The Sky Polarization Observatory

Cortiglioni, S.; Bernardi, G.; Carretti, E.; Casarini, Luciano; Cecchini, S.; Macculi, C.; Ramponi, M.; Sbarra, C.; Monari, Jader; Orfei, A.; Poloni, M.; Poppi, S.; Boella, G.; Bonometto, S. A.; Colombo, L. P. L.; Gervasi, M.; Sironi, G.; Zannoni, M.; Baralis, M.; Peverini, O. A.; Tascone, R.; Virone, G.; Fabbri, R.; Natale, Vincenzo; Nicastro, L.; Ng, Kin-Wang; Vinyajkin, E. N.; Razin, V. A.; Sazhin, M. V.; Strukov, I. A.; Negri, B.

doi:10.1016/j.newast.2003.11.004

Cited by 28 publications

(13 citation statements)

References 73 publications

(55 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…2 shows the case of the 90 GHz horn of SPOrt (Cortiglioni et al 2004). SPOrt is an experiment devoted to measure the Cosmic Microwave Background Polarization on large angular scales.…”

Section: Axisymmetric Casementioning

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

“…2 shows the case of the 90 GHz horn of SPOrt (Cortiglioni et al 2004). SPOrt is an experiment devoted to measure the Cosmic Microwave Background Polarization on large angular scales.…”

Section: Axisymmetric Casementioning

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

show abstract

“…After a long pioneering phase (Caderni et al 1978;Nanos 1979;Lubin & Smoot 1981;Masi 1984;Partridge et al 1988;Netterfield et al 1995;Wollak et al 1997), the measurement of CMB polarization is today a rapidly growing field; new interest has been sparked especially by the possibility of detecting the BB signature of the inflationary gravity wave background (Keating et al 2001;Subrahmanyan et al 2000;Hedman et al 2002;Piccirillo et al 2002;Delabrouille et al 2002;Masi et al 2002;Villa et al 2002;Kovac et al 2002;Johnson et al 2003;Keating et al 2003;Kogut et al 2003;Farese et al 2004;Leitch et al 2005;Barkats et al 2005;Readhead et al 2004;Cortiglioni et al 2004;Cartwright et al 2005). To date, statistically significant detections of CMB polarization have been reported by the experiments DASI, CAPMAP, CBI and WMAP, all using coherent techniques.…”

Section: Introductionmentioning

confidence: 99%

Instrument, method, brightness, and polarization maps from the 2003 flight of BOOMERanG

Masi¹,

Ade

Bock

et al. 2006

A&A

110

View full text Add to dashboard Cite

Aims. We present the boomerang-03 experiment, and the maps of the Stokes parameters I, Q, U of the microwave sky obtained during a 14 day balloon flight in 2003. Methods. Using a balloon-borne mm-wave telescope with polarization sensitive bolometers, three regions of the southern sky were surveyed: a deep survey (∼90 square degrees) and a shallow survey (∼750 square degrees) at high Galactic latitudes (both centered at RA 5.5h, Dec −45• ) and a survey of ∼300 square degrees across the Galactic plane at RA 9.1h, dec −47• . All three surveys were carried out in three wide frequency bands centered at 145, 245 and 345 GHz, with an angular resolution of ∼10 . Results. The 145 GHz maps of Stokes I are dominated by Cosmic Microwave Background (CMB) temperature anisotropy, which is mapped with high signal to noise ratio. The measured anisotropy pattern is consistent with the pattern measured in the same region by boomerang-98 and by WMAP. The 145 GHz maps of Stokes Q and U provide a robust statistical detection of polarization of the CMB when subjected to a power spectrum analysis. The amplitude of the detected polarization is consistent with that of the CMB in the ΛCDM cosmological scenario. At 145 GHz, in the CMB surveys, the intensity and polarization of the astrophysical foregrounds are found to be negligible with respect to the cosmological signal. At 245 and 345 GHz we detect ISD emission correlated to the 3000 GHz IRAS/DIRBE maps, and give upper limits for any other non-CMB component. When compared to monitors of different interstellar components, the intensity maps of the surveyed section of the Galactic plane show that a variety of emission mechanisms is present in that region.

show abstract

“…Together with the developed theory and the data of absolute measurements of the radio emission from the Moon in a wide frequency range (see [1,4] and references therein), this enabled using the Moon as a standard source with the reference radiation intensity at wavelengths 0.3-30 cm [6]. A number of space-borne and ground-based experiments aimed at measuring the linearly polarized component of the Galactic and cosmic microwave background (CMB) radiation at millimeter and centimeter waves are planned or carried out at present [7][8][9][10][11][12][13][14][15][16]. The Moon is a convenient and, in some cases [17], the only plausible extra-terrestrial calibration source of partially linearly polarized radiation for relatively small-size antennas used in such experiments.…”

Section: Introductionmentioning

confidence: 99%

The moon as a cosmic source of linearly polarized radio emission

Vinyaikin

Krotikov

2007

Radiophys Quantum El

View full text Add to dashboard Cite

We analyze parameters of the partially linearly polarized thermal radio emission from the Moon taking the effects of radiative heat transfer and surface roughness into account. The distributions of the Stokes parameters I, Q, and U over the visible lunar disk are considered. The polarization parameters of the integral radio emission as functions of the frequency and the Moon phase are obtained by integrating the Q and U distributions. We consider the possibility of using the Moon as a reference source of partially linearly polarized radiation for space-borne and ground-based projects aimed at studying polarization of the Galactic radio emission and the cosmic microwave background.

show abstract

The Sky Polarization Observatory

Cited by 28 publications

References 73 publications

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

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

Instrument, method, brightness, and polarization maps from the 2003 flight of BOOMERanG

The moon as a cosmic source of linearly polarized radio emission

Contact Info

Product

Resources

About