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46 results on '"gravitational radiation: primordial"'

1. Monomial warm inflation revisited

Author: Ballesteros, Guillermo, Pérez Rodríguez, Alejandro, and Pierre, Mathias
Subjects: power spectrum: scalar, curvature: fluctuation, correction: thermal, gravitational radiation: primordial, Fokker-Planck equation, dissipation, inflation: stochastic, numerical calculations, inflaton
Abstract: We revisit the idea that the inflaton may have dissipated part of its energy into a thermal bath during inflation, considering monomial inflationary potentials and three different forms of dissipation rate. Using a numerical Fokker-Planck approach to describe the stochastic dynamics of inflationary fluctuations, we confront this scenario with current bounds on the spectrum of curvature fluctuations and primordial gravitational waves. We also obtain analytical approximations that outperform those frequently used in previous analyses. We show that only our numerical Fokker-Planck method is accurate, fast and precise enough to test these models against current data. We advocate its use in future studies of warm inflation. We also apply the stochastic inflation formalism to this scenario, finding that a commonly implemented large thermal correction to the primordial spectrum--that had been argued to become apparent with it--is actually not required. Improved bounds on the scalar spectral index will further constrain warm inflation in the near future.
Published: 2023
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2. The Latest Constraints on Inflationary B-modes from the BICEP/Keck Telescopes

Author: Collaboration, BICEP/Keck, Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Thakur, R. Basu, Beck, D., Bischoff, C., Bock, J. J., Boenish, H., Bullock, E., Buza, V., Cheshire IV, J. R., Connors, J., Cornelison, J., Crumrine, M., Cukierman, A., Denison, E. V., Dierickx, M., Duband, L., Eiben, M., Fatigoni, S., Filippini, J. P., Fliescher, S., Giannakopoulos, C., Goeckner-Wald, N., Goldfinger, D. C., Grayson, J., Grimes, P., Halal, G., Hall, G., Halpern, M., Hand, E., Harrison, S., Henderson, S., Hildebrandt, S. R., Hilton, G. C., Hubmayr, J., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Karpel, E., Kefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kuo, C. L., Lau, K., Leitch, E. M., Lennox, A., Megerian, K. G., Minutolo, L., Moncelsi, L., Nakato, Y., Namikawa, T., Nguyen, H. T., O'Brient, R., Ogburn IV, R. W., Palladino, S., Petroff, M., Prouve, T., Pryke, C., Racine, B., Reintsema, C. D., Richter, S., Schillaci, A., Schmitt, B. L., Schwarz, R., Sheehy, C. D., Singari, B., Soliman, A., Germaine, T. St, Steinbach, B., Sudiwala, R. V., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C., Turner, A., Umilta, C., Verges, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wong, C. L., Wu, W. L. K., Yang, H., Yoon, K. W., Young, E., Yu, C., Zeng, L., Zhang, C., Zhang, S., Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and BICEP/Keck
Subjects: noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), beam: polarization, satellite: Planck, statistical analysis: confidence limit, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation: primordial, pole, FOS: Physical sciences, cosmic background radiation: polarization, cosmological model: dust, Astrophysics::Cosmology and Extragalactic Astrophysics, BICEP, thermal, B-mode, WMAP, cosmological model: parameter space, synchrotron, Astrophysics::Earth and Planetary Astrophysics, galaxy, inflation, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: For the past decade, the BICEP/Keck collaboration has been operating a series of telescopes at the Amundsen-Scott South Pole Station measuring degree-scale $B$-mode polarization imprinted in the Cosmic Microwave Background (CMB) by primordial gravitational waves (PGWs). These telescopes are compact refracting polarimeters mapping about 2% of the sky, observing at a broad range of frequencies to account for the polarized foreground from Galactic synchrotron and thermal dust emission. Our latest publication "BK18" utilizes the data collected up to the 2018 observing season, in conjunction with the publicly available WMAP and Planck data, to constrain the tensor-to-scalar ratio $r$. It particularly includes (1) the 3-year BICEP3 data which is the current deepest CMB polarization map at the foreground-minimum 95 GHz; and (2) the Keck 220 GHz map with a higher signal-to-noise ratio on the dust foreground than the Planck 353 GHz map. We fit the auto- and cross-spectra of these maps to a multicomponent likelihood model ($\Lambda$CDM+dust+synchrotron+noise+$r$) and find it to be an adequate description of the data at the current noise level. The likelihood analysis yields $\sigma(r)=0.009$. The inference of $r$ from our baseline model is tightened to $r_{0.05}=0.014^{+0.010}_{-0.011}$ and $r_{0.05}, Comment: 8 pages, 6 figures, contribution to the 2022 Cosmology session of the 56th Rencontres de Moriond
Published: 2022

3. Detecting primordial features with LISA

Author: Fumagalli, Jacopo, Pieroni, Mauro, Renaux-Petel, Sébastien, Witkowski, Lukas T., Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: oscillation: frequency, LISA, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitational radiation: stochastic, background: induced, principal component analysis, gravitational radiation: background, gravitational radiation: primordial, FOS: Physical sciences, Astronomy and Astrophysics, observatory, General Relativity and Quantum Cosmology, ultraviolet, inflation, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Oscillations in the frequency profile of the stochastic gravitational wave background are a characteristic prediction of small-scale features during inflation. In this paper we present a first investigation of the detection prospects of such oscillations with the upcoming space-based gravitational wave observatory LISA. As a proof of principle, we show for a selection of feature signals that the oscillations can be reconstructed with LISA, employing a method based on principal component analysis. We then perform a Fisher forecast for the parameters describing the oscillatory signal. For a sharp feature we distinguish between the contributions to the stochastic gravitational wave background induced during inflation and in the post-inflationary period, which peak at different frequencies. We find that for the latter case the amplitude of the oscillation is expected to be measurable with $< 10\%$ accuracy if the corresponding peak satisfies $h^2 \Omega_\textrm{GW} \gtrsim 10^{-12}$-$10^{-11}$, while for inflationary-era gravitational waves a detection of the oscillations requires a higher peak amplitude of $h^2 \Omega_\textrm{GW}$, as the oscillations only appear on the UV tail of the spectrum. For a resonant feature the detection prospects with LISA are maximised if the frequency of the oscillation falls into the range $\omega_\textrm{log} = 4$ to $10$. Our results confirm that oscillations in the frequency profile of the stochastic gravitational wave background are a worthwhile target for future detection efforts and offer a key for experimentally testing inflation at small scales., Comment: 28 pages, 15 figures
Published: 2022

4. Turn up the volume: Listening to phase transitions in hot dark sectors

Author: Ertas, Fatih, Kahlhöfer, Felix Karl David, and Tasillo, Carlo
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitational radiation: stochastic, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Higgs particle, dark matter, thermal, High Energy Physics - Phenomenology (hep-ph), cosmological model: parameter space, stochastic [gravitational radiation], cosmological phase transitions, ddc:530, background [gravitational radiation], dark energy, cosmology of theories beyond the SM, enhancement, LISA, photon, gravitational radiation: background, gravitational radiation: primordial, temperature, Astronomy and Astrophysics, primordial [gravitational radiation], critical phenomena, weak coupling, parameter space [cosmological model], observatory, High Energy Physics - Phenomenology, particle physics - cosmology connection, primordial gravitational waves (theory), Einstein, entropy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Seminar, Hamburg, Germany; Journal of cosmology and astroparticle physics 02, 014 (2022). doi:10.1088/1475-7516/2022/02/014, Stochastic gravitational wave (GW) backgrounds from first-order phase transitions are an exciting target for future GW observatories and may enable us to study dark sectors with very weak couplings to the Standard Model. In this work we show that such signals may be significantly enhanced for hot dark sectors with a temperature larger than the one of the SM thermal bath. The need to transfer the entropy from the dark sector to the SM after the phase transition can however lead to a substantial dilution of the GW signal. We study this dilution in detail, including the effect of number-changing processes in the dark sector (so-called cannibalism), and show that in large regions of parameter space a net enhancement remains. We apply our findings to a specific example of a dark sector containing a dark Higgs boson and a dark photon and find excellent detection prospects for LISA and the Einstein telescope., Published by IOP, London
Published: 2022
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5. Primordial gravitational waves from excited states

Author: Jacopo Fumagalli, Gonzalo A. Palma, Sébastien Renaux-Petel, Spyros Sypsas, Lukas T. Witkowski, Cristobal Zenteno, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and UAM. Departamento de Física Teórica
Subjects: High Energy Physics - Theory, Nuclear and High Energy Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitational radiation: stochastic, perturbation, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), General Relativity and Quantum Cosmology, horizon, excited state: scalar, Cosmology of Theories BSM, power spectrum: tensor, structure, inflation, enhancement, Early Universe Particle Physics, fluctuation, higher-order: 2, gravitational radiation: background, Hilbert space, gravitational radiation: primordial, Física, back reaction, oscillation, field theory: multiple, High Energy Physics - Theory (hep-th), trajectory, history, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We show that a scalar excited state with large occupation numbers during inflation leads to an enhancement of tensor modes and a characteristic pattern of order-one oscillations in the associated stochastic gravitational wave background (SGWB) sourced during inflation. An effective excited state, i.e. a departure from the Bunch-Davies vacuum, can emerge dynamically as the result of a transient non-adiabatic evolution, e.g. a sharp feature along the inflationary history. We provide an explicit example in a multifield context where the sharp feature triggering the excited state is identified with a strong turn in the inflationary trajectory. En passant, we derive a universal expression for the tensor power spectrum sourced at second order by an arbitrary number of scalar degrees of freedom during inflation, crucially taking into account the nontrivial structure of the Hilbert space in multifield setups. The SGWB sourced during inflation can overcome the standard scalar-induced SGWB sourced at horizon re-entry of the fluctuations after inflation, while being less constrained by perturbativity and backreaction bounds. In addition, one may entertain the possibility of detecting both since they peak at different frequencies exhibiting oscillations with distinct periods., Comment: 57 pages, 10 figures. v2: typos corrected in Sec. 3.2 and references added. Version published in JHEP
Published: 2021

6. Sensing Quantum Nature of Primordial Gravitational Waves Using Quantum Electromagnetic Fields

Author: Arani, F. Shojaei, Harouni, M. Bagheri, Lamine, B., Blanchard, A., Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)
Subjects: LISA, radiation: electromagnetic, Hamiltonian formalism, background: primordial, interferometer, oscillator: quantum, gravitational radiation: background, gravitational radiation: primordial, power spectrum, stability: optical, Doppler effect, laser, gravitational radiation: quantization, photon: deflection, phase shift, gravitation, electromagnetic field, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], broadening, signature
Abstract: We establish a new formalism to describe the interaction of an optical system with a background of gravitational waves based on optical medium analogy. Besides reproducing the basic formula for the response of a LISA-type interferometer in terms of the phase shift of light, other classical observables of the electromagnetic field such as light-bending, walk-off angle and Stokes parameters are investigated. At the quantum level, this approach enables us to construct a full quantum Hamiltonian describing both electromagnetic and gravitational waves as quantum entities. It turns out that the effective coupling between the electromagnetic field and gravitational wave background resembles an opto-mechanical coupling. This points to a new strategy to evident non-classical nature of gravity within the reach of future optical experiments. As an illustrative application, we investigate the optical quadrature variance as well as the power spectrum of a laser field interacting with a background of primordial gravitational wave. The effect of the relic background of quantized gravitational waves on the optical variance is analogous to the effect of a classical mechanical oscillator, which stabilizes the optical variance. It also acts similar to a Doppler-broadening mechanism which broadens the line-width of the laser field of optical frequency by $10^{-6}$Hz. This line-width broadening and also appearance of side-bands in the spectrum of light could serve as signatures of the highly squeezed nature of primordial gravitational waves.
Published: 2021

7. Probing PeV scale SUSY-breaking with Satellite Galaxies and Primordial Gravitational Waves

Author: Tsutomu T. Yanagida, Ryusuke Jinno, and Gongjun Choi
Subjects: gravitation [mass], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Milky Way, entropy: production, satellite, FOS: Physical sciences, Scale (descriptive set theory), Astrophysics, Omega, symmetry breaking [supersymmetry], High Energy Physics - Phenomenology (hep-ph), Satellite galaxy, ddc:530, inflation, supersymmetry: symmetry breaking, gravitino: mass, entropy, production, Physics, Entropy production, Gravitational wave, gravitational radiation: primordial, primordial [gravitational radiation], Supersymmetry, mass, gravitation, suppression, production [entropy], gravitational radiation, primordial, High Energy Physics - Phenomenology, gravitino, mass, supersymmetry, symmetry breaking, Gravitino, mass: gravitation, galaxy, mass [gravitino], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Physical review / D 104(9), 095018 (2021). doi:10.1103/PhysRevD.104.095018, We study an inevitable cosmological consequence in PeV scale SUSY-breaking scenarios. We focus on the SUSY-breaking scale corresponding to the gravitino mass $m_{3/2}=100{\rm eV}-1{\rm keV}$. We argue that the presence of an early matter-dominated era and the resulting entropy production are requisite for the Universe with this gravitino mass. We infer the model-independent minimum amount of the entropy production $\Delta$ by requiring that the number of dwarf satellite galaxies $N_{\rm sat}$ in the Milky Way exceed the currently observed value, i.e. $N_{\rm sat}\gtrsim63$. This entropy production is inevitably imprinted on the primordial gravitational waves (pGWs) produced during the inflationary era. We study how the information on the value of $\Delta$ and the time of entropy production are encoded in the pGW spectrum $\Omega_{\rm GW}(f_{\rm GW})$. In the case where the future GW surveys do not see any suppression in the pGW spectrum for the frequency range $\mathcal{O}(10^{-10}){\rm Hz}\lesssim f_{\rm GW}\lesssim\mathcal{O}(10^{-5}){\rm Hz}$, our study can be used to rule out all the PeV scale SUSY-breaking scenarios., Published by Inst., Melville, NY
Published: 2021

8. Anisotropic cosmological models in Horndeski gravity

Author: Sergey V. Sushkov, Alexei A. Starobinsky, Ruslan K. Muharlyamov, Rafkat Galeev, Mikhail S. Volkov, Institute of Physics [Kazan] (IoP), Kazan Federal University (KFU), L.D. Landau Institute for Theoretical Physics of RAS, Russian Academy of Sciences [Moscow] (RAS), Institut Denis Poisson (IDP), Centre National de la Recherche Scientifique (CNRS)-Université de Tours (UT)-Université d'Orléans (UO), and Centre National de la Recherche Scientifique (CNRS)-Université de Tours-Université d'Orléans (UO)
Subjects: High Energy Physics - Theory, velocity, cosmological model, coupling: nonminimal, gravitation: model, perturbation, General relativity, Initial singularity, alternative theories of gravity, FOS: Physical sciences, Context (language use), General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, space-time: Bianchi: Type I, Cosmology, photon: velocity, Gravitation, Theoretical physics, Singularity, 0103 physical sciences, inflation, initial state, 010306 general physics, Physics, Inflation (cosmology), space-time: anisotropy, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], 010308 nuclear & particles physics, gravitational radiation: primordial, gravitational radiation, stability, singularity, field theory: scalar, High Energy Physics - Theory (hep-th), gravitation, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], k-essence, Scalar field
Abstract: It was found recently that the anisotropies in the homogeneous Bianchi I cosmology considered within the context of a specific Horndeski theory are damped near the initial singularity instead of being amplified. In this work we extend the analysis of this phenomenon to cover the whole of the Horndeski family. We find that the phenomenon is absent in the K-essence and/or Kinetic Gravity Braiding theories, where the anisotropies grow as one approaches the singularity. The anisotropies are damped at early times only in more general Horndeski models whose Lagrangian includes terms quadratic and cubic in second derivatives of the scalar field. Such theories are often considered as being inconsistent with the observations because they predict a non-constant speed of gravitational waves. However, the predicted value of the speed at present can be close to the speed of light with any required precision, hence the theories actually agree with the present time observations. We consider two different examples of such theories, both characterized by a late self-acceleration and an early inflation driven by the non-minimal coupling. Their anisotropies show a maximum at intermediate times and approach zero at early and late times. The early inflationary stage exhibits an instability with respect to inhomogeneous perturbations, suggesting that the initial state of the universe should be inhomogeneous. However, more general Horndeski models may probably be stable., Comment: 21 pages, several figures
Published: 2021

9. Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season

Author: J. J. Bock, M. Amiri, B. Steinbach, Kent D. Irwin, S. Kefeli, B. Racine, E. Hand, J. E. Tolan, Abigail G. Vieregg, C. Tucker, J. Willmert, N. Goeckner-Wald, S. Richter, A. Turner, H. Hui, B. L. Schmitt, T. Namikawa, G. Halal, P. A. R. Ade, K. G. Megerian, L. Zeng, R. Schwarz, Victor Buza, L. Minutolo, T. St. Germaine, C. D. Sheehy, Jake Connors, R. Basu Thakur, S. Fliescher, C. Pryke, M. Crumrine, Bicep, Mark Halpern, C. Umilta, Sarah M. Harrison, H. Yang, Chao-Lin Kuo, Che-Hang Yu, K. Lau, Shengyu Zhang, C. Bischoff, C. Verges, S. R. Hildebrandt, S. Fatigoni, R. O'Brient, Denis Barkats, Chao Zhang, Jeffrey P. Filippini, A. Cukierman, H. Boenish, H. T. Nguyen, D. V. Wiebe, K. S. Karkare, Gene C. Hilton, E. Young, J. Grayson, M. Eiben, Y. Nakato, Z. Ahmed, D. C. Goldfinger, A. C. Weber, J. R. Cheshire, L. Duband, C. D. Reintsema, S. Henderson, T. Prouve, A. Wandui, P. Grimes, K. L. Thompson, G. P. Teply, J. Cornelison, S. Palladino, J. Kang, E. V. Denison, Marion Dierickx, A. Lennox, A. Soliman, R. W. Ogburn, R. V. Sudiwala, E. Bullock, D. Beck, C. L. Wong, A. Schillaci, E. Karpel, J. Hubmayr, G. Hall, W. L. K. Wu, L. Moncelsi, K. W. Yoon, E. M. Leitch, S. A. Kernasovskiy, J. M. Kovac, Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), BICEP, and Keck
Subjects: noise, satellite: Planck, statistical analysis: confidence limit, media_common.quotation_subject, Cosmic microwave background, General Physics and Astronomy, cosmic background radiation: polarization, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, power spectrum, 01 natural sciences, symbols.namesake, gravitation: lens, cosmological model: parameter space, 0103 physical sciences, synchrotron, Planck, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, Spectral index, 010308 nuclear & particles physics, Gravitational wave, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation: primordial, cosmological model: dust, Polarization (waves), BICEP, CMB cold spot, Sky, WMAP, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Noise (radio)
Abstract: International audience; We present results from an analysis of all data taken by the BICEP2, Keck Array, and BICEP3 CMB polarization experiments up to and including the 2018 observing season. We add additional Keck Array observations at 220 GHz and BICEP3 observations at 95 GHz to the previous 95/150/220 GHz dataset. The Q/U maps now reach depths of 2.8, 2.8, and 8.8 μKCMB arcmin at 95, 150, and 220 GHz, respectively, over an effective area of ≈600 square degrees at 95 GHz and ≈400 square degrees at 150 and 220 GHz. The 220 GHz maps now achieve a signal-to-noise ratio on polarized dust emission exceeding that of Planck at 353 GHz. We take auto- and cross-spectra between these maps and publicly available WMAP and Planck maps at frequencies from 23 to 353 GHz and evaluate the joint likelihood of the spectra versus a multicomponent model of lensed ΛCDM+r+dust+synchrotron+noise. The foreground model has seven parameters, and no longer requires a prior on the frequency spectral index of the dust emission taken from measurements on other regions of the sky. This model is an adequate description of the data at the current noise levels. The likelihood analysis yields the constraint r0.05<0.036 at 95% confidence. Running maximum likelihood search on simulations we obtain unbiased results and find that σ(r)=0.009. These are the strongest constraints to date on primordial gravitational waves.
Published: 2021

10. Revealing the Primordial Irreducible Inflationary Gravitational-Wave Background with a Spinning Peccei-Quinn Axion

Author: Servant, Geraldine, Simakachorn, Peera, and Gouttenoire, Yann
Subjects: scale: inflation, LISA, axion: dark matter, fluctuation: tensor, energy: kinetic, interferometer, gravitational radiation: background, gravitational radiation: primordial, axion: signature, big bang, trigger, oscillation, quantum chromodynamics: axion, field theory: scalar, General Relativity and Quantum Cosmology, Einstein Telescope, Peccei-Quinn, gravitational radiation: spectrum, history, equation of state
Abstract: The primordial irreducible gravitational-wave background due to quantum vacuum tensor fluctuations produced during inflation spans a large range of frequencies with an almost scale-invariant spectrum but is too low to be detected by the next generation of gravitational-wave interferometers. We show how this signal is enhanced by a short temporary kination era in the cosmological history (less than 10 e-folds), that can arise at any energy scale between a GeV and the inflationary scale $10^{16}$ GeV.We argue that such kination era is naturally generated by a spinning axion before it gets trapped by its potential.It is usually assumed that the axion starts oscillating around its minimum from its initial frozen position at rest.However, the early dynamics of the Peccei-Quinn field can induce a large kinetic energy in the axion field, triggering a kination era, either before or after the axion acquires its mass, leading to a characteristic peak in the primordial gravitational-wave background. This represents a smoking-gun signature of axion physics as no other scalar field dynamics can trigger such a sequence of equations of state in the early universe.We derive the resulting gravitational-wave spectrum, and present the parameter space that leads to such signal as well as the detectability prospects, in particular at LISA, Einstein Telescope, Cosmic Explorer and Big Bang Observer.We show both model-independent predictions and present as well results for two specific well-motivated UV completions for the QCD axion dark matter where this dynamics is built-in.
Published: 2021
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11. Overview of the Medium and High Frequency Telescopes of the LiteBIRD satellite mission

Author: Ludovic Montier, Baptiste Mot, Paolo de Bernardis, Bruno Maffei, Giampaolo Pisano, Fabio Columbro, Jon E. Gudmundsson, Sophie Henrot-Versillé, Luca Lamagna, Joshua Montgomery, Thomas Prouvé, Megan Russell, Giorgio Savini, Samantha Stever, Keith L. Thompson, Masahiro Tsujimoto, Carole Tucker, Benjamin Westbrook, Peter A. Ade, Alexandre Adler, Erwan Allys, Kam Arnold, Didier Auguste, Jonathan Aumont, Ragnhild Aurlien, Jason Austermann, Carlo Baccigalupi, Anthony J. Banday, Ranajoy Banerji, Rita B. Barreiro, Soumen Basak, Jim Beall, Dominic Beck, Shawn Beckman, Juan Bermejo, Marco Bersanelli, Julien Bonis, Julian Borrill, Francois Boulanger, Sophie Bounissou, Maksym Brilenkov, Michael Brown, Martin Bucher, Erminia Calabrese, Paolo Campeti, Alessandro Carones, Francisco J. Casas, Anthony Challinor, Victor Chan, Kolen Cheung, Yuji Chinone, Jean F. Cliche, Loris Colombo, Javier Cubas, Ari Cukierman, David Curtis, Giuseppe D'Alessandro, Nadia Dachlythra, Marco De Petris, Clive Dickinson, Patricia Diego-Palazuelos, Matt Dobbs, Tadayasu Dotani, Lionel Duband, Shannon Duff, Jean M. Duval, Ken Ebisawa, Tucker Elleflot, Hans K. Eriksen, Josquin Errard, Thomas Essinger-Hileman, Fabio Finelli, Raphael Flauger, Cristian Franceschet, Unni Fuskeland, Mathew Galloway, Ken Ganga, Jian R. Gao, Ricardo Genova-Santos, Martina Gerbino, Massimo Gervasi, Tommaso Ghigna, Eirik Gjerløw, Marcin L. Gradziel, Julien Grain, Frank Grupp, Alessandro Gruppuso, Tijmen de Haan, Nils W. Halverson, Peter Hargrave, Takashi Hasebe, Masaya Hasegawa, Makoto Hattori, Masashi Hazumi, Daniel Herman, Diego Herranz, Charles A. Hill, Gene Hilton, Yukimasa Hirota, Eric Hivon, Renee A. Hlozek, Yurika Hoshino, Elena de la Hoz, Johannes Hubmayr, Kiyotomo Ichiki, Teruhito Iida, Hiroaki Imada, Kosei Ishimura, Hirokazu Ishino, Greg Jaehnig, Tooru Kaga, Shingo Kashima, Nobuhiko Katayama, Akihiro Kato, Takeo Kawasaki, Reijo Keskitalo, Theodore Kisner, Yohei Kobayashi, Nozomu Kogiso, Alan Kogut, Kazunori Kohri, Eiichiro Komatsu, Kunimoto Komatsu, Kuniaki Konishi, Nicoletta Krachmalnicoff, Ingo Kreykenbohm, Chao-Lin L. Kuo, Akihiro Kushino, Jeff V. Lanen, Massimiliano Lattanzi, Adrian T. Lee, Clément Leloup, François Levrier, Eric Linder, Thibaut Louis, Gemma Luzzi, Thierry Maciaszek, Davide Maino, Muneyoshi Maki, Stefano Mandelli, Enrique Martinez-Gonzalez, Silvia Masi, Tomotake Matsumura, Aniello Mennella, Marina Migliaccio, Yuto Minami, Kazuhisa Mitsuda, Gianluca Morgante, Yasuhiro Murata, John A. Murphy, Makoto Nagai, Yuya Nagano, Taketo Nagasaki, Ryo Nagata, Shogo Nakamura, Toshiya Namikawa, Paolo Natoli, Simran Nerval, Toshiyuki Nishibori, Haruki Nishino, Créidhe O'Sullivan, Hideo Ogawa, Hiroyuki Ogawa, Shugo Oguri, Hiroyuki Ohsaki, Izumi S. Ohta, Norio Okada, Nozomi Okada, Luca Pagano, Alessandro Paiella, Daniela Paoletti, Guillaume Patanchon, Julien Peloton, Francesco Piacentini, Gianluca Polenta, Davide Poletti, Giuseppe Puglisi, Damien Rambaud, Christopher Raum, Sabrina Realini, Martin Reinecke, Mathieu Remazeilles, Alessia Ritacco, Gilles Roudil, Jose A. Rubino-Martin, Haruyuki Sakurai, Yuki Sakurai, Maura Sandri, Manami Sasaki, Douglas Scott, Joseph Seibert, Yutaro Sekimoto, Blake Sherwin, Keisuke Shinozaki, Maresuke Shiraishi, Peter Shirron, Giovanni Signorelli, Graeme Smecher, Radek Stompor, Hajime Sugai, Shinya Sugiyama, Aritoki Suzuki, Junichi Suzuki, Trygve L. Svalheim, Eric Switzer, Ryota Takaku, Hayato Takakura, Satoru Takakura, Yusuke Takase, Youichi Takeda, Andrea Tartari, Ellen Taylor, Yutaka Terao, Harald Thommesen, Ben Thorne, Takayuki Toda, Maurizio Tomasi, Mayu Tominaga, Neil Trappe, Matthieu Tristram, Masatoshi Tsuji, Joe Ullom, Gerard Vermeulen, Patricio Vielva, Fabrizio Villa, Michael Vissers, Nicola Vittorio, Ingunn Wehus, Jochen Weller, Joern Wilms, Berend Winter, Edward J. Wollack, Noriko Y. Yamasaki, Tetsuya Yoshida, Junji Yumoto, Mario Zannoni, Andrea Zonca, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National d’Études Spatiales [Paris] (CNES), LiteBIRD, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, European Research Council, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Lystrup, Makenzie, Montier, L, Mot, B, de Bernardis, P, Maffei, B, Pisano, G, Columbro, F, Gudmundsson, J, Henrot-Versillé, S, Lamagna, L, Montgomery, J, Prouvé, T, Russell, M, Savini, G, Stever, S, Thompson, K, Tsujimoto, M, Tucker, C, Westbrook, B, Ade, P, Adler, A, Allys, E, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Baccigalupi, C, Banday, A, Banerji, R, Barreiro, R, Basak, S, Beall, J, Beck, D, Beckman, S, Bermejo, J, Bersanelli, M, Bonis, J, Borrill, J, Boulanger, F, Bounissou, S, Brilenkov, M, Brown, M, Bucher, M, Calabrese, E, Campeti, P, Carones, A, Casas, F, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Cliche, J, Colombo, L, Cubas, J, Cukierman, A, Curtis, D, D'Alessandro, G, Dachlythra, N, De Petris, M, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Duband, L, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Gerbino, M, Gervasi, M, Ghigna, T, Gjerløw, E, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, de Haan, T, Halverson, N, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Hazumi, M, Herman, D, Herranz, D, Hill, C, Hilton, G, Hirota, Y, Hivon, E, Hlozek, R, Hoshino, Y, de la Hoz, E, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Kaga, T, Kashima, S, Katayama, N, Kato, A, Kawasaki, T, Keskitalo, R, Kisner, T, Kobayashi, Y, Kogiso, N, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kreykenbohm, I, Kuo, C, Kushino, A, Lanen, J, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Louis, T, Luzzi, G, Maciaszek, T, Maino, D, Maki, M, Mandelli, S, Martinez-Gonzalez, E, Masi, S, Matsumura, T, Mennella, A, Migliaccio, M, Minami, Y, Mitsuda, K, Morgante, G, Murata, Y, Murphy, J, Nagai, M, Nagano, Y, Nagasaki, T, Nagata, R, Nakamura, S, Namikawa, T, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, O'Sullivan, C, Ogawa, H, Oguri, S, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Peloton, J, Piacentini, F, Polenta, G, Poletti, D, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Reinecke, M, Remazeilles, M, Ritacco, A, Roudil, G, Rubino-Martin, J, Sakurai, H, Sakurai, Y, Sandri, M, Sasaki, M, Scott, D, Seibert, J, Sekimoto, Y, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Stompor, R, Sugai, H, Sugiyama, S, Suzuki, A, Suzuki, J, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Taylor, E, Terao, Y, Thommesen, H, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Ullom, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wehus, I, Weller, J, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Zannoni, M, Zonca, A, and Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris)
Subjects: cosmological model, experimental methods, detector: satellite, Cosmic microwave background, cosmic background radiation: polarization, detector: noise, magnetic field, 02 engineering and technology, LiteBIRD, cosmic microwave background, polarization measurements, space telescopes, 7. Clean energy, 01 natural sciences, law.invention, law, detector: calibration, media_common, Physics, conductivity: thermal, Settore FIS/05, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, 021001 nanoscience & nanotechnology, Polarization (waves), inflation: model, experimental equipment, B-mode, cosmic radiation, cryogenics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, 0210 nano-technology, cosmic background radiation: detector, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), lens, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, FOS: Physical sciences, LiteBIRD, Polarization measurements, Space telescopes, Astrophysics::Cosmology and Extragalactic Astrophysics, bolometer: superconductivity, frequency: high, Radio spectrum, tensor scalar: ratio, 010309 optics, Telescope, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], numerical calculations, Instrumentation and Methods for Astrophysics (astro-ph.IM), detector: angular resolution, Astrophysics::Galaxy Astrophysics, Gravitational wave, synchrotron radiation, gravitational radiation: primordial, Astronomy, Physics::History of Physics, optics, detector: sensitivity, 13. Climate action, Sky, Satellite, temperature: stability, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Event: SPIE Astronomical Telescopes + Instrumentation, 2020, Online.-- et al., LiteBIRD is a JAXA-led Strategic Large-Class mission designed to search for the existence of the primordial gravitational waves produced during the inflationary phase of the Universe, through the measurements of their imprint onto the polarization of the cosmic microwave background (CMB). These measurements, requiring unprecedented sensitivity, will be performed over the full sky, at large angular scales, and over 15 frequency bands from 34 GHz to 448 GHz. The LiteBIRD instruments consist of three telescopes, namely the Low-, Medium-and High-Frequency Telescope (respectively LFT, MFT and HFT). We present in this paper an overview of the design of the Medium-Frequency Telescope (89{224 GHz) and the High-Frequency Telescope (166{448 GHz), the so-called MHFT, under European responsibility, which are two cryogenic refractive telescopes cooled down to 5 K. They include a continuous rotating half-wave plate as the first optical element, two high-density polyethylene (HDPE) lenses and more than three thousand transition-edge sensor (TES) detectors cooled to 100 mK. We provide an overview of the concept design and the remaining specific challenges that we have to face in order to achieve the scientific goals of LiteBIRD., This work is supported in Japan by ISAS/JAXA for Pre-Phase A2 studies, by the acceleration program of JAXA research and development directorate, by the World Premier International Research Center Initiative (WPI) of MEXT, by the JSPS Core-to-Core Program of A. Advanced Research Networks, and by JSPS KAKENHI Grant Numbers JP15H05891, JP17H01115, and JP17H01125. The Italian LiteBIRD phase A contribution is supported by the Italian Space Agency (ASI Grants No. 2020-9-HH.0 and 2016-24-H.1-2018), the National Institute for Nuclear Physics (INFN) and the National Institute for Astrophysics (INAF). The French LiteBIRD phase A contribution is supported by the Centre National d’Etudes Spatiale (CNES), by the Centre National de la Recherche Scientifique (CNRS), and by the Commissariat a l’Energie Atomique (CEA). The Canadian contribution is supported by the Canadian Space Agency. The US contribution is supported by NASA grant no. 80NSSC18K0132. Norwegian participation in LiteBIRD is supported by the Research Council of Norway (Grant No. 263011). The Spanish LiteBIRD phase A contribution is supported by the Spanish Agencia Estatal de Investigacion (AEI), project refs. PID2019-110610RB-C21 and AYA2017-84185-P. Funds that support the Swedish contributions come from the Swedish National Space Agency (SNSA/Rymdstyrelsen) and the Swedish Research Council (Reg. no. 2019-03959). The German participation in LiteBIRD is supported in part by the Excellence Cluster ORIGINS, which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy (Grant No. EXC-2094 - 390783311). This research used resources of the Central Computing System owned and operated by the Computing Research Center at KEK, as well as resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy. European collaborators acknowledge support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement Nos. 772253, 819478, and 849169). The European Space Agency (ESA) has led a Concurrent Design Facility study, focused on the MHFT and Sub-Kelvin coolers, and funded Technology Research Programmes for “Large radii Half-Wave Plate (HWP) development” (contract number: 4000123266/18/NL/AF) and for the ‘Development of Large Anti-Reflection Coated Lenses for Passive (Sub)Millimeter-Wave Science Instruments” (contract number: 4000128517/19/NL/AS).
Published: 2020

