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Proceedings Paper

The status of the QUIJOTE multifrequency instrument
Author(s): R. J. Hoyland; M. Aguiar-González; B. Aja; J. Ariño; E. Artal; R. B. Barreiro; E. J. Blackhurst; J. Cagigas; J. L. Cano de Diego; F. J. Casas; R. J. Davis; C. Dickinson; B. E. Arriaga; R. Fernandez-Cobos; L. de la Fuente; R. Génova-Santos; A. Gómez; C. Gomez; F. Gómez-Reñasco; K. Grainge; S. Harper; D. Herran; J. M. Herreros; G. A. Herrera; M. P. Hobson; A. N. Lasenby; M. Lopez-Caniego; C. López-Caraballo; B. Maffei; E. Martinez-Gonzalez; M. McCulloch; S. Melhuish; A. Mediavilla; G. Murga; D. Ortiz; L. Piccirillo; G. Pisano; R. Rebolo-López; J. A. Rubiño-Martin; J. Luis Ruiz; V. Sanchez de la Rosa; R. Sanquirce; A. Vega-Moreno; P. Vielva; T. Viera-Curbelo; E. Villa; A. Vizcargüenaga; R. A. Watson
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Paper Abstract

The QUIJOTE-CMB project has been described in previous publications. Here we present the current status of the QUIJOTE multi-frequency instrument (MFI) with five separate polarimeters (providing 5 independent sky pixels): two which operate at 10-14 GHz, two which operate at 16-20 GHz, and a central polarimeter at 30 GHz. The optical arrangement includes 5 conical corrugated feedhorns staring into a dual reflector crossed-draconian system, which provides optimal cross-polarization properties (designed to be < −35 dB) and symmetric beams. Each horn feeds a novel cryogenic on-axis rotating polar modulator which can rotate at a speed of up to 1 Hz. The science driver for this first instrument is the characterization of the galactic emission. The polarimeters use the polar modulator to derive linear polar parameters Q, U and I and switch out various systematics. The detection system provides optimum sensitivity through 2 correlated and 2 total power channels. The system is calibrated using bright polarized celestial sources and through a secondary calibration source and antenna. The acquisition system, telescope control and housekeeping are all linked through a real-time gigabit Ethernet network. All communication, power and helium gas are passed through a central rotary joint. The time stamp is synchronized to a GPS time signal. The acquisition software is based on PLCs written in Beckhoffs TwinCat and ethercat. The user interface is written in LABVIEW. The status of the QUIJOTE MFI will be presented including pre-commissioning results and laboratory testing.

Paper Details

Date Published: 5 October 2012
PDF: 15 pages
Proc. SPIE 8452, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI, 845233 (5 October 2012); doi: 10.1117/12.925349
Show Author Affiliations
R. J. Hoyland, Instituto de Astrofísica de Canarias (Spain)
M. Aguiar-González, Instituto de Astrofísica de Canarias (Spain)
B. Aja, Univ. de Cantabria (Spain)
J. Ariño, IDOM (Spain)
E. Artal, Univ. de Cantabria (Spain)
R. B. Barreiro, Univ. de Cantabria (Spain)
E. J. Blackhurst, The Univ. of Manchester (United Kingdom)
J. Cagigas, Univ. de Cantabria (Spain)
J. L. Cano de Diego, Univ. de Cantabria (Spain)
F. J. Casas, Univ. de Cantabria (Spain)
R. J. Davis, The Univ. of Manchester (United Kingdom)
C. Dickinson, The Univ. of Manchester (United Kingdom)
B. E. Arriaga, IDOM (Spain)
R. Fernandez-Cobos, Univ. de Cantabria (Spain)
L. de la Fuente, Univ. de Cantabria (Spain)
R. Génova-Santos, Instituto de Astrofísica de Canarias (Spain)
A. Gómez, IDOM (Spain)
C. Gomez, IDOM (Spain)
F. Gómez-Reñasco, Instituto de Astrofísica de Canarias (Spain)
K. Grainge, Univ. of Cambridge (United Kingdom)
S. Harper, The Univ. of Manchester (United Kingdom)
D. Herran, Univ. de Cantabria (Spain)
J. M. Herreros, Instituto de Astrofísica de Canarias (Spain)
G. A. Herrera, Consultant (Spain)
M. P. Hobson, Univ. of Cambridge (United Kingdom)
A. N. Lasenby, Univ. of Cambridge (United Kingdom)
M. Lopez-Caniego, Univ. de Cantabria (Spain)
C. López-Caraballo, Instituto de Astrofísica de Canarias (Spain)
B. Maffei, The Univ. of Manchester (United Kingdom)
E. Martinez-Gonzalez, Univ. de Cantabria (Spain)
M. McCulloch, The Univ. of Manchester (United Kingdom)
S. Melhuish, The Univ. of Manchester (United Kingdom)
A. Mediavilla, Univ. de Cantabria (Spain)
G. Murga, IDOM (Spain)
D. Ortiz, Univ. de Cantabria (Spain)
L. Piccirillo, The Univ. of Manchester (United Kingdom)
G. Pisano, The Univ. of Manchester (United Kingdom)
R. Rebolo-López, Instituto de Astrofísica de Canarias (Spain)
J. A. Rubiño-Martin, Instituto de Astrofísica de Canarias (Spain)
J. Luis Ruiz, IDOM (Spain)
V. Sanchez de la Rosa, Instituto de Astrofísica de Canarias (Spain)
R. Sanquirce, IDOM (Spain)
A. Vega-Moreno, Instituto de Astrofísica de Canarias (Spain)
P. Vielva, Univ. de Cantabria (Spain)
T. Viera-Curbelo, Instituto de Astrofísica de Canarias (Spain)
E. Villa, Univ. de Cantabria (Spain)
A. Vizcargüenaga, IDOM (Spain)
R. A. Watson, The Univ. of Manchester (United Kingdom)


Published in SPIE Proceedings Vol. 8452:
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI
Wayne S. Holland, Editor(s)

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