Other
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21820701c&link_type=abstract
American Astronomical Society, AAS Meeting #218, #207.01; Bulletin of the American Astronomical Society, Vol. 43, 2011
Other
Scientific paper
The Q/U Imaging ExperimenT (QUIET) is designed to detect the CMB B-mode polarization induced by primordial gravitational waves created during the inflation era. We use polarimeters based on coherent receiver technology with HEMT (High Electron Mobility Transistor) amplifiers. We developed two of the most sensitive polarimeter arrays today; one is composed of 19 modules for the Q-band (43GHz) and the other is composed of 90 modules for the W-band (95GHz). QUIET is located on the Chajnantor plateau in the Atacama desert in northern Chile at an altitude of 5,080m, where we collected over 10,000 hours of data from 2008 October to 2010 December.
In this dissertation talk, I will discuss the Q-band analysis and results completed with the pseudo-Cl framework, which is one of the two analysis pipelines we developed. The analysis, including calibration, data selection and systematic error estimation, was validated and optimized with suites of null tests before the power spectra were obtained.
From the Q-band data, we obtained the EE, BB and EB power spectra in the multipole range from 25 to 475. The E-mode signals are detected with more than 6 sigma significance in the range of the first peak. For the B-mode spectrum, we placed an upper limit on the tensor-to-scalar ratio of r<2.2 at the 95% confidence level. We also detect the polarized foreground signal at the lowest multipole bin of the E-mode spectrum with 3 sigma significance, which is consistent with the Galactic synchrotron emission. All the systematic errors are much lower than the statistical errors. In particular, the contaminations to the primordial B-mode spectrum, at multipoles below 100, are lower than the level of r=0.1.
Chinone Yuji
QUIET Collaboration
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