The Cosmic Background Imager
description
Transcript of The Cosmic Background Imager
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1UNM – Oct 14, 2003
The Cosmic Background Imager
Steven T. Myers
National Radio Astronomy Observatory
Socorro, NM
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2UNM – Oct 14, 2003
The Cosmic Background Imager
• A collaboration between– Caltech (A.C.S. Readhead PI)– NRAO– CITA– Universidad de Chile– University of Chicago
• With participants also from– U.C. Berkeley, U. Alberta, ESO, IAP-Paris, NASA-MSFC,
Universidad de Concepción
• Funded by– 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
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3UNM – Oct 14, 2003
The Instrument
• 13 90-cm Cassegrain antennas– 78 baselines
• 6-meter platform– Baselines 1m – 5.51m
• 10 1 GHz channels 26-36 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
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4UNM – Oct 14, 2003
3-Axis mount : rotatable platform
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UNM – Oct 14, 2003 5
Other Interferometers: DASI, VSA
• DASI @ South Pole
• VSA @ Tenerife
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6UNM – Oct 14, 2003
CBI Instrumentation
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7UNM – Oct 14, 2003
CBI Operations
• Observing in Chile since Nov 1999– NSF proposal 1994, funding in 1995– Assembled and tested at Caltech in 1998– Shipped to Chile in August 1999– Continued NSF funding in 2002, to end of 2004
• Telescope at high site in Andes– 16000 ft (~5000 m)– Located on Science Preserve, co-located with ALMA– Now also ATSE (Japan) and APEX (Germany), others– Controlled on-site, oxygenated quarters in containers
• Data reduction and archiving at “low” site– San Pedro de Atacama– 1 ½ hour driving time to site
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8UNM – Oct 14, 2003
Site – Northern Chilean Andes
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9UNM – Oct 14, 2003
CBI in Chile
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10UNM – Oct 14, 2003
A Theoretical Digression
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11UNM – Oct 14, 2003
The Cosmic Microwave Background
• Discovered 1965 (Penzias & Wilson)– 2.7 K blackbody– Isotropic– Relic of hot “big bang”– 3 mK dipole (Doppler)
• COBE 1992– Blackbody 2.725 K– Anisotropies 10-5
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12UNM – Oct 14, 2003
Thermal History of the Universe
Courtesy Wayne Hu – http://background.uchicago.edu
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13UNM – Oct 14, 2003
CMB Anisotropies
• Primary Anisotropies– Imprinted on surface of “last scattering”– “recombination” of hydrogen z~1100– Primordial (power-law?) spectrum of potential fluctuations
• Collapse of dark matter potential wells inside horizon
• Photons coupled to baryons >> acoustic oscillations!
– Electron scattering density & velocity• Velocity produces quadrupole >> polarization!
– Transfer function maps P(k) >> Cl
• Depends on cosmological parameters >> predictive!
