Complementary Probes ofDark Energy Complementary Probes of Dark Energy Eric Linder Berkeley Lab.
Dark Energy with SNAP and other Next Generation Probes
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1 1 Dark Energy Dark Energy with with SNAP SNAP and other and other Next Generation Probes Next Generation Probes Eric Linder Berkeley Lab
description
Dark Energy with SNAP and other Next Generation Probes. Eric Linder Berkeley Lab. Dark Energy to z > 1. Time variation w´ is a critical clue to fundamental physics. Deep surveys of galaxies and SN to z>1 Large scale structure formation CMB constraints from z lss =1100. - PowerPoint PPT Presentation
Transcript of Dark Energy with SNAP and other Next Generation Probes
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Dark EnergyDark Energy
withwith SNAP SNAPand otherand other Next Generation Probes Next Generation Probes
Eric Linder Berkeley Lab
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Dark Energy to Dark Energy to zz > 1 > 1
New parametrization
w(a)=w0+wa (1-a)
• Model independent, 2D phase space
• Well behaved at high z
• More accurate reconstruction
• More sensitive to data!
Linder 2002 PRL; astro-ph/0208512
Time variation w´ is a critical clue to fundamental physics.
• Deep surveys of galaxies and SN to z>1
• Large scale structure formation
• CMB constraints from zlss=1100
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Evolving Equation of StateEvolving Equation of State
Linder 2002, astro-ph/0210217following Corasaniti & Copeland 2002
w(a) = w0+wa(1-a)
Accurate to 3% in EOS back to z=1.7 (vs. 27% for w1).
Accurate to 0.2% in distance back to zlss=1100!
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SN + CMB ComplementaritySN + CMB Complementarity
SNAP tightly constrains dark energy models.
SNAP+Planck have excellent complementarity, equal to a prior (M)0.01. Frieman, Huterer, Linder, & Turner 2002
SNAP+Planck can detect time variation w´ at 99% cl (e.g. SUGRA).
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Large Scale Structure Large Scale Structure
Pilot Study with KAOS
KAOS: Kilo-Aperture Optical Spectrometer
Next generation 2dF survey
Gemini South front end (8 meter)
4000 fibers, 1.5 sq.deg. FOV
400 sq.deg. area, 106 galaxies
Linder, Colless
Next generation galaxy survey:
2dF 400dF !
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Cosmic Shear Test Cosmic Shear Test
Alcock & Paczyński 1979
Transverse and radial distances are not equal, even for a sphere, because they are measured at different a(t).
z / = H(z) dz´/H(z´)
z
SNAP still offers the best hope to detect w´.
Linder astro-ph/0212301
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KAOS+SNAP: Baryon Oscillations KAOS+SNAP: Baryon Oscillations
Standard ruler:
ratio of wiggle scale to sound horizon H(z) / (mh2)1/2
Just like CMB – simple, linear physics
Eisenstein astro-ph/0301623Linder astro-ph/0304001
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Growth of Structure Growth of Structure
Growth in linear perturbation theory with w´
• vs. cosmological constant
• vs. constant w
• vs. constant w degenerate in CMB
Linder 2002
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Large Scale Structure Large Scale Structure
running!
Growth predicted to be very sensitive to w´
Running blind: SZ, cluster/halo counts, lensing
Need full scale LSS simulations with w, w´
None exist! but in planning with C. Frenk, A. Jenkins
• vs. cosmological constant
• vs. constant w
• vs. constant w degenerate in CMB
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First Simulation ResultsFirst Simulation Results
• 107 particles
• Lbox=648 Mpc/h
• M=0.3 + SUGRA DE
• Linear Pk as Hubble LCDM
• Fits Jenkins mass function
• Agrees with Hubble FOF(b0.2) to 5%
Jenkins & Linder 2003
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Expansion History of the Expansion History of the UniverseUniverse
SNAP will map the expansion history, uncovering physics just like the thermal history revealed early universe physics.
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Present Day InflationPresent Day Inflation
SNAP will map the expansion history precisely and see the transition from acceleration to
deceleration.
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Beyond Dark EnergyBeyond Dark Energy
SNAP can not only determine dark energy parameters, but test the cosmology framework – alternative gravitation, higher dimensions, etc.
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History constrains FateHistory constrains Fate
SNAP will bound the possible fate of the universe.
Axion, supergravity, decaying dark energy models leading to collapse of universe have detectable w´.
Collapsing universe (e.g. axion DE)
Work in progress, with Kallosh, Kratochvil, Linde
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SNAP Complements SNAPSNAP Complements SNAP
SN IaWeak Lensing
SN II
ClustersBaryon Oscillations
Strong Lensing
Wide, Deep and Colorful• 9000 times the area of Hubble Deep Field• 15 sq.deg. to AB mag R=30 ; 120 epochs• 300 sq.deg. to AB mag R=28
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Next Generation ResourceNext Generation Resource
For Astronomers • SNAP main survey will be 5000x larger (and as deep) than the biggest HST deep survey, the ACS survey • Complementary to NGST: target selection for rare objects• Can survey 300 sq. deg. in a year to J=28 (AB mag)• Archive data distributed • Guest Survey Program
For Cosmologists• Mapping the expansion history of the universe through the accelerating phase back into the decelerating epoch • Precision determination of cosmological parameters
For Fundamental Physicists• Exploring the nature of dark energy • Testing higher dimension theories • Testing alternate theories of gravitation
