High Resolution Observations of the CMB with the CBI Interferometer XVIII th IAP Colloquium - July 1 2002 Carlo Contaldi CITA.

Slides:



Advertisements
Similar presentations
The second LDB flight of BOOMERanG was devoted to CMB polarization measurements Was motivated by the desire to measure polarization : –at 145 GHz (higher.
Advertisements

Constraining Inflation Histories with the CMB & Large Scale Structure Dynamical & Resolution Trajectories for Inflation then & now Dick Bond.
Planck 2013 results, implications for cosmology
Cosmology topics, collaborations BOOMERanG, Cosmic Microwave Background LARES (LAser RElativity Satellite), General Relativity and extensions, Lense-Thirring.
SZE in WMAP Data Jose M. Diego & Bruce Partridge 2010, MNRAS, 402, 1179 La Thuile, March 2012.
Suzanne Staggs (Princeton) Rencontres de Blois, 1 June 2011 The Atacama Cosmology Telescope (ACT): Still More Cosmology from the Cosmic Microwave Background.
Polarization Results from the Cosmic Background Imager Steven T. Myers Jonathan Sievers (CITA) CITA 04 Oct Continued…
1 ACT  Atacama Cosmology Telescope  Funded by NSF  Will measure CMB fluctuations on small angular scales  Probe the primordial power spectrum and the.
The Sunyaev-Zel’dovich effect The Sunyaev-Zel’dovich effect AMI day, 2011 September 30 Mark Birkinshaw University of Bristol.
K.S. Dawson, W.L. Holzapfel, E.D. Reese University of California at Berkeley, Berkeley, CA J.E. Carlstrom, S.J. LaRoque, D. Nagai University of Chicago,
The Structure Formation Cookbook 1. Initial Conditions: A Theory for the Origin of Density Perturbations in the Early Universe Primordial Inflation: initial.
A Primer on SZ Surveys Gil Holder Institute for Advanced Study.
Advanced Cosmology Bolometer Array Receiver (ACBAR) on Viper Jeff Peterson - CMU –Ravinder Bhatia (Caltech) –Jamie Bock (JPL) –Andrew Lange (Caltech) –Peter.
High-ℓ CMB and the CBI Jonathan Sievers (CITA/UToronto) +CBI Collaboration.
Cosmology with the CBI EE Power Spectrum Jonathan Sievers (CITA)
Southern African Large Telescope Observations of ACT SZ-Selected Clusters Brian Kirk Catherine Cress, Matt Hilton, Steve Crawford, Jack Hughes, Felipe.
The CMB and Neutrinos. We can all measure the CMB T CMB = \ K CMB approx 1% of TV noise! 400 photons/cc at 0.28 eV/cc.
Preliminary Results from the SZA Amber Miller Columbia University Photo: Leitch New Views of the Universe Kavli Inaugural Sypmosium Dec 11th, Chicago.
Ninth Synthesis Imaging Summer School Socorro, June 15-22, 2004 Mosaicing Tim Cornwell.
Polarization-assisted WMAP-NVSS Cross Correlation Collaborators: K-W Ng(IoP, AS) Ue-Li Pen (CITA) Guo Chin Liu (ASIAA)
Early times CMB.
Modern State of Cosmology V.N. Lukash Astro Space Centre of Lebedev Physics Institute Cherenkov Conference-2004.
ASIAA NTU PHYS J.H.P.Wu & AMiBA Team To remove the ground pickup and electronic DC component in the data, we tracked the source- (P1) and tail- (P2) patches.
Relic Neutrinos, thermal axions and cosmology in early 2014 Elena Giusarma arXiv: Based on work in collaboration with: E. Di Valentino, M. Lattanzi,
Molecular Gas and Dust in SMGs in COSMOS Left panel is the COSMOS field with overlays of single-dish mm surveys. Right panel is a 0.3 sq degree map at.
CMB observations and results Dmitry Pogosyan University of Alberta Lake Louise, February, 2003 Lecture 1: What can Cosmic Microwave Background tell us.
IPAM – Jan 30, Interferometric Imaging & Analysis of the CMB Steven T. Myers National Radio Astronomy Observatory Socorro, NM.
Using the Sunyaev-Zeldovich Effect to Determine H o and the Baryon Fraction by Michael McElwain Astronomy 278: Anisotropy and Large Scale Structure in.
Galaxies and galaxy clusters at mm wavelengths: the view from the South Pole Telescope Gil Holder.
IPAM – Jan 30, Interferometric Imaging & Analysis of the CMB Steven T. Myers National Radio Astronomy Observatory Socorro, NM.
