QUIJOTE (Q-U-I JOint TEnerife) is an experiment designed to achieve CMB B-mode polarization detection and sensitive enough to detect a primordial gravitational-wave component if the B-mode amplitude is larger than r = 0.05. It consists in two telescopes and three instruments observing in the frequency range 10-42 GHz installed at the Teide Observatory in the Canary Islands, Spain. The observing strategy includes three raster scan deep integration fields for cosmology, a nominal wide survey covering the Northen Sky and specific raster scan deep integration observations in regions of specific interest. The main goals of the project are presented and the first scientific results obtained with the first instrument are reviewed.

We present the current status of the QUIJOTE (Q-U-I JOint TEnerife) experiment, a new polarimeter with the aim of characterizing the polarization of the Cosmic Microwave Background, and other galactic or extra-galactic physical processes that emit in microwaves in the frequency range 10–42 GHz, and at large angular scales (around 1 degree resolution). The experiment has been designed to reach the required sensitivity to detect a primordial gravitational wave component in the CMB, provided its tensor-to-scalar ratio is larger than r ∼ 0.05. The project consists of two telescopes and three instruments which will survey a large sky area from the Teide Observatory to provide I, Q and U maps of high sensitivity. The first QUIJOTE instrument, known as Multi-Frequency Instrument (MFI), has been surveying the northern sky in four individual frequencies between 10 and 20 GHz since November 2012, providing data with an average sensitivity of 80 µK beam−1 in Q and U in a region of 20, 000 square-degrees. The second instrument, or Thirty-GHz Instrument (TGI), is currently undergoing the commissioning phase, and the third instrument, or Forty-GHz Instrument (FGI), is in the final fabrication phase. Finally, we describe the first scientific results obtained with the MFI. Some specific regions, mainly along the Galactic plane, have been surveyed to a deeper depth, reaching sensitivities of around 40 µK beam−1. We present new upper limits on the polarization of the anomalous dust emission, resulting from these data, in the Perseus molecular complex and in the W43 molecular complex.

The QUIJOTE Experiment (Q-U-I JOint TEnerife) is a combined operation of two telescopes and three instruments working in the microwave band to measure the polarization of the Cosmic Microwave Background (CMB) from the northern hemisphere, at medium and large angular scales. The experiment is located at the Teide Observatory in Tenerife, one of the seven Canary Islands (Spain). The project is a consortium maintained by several institutions: the Instituto de Astrofísica de Canarias (IAC), the Instituto de Física de Cantabria (IFCA), the Communications Engineering Department (DICOM) at Universidad de Cantabria, and the Universities of Manchester and Cambridge. The consortium is led by the IAC.

The QUIJOTE (Q-U-I JOint Tenerife) CMB Experiment is operating at the Teide Observatory with the aim of characterizing the polarization of the CMB and other processes of Galactic and extragalactic emission in the frequency range of 10–40GHz and at large and medium angular scales. The QUIJOTE CMB experiment consists of two telescopes installed inside a single enclosure, and three instruments, the MFI (multi-frequency 10–30GHz), the TGI (26–36 GHz) and the FGI (37–47 GHz). The first QUIJOTE telescope and the MFI instrument have been in operation at the Observatory since November 2012. In this poster we present the TGI cryostat and optomechanics status, including their design, MAIT, and thermal clamp developments.

The QUIJOTE (Q-U-I JOint TEnerife) experiment is a scientific collaboration, led by the Instituto de Astrofisica de Canarias (IAC), with the aim of measuring the polarization of the Cosmic Microwave Background (CMB) in the frequency range 10-40 GHz and at large angular scales (around 1 Alpha degrees). The project is composed of 2 telescopes and 3 instruments, located in Teide Observatory (Tenerife, Spain). Idom's contribution for this project is divided in two phases.Phase I consisted on the design, assembly and factory testing of the first telescope (2008), the integration and functional tests for the 5 polarimeters of the first instrument (2009), and the design and construction supervision of the building which protects both telescopes (2009), including the installation and commissioning of the mechanism for domes apertures.Phase II comprised the design, factory assembly & testing, transport and final commissioning on site of the second telescope, which finished in January 2015. The optical design of both telescopes should allow them to reach up to 200 GHz. The required opto-mechanical performance was checked under nominal conditions, reaching a pointing and tracking accuracy lower than 5 arcsec in both axes, 8 times better than specified. Particular inspections and tests were carried out for critical systems, as the rotary joint that transmits fluid, power and signal to the rotary elements, or for the safety system to ensure personnel and hardware protection under emergency conditions.This paper contains a comprehensive description of the power electronics and acquisition/ control design required for safely operation under nominal and emergency conditions, as well as a detailed description of the factory and observatory tests required for the final acceptance of the telescope

QUIJOTE (Q-U-I JOint TEnerife) is a new polarimeter aimed to characterize the polarization of the Cosmic Microwave Background and other Galactic and extragalactic signals at medium and large angular scales in the frequency range 10--40 GHz. The multi-frequency (10--20 GHz) instrument, mounted on the first QUIJOTE telescope, saw first light on November 2012 from the Teide Observatory (2400 m a.s.l). During 2014 the second telescope has been installed at this observatory. A second instrument at 30 GHz will be ready for commissioning at this telescope during summer 2015, and a third additional instrument at 40 GHz is now being developed. These instruments will have nominal sensitivities to detect the B-mode polarization due to the primordial gravitational-wave component if the tensor-to-scalar ratio is larger than r=0.05.

