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1. The QUIJOTE CMB Experiment: status and first results with the multi-frequency instrument

Author

López-Caniego, M., Rebolo, R., Aguiar, M., Génova-Santos, R., Gómez-Reñasco, F., Gutierrez, C., Herreros, J. M., Hoyland, R. J., López-Caraballo, C., Santos, A. E. Pelaez, Poidevin, F., Rubiño-Martín, J. A., de la Rosa, V. Sanchez, Tramonte, D., Vega-Moreno, A., Viera-Curbelo, T., Vignaga, R., Martínez-González, E., Barreiro, R. B., Casaponsa, B., Casas, F. J., Diego, J. M., Fernández-Cobos, R., Herranz, D., Ortiz, D., Vielva, P., Artal, E., Aja, B., Cagigas, J., Cano, J. L., de la Fuente, L., Mediavilla, A., Terán, J. V., Villa, E., Piccirillo, L., Battye, R., Blackhurst, E., Brown, M., Davies, R. D., Davis, R. J., Dickinson, C., Grainge, K., Harper, S., Maffei, B., McCulloch, M., Melhuish, S., Pisano, G., Watson, R. A., Hobson, M., Lasenby, A., Saunders, R., and Scott, P.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract

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 14{\mu}K per one degree beam at 11, 13, 17 and 19 GHz, in both Q and U., Comment: Rencontres du Vietnam 2013: Cosmology in the Planck Era. Conference Proceedings. Typos added

Published
2014

2. The C-Band All-Sky Survey (C-BASS): Design and implementation of the northern receiver

Author

King, O. G., Jones, Michael E., Blackhurst, E. J., Copley, C., Davis, R. J., Dickinson, C., Holler, C. M., Irfan, M. O., John, J. J., Leahy, J. P., Leech, J., Muchovej, S. J. C., Pearson, T. J., Stevenson, M. A., and Taylor, Angela C.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The C-Band All-Sky Survey (C-BASS) is a project to map the full sky in total intensity and linear polarization at 5 GHz. The northern component of the survey uses a broadband single-frequency analogue receiver fitted to a 6.1-m telescope at the Owens Valley Radio Observatory in California, USA. The receiver architecture combines a continuous-comparison radiometer and a correlation polarimeter in a single receiver for stable simultaneous measurement of both total intensity and linear polarization, using custom-designed analogue receiver components. The continuous-comparison radiometer measures the temperature difference between the sky and temperature-stabilized cold electrical reference loads. A cryogenic front-end is used to minimize receiver noise, with a system temperature of $\approx 30\,$K in both linear polarization and total intensity. Custom cryogenic notch filters are used to counteract man-made radio frequency interference. The radiometer $1/f$ noise is dominated by atmospheric fluctuations, while the polarimeter achieves a $1/f$ noise knee frequency of 10 mHz, similar to the telescope azimuthal scan frequency., Comment: 15 pages, 15 figures, submitted to MNRAS

Published
2013
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3. Planck pre-launch status: calibration of the Low Frequency Instrument flight model radiometers

Author

Villa, F., Terenzi, L., Sandri, M., Meinhold, P., Poutanen, T., Battaglia, P., Franceschet, C., Hughes, N., Laaninen, M., Lapolla, P., Bersanelli, M., Butler, R. C., Cuttaia, F., D'Arcangelo, O., Frailis, M., Franceschi, E., Galeotta, S., Gregorio, A., Leonardi, R., Lowe, S. R., Mandolesi, N., Maris, M., Mendes, L., Mennella, A., Morgante, G., Stringhetti, L., Tomasi, M., Valenziano, L., Zacchei, A., Zonca, A., Aja, B., Artal, E., Balasini, M., Bernardino, T., Blackhurst, E., Boschini, L., Cappellini, B., Cavaliere, F., Colin, A., Colombo, F., Davis, R. J., De La Fuente, L., Edgeley, J., Gaier, T., Galtress, A., Hoyland, R., Jukkala, P., Kettle, D., Kilpia, V-H., Lawrence, C. R., Lawson, D., Leahy, J. P., Leutenegger, P., Levin, S., Maino, D., Malaspina, M., Mediavilla, A., Miccolis, M., Pagan, L., Pascual, J. P., Pasian, F., Pecora, M., Pospieszalski, M., Roddis, N., Salmon, M. J., Seiffert, M., Silvestri, R., Simonetto, A., Sjoman, P., Sozzi, C., Tuovinen, J., Varis, J., Wilkinson, A., and Winder, F.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Low Frequency Instrument (LFI) on-board the ESA Planck satellite carries eleven radiometer subsystems, called Radiometer Chain Assemblies (RCAs), each composed of a pair of pseudo-correlation receivers. We describe the on-ground calibration campaign performed to qualify the flight model RCAs and to measure their pre-launch performances. Each RCA was calibrated in a dedicated flight-like cryogenic environment with the radiometer front-end cooled to 20K and the back-end at 300K, and with an external input load cooled to 4K. A matched load simulating a blackbody at different temperatures was placed in front of the sky horn to derive basic radiometer properties such as noise temperature, gain, and noise performance, e.g. 1/f noise. The spectral response of each detector was measured as was their susceptibility to thermal variation. All eleven LFI RCAs were calibrated. Instrumental parameters measured in these tests, such as noise temperature, bandwidth, radiometer isolation, and linearity, provide essential inputs to the Planck-LFI data analysis., Comment: 15 pages, 18 figures. Accepted for publication in Astronomy and Astrophysics

Published
2010
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4. Design, development and verification of the 30 and 44 GHz front-end modules for the Planck Low Frequency Instrument

