1. August '04 - Joe Mohr Blanco Instrument Review Presentations to Blanco Instrument Review Panel Intro and Science 1 Mohr Intro and Science 1 Mohr Science 2 and Context Frieman Science 2 and Context Frieman Survey Design Annis Survey Design Annis Instrument Flaugher Instrument Flaugher Optical Design Kent Optical Design Kent Data Management Plante Data Management Plante Project Management Peoples Project Management Peoples

2. August '04 - Joe Mohr Blanco Instrument Review Toward an Understanding of the Dark Energy/ Cosmic Acceleration 1. Measuring (relative) distances or volumes out to z~2 2. Measuring the growth rate of cosmic structures 3. Detecting dark energy clustering in the power spectrum of density fluctuations 4. Measure evolution of gravitational potential wells using the Integrated Sachs-Wolfe effect 5. Laboratory experiments and theoretical progress Spergel et al. 2003 Cosmic acceleration is here to stay!

3. August '04 - Joe Mohr Blanco Instrument Review Key Techniques for Measuring the Dark Energy Equation of State Parameter 1. Type Ia Supernovae as standard candles 2. Power spectrum measurements using galaxies or clusters 3. Cosmic Microwave Background anisotropy 4. Weak lensing measurements 5. Galaxy cluster surveys Tegmark et al 2004

4. August '04 - Joe Mohr Blanco Instrument Review The Dark Energy Survey A study of the dark energy using four independent and complementary techniques A study of the dark energy using four independent and complementary techniques Galaxy cluster surveys Galaxy cluster surveys Galaxy angular power spectrum Galaxy angular power spectrum Weak lensing Weak lensing SN Ia distances SN Ia distances Two linked, multiband optical surveys Two linked, multiband optical surveys 5000 deg 2 g, r, i and z 5000 deg 2 g, r, i and z Repeated observations of 40 deg 2 Repeated observations of 40 deg 2 Instrument and schedule Instrument and schedule New 3 deg 2 camera on the Blanco 4m on Cerro Tololo New 3 deg 2 camera on the Blanco 4m on Cerro Tololo Construction: 2004-2009 Construction: 2004-2009 Survey Operations: 30% of telescope time over 5 years Survey Operations: 30% of telescope time over 5 years Image credit: Roger Smith/NOAO/AURA/NSF Blanco 4m on Cerro Tololo

5. August '04 - Joe Mohr Blanco Instrument Review The Dark Energy Survey Collaboration Fermilab - Camera building, Survey Planning and Simulations Fermilab - Camera building, Survey Planning and Simulations Annis, Dodelson, Flaugher, Frieman, Gladders*, Hui, Kent, Lin, Limon, Peoples, Scarpine, Stebbins, Stoughton, Tucker and Wester Annis, Dodelson, Flaugher, Frieman, Gladders*, Hui, Kent, Lin, Limon, Peoples, Scarpine, Stebbins, Stoughton, Tucker and Wester *Carnegie Fellow, Carnegie Observatories U Illinois - Data Management, Data Acquisition, SPT U Illinois - Data Management, Data Acquisition, SPT Brunner, Karliner, Mohr, Plante, Selen and Thaler Brunner, Karliner, Mohr, Plante, Selen and Thaler U Chicago - SPT, Simulations, Corrector U Chicago - SPT, Simulations, Corrector Carlstrom, Dodelson, Frieman, Hu, Kent, Sheldon and Wechsler Carlstrom, Dodelson, Frieman, Hu, Kent, Sheldon and Wechsler LBNL - Red Sensitive CCD Detectors LBNL - Red Sensitive CCD Detectors Aldering, Bebek, Levi, Perlmutter and Roe Aldering, Bebek, Levi, Perlmutter and Roe CTIO - Telescope & Camera Operations CTIO - Telescope & Camera Operations Abbott, Smith, Suntzeff and Walker Abbott, Smith, Suntzeff and Walker

