testing the cdm structure formation with strong lensing...
TRANSCRIPT
Cosmology On The Beach - January 16 2012
Testing the CDM Structure Formation with Strong Lensing Galaxy Clusters
Matt BaylissHarvard/CfA
Monday, January 16, 12
Principal Collaborators
University of Chicago/KICPMike GladdersEva Wuyts
University of MichiganKeren SharonBen Koester
Goddard Space Flight CenterJane Rigby
Max-Planck Institute for AstronomyJoe Hennawi
IMPU/University of TokyoMasamune Oguri
Johns Hopkins UniversityMegan Gralla
University of OsloHakon Dahle
Universidad Catolica de ChileFelipe BarrientosMauricio Carrasco Cristina Javiera Garcia
University of TorontoHoward Yee
South African Astrophysical ObservatoryDavid Gilbank
Monday, January 16, 12
Specific Tests for Cosmological Models of Structure Formation
✤ Giant Arc Statistics
✤ Concentration-Mass relation
Monday, January 16, 12
The Concentration-Mass Relation -A Prediction for Structure Formation
King & Mead 2011
✤ The most over-dense regions of the universe collapse to form gravitationally bound structures: ``halos’’ in the simulated universe, ``groups and clusters’’ in the real universe
✤ Halos in simulations are described by a universal density profile (NFW), and a power-law relationship between concentration and mass
Monday, January 16, 12
Fair Comparisons of Measured/Observed c-M Relations
Monday, January 16, 12
SDSS
Galaxy Cluster Search Space:
0.1 < z < 0.6
10,000 deg2
griz imaging
Galaxy Cluster Search Space:
0.2 < z < 1.1
800 deg2
grz imaging
Lens Searches Using Large Imaging Surveys
RCS-2
Monday, January 16, 12
Monday, January 16, 12
Characterizing the SDSS Lens Samples: Purity & Completeness
✤ Sorted by average score, the visual sample can be well-characterized
Avg Score Number of Candidates % Followed-up Purity (% Real)
2.5-3.0 30 100 100
2.0-2.5 39 97 92
1.5-2.0 101 97 77
1.0-1.5 281 60 26
Monday, January 16, 12
Measuring the Concentration-Mass Relation: Mass Proxies✤ Strong Lensing: provides precision
measurement of the density profile in the core
✤ Need observable that samples the mass or density profile of the cluster at large radii- e.g. weak lensing, velocity dispersion, or ICM (X-ray/SZ)
Monday, January 16, 12
The Observed c-M Relation (Dynamics + SL, N=26)
Monday, January 16, 12
The Observed c-M Relation (WL + SL, N=28)
Oguri, M., Bayliss, M. et al. 2011
Monday, January 16, 12
The Observed c-M Relation (WL + SL, N=28)
Oguri, M., Bayliss, M. et al. 2011
Monday, January 16, 12
Where Does This Leave Us?
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end
Monday, January 16, 12