A Measurement of the Polarization‐Temperature Angular Cross‐Power Spectrum of the Cosmic Microwave Background from the 2003 Flight of BOOMERANG

Piacentini, F.; Ade, Peter A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Cabella, P.; Contaldi, C. R.; Crill, B. P.; Bernardis, P. de; Gasperis, G. de; Oliveira-Costa, A. de; Troia, G. De; Stefano, Giuseppe Di; Hivon, E.; Jaffe, A. H.; Kisner, T. S.; Jones, W. C.; Lange, A. E.; Masi, S.; Mauskopf, Philip Daniel; MacTavish, C. J.; Melchiorri, A.; Montroy, T. E.; Natoli, P.; Netterfield, C. B.; Pascale, Enzo; Pogosyan, D.; Polenta, G.; Prunet, S.; Ricciardi, S.; Romeo, G.; Ruhl, J. E.; Santini, P.; Tegmark, Max; Veneziani, M.; Vittorio, N.

doi:10.1086/505557

Cited by 130 publications

(79 citation statements)

References 37 publications

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“…Even more recently, the polarization of the CMB has been detected [4] and begun to be mapped on small scales [5] and detected through its cross-correlation with the temperature [6,7]. The small-scale results are consistent with expectations based on models that fit the temperature results, and the results from three years of WMAP (Wilkinson Microwave Anisotropy Probe) indicate that reionization likely occurred at a redshift z ∼ 10 [8].…”

Section: The Cosmic Microwave Background and Inflationsupporting

confidence: 53%

Dark Matter and Dark Energy

Frampton¹

2009

Did Time Begin? Will Time End?

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This is a short review, aimed at a general audience, of several current subjects of research in cosmology. The topics discussed include the cosmic microwave background (CMB), with particular emphasis on its relevance for testing inflation; dark matter, with a brief review of astrophysical evidence and more emphasis on particle candidates; and cosmic acceleration and some of the ideas that have been put forward to explain it. A glossary of technical terms and acronyms is provided.

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Section: The Cosmic Microwave Background and Inflationsupporting

confidence: 53%

Dark Matter and Dark Energy

Frampton¹

2009

Did Time Begin? Will Time End?

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“…Similarly, the method of polarimetry employed by the HFI was demonstrated by the BOOMERANG experiment (Montroy et al 2006;Piacentini et al 2006;Jones et al 2006). The HFI itself was extensively tested on the ground during the calibration campaigns (Pajot et al 2010) at IAS in Orsay and CSL at Liège.…”

Section: Designmentioning

confidence: 96%

Planckearly results. IV. First assessment of the High Frequency Instrument in-flight performance

Ade¹,

Aghanim²,

Ansari³

et al. 2011

A&A

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139

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The Planck High Frequency Instrument (HFI) is designed to measure the temperature and polarization anisotropies of the cosmic microwave background and Galactic foregrounds in six ∼30% bands centered at 100, 143, 217, 353, 545, and 857 GHz at an angular resolution of 10 (100 GHz), 7 (143 GHz), and 5 (217 GHz and higher). HFI has been operating flawlessly since launch on 14 May 2009, with the bolometers reaching 100 mK the first week of July. The settings of the readout electronics, including bolometer bias currents, that optimize HFI's noise performance on orbit are nearly the same as the ones chosen during ground testing. Observations of Mars, Jupiter, and Saturn have confirmed that the optical beams and the time responses of the detection chains are in good agreement with the predictions of physical optics modeling and pre-launch measurements. The Detectors suffer from a high flux of cosmic rays due to historically low levels of solar activity. As a result of the redundancy of Planck's observation strategy, the removal of a few percent of data contaminated by glitches does not significantly affect the instrumental sensitivity. The cosmic ray flux represents a significant and variable heat load on the sub-Kelvin stage. Temporal variation and the inhomogeneous distribution of the flux results in thermal fluctuations that are a probable source of low frequency noise. The removal of systematic effects in the time ordered data provides a signal with an average noise equivalent power that is 70% of the goal in the 0.6−2.5 Hz range. This is slightly higher than was achieved during the pre-launch characterization but better than predicted in the early phases of the project. The improvement over the goal is a result of the low level of instrumental background loading achieved by the optical and thermal design of the HFI.

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“…From the SDSS we also include the recent measurement of the baryon acoustic oscillation feature in the 2-point correlation function [13]. Finally, we include the precision measurements of the cosmic microwave background anisotropy from the WMAP experiment [4,14,15], as well as the smaller-scale measurement by the BOOMERANG experiment [16][17][18].…”

Section: Cosmological Data and Likelihood Analysismentioning

confidence: 99%

Neutrino masses and cosmic radiation density: combined analysis

Hannestad

Raffelt

2006

J. Cosmol. Astropart. Phys.

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Abstract. We determine the range of neutrino masses and cosmic radiation content allowed by the most recent CMB and large-scale structure data. In contrast to other recent works, we vary these parameters simultaneously and provide likelihood contours in the two-dimensional parameter space of N eff , the usual effective number of neutrino species measuring the radiation density, and m ν . The allowed range of m ν and N eff has shrunk significantly compared to previous studies. The previous degeneracy between these parameters has disappeared, largely thanks to the baryon acoustic oscillation data. The likelihood contours differ significantly if m ν resides in a single species instead of the standard case of being equally distributed among all flavors. For m ν = 0 we find 2.7 < N eff < 4.6 at 95% CL while m ν < 0.62 eV at 95% CL for the standard radiation content.

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A Measurement of the Polarization‐Temperature Angular Cross‐Power Spectrum of the Cosmic Microwave Background from the 2003 Flight of BOOMERANG

Cited by 130 publications

References 37 publications

Dark Matter and Dark Energy

Dark Matter and Dark Energy

Planckearly results. IV. First assessment of the High Frequency Instrument in-flight performance

Neutrino masses and cosmic radiation density: combined analysis

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