– Gaussian fluctuations + isotropy• Angular power spectrum contains all information
• Secondary Anisotropies– Due to processes after recombination
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14UNM – Oct 14, 2003
Acoustic Oscillations
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15UNM – Oct 14, 2003
Power Spectrum of the CMB
Courtesy Wayne Hu – http://background.uchicago.edu
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16UNM – Oct 14, 2003
Dependence on Geometry
Courtesy Wayne Hu – http://background.uchicago.edu
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17UNM – Oct 14, 2003
Dependence on Baryon content
Courtesy Wayne Hu – http://background.uchicago.edu
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18UNM – Oct 14, 2003
Effects of Damping
Courtesy Wayne Hu – http://background.uchicago.edu
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19UNM – Oct 14, 2003
Secondary Anisotropies
Courtesy Wayne Hu – http://background.uchicago.edu
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20UNM – Oct 14, 2003
Courtesy Wayne Hu – http://background.uchicago.edu
Gravitational Secondaries
• Due to CMB photons passing through potential fluctuations (spatial and temporal)
• Includes:– Early ISW (decay, matter-radiation transition at last scattering)– Late ISW (decay, in open or lambda model)– Rees-Sciama (growth, non-linear structures)– Tensors (gravity waves, ‘nuff said)– Lensing (spatial distortions)
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21UNM – Oct 14, 2003
Scattering Secondaries
• Due to variations in:– Density
• Linear = Vishniac effect
• Clusters = thermal Sunyaev-Zeldovich effect
– Velocity (Doppler)• Clusters = kinetic SZE
– Ionization fraction• Coherent reionization suppression
• “Patchy” reionization
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22UNM – Oct 14, 2003
• Spectral distortion of CMB• Dominated by massive halos (galaxy clusters)• Low-z clusters: ~ 20’-30’• z=1: ~1’ expected dominant signal in CMB on small angular scales• Amplitude highly sensitive to 8
A. Cooray (astro-ph/0203048)
P. Zhang, U. Pen, & B. Wang (astro-ph/0201375)
2ndary SZE Anisotropies
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23UNM – Oct 14, 2003
Seven Pillars of the CMB
•Large Scale Anisotropies
•Acoustic Peaks/Dips
•Damping Tail
•Gaussianity
•Secondary Anisotropies
•Polarization
•Gravity Waves
Minimal Inflationary parameter set
Quintessence
Tensor fluc.
Broken Scale Invariance
(of inflationary adiabatic fluctuations)
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24UNM – Oct 14, 2003
Images of the CMB
BOOMERANG
WMAP Satellite
ACBAR
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25UNM – Oct 14, 2003
After WMAP…
• Power spectrum– measured to l < 1000– Primary CMB– First 3 peaks
Courtesy Wayne Hu – http://background.uchicago.edu
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26UNM – Oct 14, 2003
…and Planck
• Power spectrum– measured to l < 1000– Primary CMB– First 6 peaks
Courtesy Wayne Hu – http://background.uchicago.edu
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27UNM – Oct 14, 2003
CMB Interferometry
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28UNM – Oct 14, 2003
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Interferometers
• Spatial coherence of radiation pattern contains information about source structure– Correlations along wavefronts
• Equivalent to masking parts of a telescope aperture– Sparse arrays = unfilled aperture– Resolution at cost of surface brightness sensitivity
• Correlate pairs of antennas– “visibility” = correlated fraction of total signal
• Fourier transform relationship with sky brightness– Van Cittert – Zernicke theorem
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29UNM – Oct 14, 2003
The Fourier Relationship
• An interferometer “visibility” in the sky and Fourier planes:
• The aperture (antenna) size smears out the coherence function response– Like a double-slit experiment with widening slits– Interference plus diffraction pattern– Lose ability to localize wavefront direction = field-of-view– Small apertures = wide field
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30UNM – Oct 14, 2003
The uv plane and l space
• The sky can be uniquely described by spherical harmonics– CMB power spectra are described by multipole l ( the angular
scale in the spherical harmonic transform)
• For small (sub-radian) scales the spherical harmonics can be approximated by Fourier modes– The conjugate variables are (u,v) as in radio interferometry– The uv radius is given by l / 2
• The projected length of the interferometer baseline gives the angular scale – Multipole l = 2 B /
• An interferometer naturally measures the transform of the sky intensity in l space
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31UNM – Oct 14, 2003
Interferometry of the CMB
• An interferometer “visibility” in the sky and Fourier planes:
• The primary beam and aperture are related by:
CBI:
CMB peaks smaller
than this !
