PRISM (Polarized Radiation Imaging and Spectroscopy Mission): A White Paper on the Ultimate Polarimetric Spectro-Imaging of the Microwave and Far-Infrared Sky

Collaboration, PRISM; André, P.; Baccigalupi, C.; Barbosa, Domingos; Bartlett, J. G.; Bartolo, N.; Battistelli, E. S.; Battye, Richard A.; Bendo, G. J.; Bernard, J.-P.; Bersanelli, M.; Béthermin, M.; Bielewicz, P.; Bonaldi, A.; Bouchet, F. R.; Boulanger, F.; Brand, J.; Bucher, M.; Burigana, C.; Cai, Zhen-Yi; Casasola, V.; Castex, G.; Challinor, A.; Chluba, Jens; Colafrancesco, S.; Cuttaia, F.; Dalessandro, Giuseppe; Davis, R. J.; Avillez, Miguel de; Bernardis, P. de; Petris, M. De; Rosa, A. de; Zotti, G. de; Delabrouille, J.; Dickinson, C.; Diego, Jose Maria; Falgarone, É.; Ferreira, Pedro G.; Ferrière, K.; Finelli⋆, F.; Fletcher, Andrew; Fuller, G. A.; Galli, S.; Ganga, K.; García-Bellido, J.; Ghribi, A.; González‐Nuevo, J.; Grainge, Keith; Gruppuso, A.; Hall, Alex; Hernandez-Monteagudo, Carlos; Jackson, Mark J.; Jaffe, A. H.; Khatri, Rishi; Lamagna, L.; Lattanzi, M.; Leahy, Paddy; Liguori, M.; Liuzzo, E.; López‐Caniego, M.; Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Masi, S.; Mangilli, A.; Massardi, M.; Matarrese, S.; Melchiorri, A.; Melin, Jean-Baptiste; Mennella, A.; Mignano, A.; Miville-Deschênes, M.-A.; Nati, F.; Natoli, P.; Negrello, M.; Noviello, F.; Paci, F.; Paladino, R.; Paoletti, D.; Perrotta, F.; Piacentini, F.; Piat, M.; Piccirillo, L.; Pisano, G.; Polenta, G.; Ricciardi, S.; Roman, M.; Rubiño-Martín, J. A.; Salatino, Maria; Schillaci, A.; Shellard, P.; Silk, Joseph; Stompor, R.; Sunyaev, R.; Tartari, A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Trombetti, T.; Tucci, M.; Tent, B. Van; Verde, Licia; Wandelt, B. D.; Withington, S.

doi:10.48550/arxiv.1306.2259

Cited by 105 publications

(148 citation statements)

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“…Planck's maps have a sensitivity (around 85 µK-arcmin for the SMICA map) which is a factor of 4 lower than WMAP (around 360 µK-arcmin), corresponding to errors in C T B l smaller by a factor of 16. The recent PRISM satellite proposal [99] envisions full-sky polarization maps with sensitivity of 3 µK-arcmin, which would give C T B l errors smaller than the WMAP errors used here by a factor of 10 4 .…”

Section: Discussionmentioning

confidence: 94%

Primordial magnetic helicity constraints from WMAP nine-year data

et al. 2014

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If a primordial magnetic field in the Universe has nonzero helicity, the violation of parity symmetry results in nonzero correlations between cosmic microwave background temperature and B-mode polarization. In this paper we derive approximations to the relevant microwave background power spectra arising from a helical magnetic field. Using the cross-power spectrum between temperature and B-mode polarization from the WMAP nine-year data, we set a 95% confidence level upper limit on the helicity amplitude to be 10 nG 2 Gpc for helicity spectral index n H ¼ −1.9, for a cosmological magnetic field with effective field strength of 3 nG and a power-law index n B ¼ −2.9 near the scale-invariant value. Future microwave background polarization maps with greater sensitivity will be able to detect the helicity of an inflationary magnetic field well below the maximum value allowed by microwave background constraints on the magnetic field amplitude.

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Section: Discussionmentioning

confidence: 94%

Primordial magnetic helicity constraints from WMAP nine-year data

et al. 2014

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“…Actually, we can show that the kinetic mixing between axions and mesons does not change the number of massless axions [33]. The CMB experiments PIXIE [34]/PRISM [35] and the axion helio scope experiment IAXO [36] utilize the CS coupling of an axion to the EM field, g aγ E • B. Hence, they do not directly give constraints on f a .…”

Section: Potential and Self-interactions Of Axionmentioning

confidence: 99%

“…Figure 2. Various cosmophysical phenomena that may be caused by string axions and constraints by future experiments in the plane of the axion parameters (m a , f a ).The CMB experiments PIXIE[34]/PRISM[35] and the axion helio scope experiment IAXO[36] utilize the CS coupling of an axion to the EM field, g aγ E • B. Hence, they do not directly give constraints on f a .…”

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confidence: 99%

The bosenova and axiverse

Yoshino

Kodama

2015

Class. Quantum Grav.

101

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Abstract. We report some new interesting features of the dynamics of a string axion field (i.e., a (pseudo-)scalar field with tiny mass with sine-Gordon-type selfinteraction) around a rotating black hole in three respects. First, we revisit the calculation of the growth rate of superradiant instability, and show that in some cases, overtone modes have larger growth rates than the fundamental mode with the same angular quantum numbers when the black hole is rapidly rotating. Next, we study the dynamical evolution of the scalar field caused by the nonlinear self-interaction, taking attention to the dependence of the dynamical phenomena on the axion mass and the modes. The cases in which two superradiantly unstable modes are excited simultaneously are also studied. Finally, we report on our preliminary simulations for gravitational wave emission from the dynamical axion cloud in the Schwarzschild background approximation. Our result suggests that fairly strong gravitational wave burst is emitted during the bosenova, which could be detected by the ground-based detectors if it happens in Our Galaxy or nearby galaxies.

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“…However the existence of such counterexamples is of limited importance: one would like to understand when large field inflation is expected given a measurement of r even if there might be fine-tuned models which give smaller field ranges for this value of r. Given the central value for n s from Planck, our results imply that super-Planckian field ranges require a tensor-to-scalar ratio that exceeds 2 • 10 −5 . Planned future CMB experiments, such as COrE [24,25] and PRISM [26][27][28], might bring the sensitivity down to 10 −4 . In contrast to what one would conclude from the original Lyth bound, our results imply that a small detectable r still corresponds to super-Planckian field ranges.…”

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confidence: 99%

Lyth bound of inflation with a tilt

et al. 2014

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We provide strong evidence for universality of the inflationary field range: given an accurate measurement of ðn s ; rÞ, one can infer Δϕ in a model-independent way in the sub-Planckian regime for a range of universality classes of inflationary models. Both the tensor-to-scalar ratio as well as the spectral tilt are essential for the field range. Given the Planck constraints on n s , the Lyth bound is strengthened by two orders of magnitude: whereas the original bound gives a sub-Planckian field range for r ≲ 2 × 10 −3 , we find that n s ¼ 0.96 brings this down to r ≲ 2 × 10 −5 .

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PRISM (Polarized Radiation Imaging and Spectroscopy Mission): A White Paper on the Ultimate Polarimetric Spectro-Imaging of the Microwave and Far-Infrared Sky

Cited by 105 publications

References 0 publications

Primordial magnetic helicity constraints from WMAP nine-year data

Primordial magnetic helicity constraints from WMAP nine-year data

The bosenova and axiverse

Lyth bound of inflation with a tilt

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