gong-bo zhao icg, portsmouth 1106.3327 (prl submitted) 1105.0922 (prl 11) 1011.1257(prd 11)...
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Gong-Bo ZhaoICG, Portsmouth
1106.3327 (PRL submitted)
1105.0922 (PRL 11)
1011.1257(PRD 11)
1005.3810 (PASP 11)
0905.1326 (PRL 09)
Understanding the Cosmic Acceleration using KDUST
My main collaborators
Robert Crittenden (Portsmouth), Zuhui Fan (PKU)Aireza Hojjati (SFU), Kazuya Koyama (Portsmouth)Baojiu Li (Durham, Cambridge),Yinzhe Ma (UBC,
Cambridge)Jeremiah Ostriker (Princeton, Cambridge), Levon Pogosian (SFU) Alessandra Silvestri (MIT), Lifan Wang (TAMU), Hu Zhan
(NAOC) Xinmin Zhang (IHEP)
Nov 9, 2011KDUST workshop, IHEP, Beijing
Nov 9, 2011KDUST workshop, IHEP, Beijing
Weak LensingWeak
Lensing
Galaxy CountsGalaxy Counts
ISWISW
KDUST
Nov 9, 2011KDUST workshop, IHEP, Beijing
LSST 15000 sq. deg. UgrizyGBZ, H.Zhan, L. Wang, Z. Fan, X.Zhang, 1005.3810, PASP
11
15000 sq. deg.:n(z) ~ z2exp(-z/0.5)Photo-z rms: z=0.04(1+z)Photo-z bias prior: P(z)=0.2z
Shear calibration error: ±0.003Residual shear power: 6×10-10
Nov 9, 2011KDUST workshop, IHEP, Beijing
5000 sq. deg.:n(z) ~ z2exp(-z/0.6)Photo-z rms: z=0.03(1+z)Photo-z bias prior: P(z)=0.2z
Shear calibration error: ±0.002Residual shear power: 4×10-10
15000 sq. deg.:n(z) ~ z2exp(-z/0.5)Photo-z rms: z=0.04(1+z)Photo-z bias prior: P(z)=0.2z
Shear calibration error: ±0.003Residual shear power: 6×10-10
KDUST JH + LSST ugrizy
Nov 9, 2011KDUST workshop, IHEP, Beijing
10000 sq. deg.:n(z) ~ z2exp(-z/0.6)Photo-z rms: z=0.03(1+z)Photo-z bias prior: P(z)=0.2z
Shear calibration error: ±0.002Residual shear power: 4×10-10
10000 sq. deg.:n(z) ~ z2exp(-z/0.5)Photo-z rms: z=0.04(1+z)Photo-z bias prior: P(z)=0.2z
Shear calibration error: ±0.003Residual shear power: 6×10-10
KDUST JH + LSST ugrizy
Nov 9, 2011KDUST workshop, IHEP, Beijing
5000 sq. deg.:n(z) ~ z2exp(-z/0.6)Photo-z rms: z=0.03(1+z)Photo-z bias prior: P(z)=0.2z
Shear calibration error: ±0.002Residual shear power: 4×10-10
15000 sq. deg.:n(z) ~ z2exp(-z/0.5)Photo-z rms: z=0.04(1+z)Photo-z bias prior: P(z)=0.2z
Shear calibration error: ±0.003Residual shear power: 6×10-10
KDUST JH + LSST ugrizy
SNe: (z < 1.5)
KDUST—LSST Synergy KDUST—LSST Synergy credit: Hu Zhancredit: Hu Zhan
Nov 9, 2011KDUST workshop, IHEP, Beijing
Reconstructing w(a) precisely
R.Crittenden, GBZ, L.Pogosian, L.Samushia, X.Zhang To appear soon see Levon’s talk
Straightforward to apply to KDUST data!
arXiv: 1106.3327
with
Yinzhe Ma (UBC, Cambridge)
Jeremiah Ostriker (Princeton and Cambridge)
Cosmic Mach Number: A robust tool to test Einstein Gravity
Nov 9, 2011KDUST workshop, IHEP, Beijing
The shape of velocity power spectrum can be reconstructed from CMN
Power of CMN
B0<0.4 (95% CL, CMB+SN)B0<5x10-5 (95% CL, CMB+SN+CMN)
Nov 9, 2011KDUST workshop, IHEP, Beijing
CMN is a promising tool Immune to galaxy bias, overall amplitude,
nonlinearitiesHighly sensitive to the scale-dependence of the
growth, thus an ideal tool to constrain MG parameters and neutrino mass
Complimentary to weak lensing Measure CMN from KDUST??
Nov 9, 2011KDUST workshop, IHEP, Beijing
On Non-linear scale
Environmental dependence of dark matter halos
Nov 9, 2011KDUST workshop, IHEP, Beijing
f(R) Gravity
Nov 9, 2011KDUST workshop, IHEP, Beijing
Mimic GR at high z;
Accelerate the expansion at low z;
Recover GR locally to pass solar system test.
Numerical Simulations 1011.1257 GBZ, B.Li, K.Koyama, PRD 11
Code: Modified MLAPMf(R) model:
Model parameters:
Cosmological parameters: WMAP7
Nov 9, 2011KDUST workshop, IHEP, Beijing
KDUST workshop, IHEP, Beijing
In dense environment
The halos are screened so that they cannot feel the enhancement of gravity!
Nov 9, 2011
How to define “Environment”?Number of neighbours in spheres of radius RMass or density in spheres of radius RMatter density in spherical shellsAverage mass density of surrounding halosDistance to nearest halo with minimum massProjected galaxy number density out to the
Nth nearest neighbourwith a maximum radial velocity…
KDUST workshop, IHEP, Beijing Nov 9, 2011
KDUST workshop, IHEP, Beijing
Haas et al., 1103. 0547
All these quantities strongly correlate with halo mass!
Nov 9, 2011
To see the pure environmental effect, we need a new environment indicator which is uncorrelated with halo mass
KDUST workshop, IHEP, Beijing
The three-dimensional distance to the Nth nearest neighbour with a viral mass that is at least f times that of the halo under consideration, divided by the virial radius of the Nth nearest neighbour:
Haas et al., 1103. 0547
Nov 9, 2011
KDUST workshop, IHEP, Beijing
Small DAffected by the local environment
Large DAffecting the local environment
Nov 9, 2011
KDUST workshop, IHEP, Beijing
GR analysis, Haas et al., 1103. 0547
D is a clean indicator for the local environment!
Nov 9, 2011
KDUST workshop, IHEP, Beijing
f(R) analysis, 1105.0922GBZ, Baojiu Li, Kazuya Koyama (PRL 2011)
Nov 9, 2011
KDUST workshop, IHEP, Beijing
Similar pattern!!
The screening is only determined by the halo mass for the isolated halos!
Nov 9, 2011
KDUST workshop, IHEP, Beijing
Different pattern
The screening of the clustered halos is not determined by the halo mass only!
Nov 9, 2011
Measure lensing and dynamical mass for each halo;Divide the sample using D;Compare!
KDUST workshop, IHEP, Beijing Nov 9, 2011
Measure lensing and dynamical mass for each halo;Divide the sample using D;Compare!
KDUST workshop, IHEP, Beijing
Apply to KDUST data?!
Nov 9, 2011