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Villa, F.; Sandri, M.; Mandolesi, N.; Nesti, R.; Bersanelli, M.; Simonetto, A.; Sozzi, C.; D'Arcangelo, O.; Muzzini, V.; Mennella, A.; Guzzi, Pietro Hiram; Radaelli, Paolo G.; Fusi, R.; Alippi, E.

doi:10.1023/a:1026139429820

Cited by 18 publications

(8 citation statements)

References 10 publications

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“…The parameter 𝐴 (0 ≤ 𝐴 ≤ 1) modulates the first region profile between linear and pure sine squared type. The parameters 𝐿 𝑒 /(𝐿 𝑒 + 𝐿 𝑠 ), 𝐴 and 𝑅 𝑠 can be used to optimize the position and frequency stability of the phase center and the compactness of the structure [14].…”

Section: The Corrugated Horn Electromagnetic Designmentioning

confidence: 99%

The LSPE-Strip feed horn array

Franceschet,

Del Torto,

Villa

et al. 2021

Preprint

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In this paper we discuss the design, manufacturing and characterization of the feed horn array of the Strip instrument of the Large Scale Polarization Explorer (LSPE) experiment. Strip is a microwave telescope, operating in the Q-and W-band, for the observation of the polarized emissions from the sky in a large fraction (about 37%) of the Northern hemisphere with subdegree angular resolution. The Strip focal plane is populated by forty-nine Q-band and six W-band corrugated horns, each feeding a cryogenically cooled polarimeter for the detection of the Stokes 𝑄 and 𝑈 components of the polarized signal from the sky. The Q-band channel is designed to accurately monitor Galactic polarized synchrotron emission, while the combination of Q-and W-band will allow the study of atmospheric effects at the observation site, the Observatorio del Teide, in Tenerife. In this paper we focus on the development of the Strip corrugated feed horns, including design requirements, engineering and manufacturing, as well as detailed characterization and performance verification.

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Section: The Corrugated Horn Electromagnetic Designmentioning

confidence: 99%

The LSPE-Strip feed horn array

Franceschet,

Del Torto,

Villa

et al. 2021

Preprint

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“…This led to a telescope in the 1.5 m aperture class to ensure the desired resolution with an adequate rejection of straylight contamination (Mandolesi et al 2000a;Villa et al 2002). In general, a trade-off occurs between main-beam resolution (half-power beam width, HPBW) and the illumination by the feeds of the edges of both the primary and sub-reflector (edge taper), which in turn drives the stray-light contamination effect.…”

Section: Angular Resolutionmentioning

confidence: 99%

“…The LFI feeds must have highly symmetric beams, low levels of side lobes (−35 dB), cross-polarisation (−30 dB), and return loss (−25 dB), as well as good control of the phase centre location (Villa et al 2002). Dual profiled conical corrugated horns have been designed to meet these requirements, a solution that has the added advantage of high compactness and design flexibility.…”

Section: Feed Hornsmentioning

confidence: 99%

Planckpre-launch status: Design and description of the Low Frequency Instrument

Bersanelli

Mandolesi

Butler

et al. 2010

A&A

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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.

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“…The feed horn development programme started in the early stages of the mission with prototype demonstrators (Bersanelli et al 1998), followed by the elegant bread board (Villa et al 2002) and finally by the qualification (D'Arcangelo et al 2005) and flight models (Villa et al 2009).…”

Section: Opticsmentioning

confidence: 99%

Planck pre-launch status: the Planck-LFI programme

Mandolesi,

Bersanelli,

Butler

et al. 2010

Preprint

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This paper provides an overview of the Low Frequency Instrument (LFI) programme within the ESA Planck mission. The LFI instrument has been developed to produce high precision maps of the microwave sky at frequencies in the range 27-77 GHz, below the peak of the cosmic microwave background (CMB) radiation spectrum. The scientific goals are described, ranging from fundamental cosmology to Galactic and extragalactic astrophysics. The instrument design and development are outlined, together with the model philosophy and testing strategy. The instrument is presented in the context of the Planck mission. The LFI approach to ground and inflight calibration is described. We also describe the LFI ground segment. We present the results of a number of tests demonstrating the capability of the LFI data processing centre (DPC) to properly reduce and analyse LFI flight data, from telemetry information to calibrated and cleaned time ordered data, sky maps at each frequency (in temperature and polarization), component emission maps (CMB and diffuse foregrounds), catalogs for various classes of sources (the Early Release Compact Source Catalogue and the Final Compact Source Catalogue). The organization of the LFI consortium is briefly presented as well as the role of the core team in data analysis and scientific exploitation. All tests carried out on the LFI flight model demonstrate the excellent performance of the instrument and its various subunits. The data analysis pipeline has been tested and its main steps verified. In the first three months after launch, the commissioning, calibration, performance, and verification phases will be completed, after which Planck will begin its operational life, in which LFI will have an integral part.

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Cited by 18 publications

References 10 publications

The LSPE-Strip feed horn array

The LSPE-Strip feed horn array

Planckpre-launch status: Design and description of the Low Frequency Instrument

Planck pre-launch status: the Planck-LFI programme

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