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

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August '04 - Joe Mohr Blanco Instrument Review

Presentations to Presentations to Blanco Instrument Review PanelBlanco Instrument Review Panel

Intro and Science 1 Intro and Science 1 MohrMohr

Science 2 and Context Science 2 and Context FriemanFrieman

Survey Design Survey Design AnnisAnnis

Instrument Instrument FlaugherFlaugher

Optical Design Optical Design KentKent

Data Management Data Management PlantePlante

Project ManagementProject Management PeoplesPeoples

August '04 - Joe Mohr Blanco Instrument Review

Toward an Understanding of the Toward an Understanding of the Dark Energy/ Cosmic AccelerationDark Energy/ Cosmic Acceleration

1.1. Measuring (relative) distances or Measuring (relative) distances or

volumes out to z~2volumes out to z~2

2.2. Measuring the growth rate of Measuring the growth rate of

cosmic structurescosmic structures

3.3. Detecting dark energy clustering Detecting dark energy clustering

in the power spectrum of density in the power spectrum of density

fluctuationsfluctuations

4.4. Measure evolution of Measure evolution of

gravitational potential wells gravitational potential wells

using the Integrated Sachs-Wolfe using the Integrated Sachs-Wolfe

effecteffect

5.5. Laboratory experiments and Laboratory experiments and

theoretical progresstheoretical progress

H 2 z( ) = Ho2 Ωm 1+ z( )

3+ 1− Ωm − ΩE( ) 1+ z( )

2+ ΩE 1+ z( )

3 1+w( )[ ]

w ≡p

ρand ρE ∝

a

a0

⎝ ⎜

⎠ ⎟

−3 1+w( )

Spergel et al. 2003

Cosmic acceleration is here to stay!

August '04 - Joe Mohr Blanco Instrument Review

Key Techniques for Measuring the Key Techniques for Measuring the Dark Energy Equation of State Dark Energy Equation of State ParameterParameter

1.1. Type Ia Supernovae as Type Ia Supernovae as

standard candlesstandard candles

2.2. Power spectrum Power spectrum

measurements using measurements using

galaxies or clustersgalaxies or clusters

3.3. Cosmic Microwave Cosmic Microwave

Background anisotropyBackground anisotropy

4.4. Weak lensing Weak lensing

measurementsmeasurements

5.5. Galaxy cluster surveysGalaxy cluster surveys

Tegmark et al 2004

August '04 - Joe Mohr Blanco Instrument Review

The Dark Energy SurveyThe Dark Energy Survey A study of the dark energy using A study of the dark energy using

four independent and four independent and complementary techniquescomplementary techniques Galaxy cluster surveysGalaxy cluster surveys Galaxy angular power spectrum Galaxy angular power spectrum Weak lensingWeak lensing SN Ia distancesSN Ia distances

Two linked, multiband optical Two linked, multiband optical surveyssurveys 5000 deg5000 deg22 g, r, i and z g, r, i and z Repeated observations of 40 degRepeated observations of 40 deg22

Instrument and scheduleInstrument and schedule New 3 degNew 3 deg22 camera on the Blanco camera on the Blanco

4m on Cerro Tololo4m on Cerro Tololo Construction: 2004-2009Construction: 2004-2009 Survey Operations: 30% of Survey Operations: 30% of

telescope time over 5 yearstelescope time over 5 years

Image credit: Roger Smith/NOAO/AURA/NSF

Blanco 4m on Cerro Tololo

August '04 - Joe Mohr Blanco Instrument Review

The Dark Energy Survey The Dark Energy Survey CollaborationCollaboration

FermilabFermilab- Camera building, Survey Planning and - Camera building, Survey Planning and SimulationsSimulations

Annis, Dodelson, Flaugher, Frieman, Gladders*, Hui, Kent, Lin, Annis, Dodelson, Flaugher, Frieman, Gladders*, Hui, Kent, Lin, Limon, Peoples, Scarpine, Stebbins, Stoughton, Tucker and Limon, Peoples, Scarpine, Stebbins, Stoughton, Tucker and WesterWester

*Carnegie Fellow, Carnegie Observatories*Carnegie Fellow, Carnegie Observatories

U IllinoisU Illinois- Data Management, Data Acquisition, SPT- Data Management, Data Acquisition, SPT Brunner, Karliner, Mohr, Plante, Selen and ThalerBrunner, Karliner, Mohr, Plante, Selen and Thaler

