probing dark matter halos at redshifts z=[1,3] with lensing magnification
DESCRIPTION
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? - PowerPoint PPT PresentationTRANSCRIPT
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Probing dark matter halos atredshifts z=[1,3] with lensing magnification
L. Van Waerbeke
With H. Hildebrandt (Leiden) J. Ford (UBC) M. Milkeraitis (UBC)
CIfAR Lake LouiseFeb 18-21 2010
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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 formationand DM environment
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Lensing studies are exclusively interested in shear )
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Limitations/difficulties with the shear:
-requires very accurate Point Spread Function correction to measure theShape 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.
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What is cosmic magnification?
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magnification depends on shear and convergence:
The number of lensed objects at magnitude m:
Where is the number count slope.
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2D number density contrast at sky position :
d
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Convergence profile of A1689 (Taylor et al 1998)Magnification profile in A1689 (Taylor et al 1998)
Two sources of noise:-Statistical (Poisson)-Clustering of bck sources
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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?
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We looked at LBGs in CFHTLS deep data with the dropout technique(cf Ellis’s talk).
Redshift z=3 LBGSpectral energy distribution
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LBG counts in CFHTLS Deep (4 sq.deg. Deep MEGACAM) is used tocalibrate the slope
Hildebrandt et al. 2009
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ug dropout with z=[0.5,1] foregrounds
Hildebrandt et al 2009
Magnification correlation fct
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DM halo magnification: proof of concept on 15 SpARCS high-z clusters (PI: Wilson)
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Expected cumulative number density n(>z) of halos for a250 sq.deg. Survey, CFHTLS depth (i<24.5) (taken from MS, 8 adjusted):
(for
a 2
50 s
q.de
g. F
OV
)
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1-5 1013 Mo
>3 1014 Mo
1-2 1014 Mo
Stacked signal forHalos at z>1
Full error fromCFHTLSW LBGs
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Conclusions:
-new window on DM studies: magnification can probe darkmatter halos in a redsfhit range inaccessible byshear measurements.
-complementarity: combined with shear measurement forredshift z<1 clusters it can constrain intrinsic alignment.
-can be used to get the average mass from baryonicproxy (SZ, Xray, 21cm)
-much easier technically than shear: we already know itcan be done from ground based and balloon observatories.
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Caveats:
-loss in SNR is ~5, but gain in sources number densityis ~2. Net SNR loss is ~2-3.
-dust absorption. Small effect but detectable at thepercent level (Menard 2009). Multiwavelength data canactually measure both!
-Eddington bias
-need to find targets (need a cluster proxy, not necessarilymass).Easy for low mass and high mass DM halos. Not easy forlow cluster mass/groups.