12. LiteBIRD: JAXA's new strategic L-class mission for all-sky surveys of cosmic microwave background polarization

Author: Masashi Hazumi, Peter A. Ade, Alexandre Adler, Erwan Allys, Kam Arnold, Didier Auguste, Jonathan Aumont, Ragnhild Aurlien, Jason Austermann, Carlo Baccigalupi, Anthony J. Banday, R. Banjeri, Rita B. Barreiro, Soumen Basak, Jim Beall, Dominic Beck, Shawn Beckman, Juan Bermejo, Paolo de Bernardis, Marco Bersanelli, Julien Bonis, Julian Borrill, Francois Boulanger, Sophie Bounissou, Maksym Brilenkov, Michael Brown, Martin Bucher, Erminia Calabrese, Paolo Campeti, Alessandro Carones, Francisco J. Casas, Anthony Challinor, Victor Chan, Kolen Cheung, Yuji Chinone, Jean F. Cliche, Loris Colombo, Fabio Columbro, Javier Cubas, Ari Cukierman, David Curtis, Giuseppe D'Alessandro, Nadia Dachlythra, Marco De Petris, Clive Dickinson, Patricia Diego-Palazuelos, Matt Dobbs, Tadayasu Dotani, Lionel Duband, Shannon Duff, Jean M. Duval, Ken Ebisawa, Tucker Elleflot, Hans K. Eriksen, Josquin Errard, Thomas Essinger-Hileman, Fabio Finelli, Raphael Flauger, Cristian Franceschet, Unni Fuskeland, Mathew Galloway, Ken Ganga, Jian R. Gao, Ricardo Genova-Santos, Martina Gerbino, Massimo Gervasi, Tommaso Ghigna, Eirik Gjerløw, Marcin L. Gradziel, Julien Grain, Frank Grupp, Alessandro Gruppuso, Jon E. Gudmundsson, Tijmen de Haan, Nils W. Halverson, Peter Hargrave, Takashi Hasebe, Masaya Hasegawa, Makoto Hattori, Sophie Henrot-Versillé, Daniel Herman, Diego Herranz, Charles A. Hill, Gene Hilton, Yukimasa Hirota, Eric Hivon, Renee A. Hlozek, Yurika Hoshino, Elena de la Hoz, Johannes Hubmayr, Kiyotomo Ichiki, Teruhito Iida, Hiroaki Imada, Kosei Ishimura, Hirokazu Ishino, Greg Jaehnig, Tooru Kaga, Shingo Kashima, Nobuhiko Katayama, Akihiro Kato, Takeo Kawasaki, Reijo Keskitalo, Theodore Kisner, Yohei Kobayashi, Nozomu Kogiso, Alan Kogut, Kazunori Kohri, Eiichiro Komatsu, Kunimoto Komatsu, Kuniaki Konishi, Nicoletta Krachmalnicoff, Ingo Kreykenbohm, Chao-Lin L. Kuo, Akihiro Kushino, Luca Lamagna, Jeff V. Lanen, Massimiliano Lattanzi, Adrian T. Lee, Clément Leloup, François Levrier, Eric Linder, Thibaut Louis, Gemma Luzzi, Thierry Maciaszek, Bruno Maffei, Davide Maino, Muneyoshi Maki, Stefano Mandelli, Enrique Martinez-Gonzalez, Silvia Masi, Tomotake Matsumura, Aniello Mennella, Marina Migliaccio, Yuto Minami, Kazuhisa Mitsuda, Joshua Montgomery, Ludovic Montier, Gianluca Morgante, Baptiste Mot, Yasuhiro Murata, John A. Murphy, Makoto Nagai, Yuya Nagano, Taketo Nagasaki, Ryo Nagata, Shogo Nakamura, Toshiya Namikawa, Paolo Natoli, Simran Nerval, Toshiyuki Nishibori, Haruki Nishino, Fabio Noviello, Créidhe O'Sullivan, Hideo Ogawa, Hiroyuki Ogawa, Shugo Oguri, Hiroyuki Ohsaki, Izumi S. Ohta, Norio Okada, Nozomi Okada, Luca Pagano, Alessandro Paiella, Daniela Paoletti, Guillaume Patanchon, Julien Peloton, Francesco Piacentini, Giampaolo Pisano, Gianluca Polenta, Davide Poletti, Thomas Prouvé, Giuseppe Puglisi, Damien Rambaud, Christopher Raum, Sabrina Realini, Martin Reinecke, Mathieu Remazeilles, Alessia Ritacco, Gilles Roudil, Jose A. Rubino-Martin, Megan Russell, Haruyuki Sakurai, Yuki Sakurai, Maura Sandri, Manami Sasaki, Giorgio Savini, Douglas Scott, Joseph Seibert, Yutaro Sekimoto, Blake Sherwin, Keisuke Shinozaki, Maresuke Shiraishi, Peter Shirron, Giovanni Signorelli, Graeme Smecher, Samantha Stever, Radek Stompor, Hajime Sugai, Shinya Sugiyama, Aritoki Suzuki, Junichi Suzuki, Trygve L. Svalheim, Eric Switzer, Ryota Takaku, Hayato Takakura, Satoru Takakura, Yusuke Takase, Youichi Takeda, Andrea Tartari, Ellen Taylor, Yutaka Terao, Harald Thommesen, Keith L. Thompson, Ben Thorne, Takayuki Toda, Maurizio Tomasi, Mayu Tominaga, Neil Trappe, Matthieu Tristram, Masatoshi Tsuji, Masahiro Tsujimoto, Carole Tucker, Joe Ullom, Gerard Vermeulen, Patricio Vielva, Fabrizio Villa, Michael Vissers, Nicola Vittorio, Ingunn Wehus, Jochen Weller, Benjamin Westbrook, Joern Wilms, Berend Winter, Edward J. Wollack, Noriko Y. Yamasaki, Tetsuya Yoshida, Junji Yumoto, Mario Zannoni, Andrea Zonca, Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National d’Études Spatiales [Paris] (CNES), Centre National d'Études Spatiales [Toulouse] (CNES), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), LiteBIRD, Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Hélium : du fondamental aux applications (NEEL - HELFA), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Lystrup, Makenzie, Hazumi, M, Ade, P, Adler, A, Allys, E, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Baccigalupi, C, Banday, A, Banjeri, R, Barreiro, R, Basak, S, Beall, J, Beck, D, Beckman, S, Bermejo, J, de Bernardis, P, Bersanelli, M, Bonis, J, Borrill, J, Boulanger, F, Bounissou, S, Brilenkov, M, Brown, M, Bucher, M, Calabrese, E, Campeti, P, Carones, A, Casas, F, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Cliche, J, Colombo, L, Columbro, F, Cubas, J, Cukierman, A, Curtis, D, D'Alessandro, G, Dachlythra, N, De Petris, M, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Duband, L, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Gerbino, M, Gervasi, M, Ghigna, T, Gjerløw, E, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, Gudmundsson, J, de Haan, T, Halverson, N, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Henrot-Versillé, S, Herman, D, Herranz, D, Hill, C, Hilton, G, Hirota, Y, Hivon, E, Hlozek, R, Hoshino, Y, de la Hoz, E, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Kaga, T, Kashima, S, Katayama, N, Kato, A, Kawasaki, T, Keskitalo, R, Kisner, T, Kobayashi, Y, Kogiso, N, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kreykenbohm, I, Kuo, C, Kushino, A, Lamagna, L, Lanen, J, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Louis, T, Luzzi, G, Maciaszek, T, Maffei, B, Maino, D, Maki, M, Mandelli, S, Martinez-Gonzalez, E, Masi, S, Matsumura, T, Mennella, A, Migliaccio, M, Minami, Y, Mitsuda, K, Montgomery, J, Montier, L, Morgante, G, Mot, B, Murata, Y, Murphy, J, Nagai, M, Nagano, Y, Nagasaki, T, Nagata, R, Nakamura, S, Namikawa, T, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, Noviello, F, O'Sullivan, C, Ogawa, H, Oguri, S, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Peloton, J, Piacentini, F, Pisano, G, Polenta, G, Poletti, D, Prouvé, T, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Reinecke, M, Remazeilles, M, Ritacco, A, Roudil, G, Rubino-Martin, J, Russell, M, Sakurai, H, Sakurai, Y, Sandri, M, Sasaki, M, Savini, G, Scott, D, Seibert, J, Sekimoto, Y, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Stever, S, Stompor, R, Sugai, H, Sugiyama, S, Suzuki, A, Suzuki, J, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Taylor, E, Terao, Y, Thommesen, H, Thompson, K, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Tsujimoto, M, Tucker, C, Ullom, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wehus, I, Weller, J, Westbrook, B, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Zannoni, M, and Zonca, A
Subjects: cosmological model, experimental methods, detector: satellite, Physics beyond the Standard Model, Cosmic microwave background, LiteBIRD, cosmic inflation, cosmic microwave background, B-mode polarization, primordial gravi- tational waves, quantum gravity, space telescope, cosmic background radiation: polarization, detector: noise, 02 engineering and technology, 7. Clean energy, 01 natural sciences, expansion: multipole, Cosmology, General Relativity and Quantum Cosmology, B-mode: primordial, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), general relativity, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], B-mode polarization, media_common, Physics, new physics, quantum mechanics, Astrophysics::Instrumentation and Methods for Astrophysics, 021001 nanoscience & nanotechnology, BICEP, inflation: model, High Energy Physics - Phenomenology, error: statistical, experimental equipment, cryogenics, power spectrum: angular dependence, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], readout, Astrophysics::Earth and Planetary Astrophysics, dust, control system, 0210 nano-technology, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic microwave background, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, cosmic inflation, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, primordial gravi- tational waves, Cosmic background radiation, space telescope, Lagrangian point, FOS: Physical sciences, LiteBIRD, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, polarization: sensitivity, 010309 optics, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, 0103 physical sciences, ionization, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], cosmic background radiation: power spectrum, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Inflation (cosmology), synchrotron radiation, primordial gravitational waves, gravitational radiation: primordial, Astronomy, calibration, Physics::History of Physics, recombination, detector: sensitivity, angular resolution, Sky, quantum gravity, gravitational radiation: emission, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Satellite, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], experimental results
Abstract: Event: SPIE Astronomical Telescopes + Instrumentation, 2020, Online.-- et al., LiteBIRD, the Lite (Light) satellite for the study of B-mode polarization and Inflation from cosmic background Radiation Detection, is a space mission for primordial cosmology and fundamental physics. JAXA selected LiteBIRD in May 2019 as a strategic large-class (L-class) mission, with its expected launch in the late 2020s using JAXA’s H3 rocket. LiteBIRD plans to map the cosmic microwave background (CMB) polarization over the full sky with unprecedented precision. Its main scientific objective is to carry out a definitive search for the signal from cosmic inflation, either making a discovery or ruling out well-motivated inflationary models. The measurements of LiteBIRD will also provide us with an insight into the quantum nature of gravity and other new physics beyond the standard models of particle physics and cosmology. To this end, LiteBIRD will perform full-sky surveys for three years at the Sun-Earth Lagrangian point L2 for 15 frequency bands between 34 and 448 GHz with three telescopes, to achieve a total sensitivity of 2.16 µK-arcmin with a typical angular resolution of 0.5◦ at 100 GHz. We provide an overview of the LiteBIRD project, including scientific objectives, mission requirements, top-level system requirements, operation concept, and expected scientific outcomes., This work is supported in Japan by ISAS/JAXA for Pre-Phase A2 studies, by the acceleration program of JAXA research and development directorate, by the World Premier International Research Center Initiative (WPI) of MEXT, by the JSPS Core-to-Core Program of A. Advanced Research Networks, and by JSPS KAKENHI Grant Numbers JP15H05891, JP17H01115, and JP17H01125. The Italian LiteBIRD phase A contribution is supported by the Italian Space Agency (ASI Grants No. 2020-9-HH.0 and 2016-24-H.1-2018), the National Institute for Nuclear Physics (INFN) and the National Institute for Astrophysics (INAF). The French LiteBIRD phase A contribution is supported by the Centre National d’Etudes Spatiale (CNES), by the Centre National de la Recherche Scientifique (CNRS), and by the Commissariat a l’Energie Atomique (CEA). The Canadian contribution is supported by the Canadian Space Agency. The US contribution is supported by NASA grant no. 80NSSC18K0132. Norwegian participation in LiteBIRD is supported by the Research Council of Norway (Grant No. 263011). The Spanish LiteBIRD phase A contribution is supported by the Spanish Agencia Estatal de Investigacion (AEI), project refs. PID2019-110610RB-C21 and AYA2017-84185-P. Funds that support the Swedish contributions come from the Swedish National Space Agency (SNSA/Rymdstyrelsen) and the Swedish Research Council (Reg. no. 2019-03959). The German participation in LiteBIRD is supported in part by the Excellence Cluster ORIGINS, which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy (Grant No. EXC-2094 - 390783311). This research used resources of the Central Computing System owned and operated by the Computing Research Center at KEK, as well as resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy.
Published: 2020

13. The optical design of the Litebird Medium and High Frequency Telescope

Author: Alessandro Paiella, Créidhe O'Sullivan, Reijo Keskitalo, Bruno Maffei, M. De Petris, P. de Bernardis, J. Austermann, L. Montier, S. Bounissou, Berend Winter, Peter Charles Hargrave, F. Columbro, Tomotake Matsumura, F. Noviello, Johannes Hubmayr, G. Jaehnig, S. Realini, Giampaolo Pisano, N. Trappe, Jon E. Gudmundsson, Sophie Henrot-Versille, A. Ritacco, Luca Lamagna, H. Imada, A. Suzuki, Silvia Masi, B. Mot, Cristian Franceschet, Giorgio Savini, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL), and Litebird Joint Study Group
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Computer science, optics: design, satellite, Cosmic microwave background, FOS: Physical sciences, cosmic background radiation: polarization, LiteBIRD, model: optical, 02 engineering and technology, LiteBIRD, Cosmic Microwave Background, polarization measurements, millimeter wavelengths,refractive telescopes, space telescopes, optical modeling, Space telescopes, 01 natural sciences, law.invention, 010309 optics, Telescope, law, Cosmic Microwave Background, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Aerospace engineering, Instrumentation and Methods for Astrophysics (astro-ph.IM), activity report, detector: design, business.industry, Gravitational wave, gravitational radiation: primordial, Astrophysics::Instrumentation and Methods for Astrophysics, System optimization, Refractive telescopes, sensitivity, 021001 nanoscience & nanotechnology, Polarization (waves), Optical modeling, B-mode, Polarization measurements, Control system, Millimeter wavelengths, Astrophysics - Instrumentation and Methods for Astrophysics, 0210 nano-technology, business, performance, Microwave, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: LiteBIRD is a JAXA strategic L-class mission devoted to the measurement of polarization of the Cosmic Microwave Background, searching for the signature of primordial gravitational waves in the B-modes pattern of the polarization. The onboard instrumentation includes a Middle and High Frequency Telescope (MHFT), based on a pair of cryogenically cooled refractive telescopes covering, respectively, the 89-224 GHz and the 166-448 GHz bands. Given the high target sensitivity and the careful systematics control needed to achieve the scientific goals of the mission, optical modeling and characterization are performed with the aim to capture most of the physical effects potentially affecting the real performance of the two refractors. We describe the main features of the MHFT, its design drivers and the major challenges in system optimization and characterization. We provide the current status of the development of the optical system and we describe the current plan of activities related to optical performance simulation and validation., Comment: 17 pages, 13 figures, SPIE Proceeding no. 11443-283
Published: 2020

14. Oscillations in the stochastic gravitational wave background from sharp features and particle production during inflation

Author: Jacopo Fumagalli, Lukas T. Witkowski, Sébastien Renaux-Petel, Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: High Energy Physics - Theory, data analysis method, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitational radiation: stochastic, perturbation, particle: production, Scalar (mathematics), FOS: Physical sciences, Parameter space, 01 natural sciences, Gravitational wave background, General Relativity and Quantum Cosmology, power spectrum: scalar, fluctuation: scalar, 0103 physical sciences, energy: density, gravitational radiation: spectrum, gravitational radiation: energy, inflation, 010303 astronomy & astrophysics, Envelope (waves), Physics, Inflation (cosmology), oscillation: frequency, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: background, gravitational radiation, gravitational radiation: primordial, modulation: frequency, Spectral density, Astronomy and Astrophysics, Observable, back reaction, gravitational radiation detector, background: stochastic, High Energy Physics - Theory (hep-th), Quantum electrodynamics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We identify a characteristic pattern in the scalar-induced stochastic gravitational wave background from particle production during inflation. If particle production is sufficiently efficient, the scalar power spectrum exhibits $\mathcal{O}(1)$ oscillations periodic in $k$, characteristic of a sharp feature, with an exponentially enhanced envelope. We systematically study the properties of the induced spectrum of gravitational waves sourced after inflation and find that this inherits the periodic structure in $k$, resulting in a peak in the gravitational wave energy density spectrum with $\mathcal{O}(10 \%)$ modulations. The frequency of the oscillation in the scalar power spectrum is determined by the scale of the feature during inflation and in turn sets the frequency of modulations in the gravitational wave signal. We present an explicit realisation of this phenomenon in the framework of multifield inflation, in the form of a strong sharp turn in the inflationary trajectory. The resulting stochastic background is potentially detectable in future gravitational wave observatories, and considerations of backreaction and perturbativity can be used to constrain the parameter space from the theoretical side. Our work motivates more extensive research linking primordial features to observable properties of the stochastic background of gravitational waves, and dedicated development in data analysis for their detection., 46 pages, 11 figures; v2: expanded the discussion of observational prospects as well as of resonant features, references added; v3: version published in JCAP, typos corrected
Published: 2020

15. Subtracting compact binary foreground sources to reveal primordial gravitational-wave backgrounds

Author: Bangalore Suryanarayana Sathyaprakash, Surabhi Sachdev, Tania Regimbau, Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire d'Annecy de Physique des Particules (LAPP), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)
Subjects: neutron star: binary, background: primordial, media_common.quotation_subject, Population, alternative theories of gravity, FOS: Physical sciences, detector: network, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Einstein Telescope, binary: coalescence, Binary black hole, 0103 physical sciences, KAGRA, LIGO, 010306 general physics, education, Astrophysics::Galaxy Astrophysics, media_common, Physics, education.field_of_study, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: background, gravitational radiation: primordial, family: 3, critical phenomena, binary: compact, sensitivity, gravitational radiation detector, background: stochastic, Universe, detector: sensitivity, Automatic Keywords, Neutron star, VIRGO, General relativity, black hole: binary, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc]
Abstract: Detection of primordial gravitational-wave backgrounds generated during the early universe phase transitions is a key science goal for future ground-based detectors. The rate of compact binary mergers is so large that their cosmological population produces a confusion background that could masquerade the detection of potential primordial stochastic backgrounds. In this paper we study the ability of current and future detectors to resolve the confusion background to reveal interesting primordial backgrounds. The current detector network of LIGO and Virgo and the upcoming KAGRA and LIGO-India will not be able to resolve the cosmological compact binary source population and its sensitivity to stochastic background will be limited by the confusion background of these sources. We find that a network of three (and five) third generation (3G) detectors of Cosmic Explorer and Einstein Telescope will resolve the confusion background produced by binary black holes leaving only about 0.013\% (respectively, 0.00075\%) unresolved; in contrast, as many as 25\% (respectively, 7.7\%) of binary neutron star sources remain unresolved. Consequently, the binary black hole population will likely not limit observation of primordial backgrounds but the binary neutron star population will limit the sensitivity of 3G detectors to $\Omega_{\rm GW} \sim 10^{-11}$ at 10 Hz (respectively, $\Omega_{\rm GW} \sim 3\times 10^{-12}$)., Comment: 9 pages, 2 figures, submitting to PRD
Published: 2020