Author

Davis, R. J., Wilkinson, A., Davies, R. D., Winder, W. F., Roddis, N., Blackhurst, E. J., Lawson, D., Lowe, S. R., Baines, C., Butlin, M., Galtress, A., Shepherd, D., Aja, B., Artal, E., Bersanelli, M., Butler, R. C., Castelli, C., Cuttaia, F., D'Arcangelo, O., Gaier, T., Hoyland, R., Kettle, D., Leonardi, R., Mandolesi, N., Mennella, A., Meinhold, P., Pospieszalski, M., Stringhetti, L., Tomasi, M., Valenziano, L., and Zonca, A.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We give a description of the design, construction and testing of the 30 and 44 GHz Front End Modules (FEMs) for the Low Frequency Instrument (LFI) of the Planck mission to be launched in 2009. The scientific requirements of the mission determine the performance parameters to be met by the FEMs, including their linear polarization characteristics. The FEM design is that of a differential pseudo-correlation radiometer in which the signal from the sky is compared with a 4-K blackbody load. The Low Noise Amplifier (LNA) at the heart of the FEM is based on indium phosphide High Electron Mobility Transistors (HEMTs). The radiometer incorporates a novel phase-switch design which gives excellent amplitude and phase match across the band. The noise temperature requirements are met within the measurement errors at the two frequencies. For the most sensitive LNAs, the noise temperature at the band centre is 3 and 5 times the quantum limit at 30 and 44 GHz respectively. For some of the FEMs, the noise temperature is still falling as the ambient temperature is reduced to 20 K. Stability tests of the FEMs, including a measurement of the 1/f knee frequency, also meet mission requirements. The 30 and 44 GHz FEMs have met or bettered the mission requirements in all critical aspects. The most sensitive LNAs have reached new limits of noise temperature for HEMTs at their band centres. The FEMs have well-defined linear polarization characteristcs., Comment: 39 pages, 33 figures (33 EPS files), 12 tables. Planck LFI technical papers published by JINST: http://www.iop.org/EJ/journal/-page=extra.proc5/1748-0221

Published
2010
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5. Noise Properties of the Planck-LFI Receivers

Author

Meinhold, P., Leonardi, R., Aja, B., Artal, E., Battaglia, P., Bersanelli, M., Blackhurst, E., Butler, C. R., Cuevas, L. P., Cuttaia, F., D'Arcangelo, O., Davis, R., de la Fuente, M. L., Frailis, M., Franceschet, C., Franceschi, E., Gaier, T., Galeotta, S., Gregorio, A., Hoyland, R., Hughes, N., Jukkala, P., Kettle, D., Laaninen, M., Leutenegger, P., Lowe, S. R., Malaspina, M., Mandolesi, R., Maris, M., Martínez-González, E., Mendes, L., Mennella, A., Miccolis, M., Morgante, G., Roddis, N., Sandri, M., Seiffert, M., Salmón, M., Stringhetti, L., Poutanen, T., Terenzi, L., Tomasi, M., Tuovinen, J., Varis, J., Valenziano, L., Villa, F., Wilkinson, A., Winder, F., Zacchei, A., and Zonca, A.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract

The Planck Low Frequency Instrument (LFI) radiometers have been tested extensively during several dedicated campaigns. The present paper reports the principal noise properties of the LFI radiometers., Comment: this paper is part of the Prelaunch status LFI papers published on JINST: http://www.iop.org/EJ/journal/-page=extra.proc5/jinst

Published
2010
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6. Planck pre-launch status: Design and description of the Low Frequency Instrument

Author

Bersanelli, M., Mandolesi, N., Butler, R. C., Mennella, A., Villa, F., Aja, B., Artal, E., Artina, E., Baccigalupi, C., Balasini, M., Baldan, G., Banday, A., Bastia, P., Battaglia, P., Bernardino, T., Blackhurst, E., Boschini, L., Burigana, C., Cafagna, G., Cappellini, B., Cavaliere, F., Colombo, F., Crone, G., Cuttaia, F., D'Arcangelo, O., Danese, L., Davies, R. D., Davis, R. J., De Angelis, L., De Gasperis, G. C., De La Fuente, L., De Rosa, A., De Zotti, G., Falvella, M. C., Ferrari, F., Ferretti, R., Figini, L., Fogliani, S., Franceschet, C., Franceschi, E., Gaier, T., Garavaglia, S., Gomez, F., Gorski, K., Gregorio, A., Guzzi, P., Herreros, J. M., Hildebrandt, S. R., Hoyland, R., Hughes, N., Janssen, M., Jukkala, P., Kettle, D., Kilpia, V. H., Laaninen, M., Lapolla, P. M., Lawrence, C. R., Leahy, J. P., Leonardi, R., Leutenegger, P., Levin, S., Lilje, P. B., Lowe, S. R., Lubin, D. Lawson P. M., Maino, D., Malaspina, M., Maris, M., Marti-Canales, J., Martinez-Gonzalez, E., Mediavilla, A., Meinhold, P., Miccolis, M., Morgante, G., Natoli, P., Nesti, R., Pagan, L., Paine, C., Partridge, B., Pascual, J. P., Pasian, F., Pearson, D., Pecora, M., Perrotta, F., Platania, P., Pospieszalski, M., Poutanen, T., Prina, M., Rebolo, R., Roddis, N., Rubino-Martin, J. A., Salmon, n M. J., Sandri, M., Seiffert, M., Silvestri, R., Simonetto, A., Sjoman, P., Smoot, G. F., Sozzi, C., Stringhetti, L., Taddei, E., Tauber, J., Terenzi, L., Tomasi, M., Tuovinen, J., Valenziano, L., Varis, J., Vittorio, N., Wade, L. A., Wilkinson, A., Winder, F., Zacchei, A., and Zonca, A.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In this paper we present the Low Frequency Instrument (LFI), designed and developed as part of the Planck space mission, the ESA program dedicated to precision imaging of the cosmic microwave background (CMB). Planck-LFI will observe the full sky in intensity and polarisation in three frequency bands centred at 30, 44 and 70 GHz, while higher frequencies (100-850 GHz) will be covered by the HFI instrument. The LFI is an array of microwave radiometers based on state-of-the-art Indium Phosphide cryogenic HEMT amplifiers implemented in a differential system using blackbody loads as reference signals. The front-end is cooled to 20K for optimal sensitivity and the reference loads are cooled to 4K to minimise low frequency noise. We provide an overview of the LFI, discuss the leading scientific requirements and describe the design solutions adopted for the various hardware subsystems. The main drivers of the radiometric, optical and thermal design are discussed, including the stringent requirements on sensitivity, stability, and rejection of systematic effects. Further details on the key instrument units and the results of ground calibration are provided in a set of companion papers., Comment: 23 pages, 31 figures, accepted by Astronomy and Astrophysics, Planck LFI technical papers published by JINST: http://www.iop.org/EJ/journal/-page=extra.proc5/1748-0221

