1997/11/30 by L. Toffolatti, F. Argüeso Gómez, G. De Zotti +4 · 10 citations
Physics and Astronomy · #Anisotropy #Cosmic background radiation #Cosmic microwave background #Cosmic ray #Cosmology and Gravitation Theories #Extragalactic background light #Flux (metallurgy) #Galaxies: Formation, Evolution, Phenomena #Noise (video) #Planck #Quasar #Radio Astronomy Observations and Technology #Spectral density #astro-ph
paper · pdf · doi:10.1046/j.1365-8711.1998.01458.x
published as Mon.Not.Roy.Astron.Soc. 297 (1998) 117-127 · 10 pages, Latex, mn.sty, 8 figures included, MNRAS, in the press. Minor changes in the text. Sections 3.1 and 3.2 have been expanded. Source counts in Table 2 have been slightly changed. Figure 1,2,7 and 8 have been replaced by new versions
arxiv created 1998/03/06 · openalex publication_date 1998/06/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We present predictions for the counts of extragalactic sources, the contributions to fluctuations and their angular power spectrum in each channel foreseen for the Planck Surveyor (formerly COBRAS/SAMBA) mission. The contribution to fluctuations owing to clustering of both radio and far-IR sources is found to be generally small in comparison with the Poisson term; however the relative importance of the clustering contribution increases and may eventually become dominant if sources are identified and subtracted down to faint flux limits. The central Planck frequency bands are expected to be ‘clean’: at high galactic latitude (|b| > 20°), where the reduced galactic noise does not prevent the detection of the extragalactic signal, only a tiny fraction of pixels is found to be contaminated by discrete extragalactic sources. Moreover, the ‘flat’ angular power spectrum of fluctuations resulting from extragalactic sources substantially differs from that of primordial fluctuations; therefore, the removal of contaminating signals is eased even at frequencies where point sources give a sizeable contribution to the foreground noise.