The low frequency instrument of the Planck mission

Villa, F.; Mandolesi, N.; Bersanelli, M.; Butler, R. C.; Burigana, C.; Mennella, A.; Morgante, G.; Sandri, M.; Valenziano, L.

doi:10.1063/1.1471837

Cited by 15 publications

(18 citation statements)

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“…The average of the FWHM eff in the relevant regions (between ∼ −2.5 and ∼ 2.5 degrees for the 1.3m telescopes and between ∼ −2 and ∼ 2 degrees for the 1.5m telescopes) are similar for Standard and Aplanatic configurations with same aperture ( 10 arcmin for the 1.5 m telescopes and even better for the 1.75 m telescope). On the other hand the FWHM eff of beams located at angular distances from the center roughly equal or larger than 1 • , where typical Planck (LFI and also HFI) feeds are located, is somewhat better and also the spread of the FWHM eff 's of the different beams is smaller for the Aplanatic configuration (Villa et al 1998b).…”

Section: Telescope Designmentioning

confidence: 98%

“…Among other possible design configurations, an alternative to the DragoneMizuguchi Gregorian off-axis solution (in short "Standard") is represented by the Aplanatic Gregorian design (in short "Aplanatic"), firstly proposed by Mark Dragovan and the LFI Consortium in order to reduce the coma and the spherical aberration on a large portion of the focal surface (Villa et al 1998b). This new solution is obtained by changing the conic constants of both mirrors (both ellipsoids of rotation) in order to satisfy the Aplanatic Condition.…”

Section: Telescope Designmentioning

confidence: 99%

“…To analyze a general dual reflector system a dedicated software has been implemented at Istituto TeSRE/CNR (Villa et al 1998b). The code calculates the amplitude and phase distribution on a regular grid of points on the tilted aperture plane (normal to azimuth and elevation directions on the sky).…”

Section: Telescope Designmentioning

confidence: 99%

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Planck low frequency instrument

Mandolesi

Burigana

Butler

et al. 2002

AIP Conference Proceedings

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-The Low Frequency Instrument (LFI) of the "Planck Surveyor" ESA mission will perform high-resolution imaging of the Cosmic Microwave Background anisotropies at four frequencies in the 30-100 GHz range. We review the LFI main scientific objectives, the current status of the instrument design and the on-going effort to develop software simulations of the LFI observations. In particular we discuss the design status of the PLANCK telescope, which is critical for reaching adequate effective angular resolution.

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Section: Telescope Designmentioning

confidence: 98%

Section: Telescope Designmentioning

confidence: 99%

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Planck low frequency instrument

Mandolesi

Burigana

Butler

et al. 2002

AIP Conference Proceedings

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“…Bersanelli et al 1996;Tauber 2000), significant efforts have been carried out to significantly reduce the main beam distortions produced by optical aberrations (see e.g. Villa et al 1998;Mandolesi et al 2000a). On the other hand, even optimizing the optical design, a certain level of beam asymmetry can not be completely eliminated (see e.g.…”

Section: Introductionmentioning

confidence: 99%

Beam deconvolution in noisy CMB maps

Burigana¹,

Sáez²

2003

A&A

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Abstract. The subject of this paper is beam deconvolution in small angular scale CMB experiments. The beam effect is reversed using the Jacobi iterative method, which was designed to solved systems of algebraic linear equations. The beam is a non circular one which moves according to the observational strategy. A certain realistic level of Gaussian instrumental noise is assumed. The method applies to small scale CMB experiments in general (cases A and B), but we have put particular attention on P mission at 100 GHz (cases C and D). In cases B and D, where noise is present, deconvolution allows to correct the main beam distortion effect and recover the initial angular power spectrum up to the end of the fifth acoustic peak. An encouraging result whose importance is analyzed in detail. More work about deconvolution in the presence of other systematics is in progress. This paper is related to the P LFI activities.

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“…In 15 months 2 of continuous measurements from the Lagrangian point L 2 , Planck will provide cosmic-variance-and foreground-limited measurements of the cosmic microwave background temperature anisotropies by scanning the sky in almost great circles with a 1.5 m dual reflector aplanatic telescope (Tauber et al 2010;Martin et al 2004;Villa et al 2002;Dupac & Tauber 2005).…”

Section: Introductionmentioning

confidence: 99%

Planckpre-launch status: Low Frequency Instrument calibration and expected scientific performance

Mennella¹,

Bersanelli²,

Butler

et al. 2010

A&A

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We present the calibration and scientific performance parameters of the Planck Low Frequency Instrument (LFI) measured during the ground cryogenic test campaign. These parameters characterise the instrument response and constitute our optimal pre-launch knowledge of the LFI scientific performance. The LFI shows excellent 1/ f stability and rejection of instrumental systematic effects; its measured noise performance shows that LFI is the most sensitive instrument of its kind. The calibration parameters will be updated during flight operations until the end of the mission.

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The low frequency instrument of the Planck mission

Cited by 15 publications

References 0 publications

Planck low frequency instrument

Planck low frequency instrument

Beam deconvolution in noisy CMB maps

Planckpre-launch status: Low Frequency Instrument calibration and expected scientific performance

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