Max Planck Institute for Astronomy - Annual Report 2005

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122 V. People and Events Fig. V.6.2: Group photo of some of the participants in front of the portal of the Physics Center. copically study the atmospheres of these celestial bodies and possibly find evidence of life on Earth-like planets. This research goal is included in the instrumentation programs for the already working telescopes of the 10 m category and for the Extremely Large Telescope as well as for the Cornerstone Missions of the European Space Agency esa. These activities make it necessary to comprehensively prepare a new generation of scientists for this subject. This was precisely the intention of the event that took place at the Bad Honnef Physics Center. The Fig. V.6.3: The Heraeus physics students during one of the lectures. 64 participants mainly came from Western and Eastern Europe; some students even traveled from Argentina and Australia to attend the school. A total of 17 astrophysicists, geophysicists, experimental physicists, and mineralogists from German institutes reviewed the current state of knowledge and the expectations of future developments. Thomas Henning of the MPIA gave an introductory lecture about the still young history of extrasolar planet research and later explained the currently discussed scenario of planet formation. Hubert Klahr explained numerical methods for modeling planet formation, while Martin Küster discussed the chances of the radial velocity method for detecting invisible stellar companions. Finally, Sebastian Wolf provided an account of the results obtained up until now when observing and modeling protoplanetary disks. All talks covered theory and observations as well as the history and future. The interdisciplinary astrobiologists also had a chance to present their emerging field. The participants in this Physics School particularly benefited from the opportunity to ask questions and start discussions, not only during the lectures, but to also have the speakers »at their disposal« all week long until late at night. An e-mail we received a few days after the Physics School ended summarizes the general mood and positive impressions experienced by the participants: »Many thanks for this very fruitful workshop! I’ve really enjoyed the contents and the discussions with the speakers. B.O. Demory (Observatoire de Geneve)«. All lectures can be accessed on the internet at www. mpia.de/EXTRA2005 (Sebastian Wolf)
V.7 Two New Junior Research Groups at the Institute During 2005 a third Emmy Noether Group started its work at MPIA under the leadership of Henrick Beuther; and Frank van den Bosch started an independent Junior Research Group of the Max Planck Society. Henrik Beuther: Massive Star Formation With its Emmy Noether Program, the German Research Association (DFG) is supporting young post-doctoral scientists, offering them the opportunity to establish their own junior research groups. After two such groups led by Sebastian Wolf (Protoplanetary Disks) and Coryn Bailer-Jones (Formation and Properties of Sub-stellar Objects) had commenced their work in 2004, a third Emmy Noether Group started at the MPIA in 2005 under the lead of Henrik Beuther. Henrik Beuther studied physics at the University of Cologne and received his PhD from the Max Planck Institute for Radioastronomy in Bonn. Subsequently, he worked as a post-doc there for several years, as well Fig. V.7.1: Henrik Beuther in front of the Königstuhl scenery. as at the Harvard-Smithsonian Center for Astrophysics (Cambridge, USA). His research group at the MPIA will mainly study the early stages of the formation of massive stars. Many questions are still open here. For instance, it is not yet clear whether most massive stars form in accretion processes similar to low-mass stars, or whether other processes, such as mergers of protostars, are of major importance. Henrik Beuther and his group plan to tackle the issue of massive star formation from different directions and turn their attention to the following questions: What are the properties of massive accretion disks? What are the effects of the initial fragmentation of massive starforming regions? What chemical processes occur in the dust and gas of the star-forming regions? And, what is the role of the outflow and infall of gas? Since massive stars form in stellar clusters and are usually at great distances, high spatial resolution is essential to resolving these questions. At the same time, these regions emit intensive millimeter and submillimeter radiation. Accordingly, Henrik Beuther wants to concentrate on interferometric observations in these wavebands. From late 2007 on, this will be possible with the first telescopes of the Atacama Large Millimeter Array (alma). Henrik Beuther has already worked in this field with other interferometers, in particular with the Submillimeter-Array (SMA) on Mauna Kea, Hawaii, and the interferometer on Plateau de Bure in France. His group will continue to gain crucial experience using existing interferometers in order to later be able to better exploit the great capabilities of alma. Beuther’s group is growing rapidly: one PhD student from Argentina and one PhD student from the USA have already accepted offers and will come to the MPIA in summer 2006. They will deal mainly with two fields. The first involves a so-called legacy-proposal for the observation of massive accretion disks using the SMA. The other project focuses on an existing data set on the fragmentation of massive star-forming regions. Other projects are in preparation as well. Frank van den Bosch: Theoretical Cosmology and Galaxy Evolution In 2005, the cosmology group of the Institute was able to recruit an outstanding new colleague, Frank van den Bosch, who will head an independent research group dealing with galaxy evolution. The head of such a group is under no teaching obligations, and is guaranteed financial support for his or her research for at least five years. 123
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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
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40 II. Highlights log M� /pc2 �
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42 II. Highlights II.7 Observations
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44 II. Highlights log IR luminosity
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46 II.8 Dynamics, Dust, and Young S
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48 II. Highlights and we see a temp
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50 III. Selected Research Areas III
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52 III. Scientific Work Fig. III.1.
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54 III. Scientific Work the Data Ar
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56 III. Scientific Work The Field o
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58 III. Scientific Work lower than
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60 III. Scientific Work
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62 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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Page 146 and 147: 144 Staff Directors: Henning (Actin
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Page 152 and 153: 150 Conferences Conferences and Mee
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Page 172: The Max Planck Society The Max Plan
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