The QUIJOTE (Q-U-I JOint Tenerife) CMB Experiment is designed to observe the polarization of the Cosmic Microwave Background and other Galactic and extragalactic signals at medium and large angular scales in the frequency range of 10-40 GHz. The first of the two QUIJOTE telescopes and the multi-frequency (10-20 GHz) instrument have been in operation since November 2012. In 2014 a second telescope and a new instrument at 30GHz will be ready for commissioning, and an additional instrument at 40 GHz is in its final design stages. After three years of effective observations, the data obtained by these telescopes and instruments will have the required sensitivity to detect a primordial gravitational-wave component if the tensor-to-scalar ratio is larger than r = 0.05. At the moment, we have completed half of the wide Galactic survey with the multi-frequency instrument covering 18 000 square degrees of the Northern hemisphere. When we finish this survey in early 2014, we shall have reached approximately 14μK per one degree beam at 11, 13, 17 and 19 GHz, in both Q and U.

The QUIJOTE-CMB experiment (Q-U-I JOint TEnerife CMB experiment) is an ambitious project to obtain polarization measurements of the sky microwave emission in the 10 to 47 GHz range. With this aim, a pair of 2,5μm telescopes and three instruments are being sited at the Teide Observatory, in Tenerife (Canary Islands, Spain). The first telescope and the first instrument (the MFI: Multi Frequency Instrument) are both already operating in the band from 10 to 20 GHz, since November 2012. The second telescope and the second instrument (TGI: Thirty GHz instrument) is planned to be in commissioning by the end of summer 2014, covering the range of 26 to 36 GHz. After that, a third instrument named FGI (Forty GHz instrument) will be designed and manufactured to complete the sky survey in the frequency range from 37 to 47 GHz. In this paper we present an overview of the whole project current status, from the technical point of view.

The QUIJOTE TGI instrument is currently being assembled and tested at the IAC in Spain. The TGI is a 31 pixel 26-36 GHz polarimeter array designed to be mounted at the focus of the second QUIJOTE telescope. This follows a first telescope and multi-frequency instrument that have now been observing almost 2 years. The polarimeter design is based on the QUIET polarimeter scheme but with the addition of an extra 90 degrees phase switch which allows for quasiinstantaneous complete QUI measurements through each detector. The advantage of this is a reduction in the systematics associated with differencing two independent radiometer channels. The polarimeters are split into a cold front end and a warm back end. The back end is a highly integrated design by engineers at DICOM. It is also sufficiently modular for testing purposes. In this presentation the high quality wide band components used in the optical design (also designed in DICOM) are presented as well as the novel cryogenic modular design. Each polarimeter chain is accessible individually and can be removed from the cryostat and replaced without having to move the remaining pixels. The optical components work over the complete Ka band showing excellent performance. Results from the sub unit measurements are presented and also a description of the novel calibration technique that allows for bandpass measurement and polar alignment. Terrestrial Calibration for this instrument is very important and will be carried out at three points in the commissioning phase: in the laboratory, at the telescope site and finally a reduce set of calibrations will be carried out on the telescope before measurements of extraterrestrial sources begin. The telescope pointing model is known to be more precise than the expected calibration precision so no further significant error will be added through the telescope optics. The integrated back-end components are presented showing the overall arrangement for mounting on the cryostat. Many of the microwave circuits are in-house designs with performances that go beyond commercially available products. Individual component performance is be presented showing for each of the sub modules

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.

The QUIJOTE (Q-U-I JOint Tenerife) CMB Experiment will operate at the Teide Observatory with the aim of characterizing the polarisation of the CMB and other processes of Galactic and extragalactic emission in the frequency range of 10-40GHz and at large and medium angular scales. The first of the two QUIJOTE telescopes and the first multi-frequency (10-30 GHz) instrument are already built and have been tested in the laboratory. QUIJOTE-CMB will be a valuable complement at low frequencies for the Planck mission, and will have the required sensitivity to detect a primordial gravitational-wave component if the tensor-to-scalar ratio is larger than r = 0.05.

