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Dark Energy with SNAP and other Next Generation Probes

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.

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Dark Energy with SNAP and other Next Generation Probes

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  1. Dark Energy with SNAP and other Next Generation Probes Eric Linder Berkeley Lab

  2. 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 zlss=1100 Newparametrization w(a)=w0+wa (1-a) Linder 2002 PRL; astro-ph/0208512 • Model independent, 2D phase space • Well behaved at high z • More accurate reconstruction • More sensitive to data!

  3. Evolving Equation of State Linder 2002, astro-ph/0210217 following 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!

  4. SN + 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).

  5. Large Scale Structure Next generation galaxy survey: 2dF  400dF ! Pilot Study with KAOS Linder, Colless 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

  6. Cosmic Shear Test  z Alcock & Paczyński 1979 Linder astro-ph/0212301 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´) SNAP still offers the best hope to detect w´.

  7. KAOS+SNAP: Baryon Oscillations Eisenstein astro-ph/0301623 Linder astro-ph/0304001 Standard ruler: ratio of wiggle scale to sound horizon  H(z) / (mh2)1/2 Just like CMB – simple, linear physics

  8. Growth of Structure Growth in linear perturbation theory with w´ • vs. cosmological constant • vs. constant w • vs. constant w degenerate in CMB Linder 2002

  9. Large Scale Structure 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! running! • but in planning with C. Frenk, A. Jenkins • vs. cosmological constant • vs. constant w • vs. constant w degenerate in CMB

  10. First 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

  11. Expansion History of the Universe SNAP will map the expansion history, uncovering physics just like the thermal history revealed early universe physics.

  12. Present Day Inflation SNAP will map the expansion history precisely and see the transition from acceleration todeceleration.

  13. Beyond Dark Energy SNAP can not only determine dark energy parameters, but test the cosmology framework – alternative gravitation, higher dimensions, etc.

  14. History constrains Fate Collapsing universe (e.g. axion DE) SNAP will bound the possible fate of the universe. Axion, supergravity, decaying dark energy models leading to collapse of universe have detectable w´. Work in progress, with Kallosh, Kratochvil, Linde

  15. SNAP Complements SNAP Weak Lensing SN Ia SN II Strong Lensing Clusters Baryon Oscillations • 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

  16. Next Generation Resource • For Cosmologists • Mapping the expansion history of the universe through the • accelerating phase back into the decelerating epoch • Precision determination of cosmological parameters • 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 Fundamental Physicists • Exploring the nature of dark energy • Testing higher dimension theories • Testing alternate theories of gravitation

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