Max Planck Institute for Astronomy - Annual Report 2005

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90 IV. Instrumental Development NirSpeC is a spectrometer for the near-infrared range with a resolution of l /Dl � 100 and 1000. It allows simultaneous spectroscopy of more than 100 objects within its field of 3 3 3 arcminutes. For the selection of the objects of interest a silicon shutter array with small electrically-controlled micro-shutters (similar to an Advent calendar) is currently being developed. Only those shutters which are open will admit the light from the galaxies of interest. This multi-object spectrograph is developed by eSa and built by aStriuM, Germany. The MPIA is making contributions to this instrument. This instrument will allow study of, among other things, the redshifts, element abundances, excitation conditions, and spatial velocities in galaxies and quasars of various ages. Furthermore, the reionization of the universe by the first hot stars can be investigated in some detail. The development of this instrument is guided by an international science team picked from eSa member states. Miri is the most complex of the three instruments. It consists of a camera with coronagraph and a spectrometer for the mid-infrared range (5 to 28 µm). This Fig. IV.1.4: Calculated spectra of quasars and galaxies in the early universe at a redshift of z � 15. The intense radiation emitted in the visible and ultraviolet range in the rest-frame of the galaxies is observed by us today in the near- and mid-infrared region. With NirCaM’s sensitive wide-field cameras for the range from 2 to 5 µm we will be able to identify possible young objects. However, the spectra of »genuine« first galaxies Flux (nJy) 30 10 instrument is built by a consortium of European institutes, including the MPIA, with NaSa providing detectors and the cryogenic cooler. While NirCaM can identify candidate high-redshift early objects, their confirmation and characterization requires the use of Miri. Many of the most important diagnostic spectral lines – those that are key for building a physical understanding of these early objects – are in the rest-frame visible range. These lines are redshifted into the mid-infrared range for these objects (Fig. IV.1.4), permitting their reliable identification and study. The development of Miri is headed by two principal investigators: Gillian Wright of the Astronomical Technology Center ATC, Edinburgh (UK), and George Rieke of the University of Arizona, Tucson (USA). In addition to the three large instruments NirCaM, NirSpeC, and Miri the star-sensor camera of the JWST will also be used for scientific studies. It contains a filter wheel for the narrow-band wavelength selection (l / ∆l � 100) in the range from 1.6 to 4.9 µm. Because of its much simpler light path this »Tunable Filter Imager« and those of galaxies after a star formation episode (enrichment in metals → older stars) differ only very slightly in the near-infrared range. With Miri an exact classification will be possible via the strongly varying spectra in the range from 5 to 28 µm. In the visible range, these objects remain unobservable. (Miri consortium). NIRCAM 3 1 2 5 10 Wavelength [mm] MIRI Quasar Older galaxy »First light«
(TFT) of the Canadian Space Agency is much more sensitive than NirCaM and thus will be able to faster turn the attention to very young galaxies with their highly redshifted Lyman-alpha-lines. Common to the three focal-plane instruments for JWST presented above is that they have to be operated in a cryo-vacuum. For NirCaM and NirSpeC a temperature of – 240 °C suffices. Miri has to be cooled to below – 260 °C so that its own thermal emission will not outshine the cosmic infrared radiation. Miri’s infrared detectors have to be operated at – 268 °C, only 5 °C above absolute zero, in order to keep the »dark current« of the camera sufficiently low. Another common property of the instruments is that all of them have large »optical exchange additional pin electrical subassembly including the motor ratchet assembly support structure ring with 6 flexural rods index bearings ratchet subassembly filter wheel subassembly (with optical elements) IV.1 Instruments for the James Webb Space Telescope 91 wheels« with numerous gratings, filters, beam splitters, mirrors, prisms and coronagraphic masks mounted on their peripheries (Fig. IV.1.5). By exchanging these elements in the light path (i.e. by turning the wheels) it is possible to select the different operation modes of the instruments (spectroscopy, imaging, coronagraphy, calibration) as well as the particular wavelength ranges. Although every space technician is anxious to avoid mechanisms like these wheels (»… may fail …«), powerful scientific instruments without moving parts are not feasible. Because of the successful developments for the European space telescopes iSo and HerSCHel, our institute was well prepared for these high-risk challenges with Miri and NirSpeC. Fig. IV.1.5: Filter wheel for the Mid-Infrared Instrument (Miri). The 18 positions are occupied by filters for the wavelength range from 5 to 28 µm and a prism for sensitive low-resolution spectroscopy. Several coronagraphic masks allow searches for extrasolar planets near a very bright star, which is masked out. The wheel is moved by a central torque motor and positioned with a detent latching into a ball-bearing outer race. (CEA, TTL, ADR, ZeiSS, MPIA) bearing / axis subassembly with the KIP magnet ring support structure including a parallel shift assembly
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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
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.
Page 56 and 57: 54 III. Scientific Work the Data Ar
Page 58 and 59: 56 III. Scientific Work The Field o
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Page 72 and 73: 70 III. Scientific Work Column dens
Page 74 and 75: 72 III.3 The Galaxy-Dark Matter Con
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Page 112 and 113: 110 V. People and Events 1� 10�
Page 114 and 115: 112 V. People and Events V.2 Open H
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Page 120 and 121: 118 V. People and Events The IMPRS
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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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Max Planck Institute for Astronomy - Annual Report 2005

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