Published
2010
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7. Advanced pseudo-correlation radiometers for the Planck-LFI instrument

Author

Mennella, A., Bersanelli, M., Butler, R. C., Maino, D., Mandolesi, N., Morgante, G., Valenziano, L., Villa, F., Gaier, T., Seiffert, M., Levin, S., Lawrence, C., Meinhold, P., Lubin, P., Tuovinen, J., Varis, J., Karttaavi, T., Hughes, N., Jukkala, P., Sjman, P., Kangaslahti, P., Roddis, N., Kettle, D., Winder, F., Blackhurst, E., Davis, R., Wilkinson, A., Castelli, C., Aja, B., Artal, E., de la Fuente, L., Mediavilla, A., Pascual, J. P., Gallegos, J., Martinez-Gonzalez, E., de Paco, P., and Pradell, L.

Subjects
Astrophysics
Abstract

The LFI (Low Frequency Instrument) on board the ESA Planck satellite is constituted by an array of radiometric detectors actively cooled at 20 K in the 30-70 GHz frequency range in the focal plane of the Planck telescope. In this paper we present an overview of the LFI instrument, with a particular focus on the radiometer design. The adopted pseudo-correlation scheme uses a software balancing technique (with a tunable parameter called gain modulation factor) which is effective in reducing the radiometer susceptibility to amplifier instabilities also in presence of small non-idealities in the radiometric chain components, provided that the gain modulation factor is estimated with an accuracy of the order of 0.2%. These results have been recently confirmed by experimental laboratory measurements conducted on the LFI prototype radiometers at 30, 70 and 100 GHz., Comment: 6 pages, 3 figures

Published
2003

8. Development of techniques and technology for full polarimetric radar applied to concealed weapons detection

Author

Blackhurst, E. J.

Abstract

One of the biggest threats to modern society is the increasing use by criminals and terrorists of concealed weapons and person born improvised explosive devices (PBIED). Current highly mature security screening technologies using x-ray and metal detectors have limited deployment scenarios based on health and safety issues and operational range, respectively. Given that most clothing is greater than 90% transmissive in the microwave region, this spectral band is ideal for screening people for concealed threats. However, due to diffraction, imagery to screen subjects is limited due to the small number of pixels. In this regime, the exploitation of microwave polarimetry from the field of remote sensing has particular benefits, as it extracts maximum information content from a single pixel. The work presented in this thesis has assembled a full polarimetric frequency stepped radar from a vector network analyser (VNA), a linear orthogonal mode transducer (OMT) of the turnstile type and a conical corrugated horn antenna. The system’s characterisation by antenna pattern measurements, the measuring of canonical targets of the plane, dihedral, dipole and helical reflectors showed the system to be capable of making localised Sinclair matrix measurements of targets at ranges of two to three metres. The work presents a calibration procedure comprising the VNA’s internal calibration and an external calibration to compensate for dispersion and cross-polar leakage of system components. Static target measurements (canonical and various surrogate items) were analysed, using range gating for clutter rejection. Calibrated Sinclair parameter measurements compared with those from simple simulations, all software being programmed in Matlab. Measurements of moving targets revealed the phenomenon of speckle, this introducing rapid changes in the Sinclair Parameters. Data analysis performed using the coherency matrix and the Cloude/Pottier decomposition minimised the effects of speckle in the processed data. Measurements show movement from particularly rough surfaces increased the parameter of the Cloude/Pottier entropy, the level of this being directly linked to the degree of speckle. Application of the Huynen polarisation fork technique (a type of decomposition) has proved to aid the identification of static and moving targets. A detailed analysis of iii the Huynen fork responses is made of the human torso on its own, weapons on their own and then weapons positioned against the human torso. Responses of nondangerous objects such as keys and a smartphone are additionally presented.

Published
2020

9. Full polarimetric radar for concealed weapons detection: Experimental determination and simulation of the Huynen target parameters for the human torso

Author

Blackhurst, E, Salmon, N, Blackhurst, E, and Salmon, N

Abstract

© 2019 SPIE. The measurements of the human torso for two individuals are presented via the generation of the Huynen polarisation fork technique and plotted on the Poincaré sphere, to ascertain characteristics that could be used to remove the effects of the torso when concealed weapons are placed against it. Measurements are taken with a frequency modulated continuous wave (FMCW) mono-static millimetre wave full polarimetric radar, operating at k-band (18 to 26 GHz). The system has been designed to explore the feasibility of using full polarimetry for the detection of concealed weapons, and person borne improvised explosive devices (PBIED). The philosophy of this scheme is a means to extract the maximum information content from a target which is in the nominally single spatial pixel (sometimes sub-pixel) configuration of stand-off (tens of metres) and crowd surveillance scenarios. The radar comprises a vector network analyser (VNA) and an orthomode transducer.

