Program for Small Scale Anisotropy Measurements and the Ability to set Limits on Inflation.

A. Lee, L.Page and J. Ruhl

1 l>1000 CMB/SZ Experiments

ACBAR (Bolometric feed array) ACT SPT AMiBA (Taiwan, Interferometer) SuZie Upgrade AMI (UK, Interferometer) SZA (Interferometer) APEX VSA (Interferometer) Bolocam (Bolometric Camera, CSO) CBI (Interferometer)

2 Selected Bolometer-Array and SZ Roadmap

APEX SCUBA2 (~400 bolometers) (12000 bolometers) SZA Chile (Interferometer) Owens Valley ACT (3000 bolometers) Chile CMBPOL 2003 2005 2007 2004 2006 2008 SPT ALMA Polarbear-I (1000 bolometers) (Interferometer) (300 bolometers) South Pole Chile California Planck (50 bolometers) L2

3 ACT Collaboration Cardiff NASA/GSFC Princeton Peter Ade Domonic Benford Joe Fowler Cindy Hunt Jay Chervenak Norm Jarosik Phil Mauskopf Harvey Moseley Robert Lupton Carl Stahle Bob Margolis Columbia Ed Wollack Lyman Page Uros Seljak Amber Miller Penn David Spergel CUNY Angelica de Oliveira Costa Suzanne Staggs Martin Spergel Mark Devlin Simon Dicker Rutgers Haverford Bhuvnesh Jain Laura Ferrarese Steve Boughn Raul Jimenez Arthur Kosowsky Bruce Partridge Jeff Klein Jack Hughes Max Tegmark Ted Williams INOAE Licia Verde David Hughes Univ. de Catolica UMass Hernan Quintana NIST/Boulder Grant Wilson Univ. of Toronto Randy Doriese Univ. of British Columbia Kent Irwin Barth Netterfield Mark Halpern 4 Science: Observations: AtacamaACT Cosmology Telescope Growth of structure CMB: l>1000 Eqn. of state Cluster (SZ, KSZ X-rays, & optical) Neutrino mass Diffuse SZ Ionization history OV Power spectrum Lensing

X-ray

Optical Theory 5 Goals: Cosmological Parameters CMB Cosmic Structure Optical Coordinated ν Mass Approach +/- 0.1eV X-Ray Equation of State – w +/- 0.1 Theory Signature of Galactic First Stars Studies

6 Cosmic Timeline

• First galaxies • Universe is reionized • Cluster formation: Sunyaev-Zel’dovich (SZ) • Ostriker-Vishniac • Kinematic SZ • Diffuse thermal SZ • Lensing of the CMB

• Extraction of • The growth of structure is sensitive to w and mn cosmological parameters • Rich additional science from correlations among effects • Initial conditions for structure formation

z = 1100 z = 6-7 z = 1 z = .25 now

Primary CMB OV Diffuse Thermal SZ CMB Lensing Cluster Surveys 7 Inflation At low l<100, a clear signature would be the detection of B-modes or unambiguous measure of r based on TT, TE, EE + galaxies. Unadulterated (circa 1988) inflation gives: r=0.27. This implies a BB signal of roughly 0.01 uK2 at l=5. Current limit r<0.36 [95%] (Seljak et al. 2004) based on TT and TE.

ns=0.95 +/- 0.02. The current limit is 0.98+/-0.02 (Seljak et al. 2004) [WMAP alone 0.99+/-0.04]

dns/dlnk = 0. The current limit is -0.003+/- 0.01. (Seljak et al. 2004)

8 Lay of the Low l Land

Current limit G-waves on tensors decay once inside the B modes from horizon. tensors only.

B modes from lensing of E modes. Reionization peak Horizon size at decoupling (zdec=1089) (zr=20) 9 What does l>1000 add?

The limits on ns and dns/dlnk come from the combination of WMAP and SDSS + Lya. These latter two probe high l (or high k).

High l CMB measurements allow us to get at these parameters with the CMB alone, which should be less susceptible to “astrophysical systematics” than other measurements. Two mechanisms: Larger lever arm for measuring the slope.

Breaking the ns-tau-r degeneracy.

High l CMB experiments, when combined with WMAP, can reach 1% accuracy on ns but needs <1% calibration.. 10 Simulations of mm-wave data. <1% 1.40 Survey area ≈ 2% High quality area

150 GHz SZ Simulation MBAC on ACT PLANCK Burwell/Seljak 1.7’ beam MAP ACT PLANCK

Target Sensitivity

de Oliveira-Costa Hot electron gas ACT Bands imposes a unique spectral signature 145 GHz decrement

220 GHz null

270 GHz increment

1.4°x 1.4°

NO SZ Contribution in Central Band 12 145 GHz Maps Map Components

Components Summed to Scale

CMB SZ

1.4°x 1.4° KSZ/OV Point Sources 13 220 GHz Maps Map Components

Components Summed to Scale

CMB SZ

1.4°x 1.4° KSZ/OV Point Sources 14 270 GHz Maps Map Components

Components Summed to Scale

CMB SZ

1.4°x 1.4° KSZ/OV Point Sources 15 Existing PUDs 3.2 mm

SHARC II Need picture PI D. Dowell PUD Architecture.