The Twelfth Marcel Grossmann Meeting, pp. 2156-2165 (2012) No AccessTHE QUIJOTE CMB EXPERIMENT: PROGRESS REPORTRICARDO GÉNOVA-SANTOS, R. REBOLO, J.A. RUBIÑO-MARTÍN, M. AGUIAR, F. GÓMEZ-REÑASCO, J.M. HERREROS, S. HILDEBRANDT, R. HOYLAND, C. LÓPEZ-CARABALLO, R. RODRÍGUEZ, M. TUCCI, E. MARTÍNEZ-GONZÁLEZ, R.B. BARREIRO, F.J. CASAS, R. FERNÁNDEZ-COBOS, D. HERRANZ, M. LÓPEZ-CANIEGO, P. VIELVA, E. ARTAL, B. AJA, J.L. CANO, L. DE LA FUENTE, A. MEDIAVILLA, J.P. PASCUAL, E. VILLA, L. PICCIRILLO, R. BATTYE, R. DAVIES, R. DAVIS, C. DICKINSON, B. MAFFEI, G. PISANO, R.A. WATSON, M. BROWN, A. CHALLINOR, K. GRAINGE, M. HOBSON, A. LASENBY, R. SAUNDERS, P. SCOTT, J. ARIÑO, B. ETXEITA, A. GÓMEZ, C. GÓMEZ, G. MURGA, J. PAN, R. SANQUIRCE and A. VIZCARGÜENAGARICARDO GÉNOVA-SANTOSInstituto de Astrofisica de Canarias, C/Via Láactea, s/n, 38200 La Laguna, Tenerife, Spain, R. REBOLOInstituto de Astrofisica de Canarias, C/Via Láactea, s/n, 38200 La Laguna, Tenerife, Spain, J.A. RUBIÑO-MARTÍNInstituto de Astrofisica de Canarias, C/Via Láactea, s/n, 38200 La Laguna, Tenerife, Spain, M. AGUIARInstituto de Astrofisica de Canarias, C/Via Láactea, s/n, 38200 La Laguna, Tenerife, Spain, F. GÓMEZ-REÑASCOInstituto de Astrofisica de Canarias, C/Via Láactea, s/n, 38200 La Laguna, Tenerife, Spain, J.M. HERREROSInstituto de Astrofisica de Canarias, C/Via Láactea, s/n, 38200 La Laguna, Tenerife, Spain, S. HILDEBRANDTInstituto de Astrofisica de Canarias, C/Via Láactea, s/n, 38200 La Laguna, Tenerife, Spain, R. HOYLANDInstituto de Astrofisica de Canarias, C/Via Láactea, s/n, 38200 La Laguna, Tenerife, Spain, C. LÓPEZ-CARABALLOInstituto de Astrofisica de Canarias, C/Via Láactea, s/n, 38200 La Laguna, Tenerife, Spain, R. RODRÍGUEZInstituto de Astrofisica de Canarias, C/Via Láactea, s/n, 38200 La Laguna, Tenerife, Spain, M. TUCCIInstituto de Astrofisica de Canarias, C/Via Láactea, s/n, 38200 La Laguna, Tenerife, Spain, E. MARTÍNEZ-GONZÁLEZInstituto de Fisica de Cantabria, CSIC-Univ. de Cantabria, Avda. los Castros, s/n, 39005 Santander, Spain, R.B. BARREIROInstituto de Fisica de Cantabria, CSIC-Univ. de Cantabria, Avda. los Castros, s/n, 39005 Santander, Spain, F.J. CASASInstituto de Fisica de Cantabria, CSIC-Univ. de Cantabria, Avda. los Castros, s/n, 39005 Santander, Spain, R. FERNÁNDEZ-COBOSInstituto de Fisica de Cantabria, CSIC-Univ. de Cantabria, Avda. los Castros, s/n, 39005 Santander, Spain, D. HERRANZInstituto de Fisica de Cantabria, CSIC-Univ. de Cantabria, Avda. los Castros, s/n, 39005 Santander, Spain, M. LÓPEZ-CANIEGOInstituto de Fisica de Cantabria, CSIC-Univ. de Cantabria, Avda. los Castros, s/n, 39005 Santander, Spain, P. VIELVAInstituto de Fisica de Cantabria, CSIC-Univ. de Cantabria, Avda. los Castros, s/n, 39005 Santander, Spain, E. ARTALDepartamento de Ingenieria de COMunicaciones, Laboratorios de I+D de Telecomunicaciones, Plaza de la Ciencia s/n, E-39005 Santander, Spain, B. AJADepartamento de Ingenieria de COMunicaciones, Laboratorios de I+D de Telecomunicaciones, Plaza de la Ciencia s/n, E-39005 Santander, Spain, J.L. CANODepartamento de Ingenieria de COMunicaciones, Laboratorios de I+D de Telecomunicaciones, Plaza de la Ciencia s/n, E-39005 Santander, Spain, L. DE LA FUENTEDepartamento de Ingenieria de COMunicaciones, Laboratorios de I+D de Telecomunicaciones, Plaza de la Ciencia s/n, E-39005 Santander, Spain, A. MEDIAVILLADepartamento de Ingenieria de COMunicaciones, Laboratorios de I+D de Telecomunicaciones, Plaza de la Ciencia s/n, E-39005 Santander, Spain, J.P. PASCUALDepartamento de Ingenieria de COMunicaciones, Laboratorios de I+D de Telecomunicaciones, Plaza de la Ciencia s/n, E-39005 Santander, Spain, E. VILLADepartamento de Ingenieria de COMunicaciones, Laboratorios de I+D de Telecomunicaciones, Plaza de la