Published
2019

10. Full polarimetric millimetre wave radar for stand-off security screening

Author

Blackhurst, E, Salmon, N, Southgate, M, Blackhurst, E, Salmon, N, and Southgate, M

Abstract

© COPYRIGHT SPIE. Downloading of the abstract is permitted for personal use only. The development and measurements are described of a frequency modulated continuous wave (FMCW) mono-static millimetre wave full polarimetric radar, operating at k-band (18 to 26 GHz). The system has been designed to explore the feasibility of using full polarimetry for the detection of concealed weapons, and person borne improvised explosive devices (PBIED). The philosophy of this scheme is a means to extract the maximum information content from a target which is normally in the single spatial pixel (sometimes sub-pixel) configuration in stand-off (tens of metres) and crowd surveillance scenarios. The radar comprises a vector network analyser (VNA), an orthomode transducer and a conical horn antenna. A calibration strategy is discussed and demonstrated using a variety of known calibration targets with known reflective properties, including a flat metal plate, dihedral reflector, metal sphere, helix and dipole. The orthomode transducer is based on a high performance linear polarizer of the turnstile type with isolation better than - 35dB between orthogonal polarisations. The calibration enables the polarimetric Sinclair scattering matrix to be measured at each frequency for coherent polarimetry, and this can be extended using multiple measurements via the Kennaugh matrix to investigate incoherent full polarimetry.

Published
2018

11. The C-Band All-Sky Survey (C-BASS): design and implementation of the northern receiver

Author

King, O. G., primary, Jones, Michael E., additional, Blackhurst, E. J., additional, Copley, C., additional, Davis, R. J., additional, Dickinson, C., additional, Holler, C. M., additional, Irfan, M. O., additional, John, J. J., additional, Leahy, J. P., additional, Leech, J., additional, Muchovej, S. J. C., additional, Pearson, T. J., additional, Stevenson, M. A., additional, and Taylor, Angela C., additional

Published
2013
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12. Planckpre-launch status: Calibration of the Low Frequency Instrument flight model radiometers

Author

Villa, F., primary, Terenzi, L., additional, Sandri, M., additional, Meinhold, P., additional, Poutanen, T., additional, Battaglia, P., additional, Franceschet, C., additional, Hughes, N., additional, Laaninen, M., additional, Lapolla, P., additional, Bersanelli, M., additional, Butler, R. C., additional, Cuttaia, F., additional, D'Arcangelo, O., additional, Frailis, M., additional, Franceschi, E., additional, Galeotta, S., additional, Gregorio, A., additional, Leonardi, R., additional, Lowe, S. R., additional, Mandolesi, N., additional, Maris, M., additional, Mendes, L., additional, Mennella, A., additional, Morgante, G., additional, Stringhetti, L., additional, Tomasi, M., additional, Valenziano, L., additional, Zacchei, A., additional, Zonca, A., additional, Aja, B., additional, Artal, E., additional, Balasini, M., additional, Bernardino, T., additional, Blackhurst, E., additional, Boschini, L., additional, Cappellini, B., additional, Cavaliere, F., additional, Colin, A., additional, Colombo, F., additional, Davis, R. J., additional, De La Fuente, L., additional, Edgeley, J., additional, Gaier, T., additional, Galtress, A., additional, Hoyland, R., additional, Jukkala, P., additional, Kettle, D., additional, Kilpia, V.-H., additional, Lawrence, C. R., additional, Lawson, D., additional, Leahy, J. P., additional, Leutenegger, P., additional, Levin, S., additional, Maino, D., additional, Malaspina, M., additional, Mediavilla, A., additional, Miccolis, M., additional, Pagan, L., additional, Pascual, J. P., additional, Pasian, F., additional, Pecora, M., additional, Pospieszalski, M., additional, Roddis, N., additional, Salmon, M. J., additional, Seiffert, M., additional, Silvestri, R., additional, Simonetto, A., additional, Sjoman, P., additional, Sozzi, C., additional, Tuovinen, J., additional, Varis, J., additional, Wilkinson, A., additional, and Winder, F., additional

Published
2010
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13. Planckpre-launch status: Design and description of the Low Frequency Instrument

