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Deciphering Quasar Millilensing – How to Distinguish Between Dark and Luminous Lenses

Published online by Cambridge University Press:  01 June 2007

Heidi Lietzen ,
Chris Flynn ,
Erik Zackrisson  and
Pasi Nurmi
Heidi Lietzen
Affiliation:
Tuorla Observtory, University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland email: [email protected]
Chris Flynn
Affiliation:
Tuorla Observtory, University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland email: [email protected]
Erik Zackrisson
Affiliation:
Tuorla Observtory, University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland email: [email protected]
Pasi Nurmi
Affiliation:
Tuorla Observtory, University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland email: [email protected]
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Abstract

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Dwarf-galaxy sized dark matter halos may be detectable when a bright background source is gravitationally lensed on scales of milliarcseconds. Such effects can be caused by dark galaxies as well as luminous ones. Here we discuss conditions for detecting a luminous lensing object through direct imaging, via measurements of the point spread function (PSF) to subtract the quasar from the image, revealing the quasar host galaxy and any luminous lens. The technique applies to both types of millilensing effect, i.e. magnification and image splitting. We show that luminous dwarf-galaxy lenses should be detectable with this method up to redshifts z~0.2.

Keywords

gravitational lensinggalaxies: dwarfquasars: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S244: Dark Galaxies and Lost Baryons , June 2007 , pp. 368 - 369
Copyright
Copyright © International Astronomical Union 2008

References

Cellone, S. A. & Buzzoni, A. 2001, A&A, 369, 742Google Scholar
Dunlop, J. S., McLure, R. J., Kukula, M. J., et al. 2003, MNRAS, 340, 1095CrossRefGoogle Scholar
Falomo, R., Kotilainen, J., Scarpa, R. et al. 2006, New Astron. Revs, 50, 732CrossRefGoogle Scholar