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32UNM – Oct 14, 2003
Mosaicing in the uv plane
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33UNM – Oct 14, 2003
Power Spectrum and Likelihood
• Statistics of CMB (Gaussian) described by power spectrum:
Break into bandpowers Construct covariance matrices and perform maximum Likelihood calculation:
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34UNM – Oct 14, 2003
CBI Beam and uv coverage
• 78 baselines and 10 frequency channels = 780 instantaneous visibilities– Frequency channels give radial spread in uv plane
• Pointing platform rotatable to fill in uv coverage– Parallactic angle rotation gives azimuthal spread– Beam nearly circularly symmetric
• Baselines locked to platform in pointing direction– Baselines always perpendicular to source direction– Delay lines not needed– Very low fringe rates (susceptible to cross-talk and ground)
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35UNM – Oct 14, 2003
Calibration and Foreground Removal
• Calibration scale ~5%– Jupiter from OVRO 1.5m (Mason et al. 1999)– Agrees with BIMA (Welch) and WMAP
• Ground emission removal– Strong on short baselines, depends on orientation– Differencing between lead/trail field pairs (8m in RA=2deg)– Use scanning for 2002-2003 polarization observations
• Foreground radio sources– Predominant on long baselines – Located in NVSS at 1.4 GHz, VLA 8.4 GHz– Measured at 30 GHz with OVRO 40m– Projected out in power spectrum analysis
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36UNM – Oct 14, 2003
Power Spectrum Estimation
• Method described in Paper IV (Myers et al. 2003)• Large datasets
– > 105 visibilities in 6 x 7 field mosaic– ~ 103 independent
• Gridded “estimators” in uv plane– fast! – Not lossless, but information loss insignificant
• Construct covariance matrices for gridded points• Maximum likelihood using BJK method• Output bandpowers• Wiener filtered images constructed from estimators
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37UNM – Oct 14, 2003
The Computational Problem
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38UNM – Oct 14, 2003
Tests with mock data
• The CBI pipeline has been extensively tested using mock data– Use real data files for template– Replace visibilties with simulated signal and noise– Run end-to-end through pipeline– Run many trials to build up statistics
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39UNM – Oct 14, 2003
Wiener filtered images
• Covariance matrices can be applied as Wiener filter to gridded estimators
• Estimators can be Fourier transformed back into filtered images
• Filters CX can be tailored to pick out specific components– e.g. point sources, CMB, SZE– Just need to know the shape of the power spectrum
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40UNM – Oct 14, 2003
Example – Mock deep field
Raw
CMB
Noise removed
Sources
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41UNM – Oct 14, 2003
CBI Results
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42UNM – Oct 14, 2003
CBI 2000 Results
• Observations– 3 Deep Fields (8h, 14h, 20h)– 3 Mosaics (14h, 20h, 02h)– Fields on celestial equator (Dec center –2d30’)
• Published in series of 5 papers (ApJ July 2003)– Mason et al. (deep fields)– Pearson et al. (mosaics)– Myers et al. (power spectrum method)– Sievers et al. (cosmological parameters)– Bond et al. (high-l anomaly and SZ) pending
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43UNM – Oct 14, 2003
CBI Deep Fields 2000
Deep Field Observations: •3 fields totaling 4 deg^2•Fields at ~0 =8h, 14h, 20h
•~115 nights of observing•Data redundancy strong tests for systematics
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44UNM – Oct 14, 2003
Mosaic Field Observations• 3 fields totaling 40 deg^2• Fields at ~0 =2h, 14h, 20h
• ~125 nights of observing• ~ 600,000 uv points covariance matrix 5000 x 5000
CBI 2000 Mosaic Power Spectrum
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45UNM – Oct 14, 2003
CBI 2000 Mosaic Power Spectrum
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46UNM – Oct 14, 2003
Cosmological Parameters
wk-h: 0.45 < h < 0.9, t > 10 Gyr
HST-h: h = 0.71 ± 0.076
LSS: constraints on8 and from 2dF, SDSS, etc.
SN: constraints from Type 1a SNae
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47UNM – Oct 14, 2003
SZE Angular Power SpectrumSZE Angular Power Spectrum
•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
[Bond et al. 2002]
Dawson et al. 2002
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48UNM – Oct 14, 2003
• Combine CBI & BIMA (Dawson et al.) 30 GHz with ACBAR 150 GHz (Goldstein et al.)
