- #1
- 24,775
- 792
http://arxiv.org/abs/1010.0645
Cryogenic, 400 horns, Antarctica, detector plate at 100 milliKelvin
"One of the major challenges of modern cosmology is the detection of B-mode polarization anisotropies in the CMB. These originate from tensor fluctuations of the metric produced during the inflationary phase. Their detection would therefore constitute a major step towards understanding the primordial Universe. The expected level of these anisotropies is however so small that it requires a new generation of instruments with high sensitivity and extremely good control of systematic effects. We propose the QUBIC instrument based on the novel concept of bolometric interferometry..."
See the schematic diagram of the device, Figure 1, on page 3. Much of the device is enclosed in a crygenic box at 4 Kelvin. The imaging plate is at lower temperature (100 milliKelvin.)
"We plan to install a first QUBIC module at the Franco-Italian Concordia station in Dome C, Antarctica within two years. The first modulewill consist of an array of 400 horns operating at 150 GHz with 25% bandwidth and 14 degree (FWHM) primary beams. The optical combiner will have a focal length of ∼30cm and each of the two focal planes will be comprised of arrays of 30x30 bare TES bolometers of 3mm size. The full instrument will include modules at three different frequencies (90,150,220 GHz) and will constrain a tensor to scalar ratio of 0.01 in one year of data taking at the 90% confidence level..."
Cryogenic, 400 horns, Antarctica, detector plate at 100 milliKelvin
"One of the major challenges of modern cosmology is the detection of B-mode polarization anisotropies in the CMB. These originate from tensor fluctuations of the metric produced during the inflationary phase. Their detection would therefore constitute a major step towards understanding the primordial Universe. The expected level of these anisotropies is however so small that it requires a new generation of instruments with high sensitivity and extremely good control of systematic effects. We propose the QUBIC instrument based on the novel concept of bolometric interferometry..."
See the schematic diagram of the device, Figure 1, on page 3. Much of the device is enclosed in a crygenic box at 4 Kelvin. The imaging plate is at lower temperature (100 milliKelvin.)
"We plan to install a first QUBIC module at the Franco-Italian Concordia station in Dome C, Antarctica within two years. The first modulewill consist of an array of 400 horns operating at 150 GHz with 25% bandwidth and 14 degree (FWHM) primary beams. The optical combiner will have a focal length of ∼30cm and each of the two focal planes will be comprised of arrays of 30x30 bare TES bolometers of 3mm size. The full instrument will include modules at three different frequencies (90,150,220 GHz) and will constrain a tensor to scalar ratio of 0.01 in one year of data taking at the 90% confidence level..."