Author

Bersanelli, M., primary, Mandolesi, N., additional, Butler, R. C., additional, Mennella, A., additional, Villa, F., additional, Aja, B., additional, Artal, E., additional, Artina, E., additional, Baccigalupi, C., additional, Balasini, M., additional, Baldan, G., additional, Banday, A., additional, Bastia, P., additional, Battaglia, P., additional, Bernardino, T., additional, Blackhurst, E., additional, Boschini, L., additional, Burigana, C., additional, Cafagna, G., additional, Cappellini, B., additional, Cavaliere, F., additional, Colombo, F., additional, Crone, G., additional, Cuttaia, F., additional, D'Arcangelo, O., additional, Danese, L., additional, Davies, R. D., additional, Davis, R. J., additional, De Angelis, L., additional, De Gasperis, G. C., additional, De La Fuente, L., additional, De Rosa, A., additional, De Zotti, G., additional, Falvella, M. C., additional, Ferrari, F., additional, Ferretti, R., additional, Figini, L., additional, Fogliani, S., additional, Franceschet, C., additional, Franceschi, E., additional, Gaier, T., additional, Garavaglia, S., additional, Gomez, F., additional, Gorski, K., additional, Gregorio, A., additional, Guzzi, P., additional, Herreros, J. M., additional, Hildebrandt, S. R., additional, Hoyland, R., additional, Hughes, N., additional, Janssen, M., additional, Jukkala, P., additional, Kettle, D., additional, Kilpiä, V. H., additional, Laaninen, M., additional, Lapolla, P. M., additional, Lawrence, C. R., additional, Lawson, D., additional, Leahy, J. P., additional, Leonardi, R., additional, Leutenegger, P., additional, Levin, S., additional, Lilje, P. B., additional, Lowe, S. R., additional, Lubin, P. M., additional, Maino, D., additional, Malaspina, M., additional, Maris, M., additional, Marti-Canales, J., additional, Martinez-Gonzalez, E., additional, Mediavilla, A., additional, Meinhold, P., additional, Miccolis, M., additional, Morgante, G., additional, Natoli, P., additional, Nesti, R., additional, Pagan, L., additional, Paine, C., additional, Partridge, B., additional, Pascual, J. P., additional, Pasian, F., additional, Pearson, D., additional, Pecora, M., additional, Perrotta, F., additional, Platania, P., additional, Pospieszalski, M., additional, Poutanen, T., additional, Prina, M., additional, Rebolo, R., additional, Roddis, N., additional, Rubiño-Martin, J. A., additional, Salmon, M. J., additional, Sandri, M., additional, Seiffert, M., additional, Silvestri, R., additional, Simonetto, A., additional, Sjoman, P., additional, Smoot, G. F., additional, Sozzi, C., additional, Stringhetti, L., additional, Taddei, E., additional, Tauber, J., additional, Terenzi, L., additional, Tomasi, M., additional, Tuovinen, J., additional, Valenziano, L., additional, Varis, J., additional, Vittorio, N., additional, Wade, L. A., additional, Wilkinson, A., additional, Winder, F., additional, Zacchei, A., additional, and Zonca, A., additional

Published
2010
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14. The Ka-band receiver for the QUIJOTE experiment

Author

Cano, J. L., Enrique Villa, Aja, B., La Fuente, L., Artal, E., Watson, R., Blackhurst, E., Edgley, J., Baines, C., and Universidad de Cantabria

Subjects
InP, Radiometer, Radio astronomy, Very low noise receivers, Cryogenic amplifiers, Radiometry, HEMT
Abstract

The 26-36 GHz receiver for a radio astronomy radiometer, to characterize the polarization of the Cosmic Microwave Background, is presented. This receiver is based on very low noise cryogenically cooled amplifiers in the front-end module, while in the back-end module a broadband amplification and direct detection chain is operated at room temperature. Noise temperature of the low-noise amplifier (LNA) is 19 K when cooled at 18 K. Experimental results show a good sensitivity of the complete receiver with an effective bandwidth around 8 GHz. Moreover, output detected voltages agree with estimated values. This work has been funded by the Ministerio de Ciencia e Innovación (Spain) under Astronomy and Astrophysics research programme, reference AYA2007-68058-C03.

15. The QUIJOTE CMB Experiment: status and first results with the multi-frequency instrument

Author

López-Caniego, M., Rebolo, R., Aguiar, M., Génova-Santos, R., Gómez-Reñasco, F., Gutierrez, C., Herreros, J. M., Hoyland, R. J., López-Caraballo, C., Pelaez Santos, A. E., Poidevin, F., Rubiño-Martín, J. A., Sanchez La Rosa, V., Tramonte, D., Vega-Moreno, A., Viera-Curbelo, T., Vignaga, R., Martínez-González, E., Barreiro, R. B., Casaponsa, B., Casas, F. J., Diego, J. M., Fernández-Cobos, R., Herranz, D., Ortiz, D., Vielva, P., Artal, E., Aja, B., Cagigas, J., Cano, J. L., La Fuente, L., Mediavilla, A., Terán, J. V., Villa, E., Lucio Piccirillo, Richard Battye, Blackhurst, E., Michael Brown, Davies, R. D., Davis, R. J., Clive Dickinson, Keith Grainge, Harper, S., Bruno Maffei, Mcculloch, M., Melhuish, S., Pisano, G., Robert Watson, Hobson, M., Lasenby, A., Saunders, R., and Scott, P.

Subjects
Astrophysics - Cosmology and Extragalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Extragalactic Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

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 14{\mu}K per one degree beam at 11, 13, 17 and 19 GHz, in both Q and U., Comment: Rencontres du Vietnam 2013: Cosmology in the Planck Era. Conference Proceedings. Typos added

