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Evolution of the Dark Matter Distribution with 3-D Weak Lensing

Published online by Cambridge University Press:  15 June 2005

D. J. Bacon ,
A. N. Taylor ,
M. L. Brown ,
M. E. Gray ,
C. Wolf ,
K. Meisenheimer ,
S. Dye ,
L. Wisotzki ,
A. Borch  and
M. Kleinheinrich
D. J. Bacon
Affiliation:
Institute for Astronomy, University of Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ, U. K.
A. N. Taylor
Affiliation:
Institute for Astronomy, University of Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ, U. K.
M. L. Brown
Affiliation:
Institute for Astronomy, University of Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ, U. K.
M. E. Gray
Affiliation:
School of Physics and Astronomy, University of Nottingham, University Park, Nottingham, NG7 2RD, U.K.
C. Wolf
Affiliation:
Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, U.K.
K. Meisenheimer
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117, Heidelberg, Germany
S. Dye
Affiliation:
Astrophysics Group, Blackett Laboratory, Imperial College, Prince Consort Road, London SW7 2BW, U.K.
L. Wisotzki
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany
A. Borch
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117, Heidelberg, Germany
M. Kleinheinrich
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117, Heidelberg, Germany
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Abstract

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We present a direct detection of the growth of large-scale structure, using weak gravitational lensing and photometric redshift data from the COMBO-17 survey. Deep $R$-band imaging of two $0.5\times0.5$ square degree fields is used to provide shear estimates for over 52000 galaxies; these are combined with photometric redshift estimates from our 17 band survey, in order to obtain a 3-D shear field. We discuss how theoretical models for evolving matter power spectra and correlation functions cab be used to find a best fit to this 3-D shear field. We present the detection of the evolution of the power, and measurements of the rate of evolution for $0<z<1$. We discuss future refinements which will improve the accuracy with which the effect can be measured.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS225 , July 2004 , pp. 37 - 42
Copyright
© 2004 International Astronomical Union