Ciencia s/n, E-39005 Santander, Spain, L. PICCIRILLOJodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK, R. BATTYEJodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK, R. DAVIESJodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK, R. DAVISJodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK, C. DICKINSONJodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK, B. MAFFEIJodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK, G. PISANOJodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK, R.A. WATSONJodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK, M. BROWNAstrophysics Group, Cavendish Laboratory, University of Cambridge, Madingley Road, Cambridge CB3 0HE, UK, A. CHALLINORAstrophysics Group, Cavendish Laboratory, University of Cambridge, Madingley Road, Cambridge CB3 0HE, UK, K. GRAINGEAstrophysics Group, Cavendish Laboratory, University of Cambridge, Madingley Road, Cambridge CB3 0HE, UK, M. HOBSONAstrophysics Group, Cavendish Laboratory, University of Cambridge, Madingley Road, Cambridge CB3 0HE, UK, A. LASENBYAstrophysics Group, Cavendish Laboratory, University of Cambridge, Madingley Road, Cambridge CB3 0HE, UK, R. SAUNDERSAstrophysics Group, Cavendish Laboratory, University of Cambridge, Madingley Road, Cambridge CB3 0HE, UK, P. SCOTTAstrophysics Group, Cavendish Laboratory, University of Cambridge, Madingley Road, Cambridge CB3 0HE, UK, J. ARIÑOIDOM, Avda. Lehendakari Aguirre, 3, E-48014 Bilbao, Spain, B. ETXEITAIDOM, Avda. Lehendakari Aguirre, 3, E-48014 Bilbao, Spain, A. GÓMEZIDOM, Avda. Lehendakari Aguirre, 3, E-48014 Bilbao, Spain, C. GÓMEZIDOM, Avda. Lehendakari Aguirre, 3, E-48014 Bilbao, Spain, G. MURGAIDOM, Avda. Lehendakari Aguirre, 3, E-48014 Bilbao, Spain, J. PANIDOM, Avda. Lehendakari Aguirre, 3, E-48014 Bilbao, Spain, R. SANQUIRCEIDOM, Avda. Lehendakari Aguirre, 3, E-48014 Bilbao, Spain and A. VIZCARGÜENAGAIDOM, Avda. Lehendakari Aguirre, 3, E-48014 Bilbao, Spainhttps://doi.org/10.1142/9789814374552_0428Cited by:0 PreviousNext AboutSectionsPDF/EPUB ToolsAdd to favoritesDownload CitationsTrack CitationsRecommend to Library ShareShare onFacebookTwitterLinked InRedditEmail Abstract: We briefly discuss the scientific objectives of the QUIJOTE (Q-U-I JOint TEnerife) CMB experiment, and present the current status and future scheduling of this project. QUIJOTE is a new project to study the polarization of the Cosmic Microwave Background (CMB) and of the Galactic and extragalactic emission in the frequency range 10-30 GHz and with an angular resolution of 1°. It will start operations in summer 2010 from the Teide Observatory. The scientific goal of this experiment is twofold: i) to characterize at low frequencies the polarization of the synchrotron and anomalous emissions, making then possible the correction of these CMB contaminants in the data of similar experiments operating at higher frequencies; and ii) to detect (or to constrain) the imprint of the primordial gravitational-wave background in the polarization pattern of the CMB if the tensor-to-scalar ratio is larger (lower) than r = 0:05. FiguresReferencesRelatedDetails The Twelfth Marcel Grossmann MeetingMetrics History PDF download

We present the current status of the QUIJOTE (Q-U-I JOint TEnerife) CMB Experiment, a new instrument which will start operations early in 2009 at Teide Observatory with the aim of characterizing the polarization of the CMB and other processes of galactic and extragalactic emission in the frequency range 10–30GHz and at large angular scales. QUIJOTE will be a valuable complement at low frequencies for the PLANCK mission, and will have the required sensitivity to detect a primordial gravitational-wave component if the tensor-to-scalar ratio is larger than r = 0.05.