16. Results of gravitational lensing and primordial gravitational waves from the POLARBEAR experiment

Author: Peter A. R. Ade, Davide Poletti, C. Verges, Shunsuke Adachi, Kam Arnold, Yuji Chinone, A. Suzuki, Yuto Minami, Chang Feng, J. Peloton, Nathan Whitehorn, Oliver Jeong, N. W. Halverson, Yuki Inoue, T. Hamada, Akito Kusaka, Y. Zhou, A. Zahn, A. Cukierman, M. Aguilar, Carole Tucker, D. Beck, Nicoletta Krachmalnicoff, Rolando Dünner, Brian Keating, Paul L. Richards, Stephen M. Feeney, J. C. Groh, Julian Borrill, C. Tsai, Joshua Montgomery, Darcy Barron, Theodore Kisner, R. Stompor, G. Hall, D. Boettger, Tucker Elleflot, Josquin Errard, Frederick Matsuda, L. N. Lowry, D. Leon, Takayuki Tomaru, Reijo Keskitalo, Benjamin Westbrook, M. Navaroli, D. Kaneko, K. Cheung, Osamu Tajima, A. T. P. Pham, Eric V. Linder, Giulio Fabbian, A. J. Gilbert, L. Howe, Neil Goeckner-Wald, H. El-Bouhargani, Max Silva-Feaver, Hans P. Paar, M. A. Dobbs, S. Takatori, Federico Bianchini, Colin Ross, Christian L. Reichardt, John Groh, Praween Siritanasak, Julien Carron, Tomotake Matsumura, T. Fujino, Y. Akiba, H. Nishino, G. Jaehnig, Giuseppe Puglisi, Charles A. Hill, D. Tanabe, Andrew H. Jaffe, Masashi Hazumi, Nicholas Galitzki, Blake D. Sherwin, S. Kikuchi, Carlo Baccigalupi, E. M. Leitch, S. Beckman, N. Katayama, Grant Teply, A. Ducout, Aashrita Mangu, M. LeJeune, Adrian T. Lee, Nathan Stebor, Masaya Hasegawa, S. Takakura, Y. Segawa, Scott Chapman, Kevin T. Crowley, Chinone, Y, Adachi, S, Ade, P, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Elbouhargani, H, Carron, J, Chapman, S, Cheung, K, Crowley, K, Cukierman, A, Dunner, R, Dobbs, M, Ducout, A, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jaffe, A, Jeong, O, Lejeune, M, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leitch, E, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Matsumura, T, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Richards, P, Ross, C, Segawa, Y, Sherwin, B, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tomaru, T, Tsai, C, Tucker, C, Verges, C, Westbrook, B, Whitehorn, N, Zahn, A, Zhou, Y, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), POLARBEAR, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: History, satellite: Planck, Cosmic microwave background, gravitational lensing, cosmic background radiation: polarization, detector: noise, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravity waves, power spectrum, 01 natural sciences, Education, Primary mirror, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, Polarization, 0103 physical sciences, Planck, mirror, 010303 astronomy & astrophysics, Physics, COSMIC cancer database, 010308 nuclear & particles physics, Gravitational wave, Settore FIS/05, POLARBEAR experiment, Gravitational effects, gravitational radiation: primordial, Astrophysics::Instrumentation and Methods for Astrophysics, Polarization (waves), Galaxy, Computer Science Applications, Gravitational lens, B-mode, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], galaxy
Abstract: POLARBEAR is a Cosmic Microwave Background radiation (CMB) polarization experiment that is located in the Atacama Desert in Chile. The scientific goals of the experiment are to characterize the B-mode signal from gravitational lensing, as well as to search for B-mode signals created by primordial gravitational waves (PGWs). Polarbear started observations in 2012 and has published a series of results. These include the first measurement of a nonzero B-mode angular auto-power spectrum at sub-degree scales where the dominant signal is gravitational lensing of the CMB. In addition, we have achieved the first measurement of crosscorrelation between the lensing potential, which was reconstructed from the CMB polarization data alone by Polarbear, and the cosmic shear field from galaxy shapes by the Subaru Hyper Suprime-Cam (HSC) survey. In 2014, we installed a continuously rotating half-wave plate (CRHWP) at the focus of the primary mirror to search for PGWs and demonstrated the control of low-frequency noise. We have found that the low-frequency B-mode power in the combined dataset with the Planck high-frequency maps is consistent with Galactic dust foreground, thus placing an upper limit on the tensor-to-scalar ratio of r < 0.90 at the 95% confidence level after marginalizing over the foregrounds.
Published: 2020

17. Deformation of the gravitational wave spectrum by density perturbations

Author: Henrique Rubira, Valerie Domcke, and Ryusuke Jinno
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), induced [gravitational radiation], propagation [gravitational radiation], primordial [black hole], FOS: Physical sciences, Primordial black hole, General Relativity and Quantum Cosmology (gr-qc), curvature: scalar, Curvature, 01 natural sciences, curvature: perturbation: scalar, Spectral line, General Relativity and Quantum Cosmology, scalar [curvature], High Energy Physics - Phenomenology (hep-ph), curvature: primordial, gravitational radiation: propagation, 0103 physical sciences, perturbation: scalar [curvature], primordial [curvature], gravitational radiation: spectrum, ddc:530, spectrum [gravitational radiation], background [gravitational radiation], Mathematical physics, Physics, 010308 nuclear & particles physics, Gravitational wave, perturbation [curvature], Isotropy, gravitational radiation: background, gravitational radiation: primordial, Astronomy and Astrophysics, gravitational radiation: induced, primordial [gravitational radiation], background: stochastic, High Energy Physics - Phenomenology, perturbation [density], Amplitude, stochastic [background], Sachs-Wolfe effect, density: perturbation, curvature: perturbation, black hole: primordial, Order of magnitude, Scalar curvature, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Journal of cosmology and astroparticle physics 2006(06), 046 - 046 (2020). doi:10.1088/1475-7516/2020/06/046, We study the effect of primordial scalar curvature perturbations on the propagation of gravitational waves over cosmic distances. We point out that such curvature perturbations deform the isotropic spectrum of any stochastic background of gravitational waves of primordial origin through the (integrated) Sachs-Wolfe effect. Computing the changes in the amplitude and frequency of the propagating gravitational wave induced at linear order by scalar curvature perturbations, we show that the resulting deformation of each frequency bin of the gravitational wave spectrum is described by a linearly biased Gaussian with the variance σ2 &simeq; ∫ d&ln; k Δ R2, where Δ; R2(k) denotes the amplitude of the primordial curvature perturbations. The linear bias encodes the correlations between the changes induced in the frequency and amplitude of the gravitational waves. Taking into account the latest bounds on Δ R2 from primordial black hole and gravitational wave searches, we demonstrate that the resulting O(σ) deformation can be significant for extremely peaked gravitational wave spectra. We further provide an order of magnitude estimate for broad spectra, for which the net distortion is O(σ2)., Published by IOP, London
Published: 2020
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18. Gravitational Waves as a Big Bang Thermometer

Author: Carlos Tamarit, Andreas Ringwald, and Jan Schütte-Engel
Subjects: Big Bang, Particle physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), plasma: temperature, gravitational radiation: stochastic, media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, cosmic background radiation, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), stochastic [gravitational radiation], model [inflation], ddc:530, Axion, Instrumentation and Methods for Astrophysics (astro-ph.IM), media_common, Inflation (cosmology), Physics, Gravitational wave, new physics, big bang, gravitational radiation: primordial, minimal supersymmetric standard model, primordial [gravitational radiation], Astronomy and Astrophysics, Universe, inflation: model, seesaw model, High Energy Physics - Phenomenology, axion, temperature [plasma], Neutrino, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Minimal Supersymmetric Standard Model
Abstract: Journal of cosmology and astroparticle physics 2021(03), 054 (2021). doi:10.1088/1475-7516/2021/03/054, There is a guaranteed background of stochastic gravitational waves produced in the thermal plasma in the early universe. Its energy density per logarithmic frequency interval scales with the maximum temperature Tmax which the primordial plasma attained at the beginning of the standard hot big bang era. It peaks in the microwave range, at around 80 GHz [106.75/g*s(Tmax)]1/3, where g*s(Tmax) is the effective number of entropy degrees of freedom in the primordial plasma at Tmax. We present a state-of-the-art prediction of this Cosmic Gravitational Microwave Background (CGMB) for general models, and carry out calculations for the case of the Standard Model (SM) as well as for several of its extensions. On the side of minimal extensions we consider the Neutrino Minimal SM (νMSM) and the SM-Axion-Seesaw-Higgs portal inflation model (SMASH), which provide a complete and consistent cosmological history including inflation. As an example of a non-minimal extension of the SM we consider the Minimal Supersymmetric Standard Model (MSSM). Furthermore, we discuss the current upper limits and the prospects to detect the CGMB in laboratory experiments and thus measure the maximum temperature and the effective number of degrees of freedom at the beginning of the hot big bang., Published by IOP, London
Published: 2020
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19. Updated design of the CMB polarization experiment satellite LiteBIRD

Author: H. Sugai, P. A. R. Ade, Y. Akiba, D. Alonso, K. Arnold, J. Aumont, J. Austermann, C. Baccigalupi, A. J. Banday, R. Banerji, R. B. Barreiro, S. Basak, J. Beall, S. Beckman, M. Bersanelli, J. Borrill, F. Boulanger, M. L. Brown, M. Bucher, A. Buzzelli, E. Calabrese, F. J. Casas, A. Challinor, V. Chan, Y. Chinone, J.-F. Cliche, F. Columbro, A. Cukierman, D. Curtis, P. Danto, P. de Bernardis, T. de Haan, M. De Petris, C. Dickinson, M. Dobbs, T. Dotani, L. Duband, A. Ducout, S. Duff, A. Duivenvoorden, J.-M. Duval, K. Ebisawa, T. Elleflot, H. Enokida, H. K. Eriksen, J. Errard, T. Essinger-Hileman, F. Finelli, R. Flauger, C. Franceschet, U. Fuskeland, K. Ganga, J.-R. Gao, R. Génova-Santos, T. Ghigna, A. Gomez, M. L. Gradziel, J. Grain, F. Grupp, A. Gruppuso, J. E. Gudmundsson, N. W. Halverson, P. Hargrave, T. Hasebe, M. Hasegawa, M. Hattori, M. Hazumi, S. Henrot-Versille, D. Herranz, C. Hill, G. Hilton, Y. Hirota, E. Hivon, R. Hlozek, D.-T. Hoang, J. Hubmayr, K. Ichiki, T. Iida, H. Imada, K. Ishimura, H. Ishino, G. C. Jaehnig, M. Jones, T. Kaga, S. Kashima, Y. Kataoka, N. Katayama, T. Kawasaki, R. Keskitalo, A. Kibayashi, T. Kikuchi, K. Kimura, T. Kisner, Y. Kobayashi, N. Kogiso, A. Kogut, K. Kohri, E. Komatsu, K. Komatsu, K. Konishi, N. Krachmalnicoff, C. L. Kuo, N. Kurinsky, A. Kushino, M. Kuwata-Gonokami, L. Lamagna, M. Lattanzi, A. T. Lee, E. Linder, B. Maffei, D. Maino, M. Maki, A. Mangilli, E. Martínez-González, S. Masi, R. Mathon, T. Matsumura, A. Mennella, M. Migliaccio, Y. Minami, K. Mistuda, D. Molinari, L. Montier, G. Morgante, B. Mot, Y. Murata, J. A. Murphy, M. Nagai, R. Nagata, S. Nakamura, T. Namikawa, P. Natoli, S. Nerval, T. Nishibori, H. Nishino, Y. Nomura, F. Noviello, C. O’Sullivan, H. Ochi, H. Ogawa, H. Ohsaki, I. Ohta, N. Okada, L. Pagano, A. Paiella, D. Paoletti, G. Patanchon, F. Piacentini, G. Pisano, G. Polenta, D. Poletti, T. Prouvé, G. Puglisi, D. Rambaud, C. Raum, S. Realini, M. Remazeilles, G. Roudil, J. A. Rubiño-Martín, M. Russell, H. Sakurai, Y. Sakurai, M. Sandri, G. Savini, D. Scott, Y. Sekimoto, B. D. Sherwin, K. Shinozaki, M. Shiraishi, P. Shirron, G. Signorelli, G. Smecher, P. Spizzi, S. L. Stever, R. Stompor, S. Sugiyama, A. Suzuki, J. Suzuki, E. Switzer, R. Takaku, H. Takakura, S. Takakura, Y. Takeda, A. Taylor, E. Taylor, Y. Terao, K. L. Thompson, B. Thorne, M. Tomasi, H. Tomida, N. Trappe, M. Tristram, M. Tsuji, M. Tsujimoto, C. Tucker, J. Ullom, S. Uozumi, S. Utsunomiya, J. Van Lanen, G. Vermeulen, P. Vielva, F. Villa, M. Vissers, N. Vittorio, F. Voisin, I. Walker, N. Watanabe, I. Wehus, J. Weller, B. Westbrook, B. Winter, E. Wollack, R. Yamamoto, N. Y. Yamasaki, M. Yanagisawa, T. Yoshida, J. Yumoto, M. Zannoni, A. Zonca, Sugai, H, Ade, P, Akiba, Y, Alonso, D, Arnold, K, Aumont, J, Austermann, J, Baccigalupi, C, Banday, A, Banerji, R, Barreiro, R, Basak, S, Beall, J, Beckman, S, Bersanelli, M, Borrill, J, Boulanger, F, Brown, M, Bucher, M, Buzzelli, A, Calabrese, E, Casas, F, Challinor, A, Chan, V, Chinone, Y, Cliche, J, Columbro, F, Cukierman, A, Curtis, D, Danto, P, de Bernardis, P, de Haan, T, De Petris, M, Dickinson, C, Dobbs, M, Dotani, T, Duband, L, Ducout, A, Duff, S, Duivenvoorden, A, Duval, J, Ebisawa, K, Elleflot, T, Enokida, H, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Ganga, K, Gao, J, Génova-Santos, R, Ghigna, T, Gomez, A, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, Gudmundsson, J, Halverson, N, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Hazumi, M, Henrot-Versille, S, Herranz, D, Hill, C, Hilton, G, Hirota, Y, Hivon, E, Hlozek, R, Hoang, D, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Jones, M, Kaga, T, Kashima, S, Kataoka, Y, Katayama, N, Kawasaki, T, Keskitalo, R, Kibayashi, A, Kikuchi, T, Kimura, K, Kisner, T, Kobayashi, Y, Kogiso, N, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kuo, C, Kurinsky, N, Kushino, A, Kuwata-Gonokami, M, Lamagna, L, Lattanzi, M, Lee, A, Linder, E, Maffei, B, Maino, D, Maki, M, Mangilli, A, Martínez-González, E, Masi, S, Mathon, R, Matsumura, T, Mennella, A, Migliaccio, M, Minami, Y, Mistuda, K, Molinari, D, Montier, L, Morgante, G, Mot, B, Murata, Y, Murphy, J, Nagai, M, Nagata, R, Nakamura, S, Namikawa, T, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, Nomura, Y, Noviello, F, O’Sullivan, C, Ochi, H, Ogawa, H, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Piacentini, F, Pisano, G, Polenta, G, Poletti, D, Prouvé, T, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Remazeilles, M, Roudil, G, Rubiño-Martín, J, Russell, M, Sakurai, H, Sakurai, Y, Sandri, M, Savini, G, Scott, D, Sekimoto, Y, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Spizzi, P, Stever, S, Stompor, R, Sugiyama, S, Suzuki, A, Suzuki, J, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takeda, Y, Taylor, A, Taylor, E, Terao, Y, Thompson, K, Thorne, B, Tomasi, M, Tomida, H, Trappe, N, Tristram, M, Tsuji, M, Tsujimoto, M, Tucker, C, Ullom, J, Uozumi, S, Utsunomiya, S, Van Lanen, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Voisin, F, Walker, I, Watanabe, N, Wehus, I, Weller, J, Westbrook, B, Winter, B, Wollack, E, Yamamoto, R, Yamasaki, N, Yanagisawa, M, Yoshida, T, Yumoto, J, Zannoni, M, Zonca, A, World Premier International Research Center (Japan), Japan Society for the Promotion of Science, Ministry of Education, Culture, Sports, Science and Technology (Japan), Agenzia Spaziale Italiana, Istituto Nazionale di Fisica Nucleare, Centre National D'Etudes Spatiales (France), Centre National de la Recherche Scientifique (France), Commissariat à l'Ènergie Atomique et aux Ènergies Alternatives (France), European Space Agency, Canadian Space Agency, National Aeronautics and Space Administration (US), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National d’Études Spatiales [Paris] (CNES), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Sugai, H. [0000-0001-6501-3871], and Apollo - University of Cambridge Repository
Subjects: Passive cooling, Cosmic Microwave Background, Cosmology, Polarimetry, Instrumentation, Inflation, Cosmic microwave background, cosmic background radiation: polarization, 7. Clean energy, 01 natural sciences, Polarization, General Materials Science, 010303 astronomy & astrophysics, media_common, Physics, Settore FIS/01, Settore FIS/05, Astrophysics::Instrumentation and Methods for Astrophysics, suppression, Condensed Matter Physics, Polarization (waves), Atomic and Molecular Physics, and Optics, Infation, adiabatic, Astrophysics - Instrumentation and Methods for Astrophysics, signature, Astrophysics and Astronomy, media_common.quotation_subject, Lagrangian point, Inflation, Primordial gravitational wave, Satellite, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Noise (electronics), Article, NO, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, noise: thermal, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010308 nuclear & particles physics, Gravitational wave, PE9_14, beam: width, gravitational radiation: primordial, Astronomy, 13. Climate action, Sky, spectral, galaxy, astro-ph.IM
Abstract: H. Sugai, et al., Recent developments of transition-edge sensors (TESs), based on extensive experience in ground-based experiments, have been making the sensor techniques mature enough for their application on future satellite cosmic microwave background (CMB) polarization experiments. LiteBIRD is in the most advanced phase among such future satellites, targeting its launch in Japanese Fiscal Year 2027 (2027FY) with JAXA’s H3 rocket. It will accommodate more than 4000 TESs in focal planes of reflective low-frequency and refractive medium-and-high-frequency telescopes in order to detect a signature imprinted on the CMB by the primordial gravitational waves predicted in cosmic inflation. The total wide frequency coverage between 34 and 448 GHz enables us to extract such weak spiral polarization patterns through the precise subtraction of our Galaxy’s foreground emission by using spectral differences among CMB and foreground signals. Telescopes are cooled down to 5 K for suppressing thermal noise and contain polarization modulators with transmissive half-wave plates at individual apertures for separating sky polarization signals from artificial polarization and for mitigating from instrumental 1/f noise. Passive cooling by using V-grooves supports active cooling with mechanical coolers as well as adiabatic demagnetization refrigerators. Sky observations from the second Sun–Earth Lagrangian point, L2, are planned for 3 years. An international collaboration between Japan, the USA, Canada, and Europe is sharing various roles. In May 2019, the Institute of Space and Astronautical Science, JAXA, selected LiteBIRD as the strategic large mission No. 2., This work was supported by World Premier International Research Center Initiative (WPI), MEXT, Japan, by JSPS Core-to-Core Program, A. Advanced Research Networks, and by JSPS KAKENHI Grant Numbers JP15H05891, JP17H01115, and JP17H01125. The Italian contribution to the LiteBIRD phase A is supported by the Italian Space Agency (ASI Grant No. 2016-24- H.1-2018) and the National Institute for Nuclear Physics (INFN). The French contribution to the LiteBIRD phase A is supported by the Centre National d’Etudes Spatiale (CNES), by the Centre National de la Recherche Scientifque (CNRS), and by the Commissariat à l’Energie Atomique (CEA). A Concurrent Design Facility study focused on the MHFT and Sub-Kelvin coolers has been led by the European Space Agency (ESA). The Canadian contribution to LiteBIRD is supported by the Canadian Space Agency. The US contribution is supported by NASA Grant no. 80NSSC18K0132
Published: 2020
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20. A Demonstration of Improved Constraints on Primordial Gravitational Waves with Delensing

