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Theoretical Astrophysics @ FNAL: Dark Energy

Theoretical Astrophysics @ FNAL: Dark Energy. Breakout session, DOE Review May 17, 2006. Pre-SN work on Natural Dark Energy Models. Very small mass scale of quintessence field (10 -33 eV) related to ratio of explicit breaking scale and spontaneous breaking scale:.

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Theoretical Astrophysics @ FNAL: Dark Energy

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  1. Theoretical Astrophysics @ FNAL: Dark Energy Breakout session, DOE Review May 17, 2006

  2. Pre-SN work on Natural Dark Energy Models Very small mass scale of quintessence field (10-33 eV) related to ratio of explicit breaking scale and spontaneous breaking scale: M is neutrino mass and f close to Planck mass Frieman, Hill, Stebbins, & Waga 1995

  3. Understood importance of CMB/LSS for testing models Coble, Dodelson, & Frieman 1997

  4. Model with Early Dark Energy • Tweaks tracker model, with exponential potential • Solves “Why now?” problem • Important to bear in mind when planning experiments Dodelson, Kaplinghat, & Stewart 2000

  5. Analyzed early CMB data to prove flatness Dodelson & Knox 1999 Coupled with constraints on matter density, flatness is evidence for dark energy

  6. Radiation Ripples From Big Bang Illuminate Geometry of Universe By JAMES GLANZ (NYT) 1571 wordsPublished: November 26, 1999Like the great navigators who first sailed around the world, establishing its size and the curvature of its surface, astronomers have made new observations that show with startling directness the large-scale geometry of the universe and the total amount of matter and energy that it contains. … And that leads astronomers to their next conclusion: because the amount of matter found by astronomers cannot produce a flat universe, Dr. Dodelson said, ''the inescapable conclusion is that there is some unknown form of energy contributing to the total density.'' (This unknown energy is distinct from so-called dark matter, once described as the missing mass of the universe.)

  7. Took the lead in analyzing early SDSS data, leading to robust constraints on matter density Γ is Ωmh, so SDSS implies a matter density much smaller than critical Dodelson et al. 2002 One of 6 papers analyzing early SDSS data w/ Frieman, Hui, Johnston, Scranton, Sheth, Stebbins, Zehavi

  8. More evidence for dark energy in correlation of CMB and SDSS SDSS galaxies are nowhere near last scattering surface, but are correlated w/ WMAP because potential wells decay in a universe w/ dark energy. Scranton et al. 2003 w/ Stebbins, Frieman, & Johnston

  9. Dark Energy Papers over the Past 12 Months • Cosmology and the Bispectrum.Emiliano Sefusatti et al. e-Print Archive: astro-ph/0604505 • What can gamma ray bursts teach us about dark energy?Dan Hooper (Fermilab) , Scott Dodelson (Fermilab & Chicago U., Astron. Astrophys. Ctr.) e-Print Archive: astro-ph/0512232 • Testing Gravity Against Early Time Integrated Sachs-Wolfe Effect.Pengjie Zhang (Shanghai, Astron. Observ. & Fermilab) e-Print Archive: astro-ph/0511218 • Learning from the scatter in type ia supernovae.Scott Dodelson (Fermilab & Chicago U., Astron. Astrophys. Ctr.) , Alberto Vallinotto (Fermilab & Chicago U.) . e-Print Archive: astro-ph/0511086 • Comments on backreaction and cosmic acceleration. Edward W. Kolb (Fermilab & Chicago U., Astron. Astrophys. Ctr. & Chicago U., EFI) , Sabinio Matarrese (Padua U. & INFN, Padua) , Antonion Riotto (CERN) e-Print Archive: astro-ph/0511073 • Statistics of physical properties of dark matter clusters.Laurie Shaw , Jochen Weller et al. e-Print Archive: astro-ph/0509856 • Reduced shear power spectrum. Scott Dodelson (Fermilab & Chicago U., Astron. Astrophys. Ctr. & Northwestern U.) , Charles Shapiro (Chicago U. & KICP, Chicago) , Martin J. White (UC, Berkeley, Astron. Dept. & UC, Berkeley) . Published in Phys.Rev.D73:023009,2006 • Mapping dark matter with cosmic magnification. Pengjie Zhang (Fermilab) , Ue-Li Pen (Canadian Inst. Theor. Astrophys.) . Published in Phys.Rev.Lett.95:241302,2005 • On cosmic acceleration without dark energy.E.W. Kolb et al. e-Print Archive: astro-ph/0506534 • The dark energy survey. By Dark Energy Survey Collaboration (T. Abbott et al.). Oct 2005. 42pp. White Paper submitted to Dark Energy Task Force. e-Print Archive: astro-ph/0510346 • Constraining dark energy with the dark energy survey: theoretical challenges. White Paper submitted to Dark Energy Task Force. e-Print Archive: astro-ph/0510195 • Dark energy studies: challenges to computational cosmology. By DES Collaboration White Paper submitted to Dark Energy Task Force. e-Print Archive: astro-ph/0510194 • Probing dark energy via weak gravitational lensing with the Supernova Acceleration Probe (SNAP).By SNAP Collaboration White Paper to Dark Energy Task Force. e-Print Archive: astro-ph/0507460 • Supernova Acceleration Probe: Studying dark energy with Type Ia supernovae. By SNAP Collaboration White Paper to Dark Energy Task Force. e-Print Archive: astro-ph/0507459 • Seeing the nature of the accelerating physics: It's a SNAP. By SNAP Collaboration White Paper to the Dark Energy Task Force. e-Print Archive: astro-ph/0507458

