Making maps from Planck LFI 30 GHz data with asymmetric beams and cooler noise

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dc.contributor University of Helsinki, Particle Physics and Astrophysics en
dc.contributor University of Helsinki, Helsinki Institute of Physics en
dc.contributor University of Helsinki, Helsinki Institute of Physics en
dc.contributor University of Helsinki, Helsinki Institute of Physics en
dc.contributor.author Ashdown, M. A. J
dc.contributor.author Bacciagalupi, C
dc.contributor.author Bartlett, J. G
dc.contributor.author Borrill, J
dc.contributor.author Cantalupo, G. de
dc.contributor.author Troia, G. de
dc.contributor.author Gorski, K. M
dc.contributor.author Keihänen, Elina
dc.contributor.author Keskitalo, Reijo
dc.contributor.author Kurki-Suonio, Hannu
dc.contributor.author Poutanen, Torsti
dc.date.accessioned 2018-03-23T10:19:01Z
dc.date.available 2018-03-23T10:19:01Z
dc.date.issued 2009
dc.identifier.citation Ashdown , M A J , Bacciagalupi , C , Bartlett , J G , Borrill , J , Cantalupo , G D , Troia , G D , Gorski , K M , Keihänen , E , Keskitalo , R , Kurki-Suonio , H & Poutanen , T 2009 , ' Making maps from Planck LFI 30 GHz data with asymmetric beams and cooler noise ' , Astronomy & Astrophysics , vol. 493 , pp. 753-783 . https://doi.org/10.1051/0004-6361:200810381 en
dc.identifier.issn 0004-6361
dc.identifier.other PURE: 1158595
dc.identifier.other PURE UUID: 10d6e78b-0929-43c0-b96d-2c9bbc0e8ad9
dc.identifier.other dawa_publication: 189969
dc.identifier.other WOS: 000262601300046
dc.identifier.other Scopus: 59049099299
dc.identifier.other ORCID: /0000-0002-4618-3063/work/43223683
dc.identifier.other ORCID: /0000-0003-1804-7715/work/43224025
dc.identifier.uri http://hdl.handle.net/10138/233744
dc.description.abstract The Planck satellite will observe the full sky at nine frequencies from 30 to 857 GHz. Temperature and polarization frequency maps made from these observations are prime deliverables of the Planck mission. The goal of this paper is to examine the effects of four realistic instrument systematics in the 30 GHz frequency maps: non-axially-symmetric beams, sample integration, sorption cooler noise, and pointing errors. We simulated one-year long observations of four 30 GHz detectors. The simulated timestreams contained cosmic microwave background (CMB) signal, foreground components ( both galactic and extra-galactic), instrument noise ( correlated and white), and the four instrument systematic effects. We made maps from the timelines and examined the magnitudes of the systematics effects in the maps and their angular power spectra. We also compared the maps of different mapmaking codes to see how they performed. We used five mapmaking codes ( two destripers and three optimal codes). None of our mapmaking codes makes any attempt to deconvolve the beam from its output map. Therefore all our maps had similar smoothing due to beams and sample integration. This is a complicated smoothing, because each map pixel has its own effective beam. Temperature to polarization cross-coupling due to beam mismatch causes a detectable bias in the TE spectrum of the CMB map. The effects of cooler noise and pointing errors did not appear to be major concerns for the 30 GHz channel. The only essential difference found so far between mapmaking codes that affects accuracy ( in terms of residual root-mean-square) is baseline length. All optimal codes give essentially indistinguishable results. A destriper gives the same result as the optimal codes when the baseline is set short enough ( Madam). For longer baselines destripers (Springtide and Madam) require less computing resources but deliver a noisier map. sv
dc.format.extent 31
dc.language.iso eng
dc.relation.ispartof Astronomy & Astrophysics
dc.rights en
dc.subject 114 Physical sciences en
dc.title Making maps from Planck LFI 30 GHz data with asymmetric beams and cooler noise en
dc.type Article
dc.description.version Peer reviewed
dc.identifier.doi https://doi.org/10.1051/0004-6361:200810381
dc.type.uri info:eu-repo/semantics/other
dc.type.uri info:eu-repo/semantics/publishedVersion
dc.contributor.pbl
dc.contributor.pbl

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