Author: Roger O'Brient, John M Kovac, Kirit Karkare, T. Natoli, Kent D. Irwin, A. E. Lowitz, N. Huang, Y. Omori, Victor Buza, Robert I. Citron, S. A. Kernasovskiy, W. L. Holzapfel, Ahmed Soliman, Jeff McMahon, C. Corbett Moran, P. A. R. Ade, Lingzhen Zeng, S. Henderson, W. B. Everett, J. D. Hrubes, Jessica Avva, C. Yu, Calvin B. Netterfield, Lorenzo Moncelsi, J. R. Cheshire, Jason W. Henning, J. A. Grayson, S. Patil, K. K. Schaffer, Elizabeth George, Abigail G. Vieregg, Denis Barkats, V. G. Yefremenko, Jason E. Austermann, N. W. Halverson, A. Cukierman, H. Boenish, B. L. Schmitt, Marion Dierickx, M. Crumrine, K. W. Yoon, Joaquin Vieira, E. Young, G. Hall, Stefan Richter, C. Sievers, Toshiya Namikawa, Graeme Smecher, C. Umilta, D. V. Wiebe, S. Fliescher, T.-L. Chou, H. C. Chiang, Johannes Hubmayr, H. Yang, C. D. Sheehy, Chao-Lin Kuo, Mark Halpern, Christian L. Reichardt, Marius Millea, Joshua Montgomery, S. Kefeli, J. Cornelison, J. J. Bock, Bryan Steinbach, Howard Hui, Gensheng Wang, Andreas Bender, Neil Goeckner-Wald, J. E. Ruhl, Dale Li, C. Tucker, K. G. Megerian, T. M. Crawford, M. A. Dobbs, Mandana Amiri, V. Novosad, R. Schwarz, S. Fatigoni, S. R. Hildebrandt, S. Padin, John E. Carlstrom, E. Bullock, Chao Zhang, T. de Haan, D. C. Goldfinger, John P. Nibarger, Andrew Nadolski, J. Willmert, Carl D. Reintsema, Gene C. Hilton, N. Whitehorn, B. Racine, H. T. Nguyen, A. A. Stark, E. M. Leitch, Alessandro Schillaci, A. D. Turner, E. Karpel, T. Veach, R. Basu Thakur, K. L. Thompson, T. Prouve, A. T. Crites, C. Pryke, C. L. Wong, C. L. Chang, J. Kang, Adam Anderson, Grant Teply, Benjamin Saliwanchik, A. Wandui, Gilbert Holder, A. Manzotti, A. C. Weber, G. I. Noble, Federico Bianchini, Nikhel Gupta, Jeffrey P. Filippini, R. V. Sudiwala, Adrian T. Lee, Bradford Benson, Lloyd Knox, W. L. K. Wu, Colin A. Bischoff, S. S. Meyer, Jason Gallicchio, T. St. Germaine, S. Palladino, L. Duband, J. E. Tolan, Zeeshan Ahmed, L. M. Mocanu, Jake Connors, Kei May Lau, Sarah M. Harrison, Lindsey Bleem, R. W. Ogburn, J. A. Beall, Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), SPTpol, BICEP/Keck, BICEP, and Keck
Subjects: data analysis method, satellite: Planck, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, Cosmic background radiation, cosmic background radiation: polarization, FOS: Physical sciences, cosmic background radiation, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, cosmic rays, gravitation: lens, statistical analysis, Cosmic infrared background, 0103 physical sciences, Experiments in gravity, Sample variance, Planck, numerical calculations, 010306 general physics, Astrophysics::Galaxy Astrophysics, Physics, polarization, background, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: primordial, BICEP, South Pole Telescope, Gravitational lens, B-mode, infrared, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a constraint on the tensor-to-scalar ratio, $r$, derived from measurements of cosmic microwave background (CMB) polarization $B$-modes with "delensing," whereby the uncertainty on $r$ contributed by the sample variance of the gravitational lensing $B$-modes is reduced by cross-correlating against a lensing $B$-mode template. This template is constructed by combining an estimate of the polarized CMB with a tracer of the projected large-scale structure. The large-scale-structure tracer used is a map of the cosmic infrared background derived from Planck satellite data, while the polarized CMB map comes from a combination of South Pole Telescope, BICEP/Keck, and Planck data. We expand the BICEP/Keck likelihood analysis framework to accept a lensing template and apply it to the BICEP/Keck data set collected through 2014 using the same parametric foreground modelling as in the previous analysis. From simulations, we find that the uncertainty on $r$ is reduced by $\sim10\%$, from $��(r)$= 0.024 to 0.022, which can be compared with a $\sim26\%$ reduction obtained when using a perfect lensing template. Applying the technique to the real data, the constraint on $r$ is improved from $r_{0.05} < 0.090$ to $r_{0.05} < 0.082$ (95\% C.L.). This is the first demonstration of improvement in an $r$ constraint through delensing., 23 pages, 11 figures; match published version
Published: 2020
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21. Primordial gravitational waves in a minimal model of particle physics and cosmology

Author: Ringwald, Andreas, Saikawa, Ken’ichi, and Tamarit, Carlos
Subjects: cosmological model, fluctuation: tensor, interferometer, gravitational radiation: primordial, temperature, Astrophysics::Cosmology and Extragalactic Astrophysics, critical phenomena, sensitivity, dark matter, horizon, Peccei-Quinn, axion, baryon: asymmetry, neutrino: mass, inflation, strong interaction: CP, model: minimal, equation of state
Abstract: In this paper we analyze the spectrum of the primordial gravitational waves (GWs) predicted in the Standard Model*Axion*Seesaw*Higgs portal inflation (SMASH) model, which was proposed as a minimal extension of the Standard Model that addresses five fundamental problems of particle physics and cosmology (inflation, baryon asymmetry, neutrino masses, strong CP problem, and dark matter) in one stroke. The SMASH model has a unique prediction for the critical temperature of the second order Peccei-Quinn (PQ) phase transition $T_c \sim 10^8\,\mathrm{GeV}$, implying that there is a drastic change in the equation of state of the universe at that temperature. Such an event is imprinted on the spectrum of GWs originating from the primordial tensor fluctuations during inflation and entering the horizon at $T \sim T_c$, which corresponds to $f \sim 1\,\mathrm{Hz}$, pointing to a best frequency range covered by future space-borne GW interferometers. We give a precise estimation of the effective relativistic degrees of freedom across the PQ phase transition and use it to evaluate the spectrum of GWs observed today. It is shown that the future high sensitivity GW experiment -- ultimate DECIGO -- can probe the nontrivial feature resulting from the PQ phase transition in this model.
Published: 2020
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22. A Measurement of the Degree Scale CMB B-mode Angular Power Spectrum with POLARBEAR

Author: Julien Carron, M. A. Dobbs, C. Tsai, Dominic Beck, D. Leon, Ted Kisner, Aashrita Mangu, D. Boettger, Christian L. Reichardt, A. T. P. Pham, Kam Arnold, Akito Kusaka, Nicoletta Krachmalnicoff, T. Hamada, John Groh, S. Beckman, Josquin Errard, Ben Westbrook, Nathan Stebor, Neil Goeckner-Wald, Reijo Keskitalo, Daisuke Kaneko, Greg Jaehnig, Kevin T. Crowley, S. Takatori, Masaya Hasegawa, D. Tanabe, Tucker Elleflot, Giulio Fabbian, L. Howe, A. Cukierman, T. Fujino, Y. Zhou, S. Takakura, Eric V. Linder, Julian Borrill, N. Katayama, Yuki Inoue, Davide Poletti, Praween Siritanasak, Haruki Nishino, Yuto Minami, Yuji Chinone, Y. Segawa, H. El Bouhargani, Osamu Tajima, Aritoki Suzuki, N. W. Halverson, Darcy Barron, Masashi Hazumi, L. N. Lowry, G. Hall, Frederick Matsuda, Federico Bianchini, Scott Chapman, M. Navaroli, R. Stompor, Nicholas Galitzki, Clara Vergès, Maximiliano Silva-Feaver, Oliver Jeong, M. A. O. Aguilar Faúndez, Grant Teply, Brian Keating, Shunsuke Adachi, S. Kikuchi, K. Cheung, Adrian T. Lee, Giuseppe Puglisi, Charles A. Hill, Chang Feng, C. Baccigalupi, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), POLARBEAR, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Adachi, S, Aguilar Faundez, M, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Cukierman, A, Dobbs, M, Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Fujino, T, Galitzki, N, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jeong, O, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Minami, Y, Navaroli, M, Nishino, H, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Segawa, Y, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), APC - Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmic microwave background radiation, Cosmic inflation, Cosmology, Observational cosmology, cosmological model, 010504 meteorology & atmospheric sciences, Cosmic microwave background, Astrophysics, 01 natural sciences, Atomic, Physical Chemistry, Spectral line, thermal, Cosmic microwave background radiationCosmic inflationCosmologyObservational cosmology, Particle and Plasma Physics, polarization: power spectrum, 010303 astronomy & astrophysics, media_common, Physics, Settore FIS/05, Polarization (waves), symbols, astro-ph.CO, power spectrum: angular dependence, Astronomical and Space Sciences, Physical Chemistry (incl. Structural), Astrophysics - Cosmology and Nongalactic Astrophysics, data analysis method, noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, frequency: high, cosmic background radiation: B-mode, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, statistical analysis, 0103 physical sciences, Nuclear, Planck, cosmic background radiation: power spectrum, inflation, 0105 earth and related environmental sciences, gravitational radiation: primordial, gravitational radiation, Spectral density, Molecular, Astronomy and Astrophysics, Square degree, detector: sensitivity, Space and Planetary Science, Sky, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We present a measurement of the $B$-mode polarization power spectrum of the cosmic microwave background (CMB) using taken from July 2014 to December 2016 with the POLARBEAR experiment. The CMB power spectra are measured using observations at 150 GHz with an instantaneous array sensitivity of $\mathrm{NET}_\mathrm{array}=23\, \mu \mathrm{K} \sqrt{\mathrm{s}}$ on a 670 square degree patch of sky centered at (RA, Dec)=($+0^\mathrm{h}12^\mathrm{m}0^\mathrm{s},-59^\circ18^\prime$). A continuously rotating half-wave plate is used to modulate polarization and to suppress low-frequency noise. We achieve $32\,\mu\mathrm{K}$-$\mathrm{arcmin}$ effective polarization map noise with a knee in sensitivity of $\ell = 90$, where the inflationary gravitational wave signal is expected to peak. The measured $B$-mode power spectrum is consistent with a $\Lambda$CDM lensing and single dust component foreground model over a range of multipoles $50 \leq \ell \leq 600$. The data disfavor zero $C_\ell^{BB}$ at $2.2\sigma$ using this $\ell$ range of POLARBEAR data alone. We cross-correlate our data with Planck high frequency maps and find the low-$\ell$ $B$-mode power in the combined dataset to be consistent with thermal dust emission. We place an upper limit on the tensor-to-scalar ratio $r < 0.90$ at 95% confidence level after marginalizing over foregrounds.
Published: 2019

23. Removal of Galactic foregrounds for the Simons Observatory primordial gravitational wave search

Author: Thorne, Ben, Dunkley, Jo, Alonso, David, Abitbol, Maximilian H., Errard, Josquin, Hill, J. Colin, Keating, Brian, Teply, Grant, Wollack, Edward J., AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: data analysis method, Cosmology and Nongalactic Astrophysics (astro-ph.CO), synchrotron radiation, Astrophysics::Instrumentation and Methods for Astrophysics, energy spectrum, gravitational radiation: primordial, FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, parametric, power spectrum, thermal, statistical analysis, numerical methods, galaxy, numerical calculations, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Upcoming observations from the Simons Observatory have been projected to constrain the tensor-to-scalar ratio, $r$, at the level of $\sigma(r)=$0.003. Here we describe one of the forecasting algorithms for the Simons Observatory in more detail, based on cleaning CMB polarization maps using a parametric model. We present a new code to perform this end-to-end forecast, and explore the assumptions in greater detail. If spatial uniformity of the spectral energy distribution of synchrotron radiation and thermal dust emission is assumed over the region planned for observations, covering almost a fifth of the sky, a bias of order 1--3$\sigma$ in $r$ is projected for foreground models consistent with current data. We find that by masking the most contaminated regions of sky, or by adopting more parameters to describe the spatial variation in spectral index for synchrotron and dust, such a bias can be mitigated for the foreground models we consider. We also explore strategies for testing whether the cleaned CMB polarization maps contain residual foreground contamination, including cross-correlating with maps tracing the foregrounds. This method also has applications for other CMB polarization experiments., Comment: 13 pages, 9 figures
Published: 2019

24. LiteBIRD: A Satellite for the Studies of B-Mode Polarization and Inflation from Cosmic Background Radiation Detection

Author: Josquin Errard, Kent D. Irwin, Ingunn Kathrine Wehus, Kazunori Kohri, Kam Arnold, Atsushi Okamoto, Osamu Tajima, T. Tomida, Hirokazu Ishino, L. Montier, T. Kawasaki, M. Willer, Ryo Yamamoto, Nobuhiko Katayama, B. Thorne, Eiichiro Komatsu, Takayuki Tomaru, Benjamin Westbrook, Toshiaki Iida, Tadayasu Dotani, Yuki Inoue, T. Funaki, Chiko Otani, Bruno Maffei, L. Hayes, Charles A. Hill, F. Vansyngel, T. Nagasaki, L. Duband, Tucker Elleflot, H. Imada, Johannes Hubmayr, A. Cukierman, M. Nakajima, T. Hasebe, Paul Turin, A. Dominjon, Eric V. Linder, S. Takatori, Toshifumi Shimizu, Yuto Minami, Shin Utsunomiya, Y. Sato, Yoshinori Uzawa, D. Tanabe, J. M. Duval, F. Boulanger, Takahiro Okamura, Jo Dunkley, Hiroyuki Sugita, Masato Naruse, Julian Borrill, Makoto Hattori, Theodore Kisner, Yuji Chinone, Tom Nitta, Dale Li, Mathieu Remazeilles, K. Ganga, Hideo Ogawa, Reijo Keskitalo, Masashi Hazumi, Giampaolo Pisano, E. Taylor, S. Takakura, H. Kanai, Jun-ichi Suzuki, N. Sato, Masahiro Tsujimoto, Yutaro Sekimoto, Shin-ichiro Sakai, Kimihiro Kimura, M. Nagai, N. W. Halverson, Anna Mangilli, Seongjae Cho, M. Tristram, S. A. Kernasovskiy, Jonathan Aumont, Blake D. Sherwin, Carole Tucker, Tomotake Matsumura, Kiyotomo Ichiki, Satoru Mima, T. de Haan, T. Hamada, N. Tomita, G. Patanchon, K. Komatsu, Shuji Matsuura, J. Grain, Paul L. Richards, Norio Okada, N. Hidehira, Kazuhisa Mitsuda, Soumen Basak, Yasuhiro Yamada, Aritoki Suzuki, H. K. Eriksen, Hajime Sugai, Shogo Nakamura, Peter A. R. Ade, Alex Lazarian, T. Fujino, Y. Akiba, Gabriel M. Rebeiz, H. Nishino, Nathan Whitehorn, Martin Bucher, R. Stompor, Shingo Kashima, A. Kibayashi, Y. Kida, Noah Kurinsky, D. W. Curtis, M. Inoue, Masaya Hasegawa, Adrian T. Lee, Shugo Oguri, Y. Segawa, David Alonso, A. Ducout, Carlo Baccigalupi, U. Fuskeland, S. Beckman, Uroš Seljak, R. Nagata, J. Fischer, Mitsuhiro Yoshida, K. L. Thompson, Darcy Barron, Gene C. Hilton, Noriko Y. Yamasaki, Erminia Calabrese, Neil Goeckner-Wald, R. Takaku, Suguru Takada, M. A. Dobbs, Oliver Jeong, Toshiya Namikawa, Yuki Sakurai, Chao-Lin Kuo, Kaori Hattori, Keisuke Shinozaki, D. Meilhan, M. Maki, Makoto Sawada, D. Kaneko, T. Yamashita, S. Uozumi, Takashi Noguchi, Akito Kusaka, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Service des Basses Températures (SBT ), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)
Subjects: detector: cryogenics, Cosmic microwave background, Cosmic background radiation, cosmic background radiation: polarization, Lagrangian point, B-mode polarization, Cosmic inflation, Primordial gravitational wave, Quantum gravity, Satellite, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 010305 fluids & plasmas, law.invention, Telescope, Settore FIS/05 - Astronomia e Astrofisica, bolometer, law, 0103 physical sciences, General Materials Science, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], detector: optical, 010306 general physics, Physics, Bolometer, gravitational radiation: primordial, Astrophysics::Instrumentation and Methods for Astrophysics, Condensed Matter Physics, Polarization (waves), inflation: model, Atomic and Molecular Physics, and Optics, detector: sensitivity, modulation, Cardinal point, B-mode, angular resolution, moment: multipole, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Multipole expansion
Abstract: 著者人数: 152名(所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 羽澄, 昌史; 堂谷, 忠靖; 長谷部, 孝; 今田, 大皓; 満田, 和久; 坂井, 真一郎; 関本, 裕太郎; Tomida, T.; 辻本, 匡弘; Yamamoto, R.; 山崎, 典子), Accepted: 2019-01-18, 資料番号: SA1180402000
Published: 2019