6. August '04 - Joe Mohr Blanco Instrument Review Cluster Survey Studies of the Dark Energy are Complementary and Competitive Cluster constraints on dark energy: Cluster constraints on dark energy: The cluster redshift distribution, the cluster power spectrum and 30% accurate mass measurements for 100 clusters between z of 0.3-1.2 The cluster redshift distribution, the cluster power spectrum and 30% accurate mass measurements for 100 clusters between z of 0.3-1.2 Fiducial cosmology (WMAP:  8 =0.84,  m =0.27); 29000 clusters in the 4000 deg 2 SPT survey. Fiducial cosmology (WMAP:  8 =0.84,  m =0.27); 29000 clusters in the 4000 deg 2 SPT survey. The joint constraints on w and  m : The joint constraints on w and  m : Curvature free to vary (dashed); fixed (solid) Curvature free to vary (dashed); fixed (solid) Marginalized constant w 68% uncertainty is 0.046 (flat) or 0.071 (curvature varying) Marginalized constant w 68% uncertainty is 0.046 (flat) or 0.071 (curvature varying) Parameter degeneracies complementary Parameter degeneracies complementary SPT: Majumdar & Mohr 2003 SNAP: Perlmutter & Schmidt 2003 WMAP: Spergel et al 2003

7. August '04 - Joe Mohr Blanco Instrument Review Cluster Redshift Distribution is Sensitive to the Dark Energy Equation of State Parameter Raising w at fixed  E : decreases volume surveyed decreases volume surveyed Volume effect Growth effect decreases growth rate of density perturbations decreases growth rate of density perturbations w constraints:

8. August '04 - Joe Mohr Blanco Instrument Review Precision Cosmology with Clusters Requirements Requirements 1. Quantitative understanding of the formation of dark matter halos in an expanding universe 2. Clean way of selecting a large number (~10 4 ) of massive dark matter halos (galaxy clusters) over a range of redshifts 3. Crude redshift estimates for each cluster 4. Observables that can be used as mass estimates at all redshifts Technique called self-calibration provides a framework for determining cosmology and mass- observable relation simultaneously Technique called self-calibration provides a framework for determining cosmology and mass- observable relation simultaneously Sensitivity to Mass

9. August '04 - Joe Mohr Blanco Instrument Review 10m South Pole Telescope (SPT) and 1000 Element Bolometer Array Low noise, precision telescope 20 um rms surface 1 arc second pointing 1.0 arcminute at 2 mm ‘chop’ entire telescope 3 levels of shielding - ~1 m radius on primary - inner moving shields - outer fixed shields SZE and CMB Anisotropy - 4000 sq deg SZE survey - deep CMB anisotropy fields - deep CMB Polarization fields 1000 Element Bolometer Array - 3 to 4 interchangeable bands (90) 150, 250 & 270 GHz - APEX-SZ style horn fed spider web absorbers People Carlstrom (UC) Holzapfel (UCB) Lee (UCB,LBNL) Leitch (UC) Meyer (UC) Mohr (U Illinois) Padin (UC) Pryke (UC) Ruhl (CWRU) Spieler (LBNL) Stark (CfA) NSF-OPP funded & scheduled for Nov 2006 deployment DoE (LBNL) funding of readout development

10. August '04 - Joe Mohr Blanco Instrument Review SPT Structure and Shielding 144’ across 47’ high To DSL Occultation limit: 28  Will survey extragalactic sky south of -30 0 dec

11. August '04 - Joe Mohr Blanco Instrument Review SPT Survey Region SPT will survey all the extragalactic sky south of declination  =-30 0 SPT will survey all the extragalactic sky south of declination  =-30 0 This corresponds to approximately 4000 deg 2 of reasonably clean sky This corresponds to approximately 4000 deg 2 of reasonably clean sky north of  =-75 0 north of  =-75 0 20hr <  < 7hr 20hr <  < 7hr This region is easily observable with the Blanco 4m on Cerro Tololo This region is easily observable with the Blanco 4m on Cerro Tololo