U ChicagoU Chicago- SPT, Simulations, Corrector- SPT, Simulations, Corrector Carlstrom, Dodelson, Frieman, Hu, Kent, Sheldon and Wechsler Carlstrom, Dodelson, Frieman, Hu, Kent, Sheldon and Wechsler

LBNLLBNL- Red Sensitive CCD Detectors- Red Sensitive CCD Detectors Aldering, Bebek, Levi, Perlmutter and RoeAldering, Bebek, Levi, Perlmutter and Roe

CTIOCTIO- Telescope & Camera Operations- Telescope & Camera Operations Abbott, Smith, Suntzeff and WalkerAbbott, Smith, Suntzeff and Walker

August '04 - Joe Mohr Blanco Instrument Review

Cluster Survey Studies of the Dark Cluster Survey Studies of the Dark Energy are Complementary and Energy are Complementary and CompetitiveCompetitive

Cluster constraints on dark Cluster constraints on dark energy:energy: The cluster redshift distribution, The cluster redshift distribution,

the cluster power spectrum and the cluster power spectrum and 30% accurate mass measurements 30% accurate mass measurements for 100 clusters between z of 0.3-for 100 clusters between z of 0.3-1.21.2

Fiducial cosmology (WMAP: Fiducial cosmology (WMAP: 88=0.84, =0.84, mm=0.27); 29000 clusters =0.27); 29000 clusters in the 4000 degin the 4000 deg22 SPT survey. SPT survey.

The joint constraints on w and The joint constraints on w and mm:: Curvature free to vary (dashed); Curvature free to vary (dashed);

fixed (solid)fixed (solid) Marginalized constant w 68% Marginalized constant w 68%

uncertainty is 0.046 (flat) or 0.071 uncertainty is 0.046 (flat) or 0.071 (curvature varying)(curvature varying)

Parameter degeneracies Parameter degeneracies complementarycomplementary

SPT: Majumdar & Mohr 2003SNAP: Perlmutter & Schmidt 2003

WMAP: Spergel et al 2003

August '04 - Joe Mohr Blanco Instrument Review

Cluster Redshift Distribution is Sensitive Cluster Redshift Distribution is Sensitive to the Dark Energy Equation of State to the Dark Energy Equation of State ParameterParameter

Raising Raising ww at fixed at fixed EE:: decreases volume decreases volume

surveyedsurveyed

Volume effect Growth effect

decreases growth rate decreases growth rate of density perturbationsof density perturbations

ww constraints: constraints:

dN(z)

dzdΩ=dV

dz dΩn z( )

dA ∝dz'E (z')0

z∫

August '04 - Joe Mohr Blanco Instrument Review

Precision Cosmology with ClustersPrecision Cosmology with Clusters

RequirementsRequirements1.1. Quantitative understanding of the Quantitative understanding of the

formation of dark matter halos in formation of dark matter halos in an expanding universean expanding universe

2.2. Clean way of selecting a large Clean way of selecting a large number (~10number (~1044) of massive dark ) of massive dark matter halos (galaxy clusters) matter halos (galaxy clusters) over a range of redshiftsover a range of redshifts

3.3. Crude redshift estimates for each Crude redshift estimates for each clustercluster

4.4. Observables that can be used as Observables that can be used as mass estimates at all redshiftsmass estimates at all redshifts

Technique called self-calibration Technique called self-calibration provides a framework for provides a framework for determining cosmology and determining cosmology and mass-observable relation mass-observable relation simultaneouslysimultaneously

Sensitivity to Mass

dN(z)dzdΩ

= cH z( )

dA2 1+z( )2 dM

dnM,z( )

dMf M( )

0

∞∫

August '04 - Joe Mohr Blanco Instrument Review

10m South Pole Telescope10m South Pole Telescope (SPT)(SPT)and 1000 Element Bolometer Arrayand 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

PeopleCarlstrom (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 deploymentDoE (LBNL) funding of readout development

August '04 - Joe Mohr Blanco Instrument Review

SPT Structure and ShieldingSPT Structure and Shielding

144’ across

47’

high

To DSL

Occultation limit: 28

Will survey extragalactic sky south of -300 dec

August '04 - Joe Mohr Blanco Instrument Review

SPT Survey RegionSPT Survey Region

SPT will survey all the SPT will survey all the extragalactic sky south of extragalactic sky south of declination declination =-30=-3000