16. The QUIJOTE-CMB experiment: studying the polarisation of the galactic and cosmological microwave emissions

Author

Stepp, Larry M., Gilmozzi, Roberto, Hall, Helen J., Rubiño-Martín, J. A., Rebolo, R., Aguiar, M., Génova-Santos, R., Gómez-Reñasco, F., Herreros, J. M., Hoyland, R. J., López-Caraballo, C., Pelaez Santos, A. E., Sanchez de la Rosa, V., Vega-Moreno, A., Viera-Curbelo, T., Martínez-Gonzalez, E., Barreiro, R. B., Casas, F. J., Diego, J. M., Fernández-Cobos, R., Herranz, D., López-Caniego, M., Ortiz, D., Vielva, P., Artal, E., Aja, B., Cagigas, J., Cano, J. L., de la Fuente, L., Mediavilla, A., Terán, J. V., Villa, E., Piccirillo, L., Battye, R., Blackhurst, E., Brown, M., Davies, R. D., Davis, R. J., Dickinson, C., Harper, S., Maffei, B., McCulloch, M., Melhuish, S., Pisano, Giampaolo, Watson, R. A., Hobson, M., Grainge, K., Lasenby, A., Saunders, R., Scott, P., Stepp, Larry M., Gilmozzi, Roberto, Hall, Helen J., Rubiño-Martín, J. A., Rebolo, R., Aguiar, M., Génova-Santos, R., Gómez-Reñasco, F., Herreros, J. M., Hoyland, R. J., López-Caraballo, C., Pelaez Santos, A. E., Sanchez de la Rosa, V., Vega-Moreno, A., Viera-Curbelo, T., Martínez-Gonzalez, E., Barreiro, R. B., Casas, F. J., Diego, J. M., Fernández-Cobos, R., Herranz, D., López-Caniego, M., Ortiz, D., Vielva, P., Artal, E., Aja, B., Cagigas, J., Cano, J. L., de la Fuente, L., Mediavilla, A., Terán, J. V., Villa, E., Piccirillo, L., Battye, R., Blackhurst, E., Brown, M., Davies, R. D., Davis, R. J., Dickinson, C., Harper, S., Maffei, B., McCulloch, M., Melhuish, S., Pisano, Giampaolo, Watson, R. A., Hobson, M., Grainge, K., Lasenby, A., Saunders, R., and Scott, P.

Abstract

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 (10-30GHz) 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. © (2012) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.

17. The status of the QUIJOTE multi-frequency instrument

Author

Holland, Wayne S., Zmuidzinas, Jonas, Hoyland, R. J., Aguiar-González, M., Aja, B., Ariño, J., Artal, E., Barreiro, R. B., Blackhurst, E. J., Cagigas, J., Cano de Diego, J. L., Casas, F. J., Davis, R. J., Dickinson, C., Arriaga, B. E., Fernandez-Cobos, R., de la Fuente, L., Génova-Santos, R., Gómez, A., Gomez, C., Gómez-Reñasco, F., Grainge, K., Harper, S., Herran, D., Herreros, J. M., Herrera, G. A., Hobson, M. P., Lasenby, A. N., Lopez-Caniego, M., López-Caraballo, C., Maffei, Bruno, Martinez-Gonzalez, E., McCulloch, M., Melhuish, SImon John, Mediavilla, A., Murga, G., Ortiz, D., Piccirillo, Lucio, Pisano, Giampaolo, Rebolo-López, R., Rubiño-Martin, J. A., Ruiz, J. Luis, Sanchez de la Rosa, V., Sanquirce, R., Vega-Moreno, A., Vielva, P., Viera-Curbelo, T., Villa, E., Vizcargüenaga, A., Watson, R. A., Holland, Wayne S., Zmuidzinas, Jonas, Hoyland, R. J., Aguiar-González, M., Aja, B., Ariño, J., Artal, E., Barreiro, R. B., Blackhurst, E. J., Cagigas, J., Cano de Diego, J. L., Casas, F. J., Davis, R. J., Dickinson, C., Arriaga, B. E., Fernandez-Cobos, R., de la Fuente, L., Génova-Santos, R., Gómez, A., Gomez, C., Gómez-Reñasco, F., Grainge, K., Harper, S., Herran, D., Herreros, J. M., Herrera, G. A., Hobson, M. P., Lasenby, A. N., Lopez-Caniego, M., López-Caraballo, C., Maffei, Bruno, Martinez-Gonzalez, E., McCulloch, M., Melhuish, SImon John, Mediavilla, A., Murga, G., Ortiz, D., Piccirillo, Lucio, Pisano, Giampaolo, Rebolo-López, R., Rubiño-Martin, J. A., Ruiz, J. Luis, Sanchez de la Rosa, V., Sanquirce, R., Vega-Moreno, A., Vielva, P., Viera-Curbelo, T., Villa, E., Vizcargüenaga, A., and Watson, R. A.

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.