25. Is patchy reionization an obstacle in detecting the primordial gravitational wave signal?

Author: S. Paul, Suvodip Mukherjee, Tirthankar Roy Choudhury, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, Sorbonne Université (SU), and Sorbonne Universités
Subjects: electron, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, first stars, Cosmic background radiation, halo, cosmic background radiation: polarization, FOS: Physical sciences, Astrophysics, cosmic background radiation, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, B-mode: primordial, cosmic background radiation: B-mode, 0103 physical sciences, ionization, cosmic background radiation: power spectrum, dark ages, 010303 astronomy & astrophysics, Reionization, Physics, spatial distribution, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: primordial, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, recombination, observatory, Amplitude, frequency: low, Space and Planetary Science, efficiency, cosmology: observations, Astrophysics of Galaxies (astro-ph.GA), Dark Ages, reionization, Halo, history, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The large-scale CMB B-mode polarization is the direct probe to the low frequency primordial gravitational wave signal. However, unambiguous measurement of this signal requires a precise understanding of the possible contamination. One such potential contamination arises from the patchiness in the spatial distribution of free electrons during the epoch of reionization. We estimate the B-mode power spectrum due to patchy reionization using a combination of \emph{photon-conserving} semi-numerical simulation and analytical calculation, and compare its amplitude with the primordial B-mode signal. For a reionization history which is in agreement with several latest observations, we find that a stronger secondary B-mode polarization signal is produced when the reionization is driven by the sources in massive halos and its amplitude can be comparable to the recombination bump for tensor to scalar ratio $(r) \lesssim 5 \times 10^{-4}$. If contamination from patchy reionization is neglected in the analysis of B-mode polarization data, then for the models of reionization considered in this analysis, we find a maximum bias of about $30\%$ in the value of $r=\,10^{-3}$ when spatial modes between $\ell \in [50, 200]$ are used with a delensing efficiency of $50\%$. The inferred bias from patchy reionization is not a severe issue for the upcoming ground-based CMB experiment Simons Observatory, but can be a potential source of confusion for proposed CMB experiments which target to detect the value of $r< 10^{-3}$. However, this obstacle can be removed by utilizing the difference in the shape of the power spectrum from the primordial signal., 9 pages, 6 figures. Reference added
Published: 2019
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26. Electrical characterization and tuning of the integrated POLARBEAR-2a focal plane and readout (Conference Presentation)

Author: J. Borrill, Paul L. Richards, Stephen M. Feeney, A. T. P. Pham, J. Peloton, Darcy Barron, Mario Aguilar, Josquin Errard, L. N. Lowry, D. Beck, A. Cukierman, Akito Kusaka, M. Le Jeune, Neil Goeckner-Wald, Max Silva Feaver, W. L. Holzapfel, Nicoletta Krachmalnicoff, Gabriele Coppi, H. Roberts, Peter Ashton, A. Tikhomirov, M. A. Dobbs, Osamu Tajima, D. Leon, Masashi Hazumi, P. A. R. Ade, Grant Teply, Nathan J. Miller, Colin Ross, Nicholas Galitzki, P. Siritanasak, Blake D. Sherwin, Tucker Elleflot, Y. Akiba, K. M. Rotermund, S. Beckman, A. J. Gilbert, Christian L. Reichardt, R. Dunner, Gary A. Fuller, Oliver Jeong, Eric V. Linder, A. Madurowicz, Giulio Fabbian, John Groh, Jessica Avva, Yuki Inoue, S. Takatori, G. Jaehnig, Carlo Baccigalupi, Giuseppe Puglisi, Charles A. Hill, S. Takakura, Andrew May, Scott Chapman, D. Plambeck, Kevin T. Crowley, D. Tanabe, Kam Arnold, Brian Keating, Aamir Ali, Benjamin Westbrook, M. Navroli, Adrian T. Lee, Jennifer Ito, Masaya Hasegawa, Aritoki Suzuki, Federico Bianchini, Theodore Kisner, Julien Carron, Tomotake Matsumura, Reijo Keskitalo, Daisuke Kaneko, Y. Segawa, T. Natoli, Frederick Matsuda, Yuji Chinone, N. W. Halverson, R. Stompor, T. de Haan, T. Hamada, A. Zahn, Amy N. Bender, D. Boettger, Takayuki Tomaru, R. Tat, A. Lowitz, Chang Feng, C. Tsai, Lucio Piccirillo, Leo Steinmetz, Nobuhiko Katayama, Daisy Mak, Davide Poletti, C. Verges, L. Howe, Haruki Nishino, A. Anderson, Yuto Minami, Gabriel M. Rebeiz, Nathan Whitehorn, Christopher Raum, Joshua Montgomery, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: temperature: transition, Cosmic microwave background, cosmic background radiation: polarization, frequency-division multiplexing, Astrophysics::Cosmology and Extragalactic Astrophysics, SQUID, 01 natural sciences, 010305 fluids & plasmas, law.invention, cosmic background radiation: B-mode, Optics, bolometer, gravitation: lens, law, 0103 physical sciences, millimeter-wave, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], inflation, 010306 general physics, Physics, Gravitational wave, business.industry, superconductivity, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation: primordial, Spectral density, cosmic microwave background polarization, stability, Polarization (waves), transition-edge sensor, Extremely high frequency, resonance: frequency, power spectrum: angular dependence, readout, dfmux, Transition edge sensor, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; POLARBEAR is a cosmic microwave background (CMB) polarization experiment located in the Atacama desert in Chile. The science goals of the POLARBEAR project are to do a deep search for CMB B-mode polarization created by inflationary gravitational waves, as well as characterize the CMB B-mode signal from gravitational lensing. POLARBEAR-1 started observations in 2012, and the POLARBEAR team has published a series of results from its first two seasons of observations, including the first measurement of a non-zero B-mode polarization angular power spectrum, measured at sub-degree scales where the dominant signal is gravitational lensing of the CMB. The Simons Array expands POLARBEAR to include an additional two telescopes with next-generation POLARBEAR-2 multi-chroic receivers, observing at 95, 150, 220, and 270 GHz.The POLARBEAR-2A focal plane has 7,588 transition-edge sensor bolometers, read out with frequency-division multiplexing, with 40 frequency channels within the readout bandwidth of 1.5 to 4.5 MHz. The frequency channels are defined by a low-loss lithographed aluminum spiral inductor and interdigitated capacitor in series with each bolometer, creating a resonant frequency for each channel's unique voltage bias and current readout. Characterization of the readout includes measuring resonant peak locations and heights and fitting to a circuit model both above and below the bolometer superconducting transition temperature. This information is used determine the optimal detector bias frequencies and characterize stray impedances which may affect bolometer operation and stability. The detector electrical characterization includes measurements of the transition properties by sweeping in temperature and in voltage bias, measurements of the bolometer saturation power, as well as measuring and removing any biases introduced by the readout circuit. We present results from the characterization, tuning, and operation of the fully integrated focal plane and readout for the first POLARBEAR-2 receiver, POLARBEAR-2A, during its pre-deployment integration run.
Published: 2018

27. Ultra-thin large-aperture vacuum windows for millimeter wavelengths receivers

Author: R. W. Ogburn, E. Bullock, Mark Halpern, B. Racine, Grant Teply, M. Lueker, K. Lau, J. Willmert, S. J. Benton, G. Hall, H. T. Nguyen, I. Buder, Peter A. R. Ade, Lorenzo Moncelsi, Bryan Steinbach, J. Kang, R. Bowens-Rubin, Hong Yang, Abigail G. Vieregg, Randol W. Aikin, M. Crumrine, J. Connors, K. L. Thompson, B. G. Keating, Howard Hui, J. P. Kaufman, K. G. Megerian, C. L. Kuo, S. A. Harrison, S. Palladino, Marion Dierickx, Justus A. Brevik, Carole Tucker, S. Fliescher, Chris Pentacoff, N. A. Larsen, Zeeshan Ahmed, S. A. Kernasovskiy, S. R. Hildebrandt, Victor Buza, A. Wandui, J. E. Tolan, Denis Barkats, C. L. Wong, Kate D. Alexander, Roger O'Brient, E. Karpel, C. Pryke, Jeffrey P. Filippini, J. J. Bock, R. V. Sudiwala, S. Kefeli, W. L. K. Wu, C. D. Sheehy, K. W. Yoon, D. V. Wiebe, Cora Dvorkin, R. Schwarz, E. M. Leitch, J. Cornelison, C. Umiltà, A. C. Weber, John M Kovac, G. C. Hilton, Kirit Karkare, Kent D. Irwin, S. Richter, Colin A. Bischoff, B. P. Crill, Alessandro Schillaci, T. St. Germaine, Ahmed Soliman, J. A. Grayson, C. Zhang, A. D. Turner, L. Duband, T. Namikawa, Z. K. Staniszewski, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Zmuidzinas, Jonas, and Gao, Jian-Rong
Subjects: Cryostat, Materials science, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Transmission loss, polymer, Cosmic microwave background, FOS: Physical sciences, cosmic background radiation: polarization, fabrication, 7. Clean energy, 01 natural sciences, microwaves, 010309 optics, Optics, Vacuum Windows, Polarization, 0103 physical sciences, Cosmic Microwave Background, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), attenuation, Primordial Gravitational Waves, business.industry, Attenuation, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation: primordial, Polymer Materials, Polarization (waves), sensitivity, BICEP, vacuum system, Wavelength, Millimeter Wavelengths, cryogenics, Keck Array, Millimeter, atmosphere: pressure, business, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Microwave, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Targeting faint polarization patterns arising from Primordial Gravitational Waves in the Cosmic Microwave Background requires excellent observational sensitivity. Optical elements in small aperture experiments such as Bicep3 and Keck Array are designed to optimize throughput and minimize losses from transmission, reflection and scattering at millimeter wavelengths. As aperture size increases, cryostat vacuum windows must withstand larger forces from atmospheric pressure and the solution has often led to a thicker window at the expense of larger transmission loss. We have identified a new candidate material for the fabrication of vacuum windows: with a tensile strength two orders of magnitude larger than previously used materials, woven high-modulus polyethylene could allow for dramatically thinner windows, and therefore significantly reduced losses and higher sensitivity. In these proceedings we investigate the suitability of high-modulus polyethylene windows for ground-based CMB experiments, such as current and future receivers in the Bicep/Keck Array program. This includes characterizing their optical transmission as well as their mechanical behavior under atmospheric pressure. We find that such ultra-thin materials are promising candidates to improve the performance of large-aperture instruments at millimeter wavelengths, and outline a plan for further tests ahead of a possible upcoming field deployment of such a science-grade window., Comment: Published in Proc. SPIE. Presented at SPIE Astronomical Telescopes and Instrumentation Conference 10708: Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XI, June 2018. 14 pages, 7 figures
Published: 2018

28. Simulations and performance of the QUBIC optical beam combiner

Author: Emory F. Bunn, M.-A. Bigot-Sazy, Y. Giraud-Héraud, A. Zullo, Alessandro Buzzelli, M. Gómez Berisso, M. Giard, F. Voisin, J. Aumont, L. Mele, N. Bleurvacq, L. Dumoulin, L. Grandsire, Nicola Vittorio, Giuseppe D'Alessandro, P. Ringegni, F. Piacentini, Peter T. Timbie, P. Chanial, D. Viganò, M. C. Medina, Alessandro Schillaci, Créidhe O'Sullivan, Laurent Bergé, G. Polenta, Gabriele Coppi, Steve Torchinsky, P. Battaglia, L. Montier, X. Garrido, J.-P. Thermeau, Massimo Gervasi, V. Truongcanh, Rocco D'Agostino, M. Gaspard, R. Puddu, J. Bonaparte, Luca Lamagna, S. Spinelli, C. Chapron, G. de Gasperis, Victor Haynes, A. Etchegoyen, S. Loucatos, Gregory S. Tucker, L. M. Mundo, Marco Bersanelli, A. Lowitz, G. Bordier, E. Guerrard, Mario Zannoni, A. Pelosi, G. Amico, Vladimir V. Luković, D. Buzi, E. Olivieri, R. Luterstein, S. Scully, D. Prêle, H. Pastoriza, A. Mattei, J. Kaplan, F. Columbro, A. Gault, A. Passerini, F. Pajot, D. Harari, Silvia Masi, A. Di Donato, B. Watson, M. Stolpovskiy, Gustavo E. Romero, E. Bréelle, R. Charlassier, J. Bonis, Elia S. Battistelli, D. Gayer, M. De Leo, A. Tartari, Peter A. R. Ade, J. D. Murphy, B. Bélier, S. Banfi, Alessandro Paiella, P. de Bernardis, S. Vanneste, Andrew May, M. De Petris, G. Barbarán, Giampaolo Pisano, Francesco Cavaliere, Cristian Franceschet, D. T. Hoang, Matthieu Tristram, D. Burke, F. Incardona, F. Suarez, J. A. Murphy, C. Kristukat, Marcin Gradziel, F. Couchot, Bruce Rafael Mellado Garcia, A. Mennella, Alessandro Coppolecchia, M. M. Gamboa Lerena, Andrei Korotkov, A. Fasciszewski, D. Bennett, Damien Rambaud, M. González, Bruno Maffei, F. Wicek, Mark McCulloch, S. Marnieros, O. Perdereau, Maria Salatino, D. Auguste, J.-Ch. Hamilton, C. Perbost, C. Scóccola, Carole Tucker, Federico Pezzotta, M. Piat, E. Jules, Lucio Piccirillo, Thibaut Louis, Sophie Henrot-Versille, Simon J. Melhuish, A. Baù, J.-Ph. Bernard, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre de Nanosciences et de Nanotechnologies [Orsay] (C2N), Université Paris-Sud - Paris 11 (UP11)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Zmuidzinas, Jonas, Gao, Jian-Rong, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Zmuidzinas, J, Gao, JR, Zullo, A, Wicek, F, Watson, B, Voisin, F, Vittorio, N, Viganò, D, Vanneste, S, Tucker, G, Tucker, C, Truongcanh, V, Tristram, M, Torchinsky, S, Timbie, P, Thermeau, J, Tartari, A, Suarez, F, Stolpovskiy, M, Spinelli, S, Scóccola, C, Schillaci, A, Salatino, M, Romero, G, Ringegni, P, Rambaud, D, Puddu, R, Prêle, D, Polenta, G, Pisano, G, Piccirillo, L, Piat, M, Piacentini, F, Pezzotta, F, Perdereau, O, Perbost, C, Pelosi, A, Pastoriza, H, Passerini, A, Pajot, F, Paiella, A, Olivieri, E, Murphy, J, Mundo, L, Montier, L, Melhuish, S, Medina, M, Mele, L, Mcculloch, M, May, A, Mattei, A, Masi, S, Marnieros, S, Maffei, B, Luterstein, R, Lukovic, V, Lowitz, A, Louis, T, Loucatos, S, Lamagna, L, Kristukat, C, Korotkov, A, Kaplan, J, Jules, E, Incardona, F, Hoang, D, Henrot-Versillé, S, Haynes, V, Harari, D, Grandsire, L, Gradziel, M, González, M, Gómez Berisso, M, Giraud-Héraud, Y, Giard, M, Gervasi, M, Gault, A, Gaspard, M, Garrido, X, García, B, Gamboa Lerena, M, Franceschet, C, Fasciszewski, A, Etchegoyen, A, Dumoulin, L, Di Donato, A, de Gasperis, G, de Bernardis, P, D’Alessandro, G, D'Agostino, R, Couchot, F, Coppolecchia, A, Coppi, G, Columbro, F, Charlassier, R, Chapron, C, Chanial, P, Cavaliere, F, Buzzelli, A, Buzi, D, Bunn, E, Bréelle, E, Bordier, G, Bonis, J, Bonaparte, J, Bleurvacq, N, Bigot-Sazy, M, Bersanelli, M, Bernard, J, Bergé, L, Bennett, D, Bélier, B, Baù, A, Battistelli, E, Battaglia, P, Barbarán, G, Banfi, S, Aumont, J, Auguste, D, Amico, G, Ade, P, Hamilton, J, Zannoni, M, Mennella, A, De Leo, M, De Petris, M, Scully, S, Guerrard, E, Gayer, D, Burke, D, and O'Sullivan, C
Subjects: cosmological model, higher-order, QUBIC, Cosmic microwave background, CMB, Interference (wave propagation), 01 natural sciences, 7. Clean energy, Cosmology, B-mode: primordial, law.invention, law, B-modes, Anisotropy, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, Applied Mathematics, Astrophysics::Instrumentation and Methods for Astrophysics, Computer Science Applications1707 Computer Vision and Pattern Recognition, bolometric interferometry, Condensed Matter Physics, Physical optics, physical optics, Interferometry, Horn antenna, detector: performance, polarization: anisotropy, Astrophysics::High Energy Astrophysical Phenomena, interferometer, interference, Astrophysics::Cosmology and Extragalactic Astrophysics, model: optical, programming, 010309 optics, FIS/05 - ASTRONOMIA E ASTROFISICA, Optics, 0103 physical sciences, Electronic, Optical and Magnetic Materials, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Electrical and Electronic Engineering, Astrophysics::Galaxy Astrophysics, Millimeter, Submillimeter, Far-Infrared, Detectors, Instrumentation, Cosmic Microwave Background, Polarization, business.industry, Bolometer, gravitational radiation: primordial, optics, detector: sensitivity, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Electronic, Optical and Magnetic Materials, cosmic background radiation: anisotropy
Abstract: QUBIC, the Q & U Bolometric Interferometer for Cosmology, is a novel ground-based instrument that aims to measure the extremely faint B-mode polarisation anisotropy of the cosmic microwave background at intermediate angular scales (multipoles of = 30 − 200). Primordial B-modes are a key prediction of Inflation as they can only be produced by gravitational waves in the very early universe. To achieve this goal, QUBIC will use bolometric interferometry, a technique that combines the sensitivity of an imager with the immunity to systematic effects of an interferometer. It will directly observe the sky through an array of back-to-back entry horns whose beams will be superimposed using a cooled quasioptical beam combiner. Images of the resulting interference fringes will be formed on two focal planes, each tiled with transition-edge sensors, cooled down to 320 mK. A dichroic filter placed between the optical combiner and the focal planes will select two frequency bands (centred at 150 GHz and 220 GHz), one frequency per focal plane. Polarization modulation will be achieved using a cold stepped half-wave plate (HWP) and polariser in front of the sky-facing horns. The full QUBIC instrument is described elsewhere1,2,3,4; in this paper we will concentrate in particular on simulations of the optical combiner (an off-axis Gregorian imager) and the feedhorn array. We model the optical performance of both the QUBIC full module and a scaled-down technological demonstrator which will be used to validate the full instrument design. Optical modelling is carried out using full vector physical optics with a combination of commercial and in-house software. In the high-frequency channel we must be careful to consider the higher-order modes that can be transmitted by the horn array. The instrument window function is used as a measure of performance and we investigate the effect of, for example, alignment and manufacturing tolerances, truncation by optical components and off-axis aberrations. We also report on laboratory tests carried on the QUBIC technological demonstrator in advance of deployment to the observing site in Argentina.
Published: 2018