This corresponds to This corresponds to approximately 4000 degapproximately 4000 deg22 of reasonably clean skyof reasonably clean sky north of north of =-75=-7500

20hr < 20hr < < 7hr < 7hr

This region is easily This region is easily observable with the observable with the Blanco 4m on Cerro Blanco 4m on Cerro TololoTololo

August '04 - Joe Mohr Blanco Instrument Review

DES Cluster Photo-z’sDES Cluster Photo-z’s DES data will enable cluster photometric redshifts with DES data will enable cluster photometric redshifts with

z~0.02 for all SPT clusters out to z~1.3z~0.02 for all SPT clusters out to z~1.3

Figure from Huan Lin

Uses Monte-carlo Uses Monte-carlo estimates of galaxy photo-z estimates of galaxy photo-z uncertainties, which uncertainties, which include appropriate include appropriate photometric noise [Huan photometric noise [Huan Lin]Lin]

Uses halo occupation Uses halo occupation number N(M) measured in number N(M) measured in ~100 local groups and ~100 local groups and clusters [Y-T Lin, Mohr & clusters [Y-T Lin, Mohr & Stanford 2004]Stanford 2004]

Adopts redshift evolution of Adopts redshift evolution of N(M)~(1+z) and passive N(M)~(1+z) and passive evolution of galactic starsevolution of galactic stars

August '04 - Joe Mohr Blanco Instrument Review

Why a Large SZE Cluster Why a Large SZE Cluster Survey?Survey?

Improved halo mass estimates- the mass-observable relations Improved halo mass estimates- the mass-observable relations in the optical are not as clean 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 Improved cluster selection- projection and environment issues are not as severe (optical data complementary)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 clusters28% scatter

Kochanek et al. 2003

84 clusters81% scatter

August '04 - Joe Mohr Blanco Instrument Review

DES Galaxy Angular Power DES Galaxy Angular Power SpectrumSpectrum

DES main survey will yield photo-z’s on DES main survey will yield photo-z’s on approximately 300 million galaxies approximately 300 million galaxies extending beyond a redshift z~1extending beyond a redshift z~1

Photo-z uncertainties are too large to Photo-z uncertainties are too large to allow a full study of the 3D galaxy allow a full study of the 3D galaxy clustering, but we can study the angular clustering, but we can study the angular clustering within redshift shells to z~1clustering within redshift shells to z~1

Features in the angular power spectrum Features in the angular power spectrum reflect “standard rods” that follow from reflect “standard rods” that follow from simple physical arguments and can be simple physical arguments and can be calibrated using CMB anisotropy data.calibrated using CMB anisotropy data.

Apparent sizes of features provide Apparent sizes of features provide angular diameter distances to each angular diameter distances to each redshift shell (i.e. Cooray et al 2001). redshift shell (i.e. Cooray et al 2001). The clustering The clustering amplitudeamplitude is unimportant, is unimportant, and so the unknown galaxy bias is no and so the unknown galaxy bias is no problem.problem.

SPT Cluster Angular Power Spectrum

Figure from Cooray et al ApJ 2001

August '04 - Joe Mohr Blanco Instrument Review

Galaxy Angular Power Spectrum Galaxy Angular Power Spectrum CosmologyCosmology

We use the galaxy angular power We use the galaxy angular power spectrum within redshift shells, spectrum within redshift shells, concentrating only on the portion concentrating only on the portion with 50 < ell < 300with 50 < ell < 300

We marginalize over 5 halo model We marginalize over 5 halo model parameters in each redshift binparameters in each redshift bin

With Planck priors, With Planck priors, constraints on a constant constraints on a constant equation of state parameter equation of state parameter w are better than w are better than w~0.1w~0.1

Angular Power Spectrum for 0.90 < z < 1

Figures from Wayne Hu

August '04 - Joe Mohr Blanco Instrument Review

Presentations to Presentations to Blanco Instrument Review PanelBlanco Instrument Review Panel

Intro and Science 1 Intro and Science 1 MohrMohr

Science 2 and Context Science 2 and Context FriemanFrieman

Survey Design Survey Design AnnisAnnis

Instrument Instrument FlaugherFlaugher

Optical Design Optical Design KentKent

Data Management Data Management PlantePlante

Project ManagementProject Management PeoplesPeoples