18. Planck pre-launch status:Design and description of the Low Frequency Instrument

Author

M. Bersanelli, N. Mandolesi, R. C. Butler, A. Mennella, F. Villa, B. Aja, E. Artal, E. Artina, C. Baccigalupi, M. Balasini, G. Baldan, A. Banday, P. Bastia, P. Battaglia, T. Bernardino, E. Blackhurst, L. Boschini, C. Burigana, G. Cafagna, B. Cappellini, F. Cavaliere, F. Colombo, G. Crone, F. Cuttaia, O. D'Arcangelo, L. Danese, R. D. Davies, R. J. Davis, L. De Angelis, G. C. De Gasperis, L. De La Fuente, A. De Rosa, G. De Zotti, M. C. Falvella, F. Ferrari, R. Ferretti, L. Figini, S. Fogliani, C. Franceschet, E. Franceschi, T. Gaier, S. Garavaglia, F. Gomez, K. Gorski, A. Gregorio, P. Guzzi, J. M. Herreros, S. R. Hildebrandt, R. Hoyland, N. Hughes, M. Janssen, P. Jukkala, D. Kettle, V. H. Kilpiä, M. Laaninen, P. M. Lapolla, C. R. Lawrence, D. Lawson, J. P. Leahy, R. Leonardi, P. Leutenegger, S. Levin, P. B. Lilje, S. R. Lowe, P. M. Lubin, D. Maino, M. Malaspina, M. Maris, J. Marti-Canales, E. Martinez-Gonzalez, A. Mediavilla, P. Meinhold, M. Miccolis, G. Morgante, P. Natoli, R. Nesti, L. Pagan, C. Paine, B. Partridge, J. P. Pascual, F. Pasian, D. Pearson, M. Pecora, F. Perrotta, P. Platania, M. Pospieszalski, T. Poutanen, M. Prina, R. Rebolo, N. Roddis, J. A. Rubiño-Martin, M. J. Salmon, M. Sandri, M. Seiffert, R. Silvestri, A. Simonetto, P. Sjoman, G. F. Smoot, C. Sozzi, L. Stringhetti, E. Taddei, J. Tauber, L. Terenzi, M. Tomasi, J. Tuovinen, L. Valenziano, J. Varis, N. Vittorio, L. A. Wade, A. Wilkinson, F. Winder, A. Zacchei, A. Zonca, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), PLANCK, Universidad de Cantabria, Bersanelli, M, Mandolesi, N, BUTLER R., C, Mennella, A, Villa, F, Aja, B, Artal, E, Artina, E, Baccigalupi, C, Balasini, M, Baldan, G, Banday, A, Bastia, P, Battaglia, P, Bernardino, T, Blackhurst, E, Boschini, L, Burigana, C, Cafagna, G, Cappellini, B, Cavaliere, F, Colombo, F, Crone, G, Cuttaia, F, Darcangelo, O, Danese, L, DAVIES R., D, DAVIS R., J, DE ANGELIS, L, DE GASPERIS G., C, DE LA FUENTE, L, DE ROSA, A, DE ZOTTI, G, FALVELLA M., C, Ferrari, F, Ferretti, R, Figini, L, Fogliani, S, Franceschet, C, Franceschi, E, Gaier, T, Garavaglia, S, Gomez, F, Gorski, K, Gregorio, Anna, Guzzi, P, HERREROS J., M, HILDEBRANDT S., R, Hoyland, R, Hughes, N, Janssen, M, Jukkala, P, Kettle, D, KILPIA V., H, Laaninen, M, LAPOLLA P., M, LAWRENCE C., R, Lawson, D, LEAHY J., P, Leonardi, R, Leutenegger, P, Levin, S, LILJE P., B, LOWE S., R, LUBIN P., M, Maino, D, Malaspina, M, Maris, M, MARTI CANALES, J, MARTINEZ GONZALEZ, E, Mediavilla, A, Meinhold, P, Miccolis, M, Morgante, G, Natoli, P, Nesti, R, Pagan, L, Paine, C, Partridge, B, PASCUAL J., P, Pasian, F, Pearson, D, Pecora, M, Perrotta, F, Platania, P, Pospieszalski, M, Poutanen, T, Prina, M, Rebolo, R, Roddis, N, RUBINO MARTIN J., A, SALMON M., J, Sandri, M, Seiffert, M, Silvestri, R, Simonetto, A, Sjoman, P, SMOOT G., F, Sozzi, C, Stringhetti, L, Taddei, E, Tauber, J, Terenzi, L, Tomasi, M, Tuovinen, J, Valenziano, L, Varis, J, Vittorio, N, WADE L., A, Wilkinson, A, Winder, F, Zacchei, A, Zonca, A., Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
detectors – instrumentation, Computer science, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmic microwave background, cosmic microwave background, cosmology: observations, space vehicles: instruments, 01 natural sciences, 7. Clean energy, CMB physics, observations [Cosmology], 010303 astronomy & astrophysics, Planck ESA mission, Astrophysics::Instrumentation and Methods for Astrophysics, Polarization (waves), symbols, Radiometric dating, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Low frequency, Radio spectrum, instruments – instrumentation [cosmic microwave background – telescopes – space vehicles], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], instruments [Space vehicles], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Electronic engineering, Calibration, Black-body radiation, Sensitivity (control systems), Planck, Instrumentation and Methods for Astrophysics (astro-ph.IM), cosmic microwave background – telescopes – space vehicles: instruments – instrumentation, Radiometer, cosmology-observations, 010308 nuclear & particles physics, Amplifier, Astronomy and Astrophysics, polarimeters – submillimeter, Space and Planetary Science, general, space vehicles-instruments, Microwave
Abstract

21 páginas, 23 figuras, 13 tablas.-- et al., In this paper we present the Low Frequency Instrument (LFI), designed and developed as part of the Planck space mission, the ESA programme dedicated to precision imaging of the cosmic microwave background (CMB). Planck-LFI will observe the full sky in intensity and polarisation in three frequency bands centred at 30, 44 and 70 GHz, while higher frequencies (100–850 GHz) will be covered by the HFI instrument. The LFI is an array of microwave radiometers based on state-of-the-art indium phosphide cryogenic HEMT amplifiers implemented in a differential system using blackbody loads as reference signals. The front end is cooled to 20 K for optimal sensitivity and the reference loads are cooled to 4 K to minimise low-frequency noise. We provide an overview of the LFI, discuss the leading scientific requirements, and describe the design solutions adopted for the various hardware subsystems. The main drivers of the radiometric, optical, and thermal design are discussed, including the stringent requirements on sensitivity, stability, and rejection of systematic effects. Further details on the key instrument units and the results of ground calibration are provided in a set of companion papers., T.P.’s work was supported in part by the Academy of Finland grants 205800, 214598, 121703, and 121962. T.P. thanks the Waldemar von Frenckells Stiftelse, Magnus Ehrnrooth Foundation, and Väisälä Foundation for financial support. We acknowledge partial support from the NASA LTSA Grant NNG04CG90G.