Joint analysis of Archeops and WMAP observations of the CMB G. Patanchon (University of British Columbia) for the Archeops collaboration.
Academia Sinica National Taiwan University AMiBA System Performance Kai-yang Lin 1,2 and AMiBA Team 1,2,3 1 Institute of Astronomy and Astrophysics, Academia.
SUNYAEV-ZELDOVICH EFFECT. OUTLINE  What is SZE  What Can we learn from SZE  SZE Cluster Surveys  Experimental Issues  SZ Surveys are coming: What.
Fundamental limits of radio interferometers: Source parameter estimation Cathryn Trott Randall Wayth Steven Tingay Curtin University International Centre.
X-Ray Radio Connections – Feb 6, CBI Observations of the Sunyaev-Zeldovich Effect Steven T. Myers*, *National Radio Astronomy Observatory Socorro,
The Structure Formation Cookbook 1. Initial Conditions: A Theory for the Origin of Density Perturbations in the Early Universe Primordial Inflation: initial.
Joint Analysis of Weak Lensing and SZE data from the Arcminute Microkelvin Imager Natasha Hurley-Walker in collaboration with Farhan Feroz, Jonathan Zwart,
The Very Small Array Angela Taylor & Anze Slosar Cavendish Astrophysics University of Cambridge.
Chao-Lin Kuo Stanford Physics/SLAC
High Resolution Measurements of CMB Anisotropies with ACBAR U.C. Berkeley: W.L. Holzapfel (co-PI) M.D. Daub M. Lueker Case-Western: J. Ruhl (co-PI) J.
Array for Microwave Background Anisotropy AMiBA SZ Science AMiBA Team NTU Physics Figure 4. Simulated AMiBA deep surveys of a 1deg 2 field (no primary.
INFRARED-BRIGHT GALAXIES IN THE MILLENNIUM SIMULATION AND CMB CONTAMINATION DANIEL CHRIS OPOLOT DR. CATHERINE CRESS UWC.
EBEx foregrounds and band optimization Carlo Baccigalupi, Radek Stompor.
Santa Fe Cosmology Workshop – Jul 7, SZ Interferometry: CBI & Beyond Steven T. Myers* *National Radio Astronomy Observatory Socorro, NM and the.
L2: The Cosmic Microwave Background & the Fluctuation History of the Universe & the Basic Cosmological Parameters Dick Bond.
The Planck Satellite Hannu Kurki-Suonio University of Helsinki Finnish-Japanese Workshop on Particle Cosmology, Helsinki
Clusters of Galaxies in the Microwaves
The Cosmic Background Imager – U. Sydney, 22 Oct CMB Polarization Results from the Cosmic Background Imager Steven T. Myers National Radio Astronomy.
Polarization Results from the Cosmic Background Imager Steven T. Myers Jonathan Sievers (CITA) Cosmo 04 Continued…
The Cosmic Background Imager – Berkeley, 28 Sep CMB Polarization Results from the Cosmic Background Imager Steven T. Myers National Radio Astronomy.
Tim Pearson US Planck Data Analysis Review 9-10 May 2006 US Planck Data Analysis Review Source Extraction Tim Pearson.
Gravitational Lensing
The Cosmic Background Imager – AAS Denver, June Latest Results from the Cosmic Background Imager Steven T. Myers National Radio Astronomy Observatory.
Trajectories Bond, Contaldi, Frolov, Kofman, Souradeep, Vaudrevange 05.
2-year Total Intensity Observations year Polarization Observations Cosmic Background Imager Tony Readhead Zeldovich celebration.
APEX stuff – 4 Feb 2003 Martin White Department of Physics Department of Astronomy UC Berkeley Lawrence Berkeley National Lab.
The Cosmic Background Imager – COSMO-04, 18 Sep CMB Polarization Results from the Cosmic Background Imager Steven T. Myers National Radio Astronomy.
Towards the first detection using SPT polarisation
Jean-Baptiste Melin U.C. Davis J. Bartlett J. Delabrouille
Simulating Interferometers for the CMB Sky
The Cosmic Background Imager
Interferometric Imaging & Analysis of the CMB
CBI Observations of the Sunyaev-Zeldovich Effect
The Cosmic Background Imager
Miller Lab - Columbia Currently in the lab…
No calibration errors. All measurements of the anisotropy.
CBI Polarization New Results! Brought to you by:
The Instrument cm Cassegrain antennas 6-meter platform
Coherent analysis of CMB anisotropies CMB, structures and Foregrounds
CMB Observations with the Cosmic Background Imager
Presentation transcript:

