An iterative destriping technique for diffuse background polarization data

Sbarra, C.; Carretti, E.; Cortiglioni, S.; Zannoni, M.; Fabbri, R.; Macculi, C.; Tucci, M.

doi:10.1051/0004-6361:20030200

Cited by 17 publications

(15 citation statements)

References 21 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Destriping (Burigana et al 1997b;Delabrouille 1998;Maino et al 1999Maino et al , 2002Revenu et al 2000;Sbarra et al 2003;Poutanen et al 2004;Sutton et al 2009) is a fast map-making method that removes correlated lowfrequency noise from the TOD utilizing crossing points, i.e., the same locations on the sky observed at different times. Correlated noise is modeled as a sequence of ("uniform") baselines, i.e., constant offsets in the TOD.…”

Section: Introductionmentioning

confidence: 99%

Destriping CMB temperature and polarization maps

Kurki-Suonio

Keihänen²,

Keskitalo

et al. 2009

A&A

View full text Add to dashboard Cite

We study destriping as a map-making method for temperature-and-polarization data for cosmic microwave background observations. We present a particular implementation of destriping and study the residual error in output maps, using simulated data corresponding to the 70 GHz channel of the Planck satellite, but assuming idealized detector and beam properties. The relevant residual map is the difference between the output map and a binned map obtained from the signal + white noise part of the data stream. For destriping it can be divided into six components: unmodeled correlated noise, white noise reference baselines, reference baselines of the pixelization noise from the signal, and baseline errors from correlated noise, white noise, and signal. These six components contribute differently to the different angular scales in the maps. We derive analytical results for the first three components. This study is related to Planck LFI activities.

show abstract

Section: Introductionmentioning

confidence: 99%

Destriping CMB temperature and polarization maps

Kurki-Suonio

Keihänen²,

Keskitalo

et al. 2009

A&A

View full text Add to dashboard Cite

show abstract

“…One should also note that the contamination from the anisotropy term is not easily removed by destriping techniques, its level being not constant over the scans performed to observe the sky (e.g. see Revenu et al 2000;Sbarra et al 2003, and references therein for descriptions of destriping techniques), so that a clean instrument is necessary to avoid complex data reductions.…”

Section: Introductionmentioning

confidence: 99%

Antenna instrumental polarization and its effects on E- and B-modes for CMBP observations

Carretti¹,

Cortiglioni²,

Sbarra³

et al. 2004

A&A

Self Cite

View full text Add to dashboard Cite

Abstract. We analyze the instrumental polarization generated by the antenna system (optics and feed horn) due to the unpolarized sky emission. Our equations show that it is given by the convolution of the unpolarized emission map T b (θ, φ) with a sort of instrumental polarization beam Π defined by the co-and cross-polar patterns of the antenna. This result is general, it can be applied to all antenna systems and is valid for all schemes to detect polarization, like correlation and differential polarimeters. The axisymmetric case is attractive: it generates an E-mode-like Π pattern, the contamination does not depend on the scanning strategy and the instrumental polarization map does not have B-mode contamination, making axisymmetric systems suitable to detect the faint B-mode signal of the Cosmic Microwave Background Polarization. The E-mode of the contamination only affects the FWHM scales leaving the larger ones significantly cleaner. Our analysis is also applied to the SPOrt experiment where we find that the contamination of the E-mode is negligible in the -range of interest for CMBP large angular scale investigations (multipole < 10).

show abstract

“…This situation makes having a reliable synchrotron polarized emission template in the 20–100 GHz range very important. This would allow, for instance, reliable numerical simulations to set up and test destriping techniques or foreground separation methods (Revenu et al 2000; Tegmark et al 2000; Sbarra et al 2003, and references therein). At present, only toy models exist, which do not account for the real spatial distribution of both polarization intensity and polarization angles (Kogut & Hinshaw 2000; Giardino et al 2002).…”

Section: Introductionmentioning

confidence: 99%

A new approach for a Galactic synchrotron polarized emission template in the microwave range

Bernardi

Carretti²,

Fabbri

et al. 2003

Monthly Notices RAS

Self Cite

View full text Add to dashboard Cite

We present a new approach to modelling the polarized Galactic synchrotron emission in the microwave range (20–100 GHz), where this radiation is expected to play the leading role in contaminating the cosmic microwave background data. Our method is based on real surveys and aims at providing the real spatial distributions of both polarized intensity and polarization angles. Its main features are the modelling of a polarization horizon to determine the polarized intensity, and the use of starlight optical data to model the polarization angle pattern. Our results are consistent with several existing data, and our template is virtually free from Faraday rotation effects as required at frequencies in the cosmological window.

show abstract

An iterative destriping technique for diffuse background polarization data

Cited by 17 publications

References 21 publications

Destriping CMB temperature and polarization maps

Destriping CMB temperature and polarization maps

Antenna instrumental polarization and its effects on E- and B-modes for CMBP observations

A new approach for a Galactic synchrotron polarized emission template in the microwave range

Contact Info

Product

Resources

About