SWIPE: a bolometric polarimeter for the Large-Scale Polarization Explorer

被引：25

作者：

de Bernardis, P. ^{[1
]}

Aiola, S. ^{[1
]}

Amico, G. ^{[1
]}

Battistelli, E. ^{[1
]}

Coppolecchia, A. ^{[1
]}

Cruciani, A. ^{[1
]}

D' Addabbo, A. ^{[1
]}

D' Alessandro, G. ^{[1
]}

De Gregori, S. ^{[1
]}

De Petris, M. ^{[1
]}

Goldie, D.

Gualtieri, R. ^{[1
]}

Haynes, V.

Lamagna, L. ^{[1
]}

Maffei, B.

Masi, S. ^{[1
]}

Nati, F. ^{[1
]}

Ng, M. Wah

Pagano, L. ^{[1
]}

Piacentini, F. ^{[1
]}

Piccirillo, L.

Pisano, G.

Romeo, G.

Salatino, M. ^{[1
]}

Schillaci, A. ^{[1
]}

Tommasi, E.

Withington, S.

机构：

[1] Univ Roma La Sapienza, Dipartimento Fis, Ple A Moro 2, I-00185 Rome, Italy

来源：

MILLIMETER, SUBMILLIMETER, AND FAR-INFRARED DETECTORS AND INSTRUMENTATION FOR ASTRONOMY VI | 2012年 / 8452卷

关键词：

Cosmic Microwave Backgorund; Polarization; Bolometer; Overmoded Microwave Optics; HALF-WAVE PLATE; PHOTOLITHOGRAPHIC POLARIZER; MILLIMETER; EMISSION;

D O I：

10.1117/12.926569

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The balloon-borne LSPE mission is optimized to measure the linear polarization of the Cosmic Microwave Background at large angular scales. The Short Wavelength Instrument for the Polarization Explorer (SWIPE) is composed of 3 arrays of multi-mode bolometers cooled at 0.3K, with optical components and filters cryogenically cooled below 4K to reduce the background on the detectors. Polarimetry is achieved by means of large rotating half-wave plates and wire-grid polarizers in front of the arrays. The polarization modulator is the first component of the optical chain, reducing significantly the effect of instrumental polarization. In SWIPE we trade angular resolution for sensitivity. The diameter of the entrance pupil of the refractive telescope is 45 cm, while the field optics is optimized to collect tens of modes for each detector, thus boosting the absorbed power. This approach results in a FWHM resolution of 1.8, 1.5, 1.2 degrees at 95, 145, 245 GHz respectively. The expected performance of the three channels is limited by photon noise, resulting in a final sensitivity around 0.1-0.2 mu K per beam, for a 13 days survey covering 25% of the sky.

引用

页数：11

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