Testing the Dark Energy Paradigm Piran@60
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Testing the Dark Energy Paradigm
Piran@60
Ofer Lahav University College London
- Collaborating with Tsvi - Brief History of Dark Energy - The Dark Energy Survey and Euclid- The Next Paradigm Shift?
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Less-extreme papers with Tsvi
Treyer et al. (1998) XRB LSS
Scharf et al. (2000) the XRB dipole
(1990)
(1997)
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The Chequered History of theCosmological Constant
* The old CC problem:Theory exceeds observational limits on by 10120 !
* The new CC problem:Why are the amounts of Dark Matter and Dark Energy so similar?
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Dark Energy Pre-SNIa
• Peebles (1984) advocated Lambda
• APM result for low matter density (Efstathiou et al 1990)
• Baryonic fraction in clusters (White et al. 1993)
• The case for adding Lambda (Ostriker & Steinhardt 1995)
• Others…
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The Dark Energy problem: 10, 90 or 320 years old?The weak field limit of GR:F = -GM/r2 + /3 r
X *
Lucy Calder & OLA&G Feb 08 issuehttp://www.star.ucl.ac.uk/~lahav/CLrev.pdf (revised)
“I have now explained the TWO principle cases of attraction…which is very remarkable” Isaac Newton, Principia (1687)
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“Evidence” for Dark Energy
Observational data• Type Ia Supernovae • Galaxy Clusters• Cosmic Microwave Background• Large Scale Structure• Gravitational Lensing• Integrated Sachs-Wolfe
Physical effects: • Geometry • Growth of StructureBoth depend on the Hubble expansion rate:
H2(z) = H20 [M (1+z) 3 + DE (1+z) 3 (1+w) ] (flat)
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Standard rulers
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Baryonic Acoustic Oscillations
SDSS Luminous Red GalaxiesDensity fluctuations
CMB WMAPTemperature fluctuations
Comving distance Harmonic l
z=0.5 z=1000
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The Integrated Sachs-Wolfe Effect
gravitational potential traced by galaxy density
potential depth changes as cmb photons pass through
In EdS the potential is constant with time, hence no ISW effect.
An effect is expected in a universe with DE, and it can be detected
by cross-correlating the CMB with galaxy maps (Crittenden et al).
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Cross-correlation of WMAP and 2MASS
Rassat, Land, OL, Abdalla (2006); Francis & Peacock (2009)
CCF consistent with no correlation, as well as with < 0.89 (95% CL)
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Probing the Geometryof the Universe with
Supernovae Ia
‘Union’ SN Ia sample (Kowalski et al. 2008)
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In 3 Dimensions
Massey et al. 2007
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Spectroscopic Surveys
CfA
SDSS
2dFGRS
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Deviations from standard GR?
Bean (2009) using Cosmos2007Soon with Cosmos2009
Lensing sensitive to the sum of potentials
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The Future of the Local Universem =0.3
LCDMa = 1 (t= 13.5 Gyr)
OCDMa = 1 (t= 11.3 Gyr)
LCDMa = 6 (t= 42.4 Gyr)
OCDMa = 6 (t= 89.2 Gyr)
Hoffman, OL, Yepes & Dover 0705.4477
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Galaxy Surveys2010-2020
Photometric surveys: DES, Pan-STARRS, HSC, Skymapper, PAU, LSST, Euclid (EIC), JDEM(SNAP-like), …
Spetroscopic surveys: WiggleZ, BOSS, BigBOSS, hetdex, WFMOS/Sumire, Euclid (NIS), JDEM (Adept-like), SKA, …
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Photometric redshifts
• Probe strong spectral features (e.g. 4000 break)
• Template vs. Training methods
z=3.7z=0.1
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MegaZ-LRG
• Input: 10,000 galaxies with spectra
• Train a neural network
•ANNz, Collister & Lahav 2004
• Output: 1,000,000 photo-z•Collister, Lahav et al. 2007
•Update using 6 photo-z methods *Abdalla et al. 2009
3 (Gpc/h)3: the largest ever galaxy redshift survey!
