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Weighing dark matter haloes with gravitationally lensed supernovae

Authors

  • J. Jönsson,

    Corresponding author
    1. University of Oxford Astrophysics, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH
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  • T. Dahlén,

    1. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
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  • I. Hook,

    1. University of Oxford Astrophysics, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH
    2. INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio (RM), Italy
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  • A. Goobar,

    1. Physics Department, Stockholm University, AlbaNova University Center, SE–106 91 Stockholm, Sweden
    2. The Oskar Klein Center, Stockholm University, SE–106 91 Stockholm, Sweden
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  • E. Mörtsell

    1. Physics Department, Stockholm University, AlbaNova University Center, SE–106 91 Stockholm, Sweden
    2. The Oskar Klein Center, Stockholm University, SE–106 91 Stockholm, Sweden
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E-mail: jacke@astro.ox.ac.uk

ABSTRACT

High-redshift Type Ia supernovae (SNe Ia) are likely to be gravitationally lensed by dark matter haloes of galaxies in the foreground. Since SNe Ia have very small dispersion after light-curve shape and colour corrections, their brightness can be used to measure properties of the dark matter haloes via gravitational magnification. We use observations of galaxies and SNe Ia within the Great Observatories Origins Deep Survey (GOODS) to measure the relation between galaxy luminosity and dark matter halo mass. The relation we investigate is a scaling law between velocity dispersion and galaxy luminosity in the B band: σ=σ*(L/L*)η, where L*= 1010 h−2 L. The best-fitting values to this relation are σ*= 136 km s−1 and η= 0.27. We find σ*≲ 190 km s−1 at the 95 per cent confidence level. This method provides an independent cross-check of measurements of dark matter halo properties from galaxy–galaxy lensing studies. Our results agree with the galaxy–galaxy lensing results, but have much larger uncertainties. The GOODS sample of SNe Ia is relatively small (we include 24 SNe) and the results therefore depend on individual SNe Ia. We have investigated a number of potential systematic effects. Light-curve fitting, which affects the inferred brightness of the SNe Ia, appears to be the most important one. Results obtained using different light-curve fitting procedures differ at the 68.3 per cent confidence level.

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