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Probing dark matter halos at redshifts z=[1,3] with lensing magnification

Probing dark matter halos at redshifts z=[1,3] with lensing magnification. L. Van Waerbeke With H. Hildebrandt (Leiden) J. Ford (UBC) M. Milkeraitis (UBC). CIfAR Lake Louise Feb 18-21 2010. Why are high redshift DM halos interesting?

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Probing dark matter halos at redshifts z=[1,3] with lensing magnification

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  1. Probing dark matter halos at redshifts z=[1,3] with lensing magnification L. Van Waerbeke With H. Hildebrandt (Leiden) J. Ford (UBC) M. Milkeraitis (UBC) CIfAR Lake Louise Feb 18-21 2010

  2. Why are high redshift DM halos interesting? -N(M,z) is a strong probe of cosmology/DE (cf Gill’s talk) -DM halo shape/profile can provide a test of CDM -make an observational connection between galaxy/cluster formation and DM environment

  3. Lensing studies are exclusively interested in shear g=(g1,g2)

  4. Limitations/difficulties with the shear: -requires very accurate Point Spread Function correction to measure the Shape of distant galaxies -this limits how small source galaxies can be, i.e. how far they can be. In practice there is little hope to precise measurement above zsource ~1 -this limits the maximum redshift one can probe the dark matter distribution, i.e. zlens ~0.5-1.

  5. What is cosmic magnification?

  6. magnification depends on shear and convergence: The number of lensed objects at magnitude m: Where a is the number count slope.

  7. 2D number density contrast at sky position q: q q+dq

  8. Magnification profile in A1689 (Taylor et al 1998) Convergence profile of A1689 (Taylor et al 1998) Two sources of noise: -Statistical (Poisson) -Clustering of bck sources

  9. Advantages of magnification: -does NOT requires Point Spread Function correction to measure the photometry. -there is NO limits how small source galaxies can be, i.e. how far they can be. -there is NO limits on the maximum redshift one can probe the dark matter distribution as long you can find enough sources behind. Can we probe redshift z=[1,3] dark matter halos with optical data?

  10. We looked at LBGs in CFHTLS deep data with the dropout technique (cf Ellis’s talk). Redshift z=3 LBG Spectral energy distribution

  11. LBG counts in CFHTLS Deep (4 sq.deg. Deep MEGACAM) is used to calibrate the slope a Hildebrandt et al. 2009

  12. Magnification correlation fct ug dropout with z=[0.5,1] foregrounds Hildebrandt et al 2009

  13. DM halo magnification: proof of concept on 15 SpARCS high-z clusters (PI: Wilson)

  14. Expected cumulative number density n(>z) of halos for a250 sq. deg. Survey, CFHTLS depth (i<24.5) (taken from MS, s8 adjusted): (for a 250 sq.deg. FOV)

  15. Stacked signal for Halos at z>1 >3 1014 Mo Full error from CFHTLSW LBGs 1-2 1014 Mo 1-5 1013 Mo

  16. Conclusions: -new window on DM studies:magnification can probe dark matter halos in a redsfhit range inaccessible by shear measurements. -complementarity: combined with shear measurement for redshift z<1 clusters it can constrain intrinsic alignment. -can be used to get the average mass from baryonic proxy (SZ, Xray, 21cm) -much easier technically than shear: we already know it can be done from ground based and balloon observatories.

  17. Caveats: -loss in SNR is ~5, but gain in sources number density is ~2. Net SNR loss is ~2-3. -dust absorption. Small effect but detectable at the percent level (Menard 2009). Multiwavelength data can actually measure both! -Eddington bias -need to find targets (need a cluster proxy, not necessarily mass). Easy for low mass and high mass DM halos. Not easy for low cluster mass/groups.

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