Presentation on theme: "Surveys of Dark Energy: Challenges and Prospects Ofer Lahav University College London Cosmology post WMAP/2dF/SDSS/… The Dark Energy Survey Photometric."— Presentation transcript:
Surveys of Dark Energy: Challenges and Prospects Ofer Lahav University College London Cosmology post WMAP/2dF/SDSS/… The Dark Energy Survey Photometric redshifts, and cross-talk with cosmic probes The future of the local universe
“Evidence” for Dark Energy SN Ia CMB LSS – Baryonic Oscillations Cluster counts Weak Lensing Integrated Sachs Wolfe Physical effects: * Geometry * Growth of Structure
The Chequered History of the Cosmological Constant The old CC problem: Theory exceeds observational limits on by ! The new CC problem: Why are the amounts of Dark Matter and Dark Energy so similar?
Globalisation and the New Cosmology How is the New Cosmology affected by Globalisation? Recall the Cold War era: Hot Dark Matter/top-down (East) vs. Cold Dark Matter/bottom-up (West) Is the agreement on the `concordance model’ a product of Globalisation? OL, astro-ph/
Matter and Dark Energy tell space how to curve: k = 1 - m - Curvature Matter Dark Energy(Vacuum)
Matter and Dark Energy tell space how to curve: k = 1 - m - Curvature Matter Dark Energy(Vacuum) OR modified curvature k + = 1 - m
The Universe is accelerating at present if q 0 = m /2 - < 0 e.g. For m = 0.3 and = 0.7 : k = 0 (the Universe is flat) and the Universe is accelerating (but only ‘recently’, z<0.7)
Spherical Collapse d 2 r/dt 2 = -GM/r 2 + ( /3) r cf. Newton-Hooke force cf. Inflation For the mass of the Local Group (MW+M31) the forces are equal at r= 1.3 Mpc Dark Energy also affects the virialization radius the collapsed object (OL et al. 91; Maor & OL 05)
Through the history of the expansion rate: H 2 (z) = H 2 0 [ M (1+z) 3 + DE (1+z) 3 (1+w) ] (flat Universe) matter dark energy (constant w) P = w Comoving distance r(z) = dz/H(z) Standard Candles d L (z) = (1+z) r(z) Standard Rulers d A (z) = (1+z) 1 r(z) The rate of growth of structure also determined by H(z) and by any modifications of gravity on large scales Probing Dark Matter & Dark Energy
Baryon Wiggles as Standard Rulers
DUNE: Dark UNiverse Explorer Mission baseline: 1.2m telescope FOV 0.5 deg 2 PSF FWHM 0.23’’ Pixels 0.11’’ GEO (or HEO) orbit Surveys (3-year initial programme): WL survey: 20,000 deg 2 in 1 red broad band, 35 galaxies/amin 2 with median z ~ 1, ground based complement for photo-z’s Near-IR survey (J,H). Deeper than possible from ground. Secures z > 1 photo-z’s SNe survey: 2 £ 60 deg 2, observed for 9 months each every 4 days in 6 bands, SNe out to z ~ 1.5, ground based spectroscopy
US Dark Energy Task Force Recommendations An immediate start of a near- term program (which we call Stage III) designed to advance our knowledge of dark energy and prepare for the ultimate “Stage IV” program, which consists of a combination of large survey telescopes and/or a space mission. cf. PPARC and ESO/ESA reports Advocate ‘a Figure of Merit’
DETF FoM / 1/[ellipse area]
The Dark Energy Survey Study Dark Energy using 4 complementary techniques: I. Cluster Counts II. Weak Lensing III. Baryon Acoustic Oscillations IV. Supernovae Two multi-band surveys 5000 deg 2 g, r, i, z 40 deg 2 repeat (SNe) Build new 3 deg 2 camera and data management system Survey (525 nights) Response to NOAO AO Blanco 4-meter at CTIO 300,000,000 photometric redshifts
The DES Collaboration Fermilab: J. Annis, H. T. Diehl, S. Dodelson, J. Estrada, B. Flaugher, J. Frieman, S. Kent, H. Lin, P. Limon, K. W. Merritt, J. Peoples, V. Scarpine, A. Stebbins, C. Stoughton, D. Tucker, W. Wester University of Illinois at Urbana-Champaign: C. Beldica, R. Brunner, I. Karliner, J. Mohr, R. Plante, P. Ricker, M. Selen, J. Thaler University of Chicago: J. Carlstrom, S. Dodelson, J. Frieman, M. Gladders, W. Hu, S. Kent, R. Kessler, E. Sheldon, R. Wechsler Lawrence Berkeley National Lab: N. Roe, C. Bebek, M. Levi, S. Perlmutter University of Michigan: R. Bernstein, B. Bigelow, M. Campbell, D. Gerdes, A. Evrard, W. Lorenzon, T. McKay, M. Schubnell, G. Tarle, M. Tecchio NOAO/CTIO: T. Abbott, C. Miller, C. Smith, N. Suntzeff, A. Walker CSIC/Institut d'Estudis Espacials de Catalunya (Barcelona): F. Castander, P. Fosalba, E. Gaztañaga, J. Miralda-Escude Institut de Fisica d'Altes Energies (Barcelona): E. Fernández, M. Martínez CIEMAT (Madrid): C. Mana, M. Molla, E. Sanchez, J. Garcia-Bellido University College London: O. Lahav, D. Brooks, P. Doel, M. Barlow, S. Bridle, S. Viti, J. Weller University of Cambridge: G. Efstathiou, R. McMahon, W. Sutherland University of Edinburgh: J. Peacock University of Portsmouth: R. Crittenden, R. Nichol, R. Maartnes, W. Percival University of Sussex: A. Liddle, K. Romer plus postdocs and students
The Dark Energy Survey UK Consortium (I) PPARC funding: O. Lahav (PI), P. Doel, M. Barlow, S. Bridle, S. Viti, J. Weller (UCL), R. Nichol (Portsmouth), G. Efstathiou, R. McMahon, W. Sutherland (Cambridge) J. Peacock (Edinburgh) Submitted a proposal to PPARC requesting £ 1.7M for the DES optical design. In March 2006, PPARC Council announced that it “will seek participation in DES”. PPARC already approved £220K for current R&D. (II) SRIF3 funding: R. Nichol, R. Crittenden, R. Maartens, W. Percival (ICG Portsmouth) K. Romer, A. Liddle (Sussex) Funding the optical glass blanks for the UCL DES optical work These scientists will work together through the UK DES Consortium. Other DES proposals are under consideration by US and Spanish funding agencies.