Semiconductors Completed “close-packed” 12x32 bolometer array Dowell et al, 2003 SHARC II 12x32 Popup Array FIBRE Torsional yoke attachment PI D. Benford PUD Architecture. TES+SQUID Mux 1 mm Coming soon: SCUBA SCUBA-2 PD W. Duncan

HAWC Linear array after folding PI A. Harper One element of array 16 Where?

The Atacama in Chile: The ideal site for our science.

• 5200 meter elevation • One of driest places on planet • The future site for ALMA • Logistical support available • Only 26 hours travel from East Coast to site

17 Cross Linked Scan Strategy is Crucial to Making Maps on Degree Angular Scales

• 240 square degrees in circle • 100 square degrees for CMB • Rich Galactic data set

QuickTime™ and a BMP decompressor are needed to see this picture.

18 Cross-linked and Overlapping Scans

• Subtract a single level and gradient from East and West scans to link at the center.

• The largest total offset before full interlocking mapping solution, at l ~ 300, is less than 100 µK. East Scan West Scan • Each detector samples all points of the map without EVER changing elevation.

• Multiple pixels per PSF. All scans done at constant elevation. • Produce many 1.4° x 1.4° maps. Cross-linking key to WMAP, PLANCK, BOOMERanG, MAXIMA, QMAP 19 Timeline

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

DoE (LBNL) funding of readout development 21 SPT Science Goals

• Galaxy Cluster Surveys » High-ell primary and kSZ/OV • Polarization

22 Science Goal #2: Secondary CMB

1. Measure the SZ power spectrum after removing obvious clusters…

2. Measure CMB-spectrum power spectrum at high l after removing thermal SZ signal… requires multiple colors.

500 sq. deg. surveys, Noise is on CMB-only after perfect tSZ subtraction.

Figure: T. Crawford, spectra from W. Hu 23 Telescope Design Goals 1. Angular resolution for clusters (~ 1') at 150 GHz: Originally 8m + (1m radius “guard ring”), now 10m precision surface, no “guard ring” 2. Observe CMB & foregrounds from 1-3mm rms < 1mm/100 = 10 microns on small scales, rms < 1mm/20 = 50 microns on large scales pointing reconstruction ~ 1 arcsecond rms 3. Surveys ⇒ 1° diameter field of view at 150 GHz 4. Low offsets, low loading, low sidelobes fixed Gregorian w/ cold secondary and stop, 2 levels of ground shields. 5. Capable of sub-mm observations in the future rms < 20 microns overall (in future) 6. Flexibility for future use pure parabolic primary, large optics cabin

24 The Facility and Site

Moon Door

Existing Dark Sector Laboratory

25 Optical Design: Off-axis Gregorian

Parabolic Primary focal plane (f/0.7) Elliptical lens Secondary

Note: no chopper.

S. Padin 26 10 Kelvin Secondary and Baffle

4 K plastic 300mK

300mK

10 K 10 K black

27 Telescope

Drive components Receiver cabin are all in docks to control warm room for access environment

28 Structure and Shielding

144’ across Occultation limit: 28° Inner Shield (moves) 47’ high Outer Shield (fixed)

To DSL

29 SZ Focal Plane 2fλ Feedhorn Coupled, ~1000 elements

Horn array plate

Bolometers

Figure: W. Holzapfel 30 TES Bolometer Array

1 real wedge, 5 “Photoshop”

SiN suspended web

Cryogenics: Cooled with closed cycle 3He and pulse tubes, no LHe supply… Adrian Lee, UC Berkeley, APEX prototype 31 Band selection: which of 90, 150, 220, 270, 345 GHz ?

CMB 150 + 220 GHz Thermal SZ IR point sources 270 GHz Radio point sources 90 GHz ? (but resolution gets worse…)

Expected performance of these bands if used on the SPT

(trans)

32 Ongoing Work

Band selection: need more info on radio point sources populations, their correlations with clusters. Currently doing simulations to optimize bands and weighting… Depth vs. Area: more simulations… Scan speeds and patterns: more simulations with model atmosphere, elevation scanning, etc…

+ hardware, hardware, hardware… Planned First Observing Season: Austral Winter 2007

33 END

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