Foregrounds and CMB experiments

Bouchet, F. R.; Gispert, R.

doi:10.1016/s1384-1076(99)00027-5

Cited by 153 publications

(167 citation statements)

References 68 publications

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“…The spectral index of α T = 1.67 ± 0.15 that we derived from the Parkes data for the total intensity (T ) is significantly lower than the spectral index values derived from large sky radio survey (Bouchet & Gispert 1999;Giardino et al 2001). However this value refers to the raw data which beside the diffuse emission contains a significant population of point sources.…”

Section: Comparison With Previous Results and Discussioncontrasting

confidence: 72%

Towards a model of full-sky Galactic synchrotron intensity and linear polarisation: A re-analysis of the Parkes data

Giardino

Banday

Górski

et al. 2002

A&A

133

198

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Abstract. We have analysed the angular power spectra of the Parkes radio continuum and polarisation survey of the Southern galactic plane at 2.4 GHz. We have found that in the multipole range l = 40−250 the angular power spectrum of the polarised intensity is well described by a power-law spectrum with fitted spectral index αL = 2.37 ± 0.21. In the same multipole range the angular power spectra of the E and B components of the polarised signal are significantly flatter, with fitted spectral indices respectively of αE = 1.57 ± 0.12 and αB = 1.45 ± 0.12. Temperature fluctuations in the E and B components are mostly determined by variations in polarisation angle. We have combined these results with other data from available radio surveys in order to produce a full-sky toy model of Galactic synchrotron intensity and linear polarisation at high frequencies (ν > ∼ 10 GHz). This can be used to study the feasibility of measuring the Cosmic Microwave Background polarisation with forthcoming experiments and satellite missions.

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Section: Comparison With Previous Results and Discussioncontrasting

confidence: 72%

Towards a model of full-sky Galactic synchrotron intensity and linear polarisation: A re-analysis of the Parkes data

Giardino

Banday

Górski

et al. 2002

A&A

133

198

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“…3, dotted long-dashed line). The component separation was performed using Wiener filtering (Bouchet & Gispert 1999), and the residuals account for the galactic contributions and the instrumental noise. The total δv rms (including the contribution from the CMB and kinetic SZ effect (Fig.…”

Section: Resultsmentioning

confidence: 99%

“…This requires a good separation of the thermal and kinetic components of the SZ effect which can be achieved, in principle, through accurate measurements at two or more millimetre/submillimetre wavelengths (Hobson et al 1998;Bouchet & Gispert 1999) as expected for the Planck mission. Astrophysical or instrumental contributions will introduce systematic errors into the determination of the peculiar velocity v r .…”

Section: Methodsmentioning

confidence: 99%

How accurately can the SZ effect measure peculiar cluster velocities and bulk flows?

Aghanim

Górski

Puget

2001

A&A

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Abstract. The Sunyaev-Zel'dovich effect is a powerful tool for cosmology that can be used to measure the radial peculiar velocities of galaxy clusters, and thus to test, and constrain theories of structure formation and evolution. This requires, in principle, an accurate measurement of the effect, a good separation between the SunyaevZel'dovich components, and a good understanding of the sources contributing to the signal and their effect on the measured velocity. In this study, we evaluate the error in the individual radial peculiar velocities determined with Sunyaev-Zel'dovich measurements. We estimate, for three cosmological models, the errors induced by the major contributing signals (primary Cosmic Microwave Background anisotropies, Sunyaev-Zel'dovich effect due to the background cluster population, residuals from component separation and instrumental noise). We generalise our results to estimate the error in the bulk velocity on large scales. In this context, we investigate the limitation due to the Sunyaev-Zel'dovich source (or spatial) confusion in a Planck-like instrumental configuration. Finally, we propose a strategy based on the future all-sky Sunyaev-Zel'dovich survey, that will be provided by the Planck mission, to measure accurately the bulk velocities on large scales up to redshift 1, or more.

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“…It has long been recognised that planning future observations and developing methods for analysing CMB data sets both require realistic models and simulations of the sky emission and of its observations (Gawiser et al 1998;Bouchet & Gispert 1999;Giardino et al 2002;de Oliveira-Costa et al 2008;Sehgal et al 2007Sehgal et al , 2010. For preparing the analysis of CMB data sets such as those of the Planck mission, it has proven useful to put a model of sky emission together, the Planck Sky Model (PSM), which can be used to predict or simulate sky emission for various A&A 553, A96 (2013) assumptions and various parameter sets.…”

Section: Introductionmentioning

confidence: 99%

The pre-launchPlanckSky Model: a model of sky emission at submillimetre to centimetre wavelengths

Delabrouille

Betoule

Melin

et al. 2013

A&A

214

231

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We present the Planck Sky Model (PSM), a parametric model for generating all-sky, few arcminute resolution maps of sky emission at submillimetre to centimetre wavelengths, in both intensity and polarisation. Several options are implemented to model the cosmic microwave background, Galactic diffuse emission (synchrotron, free-free, thermal and spinning dust, CO lines), Galactic H ii regions, extragalactic radio sources, dusty galaxies, and thermal and kinetic Sunyaev-Zeldovich signals from clusters of galaxies. Each component is simulated by means of educated interpolations/extrapolations of data sets available at the time of the launch of the Planck mission, complemented by state-of-the-art models of the emission. Distinctive features of the simulations are spatially varying spectral properties of synchrotron and dust; different spectral parameters for each point source; modelling of the clustering properties of extragalactic sources and of the power spectrum of fluctuations in the cosmic infrared background. The PSM enables the production of random realisations of the sky emission, constrained to match observational data within their uncertainties. It is implemented in a software package that is regularly updated with incoming information from observations. The model is expected to serve as a useful tool for optimising planned microwave and sub-millimetre surveys and testing data processing and analysis pipelines. It is, in particular, used to develop and validate data analysis pipelines within the Planck collaboration. A version of the software that can be used for simulating the observations for a variety of experiments is made available on a dedicated website.

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Foregrounds and CMB experiments

Cited by 153 publications

References 68 publications

Towards a model of full-sky Galactic synchrotron intensity and linear polarisation: A re-analysis of the Parkes data

Towards a model of full-sky Galactic synchrotron intensity and linear polarisation: A re-analysis of the Parkes data

How accurately can the SZ effect measure peculiar cluster velocities and bulk flows?

The pre-launchPlanckSky Model: a model of sky emission at submillimetre to centimetre wavelengths

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