The Dark Energy Survey Camera: DECam DECam will replace the prime focus cage 4m Blanco telescope
Supernovae Ia Geometric Probe of Dark Energy Repeat observations of 40 deg 2, using 10% of survey time ~1900 well-measured SN Ia lightcurves, 0.25 < z < 0.75 Larger sample, improved z-band response compared to ESSENCE, SNLS; address issues they raise Improved photometric precision via in- situ photometric response measurements SDSS
Observer Dark matter halos Background sources Statistical measure of shear pattern, ~1% distortion Radial distances depend on geometry of Universe Foreground mass distribution depends on growth of structure A. Taylor
DES Forecasts: Power of Multiple Techniques Ma, Weller, Huterer, etal Assumptions: Clusters: SPT-selected, 8 =0.75, z max =1.5, WL mass calibration (no clustering self-calibration) Mass-observable power-law w/ Lognormal spread BAO: l max =300 WL: l max =1000 (no bispectrum or galaxy-shear) Statistical+photo-z systematic errors only Spatial curvature, galaxy bias marginalized Planck CMB prior w(z) =w 0 +w a (1–a) 68% CL
DES – Figure of Merit
Photo-z – WL – BAO - SNIa cross talk Approximately, for a photo-z slice: ( w/ w) = a ( z/ z) = a ( z /z) N s -1/2 => the target accuracy in w and photo-z scatter z dictate the number of required spectroscopic redshifts N s =
Photometric redshifts Probe strong spectral features (e.g break) z=3.7z=0.1
*Training on ~13,000 2SLAQ *Generating with ANNz Photo-z for ~1,000,000 LRGs MegaZ-LRG z = Collister, Lahav, Blake et al., astro-ph/
Excess Power on Gpc Scale? Blake et al. 06 Padmanabhan et al. 06
DES and VDES DES (griz)DES+VISTA(JK) VISTA J (<21) and K (<19) would improve photo-z by a factor of 2 for z> 1 F. Abdalla, M. Banerji, OL, H. Lin, et al.
* 4-5 complementary probes * Survey strategy delivers substantial DE science after 2 years * Relatively modest (~ $20-30M), low-risk, near-term project with high discovery potential * Synergy with SPT and VISTA on the DETF Stage III timescale * Scientific and technical precursor to the more ambitious Stage IV Dark Energy projects to follow: LSST and JDEM DES and a Dark Energy Programme
The Future of the Local Universe m =0.3 LCDM a = 1 (t= 13.5 Gyr) OCDM a = 1 (t= 11.3 Gyr) LCDM a = 6 (t= 42.4 Gyr) OCDM a = 6 (t= 89.2 Gyr) Hoffman, Dover, Yepes, OL
Some Outstanding Questions: * Vacuum energy (cosmological constant, w= after all?) * Dynamical scalar field? * Modified gravity? * Why / m = 3 ? * Non-zero Neutrino mass < 1eV ? * The exact value of the spectral index: n < 1 ? * Excess power on large scales? * Is the curvature zero exactly ?
Expected performance of DECAM, Blanco, and CTIO site Blanco Effective Aperture/ f prime focus4 m/ 2.7 Blanco Primary Mirror - 80% encircled energy0.25 arcsec Optical Corrector Field of View2.2 deg. Corrector Wavelength Sensitivity< nm FiltersSDSS g, r, i, z ( nm) Effective Area of CCD Focal Plane3.0 sq. deg. Image CCD pixel format/ total # pixels2K X 4K/ 520 Mpix Guide, Focus & Wavefront Sensor CCD pixel format2K X 2K Pixel Size0.27 arcsec/ 15 μm Readout Speed/Noise requirement250 kpix/sec/ 10 e Survey Area SPT overlap SDSS stripe 82 Connection region 5,000 sq. deg. total RA -60 to 105, DEC -30 to -65 RA -75 to -60, DEC -45 to -65 RA -50 to 50, Dec -1 to 1 RA 20 to 50, Dec -30 to -1 Survey Time/Duration525/5 (nights/years) Median Site Seeing Sept. – Feb.0.65 arcsec Median Delivered Seeing with Mosaic II on the Blanco arcsec (V band) Limiting Magnitude: 10 in 1.5” aperture assuming 0.9” seeing g=24.6, r=24.1, i=24.3, z=23.9 Limiting Magnitude: 5 for point sources assuming 0.9” seeing g=26.1,r=25.6, i=25.8, z=25.4