Isotropic wavelets: a powerful tool to extract point sources from cosmic microwave background maps |
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| Authors: | L Cayón J L Sanz † R B Barreiro E Martínez-González P Vielva L Toffolatti J Silk J M Diego F Argüeso |
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| Institution: | Instituto de Física de Cantabria, Fac. Ciencias, Av. los Castros s/n, 39005 Santander, Spain;Departamento de Física Moderna, Universidad de Cantabria, 39005 Santander, Spain;Astrophysics Group, Cavendish Laboratory, Madingley Road, Cambridge CB3 0HE;Departamento de Física, Universidad de Oviedo, c/ Calvo Sotelo s/n, 33007 Oviedo, Spain;Department of Physics, Nuclear &Astrophysics Laboratory, Keble Road, Oxford OX1 3RH; Departamento de Matemáticas, Universidad de Oviedo, c/ Calvo Sotelo s/n, 33007 Oviedo, Spain |
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| Abstract: | It is the aim of this paper to introduce the use of isotropic wavelets to detect and determine the flux of point sources appearing in cosmic microwave background (CMB) maps. The most suitable wavelet to detect point sources filtered with a Gaussian beam is the 'Mexican Hat'. An analytical expression of the wavelet coefficient obtained in the presence of a point source is provided and used in the detection and flux estimation methods presented. For illustration the method is applied to two simulations (assuming Planck mission characteristics) dominated by CMB (100 GHz) and dust (857 GHz), as these will be the two signals dominating at low and high frequencies respectively in the Planck channels. We are able to detect bright sources above 1.58 Jy at 857 GHz (82 per cent of all sources) and above 0.36 Jy at 100 GHz (100 per cent of all), with errors in the flux estimation below 25 per cent. The main advantage of this method is that nothing has to be assumed about the underlying field, i.e. about the nature and properties of the signal plus noise present in the maps. This is not the case in the detection method presented by Tegmark & Oliveira-Costa. Both methods are compared, producing similar results. |
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| Keywords: | methods: data analysis cosmic microwave background |
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