Searching for modified growth patterns with tomographic surveys

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Presentation transcript:

Searching for modified growth patterns with tomographic surveys Gong-Bo Zhao Simon Fraser University Aug 25,2008 COSMO08 With collaborators Levon Pogosian, Alessandra Silvestri, Joel Zylberberg

Outline Introduction of modify GR - motivation Non-GR implementation theoretically & numerically Preliminary results of error forecast from future tomographic surveys – DES & LSST Summary 08/025/08 COSMO 08

Universe is currently accelerating 74% Dark Energy 22% Dark Matter 4%Atoms f(R), scalar-tensor … 08/025/08 COSMO 08

Modified gravity At background level - degenerate with LCDM. At perturbation level - richer physics, such as scale-dependent growth Need to study the cosmological structure formation to break the degeneracy See Fabian’s talk Cross- Correlations 08/025/08 COSMO 08

Newtonian Gauge GR: Non-GR: Comoving density perturbation 08/025/08 Non-GR: 08/025/08 COSMO 08

IC: GR value at z=30 Synchronous Gauge Mapping CAMB implementation 08/025/08 COSMO 08

Consistency check: Sub-horizon: Super-horizon: Consistency relation to obey causality in the infrared and the conservation of energy-momentum Bertschinger (2006) 08/025/08 COSMO 08

Non-GR parameterization Bertschinger & Zukin (2008) (BZ08) Other parameterizations (PPF, etc.), see Ignacy’s talk 08/025/08 COSMO 08

Powerful tool: Tomography Jain & Taylor (2003) Hu & Jain (2004) 08/025/08 COSMO 08

Observables for tomography We then calculate power spectra of TT, shear-shear, galaxy-galaxy, shear-CMB, galaxy-CMB and shear-galaxy by modifying CAMB code. No Limber Approximation used!! 08/025/08 COSMO 08

Surveys : SNAP, Planck, DES & LSST 08/025/08 COSMO 08

Surveys : DES & LSST 08/025/08 COSMO 08

Gal/Gal (55) Gal/WL (60) WL/WL (21) E T G1 … … G10 WL1… … WL6 G1 . G10 WL1 WL6 CMB (3) CMB/WL (6) CMB/Gal (10) Gal/Gal (55) Gal/WL (60) WL/WL (21) For LSST, we have 155 Cls for each model!! COSMO 08 08/025/08

Cutoff! Cl 21 WL Cls 3 CMB Cls 10 CMB/Gal Cls 55 Gal Cls 60 Gal/WL Cls 6 WL/CMB Cls 08/025/08 COSMO 08

Fisher Analysis Hu & Jain (2004) For CMB, WL-WL, galaxy-galaxy: For CMB-WL, CMB-galaxy, WL-galaxy cross-correlations: Hu & Jain (2004) 08/025/08 COSMO 08

Noises 08/025/08 COSMO 08

Parameters: Preliminary results: Zhao, Pogosian, Silvestri & Zylberberg (2008), appear soon 08/025/08 COSMO 08

08/025/08 COSMO 08

DES vs. LSST 08/025/08 COSMO 08

Reconstructing G_eff and gamma Fiducial model 08/025/08 COSMO 08

Summary Tomographic surveys can provide powerful constraints on possible deviation from GR; Results depends on the choice of fiducial model and parameterization; Need to further study using non-parametric methods, such as principle component analysis (PCA) (in process). 08/025/08 COSMO 08

Appendix 08/025/08 COSMO 08

08/025/08 COSMO 08

3 vs. 4 08/025/08 COSMO 08