Weak Gravitational Lensingnewviews.uchicago.edu/talks/december_10/plenary/... · 2015. 7. 1. ·...
Transcript of Weak Gravitational Lensingnewviews.uchicago.edu/talks/december_10/plenary/... · 2015. 7. 1. ·...
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Weak Gravitational LensingGary Bernstein, University of Pennsylvania
KICP Inaugural SymposiumDecember 10, 2005
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astrophysics is on the 4th floor... President Amy Gutmann215 898 7221
Physics Chair Tom Lubensky215 898 8152
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Why am I in this session?
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Shear “aperture mass”(=power spectrum)
Shear correlationfunction
Data !om Jarvis et al (2005),75-square-degree CTIO Lensing survey
(using ~2 million galaxies)
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Measurements of dark energy!
Results for flat, constant-w models from Jarvis et al (2005) from the 75-square-degree CTIO lensing survey
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Hoekstra et al 2005: 22 square degrees,
8x more data to come!
Initial Data !om the CFH Legacy Survey
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Testing the galaxy formation paradig%Mandelbaum et al 2005:
Split SDSS galaxies into stellar-mass bins, early/lateHalo models overplotted
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Calibrating galaxy clusters with WL
1011
1012
1013
i-band LumT [LO •]
1011
1012
1013
1014
M(<
r) [
h-1
MO •]
M = A (L/1010
LO •)!
A = 4.04±0.38 1014
MO •
! = 1.40±0.03
10-2 0.1 1 10R [h!1 Mpc]
0.1
1
10
102
103
"#
[h M
O • p
c!2]
0 <= Ngals <= 33 <= Ngals <= 44 <= Ngals <= 55 <= Ngals <= 77 <= Ngals <= 9
9 <= Ngals <= 1515 <= Ngals <= 2020 <= Ngals <= 3030 <= Ngals <= 4040 <= Ngals <= 5050 <= Ngals <= 75
75 <= Ngals <= 261
See Erin Sheldon’s talk...
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Cosmological Signals in Gravitational Lensing
δθ
α=4GM/bc2
DS
DLS
b
δθ =4GMbc2
D LS
D SWe observe this deflection angle (more precisely, gradients of the deflection angle).
Cosmology changes growth rate of mass structures in the Universe.
Cosmology changes the geometric distance factors.
Sensitive to both structure and geometry of Universe!
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Strong lenses: obvious deflection angles
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Weak lensing: deflection gradients
True Background Lensed Image
True Background Lensed Image
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Weak lensing in Fourier spac'
Foreground mass sinusoid produces
ellipticity pattern at the same k-vector
Lensing cannot produce ellipticity pattern
at 45 degrees to k-vector
kk
"E mode" "B mode"
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This is your brainon weak lensing
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Weak lensing inversion to dark matter maps
M. Joffre et al 2000
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Linear theory
Shear power spectrum has less information than CMB spectrum, but measures a more recent quantity.
WL has depth information - “tomography”
WL sees non-linear growth and collapse of mass structures.
WL is non-Gaussian field, so bispectrum, etc., carry new information.
WL can measure and use the relation between visible matter and dark matter - test galaxy evolution paradigm!
WL can distinguish the expansion history from and growth of structure within it. This allows us to test whether GR is correct!
Weak lensing for CMB veterans
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WL as a pure distance measuremen(
z1z2
Ratio of Deflection Angles:
δθ1
δθ2=
(DLSDS
)1(
DLSDS
)2
No knowledge of foreground mass is required!
(Jain & Taylor)
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Weak lensing is a true geometric test for curvatur'
dL
dS
dLSL
S
χ0
χL
χLS
Chord lengths are the observable angular-diameter distances
Cannot constrain manifold curvature using only chords from observer
Measure of d(LS) by lensing ties down curvature.