  10. One Focus: Gravitational Lensing Constraints on dark energy via growth of structure

  11. Compute power spectrum of cosmic shear Dodelson, Shapiro, & White 2005 Background galaxy ellipticities sensitive to reduced shear, differs from cosmic shear at the 1-10% level

  12. Biases Cosmological Parameters … unless corrected for. Showed that analytic correction formula agrees with simulations.

  13. Additional information contained in higher point functions, e.g. bispectrum Sefusatti et al. 2006 Green curve uses power spectrum only; blue curve adds in bispecturm

  14. To use this information, must understand covariance of power spectrum and bispectrum. Sefusatti et al. 2006 Requires semi-analytic and numerical calculations of 5- and 6- point functions

  15. Lensing of Radio Galaxies Square Kilometer Array 1 000 000 000 galaxies 30 000 Million Light Years was ??

  16. Magnification Maps Zhang & Pen 2005 Galaxies behind large potential wells are magnified → get more, fainter galaxies. Use galaxy counts to infer projected potential.

  17. Another Focus: Type Ia Supernovae Supernova Hubble Diagram CFHT Supernova Legacy Survey Astier etal 05 Needed: more, better data at low and intermediate redshift SDSS

  18. SDSS II Supernova SurveySept-Nov. 2005-7 • Obtain ~200 high-quality SNe Ia light curves in the `redshift desert’ z~0.05-0.35: continuous Hubble diagram • Probe Dark Energy in z regime less sensitive to evolution than, and complementary to, deeper surveys • Study SN Ia systematics with high photometric accuracy • Search for additional parameters to reduce Ia dispersion • Determine SN/SF rates/properties vs. z, environment • Rest-frame u-band templates for z >1 surveys

  19. ~130 spectroscopically confirmed Type Ia Supernovae from the Fall 2005 Season First cosmology results expected this summer

  20. Monte Carlo prediction Confirmed Ia’s Different Selection criteria from Monte Carlo

  21. Composite gri images SN 2005 ff Before After z = 0.07, confirmed at WHT Preliminary gri light curve and fit from low-z templates

  22. Composite gri images SN 2005 gb Before After z = 0.086, confirmed at ARC 3.5m Preliminary gri light curve and fit from low-z templates

  23. SDSS II SN Follow-up 2005 • Spectroscopy: mainly SN typing, redshift ARC 3.5m (31 half-nights), HET (>60 hrs), MDM 2.4m (~37 nights), Subaru (share 6 nights), WHT (6 nights), Supernova Factory (low-z targets), Keck (opportunity, 1 night) • NIR imaging: extinction/reddening and low-z light curvesCarnegie Supernova Project (selected targets) • Optical imaging: follow high-z light curves beyond SDSS limit NMSU 1m, MDM, UH 88in (6.5 nights), VATT (7 nights), WIYN (3 nights shared), INT (1 night), Liverpool Telescope (4 hours)

  24. Follow-up Spectra from Subaru

  25. Conclusions • Long history of pioneering work on dark energy • Continues today with theory, phenomenology, and experiment

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