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On the Probability for Sub-Halo Detection through Quasar Image Splitting

Published online by Cambridge University Press:  01 June 2007

T. Riehm ,
E. Zackrisson ,
K. Wiik  and
O. Möller
T. Riehm
Affiliation:
Stockholm Observatory, AlbaNova University Center, 106 91 Stockholm, Sweden
E. Zackrisson
Affiliation:
Stockholm Observatory, AlbaNova University Center, 106 91 Stockholm, Sweden Tuorla Observatory, University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland Department of Astronomy and Space Physics, Box 515, 751 20 Uppsala, Sweden
K. Wiik
Affiliation:
Tuorla Observatory, University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland
O. Möller
Affiliation:
Max Planck Institut für Astrophysik, D-85741 Garching, Germany
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Abstract

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Dark galaxies may in principle be detectable through strong-lensing image splitting of quasars on small angular scales (milliarcseconds or below). Here, we estimate the overall probabilities for such detections under the assumption that the quasars can be treated as point sources. Due to the very low probabilities derived, we conclude that it is currently not feasable to use this strategy to put the CDM predictions for the dark galaxy population to the test.

Keywords

dark matter – cosmology: observations – galaxies: halos – quasars: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S244: Dark Galaxies and Lost Baryons , June 2007 , pp. 376 - 377
Copyright
Copyright © International Astronomical Union 2008

References

Biggs, A. D., Browne, I. W. A., Jackson, N. J., York, T., Norbury, M. A., McKean, J. P. & Phillips, P. M. 2004, MNRAS 350, 949CrossRefGoogle Scholar
Gao, L., White, S. D. M., Jenkins, A., Stoehr, F. & Springel, V. 2004, MNRAS 355, 819CrossRefGoogle Scholar
Kochanek, C. S. & Dalal, N. 2004, ApJ 610, 69CrossRefGoogle Scholar
Mao, S. & Schneider, P. 1998, MNRAS 295, 587CrossRefGoogle Scholar
Metcalf, R. B. 2004, ApJ 580, 696CrossRefGoogle Scholar
Moore, B., Quinn, T., Governato, F., Stadel, J. & Lake, G. 1999, MNRAS 310, 1147CrossRefGoogle Scholar
Navarro, J. F., Frenk, C. S. & White, S. D. M. 1996, ApJ 462, 563CrossRefGoogle Scholar
Wilkinson, P. N., et al. , 2001, Phys. Rev. Lett. 86, 584CrossRefGoogle Scholar
Yonehara, A., Umemura, M. & Susa, H. 2003, PASJ 55, 1059CrossRefGoogle Scholar
Zackrisson, E., Riehm, T., Mller, O., Wiik, K. & Nurmi, P. 2007, submitted to ApJGoogle Scholar