cosmology with the cbi ee power spectrum jonathan sievers (cita)

Cosmology with the CBICosmology with the CBIEE Power SpectrumEE Power Spectrum

Jonathan Sievers (CITA)Jonathan Sievers (CITA)

The CBI CollaborationThe CBI CollaborationCaltech Team: Tony Readhead (Principal Investigator), John Cartwright, Clive Dickinson, Alison Farmer, Russ Keeney, Brian Mason, Steve Miller, Steve Padin (Project Scientist), Tim Pearson, Walter Schaal, Martin Shepherd, Jonathan Sievers, Pat Udomprasert, John Yamasaki.Operations in Chile: Pablo Altamirano, Ricardo Bustos, Cristobal Achermann, Tomislav Vucina, Juan Pablo Jacob, José Cortes, Wilson Araya.Collaborators: Dick Bond (CITA), Leonardo Bronfman (University of Chile), John Carlstrom (University of Chicago), Simon Casassus (University of Chile), Carlo Contaldi (CITA), Nils Halverson (University of California, Berkeley), Bill Holzapfel (University of California, Berkeley), Marshall Joy (NASA's Marshall Space Flight Center), John Kovac (University of Chicago), Erik Leitch (University of Chicago), Jorge May (University of Chile), Steven Myers (National Radio Astronomy Observatory), Angel Otarola (European Southern Observatory), Ue-Li Pen (CITA), Dmitry Pogosyan (University of Alberta), Simon Prunet (Institut d'Astrophysique de Paris), Clem Pryke (University of Chicago).

The CBI Project is a collaboration between the California Institute of Technology, the Canadian Institute for Theoretical Astrophysics, the National Radio Astronomy Observatory, the University of Chicago, and the Universidad de Chile. The project has been supported by funds from the National Science Foundation, the California Institute of Technology, Maxine and Ronald Linde, Cecil and Sally Drinkward, Barbara and Stanley Rawn Jr., the Kavli Institute,and the Canadian Institute for Advanced Research.

EE – A Separate View EE – A Separate View

Excellent check onconsistency of stan-dard cosmological model.

One example: path-ological primordial spectra with verydifferent params can mimic TT. However,EE changes dra-matically.

Shaped CShaped Cll Fit Fit Use WMAP’03 best-fit CUse WMAP’03 best-fit Cll in signal covariance matrix in signal covariance matrix

• bandpower relative to fiducial PSbandpower relative to fiducial PS• compute for single band encompassing all compute for single band encompassing all llss

Results for CBI data (sources projected from TT only)Results for CBI data (sources projected from TT only)• qqBB = 1.22 = 1.22 ± 0.21 (68%)± 0.21 (68%)

• EE likelihood vs. zero : equivalent significance EE likelihood vs. zero : equivalent significance 8.9 8.9 σσ

Conservative - project source subset out in Conservative - project source subset out in polarization alsopolarization also• qqBB = 1.18 = 1.18 ± 0.24 (68%)± 0.24 (68%)

• significance significance 7.0 7.0 σσ

CBI Polarization Power SpectraCBI Polarization Power Spectra 7-band fits (7-band fits (ll = 150 for 600< = 150 for 600<ll<1200) <1200) 7-band spectra consistent with model 7-band spectra consistent with model

– – χχ22EEEE=3.77 for 7 dof=3.77 for 7 dof

narrower bins (narrower bins (ll = 75) for cosmology = 75) for cosmology – increased scatter from – increased scatter from FF-1-1

fine bins give better cosmological fine bins give better cosmological constraintsconstraints

New: CBI EE Polz’n PhaseNew: CBI EE Polz’n Phase Parameterization 1: envelope plus Parameterization 1: envelope plus

shiftable sinusoidshiftable sinusoid• fit to “WMAP+ext” fiducial spectrum fit to “WMAP+ext” fiducial spectrum

using rational functionsusing rational functions

kgfa

C EE

sin

1

= 0= 0°° : EE prediction: EE prediction = 180= 180°°: aligned with TT: aligned with TT

CBI Fine EE w/ Best Fit PhaseCBI Fine EE w/ Best Fit Phase

CBI EE Polarization PhaseCBI EE Polarization Phase Peaks in EE should be offset one-half Peaks in EE should be offset one-half

cycle vs. TTcycle vs. TT• allow amplitude allow amplitude aa and phase and phase to vary to vary

best fit: best fit: aa=0.94=0.94

== 2424°±°±3333°° ( (22=1)=1)

22(1, 0(1, 0°°)=0.56)=0.56

θθ//θθ00

Angular size of sound horizon at LSS Angular size of sound horizon at LSS should be same for TT and EE. should be same for TT and EE.

CBI only has multiple solutions (shift CBI only has multiple solutions (shift spectrum by one peak).spectrum by one peak).

DASI removes degeneracy, but less DASI removes degeneracy, but less sensitive.sensitive.

CBI+DASI give scale vs. TT of 1.02 CBI+DASI give scale vs. TT of 1.02 +/- 0.03.+/- 0.03.

CBI CBI θθ//θθ00

New: CBI, DASI, CapmapNew: CBI, DASI, Capmap

New: DASI EE Polz’n PhaseNew: DASI EE Polz’n Phase Use DASI EE 5-bin bandpowers Use DASI EE 5-bin bandpowers

(Leitch et al. 2004)(Leitch et al. 2004)• bin-bin covariance matrix plus bin-bin covariance matrix plus

approximate window functionsapproximate window functions

New: CBI + DASI EE PhaseNew: CBI + DASI EE Phase Combined constraints on Combined constraints on θθ model:model:

• DASI (Leitch et al. 2004) & CBI DASI (Leitch et al. 2004) & CBI (Readhead et al. 2004)(Readhead et al. 2004)

CBI a=0.67 overtone island:CBI a=0.67 overtone island:

suppressed by DASI datasuppressed by DASI dataCBI+DASI phase lock:CBI+DASI phase lock:

θθ//θθ00== 1.02±0.031.02±0.03a=0.78a=0.78±0.15±0.15 (low DASI) (low DASI)

CBI ProjectionsCBI Projections EE phase: July 2004 vs. 2006EE phase: July 2004 vs. 2006

July 2004 (Readhead et al.)

2

2006 Forecast

CBI ProjectionsCBI Projections Will BB (lensing) be foreground Will BB (lensing) be foreground

limited?limited?

Consistency w/ WMAPConsistency w/ WMAP

Spectra consistent with the Spectra consistent with the cosmological model from WMAPext cosmological model from WMAPext datasetdataset

χχ22 = 7.98 TT, 3.77 EE, 4.33 BB (vs. = 7.98 TT, 3.77 EE, 4.33 BB (vs. 0), and 5.80 TE for 7 dof.0), and 5.80 TE for 7 dof.