Max Planck Institute for Astronomy - Annual Report 2005

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86 III. Scientific Work tribution of dark matter in galaxies. Numerical CDM simulations find concentrated »cuspy« halos, whereas observations seem to suggest halos with a constant-density core. The latter result, posing a potentially severe problem for CDM cosmology, is still subject to observational uncertainties such as the possible dominance of non-circular motions. These effects can be studied directly using the data products of Things, e.g., using two-dimensional, high-resolution velocity fields to derive accurate rotation curves and to constrain the dark matter distribution. High spatial resolution (100 – 300 pc) data near the center is especially important, as the discrepancies show themselves most clearly in the central regions. As an example, we show the rotation curve for the dwarf irregular galaxy IC 2574 (member of the M 81 group of galaxies) in Fig. III.4.7. The left panel shows the velocity field of IC 2574 (see Fig. III.4.2 for an integrated HI map of this galaxy). This velocity field (and other similar ones at different resolutions) is used to derive the circular velocities of this galaxy – such a rotation curve is shown in the right hand panel (the different colors indicate the derived rotation speed for different resolutions). In the case of IC 2574, the rotation curve rises almost linearly, indicating that the galaxy is rotating almost like a solid body out to large galactocentric distances. This is in sharp contrast to the rotation curves of more massive spiral galaxies, where the rotation curves typically rise sharply and then stay flat for most of Fig. III.4.7: Dynamical analysis of one of the Things galaxies: the dwarf galaxy IC 2574. Left: the velocity field of IC 2574 (cf. Figs. III.4.2 and III.4.4). Right: the rotation curve for IC 2574 derived from the velocity fields similar to the one shown to the left (the different colors refer to different resolutions to extract the rotation curve). For each radius, the circular rotation velocity of IC 2574 is plotted, the linear rise in rotation indicates that this dwarf galaxy is rotating like a solid body. a galaxy’s disk. Rotation curves for all Things galaxies will be used to derive the detailed dynamics and dark matter content of each galaxy. Summary The HI Nearby Galaxy Survey (Things) based at the MPIA is the largest program ever undertaken at the VLA to perform 21 cm HI observations of the highest quality (7�, 5 km/s resolution) of nearby galaxies. Things includes archival observations and totals about 500 hours of VLA time. Dedicated observations for Things started in September 2003 and were completed in summer of 2005. A sample of 34 objects at distances between 3 and 10 Mpc were targeted in Things, covering a wide range of star formation rates, total masses, absolute luminosities, evolutionary stages, and metallicities. Data from Things complements sings, the spiTzer Infrared Nearby Galaxies Survey; hence high-quality observations from the X-ray through the radio range are available at comparable resolution for each galaxy. At the MPIA, data from Things is being used to investigate issues such as the small-scale and three-dimensional structure of the ISM, the (dark) matter distribution, and the processes leading to star formation. Furthermore, Things enables studies of the variation of each of these properties as a function of galaxy environment. A major leap forward in the studies of the atomic interstellar medium of galaxies will only be possible with the advent of the next generation of radio telescopes, such as the Square Kilometer Array (SKA). velocity [km/s] 80 60 40 20 0 0� 200� (People involved at the MPIA with the Things / sings projects are: Fabian Walter, John Cannon, Frank Bigiel, Hélène Roussel and Domenico Tamburro) radius 400� 600�
IV. Instrumental Development IV.1 Instruments for the James Webb Space Telescope The launch of JWST, the successor of the HST, is foreseen for the year 2013. The 6.5 m telescope will be operated about 1.5 million kilometers away from the Earth and perform observations in the infrared. The MPIA is engaged in developing the moving parts for the instruments Nircam, Nirspec, and miri. Hubble needs a successor Space telescopes get older too: over the course of time solar cells provide less power, the gyroscopes – controlling the orientation of the spacecraft – successively fail, electronic components can be damaged by high-energy cosmic rays, and mechanisms start to fail. Furthermore, COBE/WMAP Earliest picture of the Cosmos at microwavelengths JWST ? »Dark age« HUBBLE Earliest picture of the Cosmos at visible wavelengths Age of the universe [years] 0 ~ 300000 ~ 500 Million ~ 1 Billion ~ 9 Billion ~ 13 Billion space telescopes also become outdated. Space telescopes are designed years before launch. Because of the rapid progress in electronic cameras, in computers and memory, in control engineering and in materials, a space telescope that has been in operation for some years can contain technologies a decade or more out of date. Fig. IV.1.1: Evolution of the universe from the big bang (top) until the present day (bottom). All-sky surveys of microwave radiation allow exploration of the distribution of cosmic matter from when the universe was only � 300 000 years old (Cobe/ WMap). The last � 12 billion years are accessible to large ground-based telescopes and the Hubble Space Telescope. In between lie the »dark ages« of the universe in which the first stars formed. JWST is expected to fill this gap. Big Bang The Universe is ionized The Universe becomes neutral Formation of Galaxies and Quasars begins – and therefore the reionization Reionization is complete Formation of the Solar System Today: Astronomers investigate the formation of the Universe 87
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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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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
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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
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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�
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Page 120 and 121: 118 V. People and Events The IMPRS
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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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