(GMB 2005)
dLS = (dS − dL) (1− ΩkdLdS/2) + O(Ω2k)
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Things WL analyses & forecasts should includ'
Statistics:Power spectrum tomographyGalaxy-shear cross correlationsBispectrum tomographyCluster counts/ PDF
Systematic uncertainties:Shear calibration errorsAdditive shear errors (negligible?)Photo-z biasesPhoto-z scatter, catastrophic errorsIntrinsic shape correlationsUncertainties in theoretical power spectrum
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Things I’ve included:
Statistics:Power spectrum tomographyGalaxy-shear cross correlationsBispectrum tomography
Cluster counts/ PDFSystematic uncertainties:
Shear calibration errorsAdditive shear errors (negligible?)Photo-z biasesPhoto-z scatter, catastrophic errorsIntrinsic shape correlationsUncertainties in theoretical power spectrum
Ideally: posed without dependence on specific DE/MG model
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WL data is rich
DGP
Knox, Song, & Tyson (2005)
Power spectrum only,no systematic errors
-1.6 -1.4 -1.2 -1 -0.8 -0.6 -0.4-1
-0.5
0
0.5
1
w0
wa
1% biases in 1+z per
redshift bin
All systematics except
photo-z errors
No systematics
95% CL DE constraints
LST-scale WL survey
Curvature allowed
Planck prior taken
No bispectrum
Plus: “gauranteed” neutrino-mass detection(Abazajian; Song & Knox)
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The WL sky is very richReionization-era 21 cm and CMB can be source planes as well.
Distinguish dark energy from modified GR:
Wealth of observable statistics permits most posited systematic errors to be “self-calibrated” via internal solution.
Is the dominant systematic going to be photo-z’s?
∇2φ = 4πGρ?δ + 2H δ = 4πGρδ?
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Dark-energy parameter forecasts
-1.6 -1.4 -1.2 -1 -0.8 -0.6 -0.4-1
-0.5
0
0.5
1
w0
wa
20,000 sq degground WLpessimistic systematics
optimistic sys. OR4000 sq deg space WL
SKA WL
Solid line:SNAP SNe + WFMOS BAONO systematics!
Details: 95% CL, does not assume flat, take Planck prior in each case, LCDM fiducial
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Supernova Acceleration Probe(SNAP)
600 Megapixel Cameraon HST-sized Space Telescope
Size of HST image
SNAP camerafocal plane
SNAP could harvest galaxyshapes hundreds of times
faster than the HST or JWST
An ideal instrument for weak lensing:
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The LSST Projec(
Ground-based 8-meter telescope to survey the entire visible sky every 4 days.
Measure several billion galaxy shapes over a full hemisphere
A single camera with >2 billion pixels.
4 GB image every 15 s
1 TB/hr, 8 TB/night, 2-3 PB/yr!
Yours for only $300M!
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Large Synoptic Survey Telescope (LSST)3 Degree FOV, ~2 GigapixelGround-Based 6.5-meter telescope
Supernova Acceleration Probe (SNAP)0.7 Square Degree Vis/NIR, ~0.5 GigapixelOrbiting Observatory
Large Astronomical Object (LAO)
Digital cameras that Best Buy doesn’t carry:
Makes a great holiday gift
for that special cosmologist!
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Shear Testing Program (STEP)
• Collaborative testing of shear-measurement methodologies led by Catherine Heymans
• All groups produce blind estimates of the shear on artificial sky images
• Several methods look good to 1%, the limits of this round of tests (but most are worse).
• Much more stringent tests underway by R. Nakajima, also STEP round 2 to come.
10%
1%
30%
3%
Ca
lib
ratio
n E
rror
PSF 0 PSF 1
See Heymans talk, Nakajima poster
Wi* we rea*y be able to measure weak lensing shearto parts per thousand of the already-weak signal?
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WL present and futur'Weak gravitational lensing is already constraining dark energy and galaxy formation models. Statistics-limited now at ~5% measures.
WL offers a rich set of observables that complement other cosmological data
WL data of future will be capable of self-calibrating most systematic errors, and offer strongest dark energy constraints of any single test.
WL can directly measure curvature and test GR on scales 100 kpc - 1 Gpc
Work to be done:
Non-Gaussian theory
Theory of galaxy-mass joint evolution
Signatures of GR modifications
Build wide field instruments (no hardware unknowns)
Build software and algorithms to measure shear to very high accuracy
Huge advances in photometric redshifts.Please attend the lensing and galaxy formation sessions
to hear the real news !om lensing.
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Geometric ShapesGalaxy intrinsic shape: Lensing
Shear:We see this
Image looks like this We shear it Until it looks round again
Applied shear to circularize is opposite of the lensing shear, independent of galaxy details