29. 2017 upgrade and performance of BICEP3: a 95GHz refracting telescope for degree-scale CMB polarization

Author: Jae Hwan Kang, Cheng Zhang, Ki Won Yoon, Hung-I Yang, Wai Ling K. Wu, Chin Lin Wong, Justin Willmert, Don Wiebe, Alexis C. Weber, Albert Wandui, Abigail G. Vieregg, Caterina Umiltà, Anthony D. Turner, Carole Tucker, James E. Tolan, Keith L. Thompson, Grant P. Teply, Rashmi Sudiwala, Bryan Steinbach, Zachary K. Staniszewski, Tyler St Germaine, Ahmed Soliman, Chris D. Sheehy, Robert Schwarz, Alessandro Schillaci, Steffen Richter, Benjamin Racine, Clement Pryke, Stephen Palladino, R. W. Ogburn IV, Roger O'brient, Hien T. Nguyen, C. B. Netterfield, Toshiya Namikawa, Lorenzo Moncelsi, Koko G. Megerian, Martin Lueker, Erik M. Leitch, King Lau, Nicole Larsen, Chao-Lin Kuo, John M. Kovac, Sarah A. Kernasovskiy, Sinan Kefeli, Brian G. Keating, Jonathan Kaufman, Ethan Karpel, Kirit S. Karkare, Kent D. Irwin, Howard Hui, Gene C. Hilton, Sergi Hildebrandt, Sam A. Harrison, Mark Halpern, Grantland Hall, James A. Grayson, Stefan Fliescher, Jeff P. Filippini, Cora Dvorkin, Lionel Duband, Marion Dierickx, Michael Crumrine, Brendan Crill, James Cornelison, Jake Conners, Victor Buza, Eric Bullock, Immanuel Buder, Justus A. Brevik, Rachel Bowens-Rubin, Hans Boenish, James J. Bock, Colin A. Bischoff, Steve J. Benton, Denis Barkats, Kate D. Alexander, Randol Aikin, Zeeshan Ahmed, Peter A. Ade, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Zmuidzinas, Jonas, and Gao, Jian-Rong
Subjects: noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), detector: performance, Cosmic microwave background, FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, BICEP3, law.invention, cosmic background radiation: B-mode, Optics, bolometer, law, Polarization, 0103 physical sciences, Cosmic Microwave Background, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Physics::Atmospheric and Oceanic Physics, Physics, Gravitational Waves, Gravitational wave, business.industry, beam: width, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation: primordial, Polarization (waves), detector: upgrade, Inflation, optics, Cardinal point, Upgrade, Refracting telescope, Keck Array, Transition edge sensor, Astrophysics - Instrumentation and Methods for Astrophysics, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: BICEP3 is a 520mm aperture on-axis refracting telescope observing the polarization of the cosmic microwave background (CMB) at 95GHz in search of the B-mode signal originating from inflationary gravitational waves. BICEP3's focal plane is populated with modularized tiles of antenna-coupled transition edge sensor (TES) bolometers. BICEP3 was deployed to the South Pole during 2014-15 austral summer and has been operational since. During the 2016-17 austral summer, we implemented changes to optical elements that lead to better noise performance. We discuss this upgrade and show the performance of BICEP3 at its full mapping speed from the 2017 and 2018 observing seasons. BICEP3 achieves an order-of-magnitude improvement in mapping speed compared to a Keck 95GHz receiver. We demonstrate $6.6\mu K\sqrt{s}$ noise performance of the BICEP3 receiver., Comment: 12 pages, 9 figures, Published in Proc. SPIE. Presented at SPIE Astronomical Telescopes and Instrumentation Conference 10708: Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XI, June 2018
Published: 2018

30. Multi-peaked signatures of primordial gravitational waves from multi-step electroweak phase transition

Author: António P. Morais, Roman Pasechnik, Thibault Vieu, Université Paris-Saclay, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: High Energy Physics - Theory, Phase transition, cosmological model, media_common.quotation_subject, interferometer, FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), baryogenesis, General Relativity and Quantum Cosmology, Standard Model, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [ PHYS.HTHE ] Physics [physics]/High Energy Physics - Theory [hep-th], High Energy Physics - Phenomenology (hep-ph), Astronomical interferometer, general relativity, electroweak interaction: critical phenomena, media_common, Physics, Gravitational wave, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], bubble, Electroweak interaction, formation, gravitational radiation: primordial, Universe, High Energy Physics - Phenomenology, High Energy Physics - Theory (hep-th), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], signature
Abstract: The first-order electroweak phase transition in the early universe could occur in multiple steps leading to specific multi-peaked signatures in the primordial gravitational wave (GW) spectrum. We argue that these signatures are generic phenomena in multi-scalar extensions of the Standard Model. In a simple example of such an extension, we have studied the emergence of reoccurring and nested vacuum bubble configurations and their role in the formation of multiple peaks in the GW spectrum. The conditions for potential detectability of these features by the forthcoming generation of interferometers have been studied., 7 pages, 3 captioned figures, 1 table; numerical analysis extended, conclusions unchanged; contributed talk by R. Pasechnik at the EPS-HEP2019, 10-17 July, 2019, Ghent, Belgium
Published: 2018

31. Exploring cosmic origins with CORE: Gravitational lensing of the CMB

Author: Challinor , Anthony, Allison , Rupert, Carron , Julien, Errard , Josquin, Feeney , Stephen, Kitching , Thomas, Lesgourgues , Julien, Lewis , Antony, Zubeldía , Íñigo, Achucarro , Ana, Ade , Peter, Ashdown , Mark, Ballardini , Mario, Banday , A.J., Banerji , Ranajoy, Bartlett , James, Bartolo , Nicola, Basak , Soumen, Baumann , Daniel, Bersanelli , Marco, Bonaldi , Anna, Bonato , Matteo, Borrill , Julian, Bouchet , François, Boulanger , François, Brinckmann , Thejs, Bucher , Martin, Burigana , Carlo, Buzzelli , Alessandro, Cai , Zhen-Yi, Calvo , Martino, Carvalho , Carla-Sofia, Castellano , Gabriella, Chluba , Jens, Clesse , Sebastien, Colantoni , Ivan, Coppolecchia , Alessandro, Crook , Martin, D'Alessandro , Giuseppe, De Bernardis , Paolo, De Gasperis , Giancarlo, De Zotti , Gianfranco, Delabrouille , Jacques, Di Valentino , Eleonora, Diego , Jose-Maria, Fernandez-Cobos , Raul, Ferraro , Simone, Finelli , Fabio, Forastieri , Francesco, Galli , Silvia, Genova-Santos , Ricardo, Gerbino , Martina, González-Nuevo , Joaquin, Grandis , Sebastian, Greenslade , Joshua, Hagstotz , Steffen, Hanany , Shaul, Handley , Will, Hernandez-Monteagudo , Carlos, Hervías-Caimapo , Carlos, Hills , Matthew, Luzzi , Gemma, Maffei , Bruno, Martinez-González , Enrique, Martins , C.J.A.P., Masi , Silvia, McCarthy , Darragh, Melchiorri , Alessandro, Melin , Jean-Baptiste, Molinari , Diego, Monfardini , Alessandro, Natoli , Paolo, Negrello , Mattia, Notari , Alessio, Paiella , Alessandro, Paoletti , Daniela, Patanchon , Guillaume, Piat , Michel, Pisano , Giampaolo, Polastri , Linda, Polenta , Gianluca, Pollo , Agnieszka, Poulin , Vivian, Quartin , Miguel, Remazeilles , Mathieu, Roman , Matthieu, Rubino-Martin , Jose-Alberto, Salvati , Laura, Tartari , Andrea, Tomasi , Maurizio, Tramonte , Denis, Trappe , Neil, Trombetti , Tiziana, Tucker , Carole, Valiviita , Jussi, Van De Weijgaert , Rien, Van Tent , Bartjan, Vennin , Vincent, Vielva , Patricio, Vittorio , Nicola, Young , Karl, Zannoni , Mario, Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut Lagrange de Paris, Sorbonne Universités, AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut Néel ( NEEL ), Université Grenoble Alpes [Saint Martin d'Hères]-Centre National de la Recherche Scientifique ( CNRS ), Département de Physique des Particules (ex SPP) ( DPP ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Laboratoire d'Annecy-le-Vieux de Physique Théorique ( LAPTH ), Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Théorique d'Orsay [Orsay] ( LPT ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), and CORE
Subjects: noise, deflection, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], B-mode: lens, gravitational radiation: primordial, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, redshift, calibration, estimator, gravitation: lens, non-Gaussianity, galaxy: cluster, neutrino: oscillation, neutrino: mass, gravitational radiation: power spectrum, halo: mass
Abstract: International audience; Lensing of the cosmic microwave background (CMB) is now a well-developed probe of the clustering of the large-scale mass distribution over a broad range of redshifts. By exploiting the non-Gaussian imprints of lensing in the polarization of the CMB, the CORE mission will allow production of a clean map of the lensing deflections over nearly the full-sky. The number of high-S/N modes in this map will exceed current CMB lensing maps by a factor of 40, and the measurement will be sample-variance limited on all scales where linear theory is valid. Here, we summarise this mission product and discuss the science that will follow from its power spectrum and the cross-correlation with other clustering data. For example, the summed mass of neutrinos will be determined to an accuracy of 17 meV combining CORE lensing and CMB two-point information with contemporaneous measurements of the baryon acoustic oscillation feature in the clustering of galaxies, three times smaller than the minimum total mass allowed by neutrino oscillation measurements. Lensing has applications across many other science goals of CORE, including the search for B-mode polarization from primordial gravitational waves. Here, lens-induced B-modes will dominate over instrument noise, limiting constraints on the power spectrum amplitude of primordial gravitational waves. With lensing reconstructed by CORE, one can "delens" the observed polarization internally, reducing the lensing B-mode power by 60 %. This can be improved to 70 % by combining lensing and measurements of the cosmic infrared background from CORE, leading to an improvement of a factor of 2.5 in the error on the amplitude of primordial gravitational waves compared to no delensing (in the null hypothesis of no primordial B-modes). Lensing measurements from CORE will allow calibration of the halo masses of the tens of thousands of galaxy clusters that it will find, with constraints dominated by the clean polarization-based estimators. The 19 frequency channels proposed for CORE will allow accurate removal of Galactic emission from CMB maps. We present initial findings that show that residual Galactic foreground contamination will not be a significant source of bias for lensing power spectrum measurements with CORE.
Published: 2018

32. The Impact of Primordial Magnetic Fields on Future CMB Bounds on Inflationary Gravitational Waves

Author: Fabrizio Renzi, Luca Pagano, Giovanni Cabass, Eleonora Di Valentino, Alessandro Melchiorri, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique ( LERMA ), École normale supérieure - Paris ( ENS Paris ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Cergy Pontoise ( UCP ), and Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique ( CNRS )
Subjects: gravitational radiation: polarization, Particle physics, cosmological model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, expansion: multipole, Spectral line, NO, statistical analysis, 0103 physical sciences, CMBR experiments, inflation, Anisotropy, cosmological parameters from CMBR, gravitational waves and CMBR polarization, Astronomy and Astrophysics, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: primordial, magnetic field: primordial, Polarization (waves), Magnetic field, Amplitude, Pixie, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We discuss whether an unaccounted contribution to the Cosmic Microwave Background polarization $B$-mode by primordial magnetic fields (PMFs) can bias future constraints on inflationary gravitational waves. As a case-study, we consider a scale-invariant PMF spectrum with amplitude of $\approx{1}\,{\mathrm{nG}}$ on $1\,\mathrm{Mpc}$ scales, compatible with current cosmological bounds. We find a degeneracy in the $B$-mode spectra between PMFs and inflationary gravitational waves. If PMFs of this amplitude are not accounted for, future CMB experiments could claim a false detection of a tensor-to-scalar ratio $r\approx 0.007$, close to the predictions of Starobinsky and $\alpha$-attractor models. The degeneracy can be broken if $B$-modes are measured also at multipoles $\ell\gtrsim 900$: more precisely experiments like CMB-S4 or CORE-M5 would be able to discriminate PMFs from primordial GWs at high statistical significance. Experiments like LiteBIRD or PIXIE will not be able to break the degeneracy and will need complementary bounds coming, for example, from measurements of anisotropies in the Faraday rotation angle of CMB polarization. This reinforces the importance of future experimental constraints on PMFs., Comment: 16 pages, 8 figures, matches JCAP version
Published: 2018

33. BICEP2 / Keck Array x: Constraints on Primordial Gravitational Waves using Planck, WMAP, and New BICEP2/Keck Observations through the 2015 Season

Author: Array, Keck, Collaborations, BICEP2, Ade, P. A. R., Ahmed, Z., Aikin, R. W., Alexander, K. D., Barkats, D., Benton, S. J., Bischoff, C. A., Bock, J. J., Bowens-Rubin, R., Brevik, J. A., Buder, I., Bullock, E., Buza, V., Connors, J., Cornelison, J., Crill, B. P., Crumrine, M., Dierickx, M., Duband, L., Dvorkin, C., Filippini, J. P., Fliescher, S., Grayson, J., Hall, G., Halpern, M., Harrison, S., Hildebrandt, S. R., Hilton, G. C., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Karpel, E., Kaufman, J. P., Keating, B. G., Kefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kuo, C. L., Larsen, N. A., Lau, K., Leitch, E. M., Lueker, M., Megerian, K. G., Moncelsi, L., Namikawa, T., Netterfield, C. B., Nguyen, H. T., O'Brient, R., Ogburn, R. W., Palladino, S., Pryke, C., Racine, B., Richter, S., Schillaci, A., Schwarz, R., Sheehy, C. D., Soliman, A., Germaine, T. St., Staniszewski, Z. K., Steinbach, B., Sudiwala, R. V., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C., Turner, A. D., Umilta, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wong, C. L., Wu, W. L. K., Yang, H., Yoon, K. W., Zhang, C., Institut Nanosciences et Cryogénie (INAC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), BICEP2, Keck Array, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), and Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)
Subjects: data analysis method, noise, cosmological model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation: primordial, FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, BICEP, statistical analysis, gravitation: lens, WMAP, synchrotron, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present results from an analysis of all data taken by the BICEP2/Keck CMB polarization experiments up to and including the 2015 observing season. This includes the first Keck Array observations at 220 GHz and additional observations at 95 & 150 GHz. The $Q/U$ maps reach depths of 5.2, 2.9 and 26 $\mu$K$_{cmb}$ arcmin at 95, 150 and 220 GHz respectively over an effective area of $\approx 400$ square degrees. The 220 GHz maps achieve a signal-to-noise on polarized dust emission approximately equal to that of Planck at 353 GHz. We take auto- and cross-spectra between these maps and publicly available WMAP and Planck maps at frequencies from 23 to 353 GHz. We evaluate the joint likelihood of the spectra versus a multicomponent model of lensed-$\Lambda$CDM+$r$+dust+synchrotron+noise. The foreground model has seven parameters, and we impose priors on some of these using external information from Planck and WMAP derived from larger regions of sky. The model is shown to be an adequate description of the data at the current noise levels. The likelihood analysis yields the constraint $r_{0.05}, Comment: 23 pages, 23 figures, as accepted by PRL, data and figures available for download at http://bicepkeck.org/
Published: 2018

