The Planck Mission

Tauber, J. A.

doi:10.1017/s0074180900226454

Cited by 22 publications

(14 citation statements)

References 19 publications

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“…The follow-up survey catalog is ∼100% reliable, whilst the scanning survey catalog includes some sources with only 50% reliability. It is expected that the primary use of this catalog will be to provide foreground masks for CMB missions such as Planck (Tauber, 2005) and the South Pole Telescope (Stark et al, 1998), where completeness is more important than accurate fluxes or a high reliability. Table 3 The first page of the scanning survey catalog.…”

Section: Discussionmentioning

confidence: 99%

“…Radio galaxy evolution can be explored via AGN, whilst the nature and evolution of the universe can be explored via studies of the cosmic microwave background (CMB). High resolution radio surveys are crucial for the removal of foreground radio sources (de Zotti et al, 1999) for CMB missions such as Planck (Tauber, 2005), Fermi (Ritz et al, 2009) and the South Pole Telescope (Stark et al, 1998), where foreground point sources contaminate the measured CMB anisotropy at angular scales of less than 30 arc-minutes.…”

Section: Introductionmentioning

confidence: 99%

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The Australia telescope 20 GHz survey: hardware, observing strategy, and scanning survey catalog

et al. 2011

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The Australia Telescope 20GHz (AT20G) survey is a large area (2π sr), sensitive (40 mJy), high frequency (20 GHz) survey of the southern sky. The survey was conducted in two parts: an initial fast scanning survey, and a series of more accurate follow-up observations. The follow-up survey catalog has been presented by Murphy et al. (2010). In this paper we discuss the hardware setup and scanning survey strategy as well as the production of the scanning survey catalog.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Australia telescope 20 GHz survey: hardware, observing strategy, and scanning survey catalog

et al. 2011

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“…In particular, the Wilkinson Microwave Anisotropy Probe (WMAP) [20], [21] is observing the sky at 23, 33, 41, 61 and 94 GHz and the upcoming ESA's Planck satellite [22] will observe the sky in nine frequency channels ranging from 30 to 857 GHz. Multi-wavelength data can be used to improve the detection/separation of astrophysical components.…”

Section: Introductionmentioning

confidence: 99%

Matrix Filters for the Detection of Extragalactic Point Sources in Cosmic Microwave Background Images

Herranz

Sanz

2008

IEEE J. Sel. Top. Signal Process.

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Abstract-In this paper we introduce a new linear filtering technique, the so-called matrix filters, that maximizes the signalto-interference ratio of compact sources of unknown intensity embedded in a set of images by taking into account the crosscorrelations between the different channels. By construction, the new filtering technique outperforms (or at least equals) the standard matched filter applied on individual images. An immediate application is the detection of extragalactic point sources in Cosmic Microwave Background images obtained at different wavelengths. We test the new technique in two simulated cases: a simple two-channel case with ideal correlated color noise and more realistic simulations of the sky as it will be observed by the LFI instrument of the upcoming ESA's Planck mission. In both cases we observe an improvement with respect to the standard matched filter in terms of signal-to-noise interference, number of detections and number of false alarms.

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“…For example, in the context of the ESA P project 1 (see e.g. 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).…”

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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The Planck Mission

Cited by 22 publications

References 19 publications

The Australia telescope 20 GHz survey: hardware, observing strategy, and scanning survey catalog

The Australia telescope 20 GHz survey: hardware, observing strategy, and scanning survey catalog

Matrix Filters for the Detection of Extragalactic Point Sources in Cosmic Microwave Background Images

Beam deconvolution in noisy CMB maps

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