Post on 27-Dec-2015
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
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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:
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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