MAXIPOL: Data Analysis and Results

Wu, Jiun-Huei Proty; Zuntz, Joe; Abroe, M. E.; Ade, Peter A. R.; Bock, J. J.; Borrill, J.; Collins, J.; Hanany, Shaul; Jaffe, A. H.; Johnson, Bradley R.; Jones, T. J.; Lee, A. T.; Matsumura, Tomotake; Rabii, B.; Renbarger, T.; Richards, P. L.; Smoot, George F.; Stompor, R.; Tran, Hung V.; Winant, C. D.

doi:10.1086/518112

Cited by 57 publications

(46 citation statements)

References 27 publications

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“…E-modes were first detected by Dasi in 2002, followed by other ground and balloon-borne experiments (Kovac et al 2002;Readhead et al 2004;Wu et al 2007; Montroy et al 2006;QUaD collaboration: Pryke et al 2009) covering a few percent of the sky. These detections are complemented by the Wmap satellite observations of the whole sky (Page et al 2007).…”

Section: Introductionmentioning

confidence: 98%

Planckpre-launch status: High Frequency Instrument polarization calibration

Rosset

Tristram

Ponthieu

et al. 2010

A&A

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The High Frequency Instrument of Planck will map the entire sky in the millimeter and sub-millimeter domain from 100 to 857 GHz with unprecedented sensitivity to polarization (ΔP/T cmb ∼ 4 × 10 −6 for P either Q or U and T cmb 2.7 K) at 100, 143, 217 and 353 GHz. It will lead to major improvements in our understanding of the cosmic microwave background anisotropies and polarized foreground signals. Planck will make high resolution measurements of the E-mode spectrum (up to ∼ 1500) and will also play a prominent role in the search for the faint imprint of primordial gravitational waves on the CMB polarization. This paper addresses the effects of calibration of both temperature (gain) and polarization (polarization efficiency and detector orientation) on polarization measurements. The specific requirements on the polarization parameters of the instrument are set and we report on their pre-flight measurement on HFI bolometers. We present a semi-analytical method that exactly accounts for the scanning strategy of the instrument as well as the combination of different detectors. We use this method to propagate errors through to the CMB angular power spectra in the particular case of Planck-HFI, and to derive constraints on polarization parameters. We show that in order to limit the systematic error to 10% of the cosmic variance of the E-mode power spectrum, uncertainties in gain, polarization efficiency and detector orientation must be below 0.15%, 0.3% and 1• respectively. Pre-launch ground measurements reported in this paper already fulfill these requirements.

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Section: Introductionmentioning

confidence: 98%

Planckpre-launch status: High Frequency Instrument polarization calibration

Rosset

Tristram

Ponthieu

et al. 2010

A&A

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“…After the initial detection of the much stronger E-mode polarization (Kovac et al 2002), steady improvements have been made in measuring the E-mode signal by a number of experiments (Leitch et al 2005;Barkats et al 2005;Readhead et al 2004;Montroy et al 2006;Sievers et al 2007;Page et al 2007;Wu et al 2007;Ade et al 2008;Bischoff et al 2008;Nolta et al 2009). Recently, a major step forward in precision CMB polarization measurements was achieved with the highsignificance detection of a characteristic series of acoustic peaks in the E-mode polarization power spectrum with our initial analysis of the final QUaD data set (Pryke et al 2009, hereafter Paper II).…”

Section: Introductionmentioning

confidence: 99%

IMPROVED MEASUREMENTS OF THE TEMPERATURE AND POLARIZATION OF THE COSMIC MICROWAVE BACKGROUND FROM QUaD

Brown

Ade

Bock

et al. 2009

ApJ

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241

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We present an improved analysis of the final data set from the QUaD experiment. Using an improved technique to remove ground contamination, we double the effective sky area and hence increase the precision of our cosmic microwave background (CMB) power spectrum measurements by ∼30% versus that previously reported. In addition, we have improved our modeling of the instrument beams and have reduced our absolute calibration uncertainty from 5% to 3.5% in temperature. The robustness of our results is confirmed through extensive jackknife tests, and by way of the agreement that we find between our two fully independent analysis pipelines. For the standard six-parameter ΛCDM model, the addition of QUaD data marginally improves the constraints on a number of cosmological parameters over those obtained from the WMAP experiment alone. The impact of QUaD data is significantly greater for a model extended to include either a running in the scalar spectral index, or a possible tensor component, or both. Adding both the QUaD data and the results from the Arcminute Cosmology Bolometer Array Receiver experiment, the uncertainty in the spectral index running is reduced by ∼25% compared to WMAP alone, while the upper limit on the tensor-to-scalar ratio is reduced from r < 0.48 to r < 0.33 (95% c.l.). This is the strongest limit on tensors to date from the CMB alone. We also use our polarization measurements to place constraints on parity-violating interactions to the surface of last scattering, constraining the energy scale of Lorentz violating interactions to < 1.5×10 −43 GeV (68% c.l.). Finally, we place a robust upper limit on the strength of the lensing B-mode signal. Assuming a single flat band power between = 200 and = 2000, we constrain the amplitude of B-modes to be < 0.57 μK 2 (95% c.l.).

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“…Since then, in addition to a further measurement by the DASI experiment (Leitch et al 2005), E modes measurements have been made with the CBI (Readhead et al 2004), CAPMAP (Bischoff et al 2008), BOOMERanG (Montroy et al 2006), Wmap (Page et al 2007), MAXIPol (Wu et al 2007), QUaD (Ade et al 2008) and Bicep (Chiang et al 2010). With these measurements, the C EE angular power spectrum has now been detected over a wide range of angular scales (30 1000).…”

Section: Introductionmentioning

confidence: 99%

Measurement of the Crab nebula polarization at 90 GHz as a calibrator for CMB experiments

Aumont

Conversi

Thum

et al. 2010

A&A

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Context. CMB experiments aiming at a precise measurement of the CMB polarization, such as the Planck satellite, need a strong polarized absolute calibrator on the sky to accurately set the detectors polarization angle and the cross-polarization leakage. As the most intense polarized source in the microwave sky at angular scales of few arcminutes, the Crab nebula will be used for this purpose. Aims. Our goal was to measure the Crab nebula polarization characteristics at 90 GHz with unprecedented precision. Methods. The observations were carried out with the IRAM 30 m telescope employing the correlation polarimeter XPOL and using two orthogonally polarized receivers. Results. We processed the Stokes I, Q, and U maps from our observations in order to compute the polarization angle and linear polarization fraction. The first is almost constant in the region of maximum emission in polarization with a mean value of α Sky = 152.1 ± 0.3 • in equatorial coordinates, and the second is found to reach a maximum of Π = 30% for the most polarized pixels. We find that a CMB experiment having a 5 arcmin circular beam will see a mean polarization angle of α Sky = 149.9 ± 0.2 • and a mean polarization fraction of Π = 8.8 ± 0.2%.

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MAXIPOL: Data Analysis and Results

Cited by 57 publications

References 27 publications

Planckpre-launch status: High Frequency Instrument polarization calibration

Planckpre-launch status: High Frequency Instrument polarization calibration

IMPROVED MEASUREMENTS OF THE TEMPERATURE AND POLARIZATION OF THE COSMIC MICROWAVE BACKGROUND FROM QUaD

Measurement of the Crab nebula polarization at 90 GHz as a calibrator for CMB experiments

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