2. The Instrument 13 90-cm Cassegrain antennas 6-meter platform
78 baselines
6-meter platform
Baselines 1m – 5.51m
10 1 GHz channels GHz
HEMT amplifiers (NRAO)
Cryogenic 6K, Tsys 20 K
Single polarization (R or L)
Polarizers from U. Chicago
Analog correlators
780 complex correlators
Field-of-view 44 arcmin
Image noise 4 mJy/bm 900s
Resolution 4.5 – 10 arcmin

3. CBI Deep Fields 2000 Deep Field Observations:
3 fields totaling 4 deg^2
~115 nights of observing
Data redundancy  strong tests for systematics

4. CBI 2000 Mosaic Power Spectrum
Mosaic Field Observations
3 fields totaling 40 deg^2
~125 nights of observing
~ 600,000 uv points covariance matrix 5000 x 5000

5. SZE Angular Power Spectrum
[Bond et al. 2002]
Smooth Particle Hydrodynamics (5123) [Wadsley et al. 2002]
Moving Mesh Hydrodynamics (5123) [Pen 1998]
143 Mpc 8=1.0
200 Mpc 8=1.0
200 Mpc 8=0.9
400 Mpc 8=0.9
Dawson et al. 2002
Review SZ effect – expected crossover
Use of simulations to predict power
Description of simulations
Parameters of simulations
Scaling of power with parameters confirms s8to the 7
Power for s8=1 and s8=0.9

6. SZE with CBI: z < 0.1 clusters

7. Calibration using Jupiter
Old uncertainty: 5%
2.7% high vs. WMAP Jupiter
New uncertainty: 1.3%
Ultimate goal: 0.5%

8. CBI Results

9. CBI and WMAP

10. CBI , WMAP, ACBAR

11. The CMB From NRAO HEMTs

12. CBI + COBE weak prior: t > 1010 yr
0.45 < h < 0.9
Wm > 0.1
LSS prior: constraint on amplitude of s8 and
shape of Geff (Bond et al. Ap.J. 2003)

13. weak prior: t > 1010 yr
0.45 < h < 0.9
Wm > 0.1

14. CBI Polarization CBI instrumentation 2000 Observations 2002 Upgrade
Use quarter-wave devices for linear to circular conversion
Single amplifier per receiver: either R or L only per element
2000 Observations
One antenna cross-polarized in 2000 (Cartwright thesis)
Only 12 cross-polarized baseline (cf. 66 parallel hand)
Original polarizers had 5%-15% leakage
Deep fields, upper limit ~8 mK
2002 Upgrade
Upgrade in 2002 using DASI polarizers (switchable)
Observing with 7R + 6L starting Sep 2002
Raster scans for mosaicing and efficiency
New TRW InP HEMTs from NRAO

15. CBI-Pol Projections

16. The CBI Collaboration
Caltech Team: Tony Readhead (Principal Investigator), John Cartwright, 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.