Max Planck Institute for Astronomy - Annual Report 2007

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76 III. Selected Research Areas Fig. III.2.6: The gravitational lens effect. The mass of a galaxy or a cluster of galaxies diverts the light of a background galaxy (top right) on its path to the observer (left) such that multiple log(M BH /M * ) 2 1 0 –1 0 SBS 0909532 FBQ 09512635 1 2 3 redshift z Fig. III.2.7: First results on the evolution of the M SL : M Gal ratio with time (Peng et al., 2006, ApJ, 649, 616) for gravitationally lensed quasars while making assumptions about their stellar populations: According thereto, the ratio does images are created. Thus the gravitational lens effects an increase of brightness and a magnification of the angular scales. As a result weaker and smaller systems become accessible. B 1422231 non-detection? non-evolving z0 SED assumptions Im Sbc E/SO 4 5 not significantly change up to z 1.7, but beyond this period, there are indications of an evolution toward more massive black holes in galaxies of given masses as compared to today.
seems consistent with the present value. Only beyond z 1.7 are there indications that black holes were more massive than today relative to their galaxies in the early universe. Accordingly, the black holes would have first grown quickly – their galaxies building their masses only later and more slowly. However, because of selection effects, the uncertainties of this method are still so high that these results could possibly be insignificant. Further, methodically independent approaches are necessary in order to obtain a coherent picture at these and other redshifts. To achieve this, the MPIA astronomers have started among other things an observing program using the VLT and Si n F o n i (the near infrared integral field spectrograph with camera), for which they make use of MPIAʼs guaranteed observing time from building the pa r S e c laser guidance system HE1104–1805 Host galaxy Einstein Ring (after point source removal) A B lensing galaxy 3 III.2 In What Type of Galaxies Do Quasars III.X Live? Titel 77 that supports Si n F o n i. The initial goal is to determine dynamic galaxy masses for four quasars, three of which are gravitationally lensed. Through Si n F o n i, extended line emission in the host galaxy is measured in order to derive the velocity field present there and thus dynamically determine the included masses. This method differs in principle from the above-described approach and is also complementary to the mass determinations based on the 33 FOV Source plane velocity field Image plane velocity field Fig. III.2.8: The lense system HE1104-1805. Top left: the optical image (HST), top right: the image of the host galaxy after subtraction of the quasar core pulled apart near an Einstein ring, right bottom: a velocity field likely observed according to the lens model, and left bottom: the velocity field calculated back into the source plane. 3 3 3
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Max Planck Institute for Astronomy
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Contents Preface ..................
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6 I. General I. General I.1 Scienti
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8 I. General Planet and Star Format
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10 I. General plementary. Ground-ba
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12 I. General High-fidelity imagers
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14 I. General Fig. I.6: Foreseen de
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16 I. General I.3 National and Inte
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18 I. General Edinburgh, University
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20 II. Highlights II.1 Youngest Ext
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22 II. Highlights radial velocity [
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24 II. Highlights II.2 A Search for
Page 28 and 29: 26 II. Highlights F 1 [5] -2 0 2 4
Page 30 and 31: 28 II. Highlights Number of Planets
Page 32 and 33: 30 II. Highlights z [AU] z [AU] 1 0
Page 34 and 35: 32 II. Highlights t =0 T orb t =1 T
Page 36 and 37: 34 II. Highlights II.4 An Exoplanet
Page 38 and 39: 36 II. Highlights F / F 12m 4 3 2
Page 40 and 41: 38 II. Highlights the planet disapp
Page 42 and 43: 40 II. Highlights The Hercules Dwar
Page 44 and 45: 42 II. Highlights on the giant bran
Page 46 and 47: 44 II. Highlights II.6 Black Hole A
Page 48 and 49: 46 II. Highlights F [10 -23 W cm -
Page 50 and 51: 48 II. Highlights Flux [10 -23 W cm
Page 52 and 53: 50 II. Highlights Fig. II.7.2: A 22
Page 54 and 55: 52 II. Highlights i [mag] i [mag] 1
Page 56 and 57: 54 II. Highlights Follow-up Observa
Page 58 and 59: 56 II. Highlights II.8 Unique Galay
Page 60 and 61: 58 II. Highlights NGC5055 (M63) NGC
Page 62 and 63: 60 II. Highlights V [km s -1 ] V c
Page 64 and 65: 62 II. Highlights be directly compa
Page 66 and 67: 64 III. Selected Research Areas III
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Page 72 and 73: 70 III. Selected Research Areas gal
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Page 76 and 77: 74 III. Selected Research Areas a b
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Page 90 and 91: 88 III. Selected Research Areas III
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Page 94 and 95: 92 IV. Instrumental Developments an
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Page 120 and 121: 118 V. People and Events Dr. Gerner
Page 122 and 123: 120 V. People and Events Fig. V.2.2
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Page 126 and 127: 124 V. People and Events Ludwig-Bie
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126 V. People and Events To interpr
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128 V. People and Events Within the
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130 V. People and Events Fig. V.5.1
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132 V. People and Events V.6 »A cl
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134 V. People and Events on through
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136 Staff Directors: Henning, Rix (
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138 Staff / Calar Alto / Department
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140 Teaching Activities / Service i
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142 Further Activities / Compatibil
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144 Cooperation with Industrial Com
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146 Conferences StageS workshop, MP
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148 Conferences Ralf Launhardt: Wor
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150 Conferences Anna Pasquali: ASU
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152 Publications Apai, D., A. Bik,
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154 Publications Chen, X. P., R. La
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156 Publications of an unusual dwar
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158 Publications Moreau, J. A. Peac
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160 Publications Pontoppidan, K. M.
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162 Publications Garching-Bonn Deep
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164 Publications Zirm, A. W., A. va
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166 Publications Linz, H., R. Klein
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168 Publications Güdel, M.: The su
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A656 Eppelheim Patrick- Henry- Sied
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Max Planck Institute for Astronomy - Annual Report 2007

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