Published
2010
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19. Planck pre-launch status:Calibration of the Low Frequency Instrument flight model radiometers

Author

Angel Colin, Davide Maino, Charles R. Lawrence, O. D'Arcangelo, Andrea Zonca, Jussi Varis, F. Pasian, Andrea Zacchei, R. Silvestri, Gianluca Morgante, M. J. Salmon, E. Franceschi, E. Blackhurst, M. Laaninen, D. Lawson, A. Simonetto, M. Sandri, S. R. Lowe, L. Pagan, F. Winder, S. Galeotta, L. de la Fuente, J. Edgeley, A. Mennella, M. Frailis, Althea Wilkinson, N. Hughes, J. P. Leahy, P. Sjoman, M. Balasini, F. Cuttaia, D. Kettle, V. H. Kilpiä, Anna Gregorio, A. Galtress, M. Pecora, M. Maris, P. Battaglia, Beatriz Aja, Eduardo Artal, Fabrizio Villa, P. Leutenegger, Roger J. Hoyland, Luca Valenziano, T. Poutanen, Luca Stringhetti, M. Miccolis, Peter Meinhold, N. Mandolesi, M. Tomasi, Marco Bersanelli, Marian Pospieszalski, Francesco Cavaliere, B. Cappellini, L. Mendes, P. Jukkala, Cristian Franceschet, Michael Seiffert, Carlo Sozzi, Juan Pablo Pascual, F. Colombo, L. Boschini, J. Tuovinen, A. Mediavilla, Steven Levin, N. Roddis, P. M. Lapolla, R. J. Davis, R. C. Butler, Rodrigo Leonardi, Todd Gaier, Luca Terenzi, M. Malaspina, T. Bernardino, Villa, F., Terenzi, L., Sandri, M., Meinhold, P., Poutanen, T., Battaglia, P., Franceschet, C., Hughes, N., Laaninen, M., Lapolla, P., Bersanelli, M., Butler, R. C., Cuttaia, F., D'Arcangelo, O., Frailis, M., Franceschi, E., Galeotta, S., Gregorio, Anna, Leonardi, R., Lowe, S. R., Mandolesi, N., Maris, M., Mendes, L., Mennella, A., Morgante, G., Stringhetti, L., Tomasi, M., Valenziano, L., Zacchei, A., Zonca, A., Aja, B., Artal, E., Balasini, M., Bernardino, T., Blackhurst, E., Boschini, L., Cappellini, B., Cavaliere, F., Colin, A., Colombo, F., Davis, R. J., De La Fuente, L., Edgeley, J., Gaier, T., Galtress, A., Hoyland, R., Jukkala, P., Kettle, D., Kilpia, V. H., Lawrence, C. R., Lawson, D., Leahy, J. P., Leutenegger, P., Levin, S., Maino, D., Malaspina, M., Mediavilla, A., Miccolis, M., Pagan, L., Pascual, J. P., Pasian, F., Pecora, M., Pospieszalski, M., Roddis, N., Salmon, M. J., Seiffert, M., Silvestri, R., Simonetto, A., Sjoman, P., Sozzi, C., Tuovinen, J., Varis, J., Wilkinson, A., Winder, F., and Universidad de Cantabria

Subjects
cosmic microwave background, media_common.quotation_subject, miscellaneous [Techniques], FOS: Physical sciences, Low frequency, 01 natural sciences, 7. Clean energy, Cosmic microwave background, instruments [Space vehicles], techniques-miscellaneous, CMB physics, 0103 physical sciences, cosmic microwave background – cosmology, Black-body radiation, Space vehicles: instruments, Instrumentation: detectors, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), detectors [Instrumentation], Remote sensing, media_common, Physics, Noise temperature, Radiometer, Techniques: miscellaneous, observations – space vehicles, 010308 nuclear & particles physics, Planck ESA mission, Bandwidth (signal processing), Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Linearity, Astronomy and Astrophysics, Space and Planetary Science, Sky, space vehicles-instruments, instruments, instrumentation-detectors, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

14 páginas, 17 figuras, 15 tablas.-- et al., The Low Frequency Instrument (LFI) on-board the ESA Planck satellite carries eleven radiometer subsystems, called radiometer chain assemblies (RCAs), each composed of a pair of pseudo-correlation receivers. We describe the on-ground calibration campaign performed to qualify the flight model RCAs and to measure their pre-launch performances. Each RCA was calibrated in a dedicated flight-like cryogenic environment with the radiometer front-end cooled to 20 K and the back-end at 300 K, and with an external input load cooled to 4 K. A matched load simulating a blackbody at different temperatures was placed in front of the sky horn to derive basic radiometer properties such as noise temperature, gain, and noise performance, e.g. 1/f noise. The spectral response of each detector was measured as was their susceptibility to thermal variation. All eleven LFI RCAs were calibrated. Instrumental parameters measured in these tests, such as noise temperature, bandwidth, radiometer isolation, and linearity, provide essential inputs to the Planck-LFI data analysis., Planck is a project of the European Space Agency with instruments funded by ESA member states, and with special contributions from Denmark and NASA (USA). The Planck-LFI project is developed by an International Consortium lead by Italy and involving Canada, Finland, Germany, Norway, Spain, Switzerland, UK, USA. The Italian contribution to Planck is supported by the Italian Space Agency (ASI). In Finland, the Planck LFI 70 GHz work was supported by the Finnish Funding Agency for Technology and Innovation (Tekes) T.P.’s work was supported in part by the Academy of Finland grants 205800, 214598, 121703, and 121962. T.P. thank Waldemar von Frenckells stiftelse, Magnus Ehrnrooth Foundation, and Väisälä Foundation for financial support. The Spanish participation is funded by Ministerio de Ciencia e Innovacion through the projects ESP2004-07067-C03-01 and AYA2007-68058- C03-02.

Published
2010
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