High Resolution Observations of the CMB with the CBI Interferometer XVIII th IAP Colloquium - July Carlo Contaldi CITA

T. Readhead (Caltech) T. Pearson (Caltech) S. Myers (NRAO) B. Mason (Caltech/NRAO) J. Sievers (Caltech) J. Cartwright (Caltech) P. Udompraesert (Caltech) M. Shepherd (Caltech) A.Farmer (Caltech) S. Padin (Caltech) J. R. Bond (CITA) C. Contaldi (CITA) D. Pogosyan (U of Alberta) U.-L. Pen (CITA) M. Ruetalo (CITA/UofT) P. Zhang (CITA/UofT) J. Wadsley (McMaster) S. Prunet (IAP)

13 elements 0.90 m dishes 45’ FWHM 78 baselines 10 frequency channels GHz  l~200 The Cosmic Background Imager > 5000m Atacama Plateau Chile

10-channel single pointing uv-coverage GHz single pointing uv-coverage mosaic pointings

CBI Power spectrum extraction Visibilities ‘gridded’ in uv plane [Myers at al. 2002]. Quadratic estimator solves for the ML band powers 6x7 field mosaic; ~10 hrs. 16 processor GS320 CITA Foreground templates projected out using known positions

CBI Mosaic Power Spectrum 3 6x7 field mosaics ~ 145’x165’ each ~ 40 sq. deg. [Pearson et al. 2002] “Silk” damping

Mosaic Window Functions

Weak Weak + Flat +LSS Flat + LSS + HST-h CBI+DMR [Sievers et al. 2002]

CBI Deep Field Power Spectrum BOOMERanG 2001 [Mason et al. 2002]

CBI High-l Excess Significant power above l=  inconsistent with zero and 3.1  inconsistent with best-fit model. Secondary Anisotropies from Sunyaev- Zeldovich Effect? Amplitude ~ 4.5 higher than expected signal from residual low-flux sources Estimate includes 50% error in residual source flux.

Raw map

Total Signal

CMB + ?

OVRO & NVSS Source residuals

SZE Angular Power Spectrum Smooth Particle Hydrodynamics (512 3 ) [Wadsley et al. 2002] Moving Mesh Hydrodynamics (512 3 ) [Pen 1998] 143 Mpc  8 = Mpc  8 = Mpc  8 = Mpc  8 =0.9 [Bond et al. 2002] Dawson et al. 2002

Simulation of Deep Observations by the CBI Input SZ mapReconstructed Signal

Bandpower Estimation with a SZ Foreground CBI Pipeline recovers input SZE signal at observed amplitudes Non-Gaussian scatter from the SZ signal is significant in the high-l band given the small areas observed Single Deep Field (08h) simulated observation

Flat HST-h Priors LSS parameters from CMB and other Cosmological Surveys

The CBI observations l<2000 give consistent parameters with those of previous experiments on larger angular scales Measurement of the damping tail at l>1000 6’ scales probing ~10 14 M O  seeds of clusters High-l excess; Simulations show the Sunyaev-Zeldovich Effect fits the observed power for  8 ~1.0. This is in the high- end of the range allowed by CMB and LSS surveys SZE: high-accuracy determination of  8. Break  8 -Ω M degeneracy  Ω Λ Follow-up on excess Extended mosaic data ~ 80 sq. deg. Improved hydrodynamical simulations Summary

Optimally configured for resolution of peaks Polarization upgrade nearly complete Calibration runs in August Polarization Observations 2002/3