Photoz scatter of 0.04
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1.5M LRGs (“MegaZ”) photo-z code comparison
SDSS
HpZ+BC
Le PHARE
Zebra
ANNz
HpZ+WWC
Abdalla, Banerji, OL & Rashkov0812.3831
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Neutrino mass from MegaZ-LRG
Thomas, Abdalla & OL (2009) 0911.5291
Total mass < 0.3 eV (95% CL)
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Dark Energy Science ProgramFour Probes of Dark Energy• Galaxy Clusters
• clusters to z>1• SZ measurements from SPT• Sensitive to growth of structure and geometry
• Weak Lensing• Shape measurements of 300 million galaxies • Sensitive to growth of structure and geometry
• Large-scale Structure• 300 million galaxies to z = 1 and beyond• Sensitive to geometry
• Supernovae• 15 sq deg time-domain survey• ~3000 well-sampled SNe Ia to z ~1• Sensitive to geometry
Plus QSOs, Strong Lensing, Milky Way, Galaxy Evolution
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DES Forecasts: Power of Multiple Techniques
FoM factor 4.6 tigther compared to near term projects
w(z) =w0+wa(1–a) 68% CL
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The DES Collaborationan international collaboration of ~100 scientists from ~20 institutions
US: Fermilab, UIUC/NCSA, University of Chicago,LBNL, NOAO, University of Michigan, University of Pennsylvania, Argonne National Laboratory, Ohio State University, Santa-Cruz/SLAC Consortium
Observatorio Nacional, CBPF,Universidade Federal do Rio de Janeiro, Universidade Federal do Rio Grande do Sul
Brazil Consortium:
UK Consortium:UCL, Cambridge, Edinburgh, Portsmouth, Sussex, Nottingham
Spain Consortium:CIEMAT, IEEC, IFAE
CTIO
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DES Organization
SupernovaeB. NicholJ. Marriner
ClustersJ. MohrT. McKay
Weak LensingB. JainS. Bridle
Galaxy ClusteringE. GaztanagaW. Percival
Photometric RedshiftsF. CastanderH. Lin
SimulationsA. KravtsovA. Evrard
TheoryW. HuJ. Weller
Strong LensingE. Buckley-GeerM. Makler
Galaxy EvolutionR. WechslerD. Thomas
QSOsR. McMahonP. Martini
Milky WayB. SantiagoB. Yanny
11 Science Working Groups
Over 100 scientistsfrom the US, UK, Spain and Brazil
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The Dark Energy Survey (DES)• Proposal:
– Perform a 5000 sq. deg. survey of the southern galactic cap
– Measure dark energy with 4 complementary techniques
• New Instrument:– Replace the PF cage with a
new 2.2 FOV, 520 Mega pixel optical CCD camera + corrector
• Time scale:– Instrument Construction
2008-2011• Survey:
– 525 nights during Oct.–Feb. 2011-2016
– Area overlap with SPT SZ survey and VISTA VHS
Use the Blanco4m Telescope at the Cerro TololoInter-American Observatory (CTIO)
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The 5 lenses are now being polished
C2
Polishing & coating coordinated by UCL (with 1.7M STFC funding)
C1
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DES Collab. Mtg., OSU, Nov. 8, 2008 Huan Lin
29
A single simulated DECam pointing (= tile = hex)
DECam Focal Plane
62 2kx4k Science CCDs(520 Mpix)
1 GB per single 3 deg2 pointing
Image Level Simulations
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Neutrino mass from DES:LSS & Planck
Lahav, Kiakotou, Abdalla & Blake(0910.4714)
Input: M =0.24 eV
Output: M =0.24 +- 0.12 eV (95% CL)
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Total Neutrino Mass DES vs. KATRIN
M< 0.1 eV M < 0.6 eV
t
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Galactic Plane
Deep~40 deg2
Wide Extragalactic20,000 deg2
Euclid Imaging SurveysWide Survey: Extragalactic sky (20,000 deg2 = 2 sr)
• Visible: Galaxy shape measurements to RIZAB ≤ 24.5 (AB, 10σ) at 0.16” FWHM, yielding 30-40 resolved galaxies/amin2, with a median redshift z~ 0.9
• NIR photometry: Y, J, H ≤ 24 (AB, 5σ PS), yielding photo-z’s errors of 0.03-0.05(1+z) with ground based complement (PanStarrs-2, DES. etc)
• Concurrent with spectroscopic survey
Deep Survey: 40 deg2 at ecliptic poles
•Monitoring of PSF drift (40 repeats at different orientations over life of mission)
•Produces +2 magnitude in depth for both visible and NIR imaging data.
Possible additional Galactic surveys:
•Short exposure Galactic plane•High cadence microlensing extra-solar planet surveys could be easily added within Euclid mission architecture.
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Euclid - impact on Cosmology
Euclid Imaging will challenge all sectors of the cosmological model:
• Dark Energy: wp and wa with an error of 2% and 13% respectively (no prior)
• Dark Matter: test of CDM paradigm, precision of 0.04eV on sum of neutrino masses (with Planck)
• Initial Conditions: constrain shape of primordial power spectrum, primordial non-gaussianity
• Gravity: test GR by reaching a precision of 2% on the growth exponent (dlnm/dlnam
)
Uncover new physics and Map LSS at 0<z<2: Low redshift counterpart to CMB surveys
Δwp ΔWa ΔΩm ΔΩΛ ΔΩb Δσ8 Δns Δh DE FoM
Current+WMAP 0.13 - 0.01 0.015 0.0015 0.026 0.013 0.013 ~10
Planck - - 0.008 - 0.0007 0.05 0.005 0.007 -
Weak Lensing 0.03 0.17 0.006 0.04 0.012 0.013 0.02 0.1 180
Imaging Probes 0.018 0.15 0.004 0.02 0.007 0.0009 0.014 0.07 400
Euclid 0.016 0.13 0.003 0.012 0.005 0.003 0.006 0.020 500
Euclid +Planck 0.01 0.066 0.0008 0.003 0.0004 0.0015 0.003 0.002 1500
Factor Gain 13 >15 13 5 4 17 4 7 150
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What will be the next paradigm shift?
• Vacuum energy (cosmological constant)?• Dynamical scalar field?
– w=p/– for cosmological constant: w = -1
• Manifestation of modified gravity?• Inhomogeneous Universe?
• What if cosmological constant after all?• Multiverse - Landscape?• The Anthropic Principle?
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THE END