Max Planck Institute for Astronomy - Annual Report 2005

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84 III. Scientific Work Fig. III.4.4: The spiral galaxy NGC 2403 as an example. Left: integrated HI column density map (similar to the map shown in Fig. III.4.2). Middle: velocity field of NGC 2403 – the different colors indicate different velocities: Red colors indicate emission moving away from the Earth, blue colors represent approaching material (relative to the center of mass). This information can be used to derive rotation curves and to study the fine-scale kinematics in galaxies. Right: the velocity dispersion map of NGC 2403. Red colors indicate high dispersion in the atomic ISM; blue colors indicate more quiescent regions. Such maps are used to study the energy input of star formation into to the ISM. Fig. III.4.5: The spiral galaxy M 81 in different wavebands: The distribution of atomic hydrogen from the Things project is shown in blue in all panels. The other wavebands were observed with spiTzer and the colors are explained in each panel. The 3.6 micron emission is dominated by the contribution of old stars in the bulge, the 8 micron map contains emission from stars, hot dust and so-called PAH emission features. Such comparisons provide important clues about the processes leading to star formation in galaxies of the Things sample. atomic hydrogen: blue 3.6 �m: green 24 �m: red atomic hydrogen: blue 3.6 �m: red 8 �m: green velocity at which the gas is moving. This is illustrated in Fig. III.4.3, where we show so-called channel maps for one of Things targets (M 101). In each panel, only HI emission measured at a given velocity (as labeled in the upper right in each panel) is shown. This clearly demonstrates that the different parts of the galaxy have different velocities – the »movement« from the upper left to the lower right (with increasing channel number) is due to the rotation of the galaxy (the receding side is seen in the first channels, the approaching side is in the last channels, and the systemic velocity of the galaxy is at around 240 km/s). In addition to this global rotation, the channel maps also reveal a rich degree of fine structure in the ISM. For each of the Things galaxies, these channel maps are then used to create 1) the integrated HI maps (by simply adding the channels seen in the channel maps), 2) a map of the average velocity for each pixel (so-called velocity fields) and 3) a velocity dispersion map. As an example, we present these three maps for the galaxy NGC 2403 in Fig. III.4.4. The left hand panel shows the atomic hydrogen: blue 8 �m: green 24 �m: red
Fig. III.4.6: Three-color composite of the nearby spiral galaxy M 101. The distribution of atomic hydrogen from Things is shown in green. Blue indicates emission seen by galex, a UV satellite, which traces current and recent star formation. Red integrated HI map which reveals the presence of many holes and shells in the ISM. The middle panel shows the velocity field: red colors indicate emission receding from Earth, blue colors indicate approaching gas (the global rotation of this galaxy is evident from this plot). The velocity dispersion (right panel) seems to be higher in the regions where spiral arms and star formation are present, which may be explained by the mechanical feedback of the stars in the spiral arms. Typical resolutions for Things observations are a spatial resolution of 7� and a velocity resolution of 2.5 – 5 km/s. Scientific Rationale of Things Interplay between the ISM and Star Formation. Things allows astronomers to study the interplay between star formation (as traced by Hα, Far UV, IR, and X-ray emission) and the ambient ISM at 100 – 300 pc resolution over a range of different hubble types. The location and energy input of regions of recent star formation and the impact they have on the structure and dynamics of the HI can be investigated on these small scales. With Things, a census of supergiant shells as a function of hubble type will be possible (see Fig. III.4.2). Things data products permit studies of how these structures form and how III.4 The Interstellar Medium in Nearby Galaxies 85 indicates emission seen at 24 microns with the spiTzer space telescope, which is dominated by warm dust emission powered by young starforming regions (image credits: Karl Gordon, Steward Observatory. they, in turn, might trigger secondary star formation. In combination with the multi-wavelength data from sings, a complete energy budget of the ISM can be derived. As an example, we show a multi-wavelength comparison of the spiral galaxy M 81 in Fig. III.4.5. In this figure, the distribution of atomic hydrogen is shown in blue in all panels. The other wavebands have been observed with spiTzer and the colors are explained in each panel. The 3.6 micron emission is dominated by the contribution of old stars in the bulge; the 8 micron map contains emission from stars, hot dust and so-called PAH emission features. Such comparisons provide important clues about the processes leading to star formation for the Things /sings galaxies. Another example is shown in Fig. III.4.6, where we show a three-color composite of the nearby spiral galaxy M 101. The distribution of atomic hydrogen from Things is shown in green. Blue indicates emission seen by galex, a UV satellite, which traces current and recent star formation. Red indicates emission seen at 24 microns observed with the spiTzer space telescope, which is dominated by warm dust emission powered by young star-forming regions. Global Mass Distribution. Another topical subject that can be addressed by Things is the apparent failure of cold dark matter (CDM) models to explain the dis-
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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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Page 40 and 41: 38 II. Highlights II.6 Massive Star
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Page 44 and 45: 42 II. Highlights II.7 Observations
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Page 52 and 53: 50 III. Selected Research Areas III
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Page 112 and 113: 110 V. People and Events 1� 10�
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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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Max Planck Institute for Astronomy - Annual Report 2005

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