B-Pol: detecting primordial gravitational waves generated during inflation

Bernardis, P. de; Bucher, M.; Burigana, C.; Piccirillo, L.

doi:10.1007/s10686-008-9120-y

Cited by 46 publications

(42 citation statements)

References 28 publications

(29 reference statements)

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“…The high‐frequency instrument has no active or fast signal modulation (i.e. other than scanning). CMBPOL/BPOL: design studies have been conducted for satellite mission(s) dedicated to measuring primordial B ‐modes comprising ∼2000 detectors with the ability to measure 0.001 < r < 0.01 if foregrounds allow it (Bock et al 2008; de Bernardis et al 2008). The time‐scale for launch of any selected mission is likely beyond 2020.…”

Section: Cmb Polarization Experimentsmentioning

confidence: 99%

Impact of modulation on CMBB-mode polarization experiments

Brown¹,

Challinor²,

North³

et al. 2009

Monthly Notices of the Royal Astronomical Society

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We investigate the impact of both slow and fast polarization modulation strategies on the science return of upcoming ground‐based experiments aimed at measuring the B‐mode polarization of the cosmic microwave background. Using detailed simulations of the Cℓ OVER experiment, we compare the ability of modulated and un‐modulated observations to recover the signature of gravitational waves in the polarized CMB sky in the presence of a number of anticipated systematic effects. The general expectations that fast modulation is helpful in mitigating low‐frequency detector noise, and that the additional redundancy in the projection of the instrument's polarization sensitivity directions on to the sky when modulating reduces the impact of instrumental polarization, particularly for fast modulation, are borne out by our simulations. Neither low‐frequency polarized atmospheric fluctuations nor systematic errors in the polarization sensitivity directions are mitigated by modulation. Additionally, we find no significant reduction in the effect of pointing errors by modulation. For a Cℓ OVER‐like experiment, pointing jitter should be negligible but any systematic miscalibration of the polarization coordinate reference system results in significant E–B mixing on all angular scales and will require careful control. We also stress the importance of combining data from multiple detectors in order to remove the effects of common‐mode systematics (such as un‐polarized 1/f atmospheric noise) on the measured polarization signal. Finally we compare the performance of our simulated experiment with the predicted performance from a Fisher analysis. We find good agreement between the (optimal) Fisher predictions and the simulated experiment except for the very largest scales where the power spectrum estimator we have used introduces additional variance to the B‐mode signal recovered from our simulations. In terms of detecting the total B‐mode signal, including lensing, the Fisher analysis and the simulations are in excellent agreement. For a detection of the primordial B‐mode signal only, using an input tensor‐to‐scalar ratio of r= 0.026, the Fisher analysis predictions are ∼20 per cent better than the simulated performance.

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Section: Cmb Polarization Experimentsmentioning

confidence: 99%

Impact of modulation on CMBB-mode polarization experiments

Brown¹,

Challinor²,

North³

et al. 2009

Monthly Notices of the Royal Astronomical Society

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“…LISA and LIGO III will be able to discriminate the gravity waves due to fragmentation from those of point sources, such as merging black holes and neutron stars, which have specific ''chirp'' properties [36]. Furthermore, the signal discussed here will not create a significant background for the cosmic microwave polarization experiments, such as B-Pol [37], which can detect the gravity waves with extremely long wavelength. Some additional gravitational waves can be generated by collisions and oscillations of Q balls [3,27].…”

mentioning

confidence: 92%

Gravitational Waves from Fragmentation of a Primordial Scalar Condensate into Q Balls

Kusenko

Mazumdar

2008

Phys. Rev. Lett.

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A generic consequence of supersymmetry is the formation of a scalar condensate along the flat directions of the potential at the end of cosmological inflation. This condensate is usually unstable, and it can fragment into nontopological solitons, Q balls. The gravitational waves produced by the fragmentation can be detected by the Laser Interferometer Space Antenna, Advanced Laser Interferometer Gravitational-Wave Observatory, and Big Bang Observer, which can open an important window to the early Universe and the physics at some very high energy scales.

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“…For all these reasons three studies have been carried out for the NASA (see e.g. [43]), one for the ESA [46], and a very recent one, the COrE medium mission proposal [47], is aimed at building a meter-class polarimeter with 15 frequency channels ranging from 30 to 800 GHz (and more than 6000 diffraction-limited detectors), all modulated by a large rotating reflective HWP which forms the first optical element of the instrument (see figure 4). This strategy optimizes the polarimetric purity of the instrument, thus allowing a full exploitation of the ultra high sensitivity of the focal plane.…”

Section: Cmb Polarization: the Futurementioning

confidence: 99%