dust, and Young S
Page 50 and 51: 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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64 III. Scientific Work z [AU] 1 0
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66 III. Scientific Work line observ
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68 III. Scientific Work log F /mJy
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70 III. Scientific Work Column dens
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72 III.3 The Galaxy-Dark Matter Con
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74 III. Scientific Work redshift su
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76 III. Scientific Work Mocking the
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78 III. Scientific Work tion rate o
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80 III. Scientific Work observed is
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82 III. Scientific Work DDO 53 HO I
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84 III. Scientific Work Fig. III.4.
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86 III. Scientific Work tribution o
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88 IV. Instrumental Development All
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90 IV. Instrumental Development Nir
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92 IV. Instrumental Development The
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94 IV. Instrumental Development L3
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98 IV. Instrumental Development IV.
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102 IV. Instrumental Development IV
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106 IV. Instrumental Development IV
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108 IV. Instrumental Development jo
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110 V. People and Events 1� 10�
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112 V. People and Events V.2 Open H
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114 V. People and Events V.3 Furthe
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116 V. People and Events presented.
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118 V. People and Events The IMPRS
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120 V. People and Events Fig. V.5.2
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124 V. People and Events These oppo
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130 V. People and Events V.10 The P
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132 V. People and Events Abb. V.11.
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134 V. People and Events V.13 Four
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136 V. People and Events Lemke: I w
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138 V. People and Events Fig. V.13.
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140 V. People and Events V.14 Where
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142 V. People and Events against sp
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144 Staff Directors: Henning (Actin
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146 Working Groups Rainer Lenzen, H
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148 Cooperation with industrial Fir
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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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