12. August '04 - Joe Mohr Blanco Instrument Review DES Cluster Photo-z’s DES data will enable cluster photometric redshifts with  z~0.02 for all SPT clusters out to z~1.3 DES data will enable cluster photometric redshifts with  z~0.02 for all SPT clusters out to z~1.3 Figure from Huan Lin Uses Monte-carlo estimates of galaxy photo-z uncertainties, which include appropriate photometric noise [Huan Lin] Uses Monte-carlo estimates of galaxy photo-z uncertainties, which include appropriate photometric noise [Huan Lin] Uses halo occupation number N(M) measured in ~100 local groups and clusters [Y-T Lin, Mohr & Stanford 2004] Uses halo occupation number N(M) measured in ~100 local groups and clusters [Y-T Lin, Mohr & Stanford 2004] Adopts redshift evolution of N(M)~(1+z) and passive evolution of galactic stars Adopts redshift evolution of N(M)~(1+z) and passive evolution of galactic stars

13. August '04 - Joe Mohr Blanco Instrument Review Why a Large SZE Cluster Survey? Improved halo mass estimates- the mass-observable relations in the optical are not as clean Improved halo mass estimates- the mass-observable relations in the optical are not as clean ~100% rms in optical- see below- versus 10%-25% in SZE ~100% rms in optical- see below- versus 10%-25% in SZE Improved cluster selection- projection and environment issues are not as severe (optical data complementary) Improved cluster selection- projection and environment issues are not as severe (optical data complementary) What about X-ray surveys (serendipitous and with DUO)? What about X-ray surveys (serendipitous and with DUO)? Lin, Mohr & Stanford 2004 89 clusters 28% scatter Kochanek et al. 2003 84 clusters 81% scatter

14. August '04 - Joe Mohr Blanco Instrument Review DES Galaxy Angular Power Spectrum DES main survey will yield photo-z’s on approximately 300 million galaxies extending beyond a redshift z~1 DES main survey will yield photo-z’s on approximately 300 million galaxies extending beyond a redshift z~1 Photo-z uncertainties are too large to allow a full study of the 3D galaxy clustering, but we can study the angular clustering within redshift shells to z~1 Photo-z uncertainties are too large to allow a full study of the 3D galaxy clustering, but we can study the angular clustering within redshift shells to z~1 Features in the angular power spectrum reflect “standard rods” that follow from simple physical arguments and can be calibrated using CMB anisotropy data. Features in the angular power spectrum reflect “standard rods” that follow from simple physical arguments and can be calibrated using CMB anisotropy data. Apparent sizes of features provide angular diameter distances to each redshift shell (i.e. Cooray et al 2001). The clustering amplitude is unimportant, and so the unknown galaxy bias is no problem. Apparent sizes of features provide angular diameter distances to each redshift shell (i.e. Cooray et al 2001). The clustering amplitude is unimportant, and so the unknown galaxy bias is no problem. SPT Cluster Angular Power Spectrum Figure from Cooray et al ApJ 2001

15. August '04 - Joe Mohr Blanco Instrument Review Galaxy Angular Power Spectrum Cosmology We use the galaxy angular power spectrum within redshift shells, concentrating only on the portion with 50 < ell < 300 We use the galaxy angular power spectrum within redshift shells, concentrating only on the portion with 50 < ell < 300 We marginalize over 5 halo model parameters in each redshift bin We marginalize over 5 halo model parameters in each redshift bin With Planck priors, constraints on a constant equation of state parameter w are better than  w~0.1 With Planck priors, constraints on a constant equation of state parameter w are better than  w~0.1 Angular Power Spectrum for 0.90 < z < 1 Figures from Wayne Hu

16. August '04 - Joe Mohr Blanco Instrument Review Presentations to Blanco Instrument Review Panel Intro and Science 1 Mohr Intro and Science 1 Mohr Science 2 and Context Frieman Science 2 and Context Frieman Survey Design Annis Survey Design Annis Instrument Flaugher Instrument Flaugher Optical Design Kent Optical Design Kent Data Management Plante Data Management Plante Project Management Peoples Project Management Peoples