Polarization Observations in a Low Synchrotron Emission Field at 1.4 GHz

Bernardi, G.; Carretti, E.; Cortiglioni, S.; Sault, R. J.; Kesteven, Michael; Poppi, S.

doi:10.1086/378398

Cited by 25 publications

(40 citation statements)

References 14 publications

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“…Patchy high latitude observations at frequencies between 0.408 and 1.411 GHz are collected in Brouw & Spoelstra (1976). New observations carried out with the ATCA telescope at 1.4 GHz (Bernardi et al 2003) and at 2.3 GHz (Carretti et al 2005) in the same high galactic latitude region observed by our experiment show that the polarized synchrotron emission is very weak. A naive extrapolation to 145 GHz predicts a polarization of 0.2 µK rms, small with respect to the √ EE ∼ 4 µK expected in the concordance model.…”

Section: Introductionsupporting

confidence: 74%

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

Masi¹,

Ade

Bock

et al. 2006

A&A

110

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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.

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Section: Introductionsupporting

confidence: 74%

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

Masi¹,

Ade

Bock

et al. 2006

A&A

110

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“…The other symbols show errors in relative calibration (stars), bolometer time constant (upward-pointing triangles) and polarization angle (downward-pointing triangles). Because errors in absolute calibration and polarization efficiency are multiplicative factors that act identically on each bin, their effect is left off this plot and reported instead in Table 6 1.4 GHz (Bernardi et al 2003) and 2.3 GHz (Carretti et al 2006). A naive extrapolation of these synchrotron results to 145 GHz predicts a signal of 0.2 K rms compared to a $3 K rms expected from the fiducial ÃCDM model given our beam.…”

Section: Foregroundsmentioning

confidence: 91%

A Measurement of the CMB 〈EE〉 Spectrum from the 2003 Flight of BOOMERANG

Montroy

Ade

Bock

et al. 2006

ApJ

242

177

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We report measurements of the CMB polarization power spectra from the 2003 January Antarctic flight of BOOMERANG. The primary results come from 6 days of observation of a patch covering 0.22% of the sky centered near R:A: ¼ 82N5, decl: ¼ À45 . The observations were made using four pairs of polarization-sensitive bolometers operating in bands centered at 145 GHz. Using two independent analysis pipelines, we measure a nonzero hEEi signal in the range 201 < l < 1000 with a significance of 4.8 , a 2 upper limit of 8.6 K 2 for any hBBi contribution, and a 2 upper limit of 7.0 K 2 for the hEBi spectrum. Estimates of foreground intensity fluctuations and the nondetection of hBBi and hEBi signals rule out any significant contribution from Galactic foregrounds. The results are consistent with a ÃCDM cosmology seeded by adiabatic perturbations. We note that this is the first detection of CMB polarization with bolometric detectors.

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“…The diffuse synchrotron emission of the Galaxy is considered to be one of the most relevant polarization contaminant and is expected to dominate the foreground contribution at frequencies less than 100 GHz. Recent measurements performed in a low‐emission area at both 1.4 and 2.3 GHz indicate that the synchrotron signal does not represent an obstacle for the E mode at high Galactic latitude and at frequencies higher than 30 GHz (Bernardi et al 2003; Carretti et al 2005a,b). However, this is just one sample that may not be representative of the situation throughout high Galactic latitudes, and other measurements in different areas are required to confirm this first evaluation.…”

Section: Introductionmentioning

confidence: 99%

Deep 1.4-GHz observations of diffuse polarized emission

Carretti

Poppi

Reich

et al. 2006

Monthly Notices of the Royal Astronomical Society

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Polarized diffuse emission observations at 1.4-GHz in a high Galactic latitude area of the northern Celestial hemisphere are presented. The 3.2 X 3.2 deg^2 field, centred at RA = 10h 58m, Dec = +42deg 18' (B1950), has Galactic coordinates l~172deg, b~+63deg and is located in the region selected as northern target of the BaR-SPOrt experiment. Observations have been performed with the Effelsberg 100-m telescope. We find that the angular power spectra of the E- and B-modes have slopes of beta_E = -1.79 +/- 0.13 and beta_B = -1.74 +/- 0.12, respectively. Because of the very high Galactic latitude and the smooth emission, a weak Faraday rotation action is expected, which allows both a fair extrapolation to Cosmic Microwave Background Polarization (CMBP) frequencies and an estimate of the contamination by Galactic synchrotron emission. We extrapolate the E-mode spectrum up to 32-GHz and confirm the possibility to safely detect the CMBP E-mode signal in the Ka band found in another low emission region (Carretti et al. 2005b). Extrapolated up to 90-GHz, the Galactic synchrotron B-mode looks to compete with the cosmic signal only for models with a tensor-to-scalar perturbation power ratio T/S < 0.001, which is even lower than the T/S value of 0.01 found to be accessible in the only other high Galactic latitude area investigated to date. This suggests that values as low as T/S = 0.01 might be accessed at high Galactic latitudes. Such low emission values can allow a significant red-shift of the best frequency to detect the CMBP B-mode, also reducing the contamination by Galactic dust, and opening interesting perspectives to investigate Inflation models.Comment: 8 pages, 8 figures, accepted for publication in MNRA

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Polarization Observations in a Low Synchrotron Emission Field at 1.4 GHz

Cited by 25 publications

References 14 publications

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

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

A Measurement of the CMB 〈EE〉 Spectrum from the 2003 Flight of BOOMERANG

Deep 1.4-GHz observations of diffuse polarized emission

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