• Non-Gaussian scatter for SZE– increased sample variance (factor ~3))
• Uncertainty in primary spectrum– due to various parameters, marginalize
• Explained in Goldstein et al. (astro-ph/0212517)• Use updated BIMA (Carlo Contaldi)
Constraints on SZ “density”
Courtesy Carlo Contaldi (CITA)
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49UNM – Oct 14, 2003
SZE with CBI: z < 0.1 clusters
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50UNM – Oct 14, 2003
New : Calibration from WMAP Jupiter
• Old uncertainty: 5%• 2.7% high vs. WMAP Jupiter• New uncertainty: 1.3%• Ultimate goal: 0.5%
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51UNM – Oct 14, 2003
49
Future plans
New: CBI 2000+2001 Results
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52UNM – Oct 14, 2003
CBI 2000+2001 Noise Power
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53UNM – Oct 14, 2003
CBI 2000+2001 and WMAP
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54UNM – Oct 14, 2003
CBI 2000+2001, WMAP, ACBAR
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55UNM – Oct 14, 2003
The CMB From NRAO HEMTs
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56UNM – Oct 14, 2003
Post-WMAP Unification
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57UNM – Oct 14, 2003
weak prior: t > 1010 yr 0.45 < h < 0.9 m > 0.1
LSS prior: constraint on amplitude of 8 andshape of eff (Bond et al. Ap.J. 2003)
CBI + COBECBI + COBE
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58UNM – Oct 14, 2003
weak prior: t > 1010 yr 0.45 < h < 0.9 m > 0.1
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59UNM – Oct 14, 2003
CBI Current & Future
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60UNM – Oct 14, 2003
CBI Polarization
• CBI instrumentation– 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 K
• 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
Ka-band Receiver
0
2
4
6
8
10
12
14
16
18
20
26 28 30 32 34 36 38 40
Frequency (GHz)
No
ise
Tem
per
atu
re (
K)
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61UNM – Oct 14, 2003
Polarization Sensitivity
CBI is most sensitive at the peak of the polarization power spectrum
Theoretical sensitivity ± of CBI in 450 hours (90 nights) on each of 3 mosaic fields 5 deg sq (no differencing), close-packed configuration.
EETE The compact configuration
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62UNM – Oct 14, 2003
Polarization Interferometry
“Cross hands” sensitive to linear polarization (Stokes Q and U):
where the baseline parallactic angle is defined as:
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63UNM – Oct 14, 2003
E and B modes
• A useful decomposition of the polarization signal is into gradient and curl modes – E and B:
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64UNM – Oct 14, 2003
CBI-Pol 2000 Cartwright thesis
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65UNM – Oct 14, 2003
Pol 2003 – DASI & WMAP
Courtesy Wayne Hu – http://background.uchicago.edu
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66UNM – Oct 14, 2003
CBI-Pol 2002-2004 Projections
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67UNM – Oct 14, 2003
Conclusions from CBI Data
• Definitive measurement of diffusive damping scale• Measurements of 3rd & 4th Acoustic Peaks• At Low L consistent with other experiments• At High L (>2000) indications of secondary anisotropy?
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68UNM – Oct 14, 2003
Conclusions from CBI Data
• Definitive measurement of diffusive damping scale• Measurements of 3rd & 4th Acoustic Peaks• At Low L consistent with other experiments• At High L (>2000) indications of secondary anisotropy?
Small Scale Power• ~3 sigma above expected intrinsic anisotropy• Not consistent with likely residual radio source populations (more definitive characterization needed)• Suggestive of secondary SZ anisotropy, although this would imply sigma8 ~ 1• Other possible foregrounds not ruled out at this point
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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.
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70UNM – Oct 14, 2003