34. Does the detection of primordial gravitational waves exclude low energy inflation?

Author: Tomohiro Fujita, Ryo Namba, Yuichiro Tada, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, Sorbonne Universités, Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), and Sorbonne Université (SU)
Subjects: High Energy Physics - Theory, Nuclear and High Energy Physics, Particle physics, scale: inflation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], nucleosynthesis: big bang, Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), cosmic background radiation, 01 natural sciences, General Relativity and Quantum Cosmology, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [ PHYS.HTHE ] Physics [physics]/High Energy Physics - Theory [hep-th], High Energy Physics - Phenomenology (hep-ph), fluctuation: quantum, 0103 physical sciences, axion: coupling, 010306 general physics, Axion, Quantum fluctuation, energy: low, Inflation (cosmology), Physics, graviton: fluctuation, 010308 nuclear & particles physics, Gravitational wave, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], Graviton, gravitational radiation: primordial, back reaction, lcsh:QC1-999, High Energy Physics - Phenomenology, High Energy Physics - Theory (hep-th), SU(2), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], gauge field theory, curvature: perturbation, gravitation: fluctuation, Back-reaction, [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], lcsh:Physics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We show that a detectable tensor-to-scalar ratio $(r\ge 10^{-3})$ on the CMB scale can be generated even during extremely low energy inflation which saturates the BBN bound $\rho_{\rm inf}\approx (30 {\rm MeV})^4$. The source of the gravitational waves is not quantum fluctuations of graviton but those of $SU(2)$ gauge fields, energetically supported by coupled axion fields. The curvature perturbation, the backreaction effect and the validity of perturbative treatment are carefully checked. Our result indicates that measuring $r$ alone does not immediately fix the inflationary energy scale., Comment: 6 pages, 3 figures
Published: 2018

35. Exploring cosmic origins with CORE: Gravitational lensing of the CMB

Author: A. Challinor, R. Allison, J. Carron, J. Errard, S. Feeney, T. Kitching, J. Lesgourgues, A. Lewis, Í. Zubeldía, A. Achucarro, P. Ade, M. Ashdown, M. Ballardini, A.J. Banday, R. Banerji, J. Bartlett, N. Bartolo, S. Basak, D. Baumann, M. Bersanelli, A. Bonaldi, M. Bonato, J. Borrill, F. Bouchet, F. Boulanger, T. Brinckmann, M. Bucher, C. Burigana, A. Buzzelli, Z.-Y. Cai, M. Calvo, C.-S. Carvalho, G. Castellano, J. Chluba, S. Clesse, I. Colantoni, A. Coppolecchia, M. Crook, G. d'Alessandro, P. de Bernardis, G. de Gasperis, G. De Zotti, J. Delabrouille, E. Di Valentino, J.-M. Diego, R. Fernandez-Cobos, S. Ferraro, F. Finelli, F. Forastieri, S. Galli, R. Genova-Santos, M. Gerbino, J. González-Nuevo, S. Grandis, J. Greenslade, S. Hagstotz, S. Hanany, W. Handley, C. Hernandez-Monteagudo, C. Hervías-Caimapo, M. Hills, E. Hivon, K. Kiiveri, T. Kisner, M. Kunz, H. Kurki-Suonio, L. Lamagna, A. Lasenby, M. Lattanzi, M. Liguori, V. Lindholm, M. López-Caniego, G. Luzzi, B. Maffei, E. Martinez-González, C.J.A.P. Martins, S. Masi, S. Matarrese, D. McCarthy, A. Melchiorri, J.-B. Melin, D. Molinari, A. Monfardini, P. Natoli, M. Negrello, A. Notari, A. Paiella, D. Paoletti, G. Patanchon, M. Piat, G. Pisano, L. Polastri, G. Polenta, A. Pollo, V. Poulin, M. Quartin, M. Remazeilles, M. Roman, J.-A. Rubino-Martin, L. Salvati, A. Tartari, M. Tomasi, D. Tramonte, N. Trappe, T. Trombetti, C. Tucker, J. Valiviita, R. Van de Weijgaert, B. van Tent, V. Vennin, P. Vielva, N. Vittorio, K. Young, M. Zannoni, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, Sorbonne Universités, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), CORE, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Sorbonne Université (SU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Challinor, A, Allison, R, Carron, J, Errard, J, Feeney, S, Kitching, T, Lesgourgues, J, Lewis, A, Zubeldía, Í, Achucarro, A, Ade, P, Ashdown, M, Ballardini, M, Banday, A, Banerji, R, Bartlett, J, Bartolo, N, Basak, S, Baumann, D, Bersanelli, M, Bonaldi, A, Bonato, M, Borrill, J, Bouchet, F, Boulanger, F, Brinckmann, T, Bucher, M, Burigana, C, Buzzelli, A, Cai, Z, Calvo, M, Carvalho, C, Castellano, G, Chluba, J, Clesse, S, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, de Bernardis, P, de Gasperis, G, Zotti, G, Delabrouille, J, Valentino, E, Diego, J, Fernandez-Cobos, R, Ferraro, S, Finelli, F, Forastieri, F, Galli, S, Genova-Santos, R, Gerbino, M, González-Nuevo, J, Grandis, S, Greenslade, J, Hagstotz, S, Hanany, S, Handley, W, Hernandez-Monteagudo, C, Hervías-Caimapo, C, Hills, M, Hivon, E, Kiiveri, K, Kisner, T, Kunz, M, Kurki-Suonio, H, Lamagna, L, Lasenby, A, Lattanzi, M, Liguori, M, Lindholm, V, López-Caniego, M, Luzzi, G, Maffei, B, Martinez-González, E, Martins, C, Masi, S, Matarrese, S, Mccarthy, D, Melchiorri, A, Melin, J, Molinari, D, Monfardini, A, Natoli, P, Negrello, M, Notari, A, Paiella, A, Paoletti, D, Patanchon, G, Piat, M, Pisano, G, Polastri, L, Polenta, G, Pollo, A, Poulin, V, Quartin, M, Remazeilles, M, Roman, M, Rubino-Martin, J, Salvati, L, Tartari, A, Tomasi, M, Tramonte, D, Trappe, N, Trombetti, T, Tucker, C, Valiviita, J, de Weijgaert, R, Tent, B, Vennin, V, Vielva, P, Vittorio, N, Young, K, Zannoni, M, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Helsinki Institute of Physics, Department of Physics, String Theory (ITFA, IoP, FNWI), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Cryogénie (NEEL - Cryo), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Département de Physique des Particules (ex SPP) (DPhP), and Hélium : du fondamental aux applications (NEEL - HELFA)
Subjects: deflection, Cosmic microwave background, cosmic background radiation: polarization, astro-ph.CO, Astrophysics, ST/N000927/1, ST/L000652/1, 7. Clean energy, 01 natural sciences, CMBR polarisation, gravitational lensing, inflation, neutrino masses from cosmology, ART. NO. 023003, estimator, neutrino: mass, 010303 astronomy & astrophysics, Physics, FLUCTUATIONS, GRAVITY-WAVES, Amplitude, non-Gaussianity, galaxy: cluster, Halo, gravitational radiation: power spectrum, Neutrino, CMBR polarization, gravitational lensing, ination, neutrino masses from cosmology, Astronomy and Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, CMBR polarisation, noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), B-mode: lens, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, MASS, NO, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, 0103 physical sciences, ddc:530, RECONSTRUCTION, inflation, Galaxy cluster, STFC, halo: mass, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: primordial, RCUK, 115 Astronomy, Space science, redshift, calibration, Redshift, Gravitational lens, CROSS-CORRELATION, RADIATION, neutrino: oscillation, GALAXY CLUSTERS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], MICROWAVE BACKGROUND POLARIZATION, MATTER
Abstract: Lensing of the CMB is now a well-developed probe of large-scale clustering over a broad range of redshifts. By exploiting the non-Gaussian imprints of lensing in the polarization of the CMB, the CORE mission can produce a clean map of the lensing deflections over nearly the full-sky. The number of high-S/N modes in this map will exceed current CMB lensing maps by a factor of 40, and the measurement will be sample-variance limited on all scales where linear theory is valid. Here, we summarise this mission product and discuss the science that it will enable. For example, the summed mass of neutrinos will be determined to an accuracy of 17 meV combining CORE lensing and CMB two-point information with contemporaneous BAO measurements, three times smaller than the minimum total mass allowed by neutrino oscillations. In the search for B-mode polarization from primordial gravitational waves with CORE, lens-induced B-modes will dominate over instrument noise, limiting constraints on the gravitational wave power spectrum amplitude. With lensing reconstructed by CORE, one can "delens" the observed polarization internally, reducing the lensing B-mode power by 60%. This improves to 70% by combining lensing and CIB measurements from CORE, reducing the error on the gravitational wave amplitude by 2.5 compared to no delensing (in the null hypothesis). Lensing measurements from CORE will allow calibration of the halo masses of the 40000 galaxy clusters that it will find, with constraints dominated by the clean polarization-based estimators. CORE can accurately remove Galactic emission from CMB maps with its 19 frequency channels. We present initial findings that show that residual Galactic foreground contamination will not be a significant source of bias for lensing power spectrum measurements with CORE. [abridged], 44 pages, 12 figures
Published: 2018

36. QUBIC - the Q&U Bolometric Interferometer for Cosmology: A novel way to look at the polarized Cosmic Microwave Background

Author: M. Piat, A. Passerini, M. W. Ng, J. Rodriguez Martino, A. Ghribi, Alessandro Buzzelli, M. Giard, N. Bleurvacq, F. Piacentini, S. Melhuish, L. Mele, P. Chanial, J.-Ch. Hamilton, Maria Salatino, R. Puddu, L. Grandsire, J. Lande, Peter T. Timbie, Jonathan Aumont, Carole Tucker, B. Watson, Bruno Maffei, Andrei Korotkov, Damien Rambaud, A. Zullo, O. Rigaut, C. Perbost, Massimo Gervasi, Mark McCulloch, S. Marnieros, A. Baù, A. Lowitz, Giampaolo Pisano, D. Néel, G. Bordier, M. De Petris, P. Battaglia, N. Krachmalnicoff, L. Montier, A. Mennella, D. Cammilleri, O. Perdereau, Michele De Leo, Créidhe O'Sullivan, Cristian Franceschet, F. Incardona, D. Bennett, Peter A. R. Ade, D. Buzi, Victor Haynes, F. Couchot, F. Suarez, G. S. Tucker, N. Vittori, M. Tristram, D. Harari, Lucio Piccirillo, B. Bélier, Jean Kaplan, Sophie Henrot-Versille, S. Loucatos, Luca Lamagna, L. Dumoulin, Alessandro Paiella, Bruce Rafael Mellado Garcia, Alessandro Coppolecchia, F. Columbro, A. Tartari, D. Viganò, J. Brossard, Rocco D'Agostino, Andrew May, F. Pajot, Elia S. Battistelli, D. Gayer, L. Bergé, Silvia Masi, D. Burke, Marcin Gradziel, N. Holtzer, Gabriele Coppi, Steve Torchinsky, Giuseppe D'Alessandro, M. C. Medina, C. Chapron, A. Etchegoyen, Marco Bersanelli, Mario Zannoni, A. Pelosi, S. Scully, G. de Gasperis, Bigot-Sazy, J.-Ph. Bernard, A. Gault, S. Banfi, Vladimir V. Luković, Francesco Cavaliere, E. Bunn, D. Prêle, A. Murphy, F. Voisin, M. Stolpovskiy, Gustavo E. Romero, F. Del Torto, Y. Giraud-Héraud, P. de Bernardis, A. Schillaci, T. Decourcelle, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Mennella, A, Ade, P, Aumont, J, Banfi, S, Incardona, F, Battaglia, P, Battistelli, E, Baù, A, Bélier, B, Bennett, D, Bergé, L, Bernard, J, Bersanelli, M, Bigot-Sazy, M, Bleurvacq, N, Bordier, G, Brossard, J, Bunn, E, Burke, D, Buzi, D, Buzzelli, A, Cammilleri, D, Cavaliere, F, Chanial, P, Chapron, C, Columbro, F, Coppi, G, Coppolecchia, A, Couchot, F, D'Agostino, R, D'Alessandro, G, De Bernardis, P, De Gasperis, G, De Leo, M, De Petris, M, Decourcelle, T, Del Torto, F, Dumoulin, L, Etchegoyen, A, Franceschet, C, Garcia, B, Gault, A, Gayer, D, Gervasi, M, Ghribi, A, Giard, M, Giraud-Héraud, Y, Gradziel, M, Grandsire, L, Hamilton, J, Harari, D, Haynes, V, Henrot-Versillé, S, Holtzer, N, Kaplan, J, Korotkov, A, Krachmalnicoff, N, Lamagna, L, Lande, J, Loucatos, S, Lowitz, A, Lukovic, V, Maffei, B, Marnieros, S, Martino, J, Masi, S, May, A, Mcculloch, M, Medina, M, Mele, L, Melhuish, S, Montier, L, Murphy, A, Néel, D, Ng, M, O'Sullivan, C, Paiella, A, Pajot, F, Passerini, A, Pelosi, A, Perbost, C, Perdereau, O, Piacentini, F, Piat, M, Piccirillo, L, Pisano, G, Prêle, D, Puddu, R, Rambaud, D, Rigaut, O, Romero, G, Salatino, M, Schillaci, A, Scully, S, Stolpovskiy, M, Suarez, F, Tartari, A, Timbie, P, Torchinsky, S, Tristram, M, Tucker, C, Tucker, G, Viganò, D, Vittori, N, Voisin, F, Watson, B, Zannoni, M, and Zullo, A
Subjects: cosmological model, interferometer, Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, 02 engineering and technology, cosmic background radiation, 01 natural sciences, 7. Clean energy, Cosmology, law.invention, 010309 optics, FIS/05 - ASTRONOMIA E ASTROFISICA, bolometer, law, 0103 physical sciences, Astronomical interferometer, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Physics, polarization, Gravitational wave, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation: primordial, Cosmic Microwave Background, Polarimetry, Interferometry, Bolometers, Astronomy, 021001 nanoscience & nanotechnology, Polarization (waves), sensitivity, calibration, Interferometry, duality, 0210 nano-technology, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: In this paper we describe QUBIC, an experiment that takes up the challenge posed by the detection of primordial gravitational waves with a novel approach, that combines the sensitivity of state-of-the art bolometric detectors with the systematic effects control typical of interferometers. The so-called "self-calibration" is a technique deeply rooted in the interferometric nature of the instrument and allows us to clean the measured data from instrumental effects. The first module of QUBIC is a dual band instrument (150 GHz and 220 GHz) that will be deployed in Argentina during the Fall 2018., Presented at the EPS Conference on High Energy Physics, Venice (Italy), 5-12 July 2017 Accepted for publication in conference proceedings
Published: 2017

37. Gaugid inflation

Author: David Pirtskhalava, Federico Piazza, Riccardo Rattazzi, Olivier Simon, Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 7332 ( CPT ), and Aix Marseille Université ( AMU ) -Université de Toulon ( UTLN ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: High Energy Physics - Theory, gauge field theory: abelian, scale: inflation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), triplet, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], fluctuation: spectrum, Scalar (mathematics), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, spectrum: tensor, 01 natural sciences, [ PHYS.HTHE ] Physics [physics]/High Energy Physics - Theory [hep-th], Theoretical physics, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), solids, 0103 physical sciences, density: finite, Effective field theory, Tensor, 010306 general physics, phonon, Physics, Inflation (cosmology), 010308 nuclear & particles physics, Gravitational wave, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], Graviton, gravitational radiation: primordial, Astronomy and Astrophysics, Observable, High Energy Physics - Phenomenology, perturbation: scalar, High Energy Physics - Theory (hep-th), gravitation, graviton, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Isotropic solid, nonlinear, [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The spectrum of primordial gravitational waves is one of the most robust inflationary observables, often thought of as a direct probe of the energy scale of inflation. We present a simple model, where the dynamics controlling this observable is very different than in the standard paradigm of inflation. The model is based on a peculiar finite density phase---the magnetic gaugid---which stems from a highly non-linear effective theory of a triplet of abelian gauge fields. The gaugid extends the notion of homogeneous isotropic solid, in that its spectrum of fluctuations includes helicity-2 phonons. We show how, upon implementing the gaugid to drive inflation, the helicity-2 phonon mixes with the graviton, significantly affecting the size of the primordial tensor spectrum. The rest of the features of the theory, in particular the vector and scalar perturbations, closely resemble those of solid inflation., Comment: 35+8 pages
Published: 2017

38. Excited cosmic strings with superconducting currents

Author: Florent Michel, Betti Hartmann, Patrick Peter, Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: High Energy Physics - Theory, Electromagnetic field, FOS: Physical sciences, Cosmic ray, General Relativity and Quantum Cosmology (gr-qc), curvature: scalar, 01 natural sciences, String (physics), General Relativity and Quantum Cosmology, High Energy Physics::Theory, High Energy Physics - Phenomenology (hep-ph), electromagnetic field, 0103 physical sciences, excited state, 010306 general physics, cosmic string: network, Physics, 010308 nuclear & particles physics, Gravitational wave, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], superconductivity, gravitational radiation: primordial, COSMOLOGIA, Symmetry (physics), Cosmic string, High Energy Physics - Phenomenology, Higgs field, condensation, High Energy Physics - Theory (hep-th), space-time, cosmic radiation, Excited state, Quantum electrodynamics, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], string, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Einstein equation
Abstract: We present a detailed analysis of {\it excited} cosmic string solutions which possess superconducting currents. These currents can be excited inside the string core, and - if the condensate is large enough - can lead to the excitations of the Higgs field. Next to the case with global unbroken symmetry, we discuss also the effects of the gauging of this symmetry and show that excited condensates persist when coupled to an electromagnetic field. The space-time of such strings is also constructed by solving the Einstein equations numerically and we show how the local scalar curvature is modified by the excitation. We consider the relevance of our results on the cosmic string network evolution as well as observations of primordial gravitational waves and cosmic rays., 20 pages; v2: matches version accepted for publication in Phys. Rev. D
Published: 2017

39. Cosmic Microwave Background Science at Commercial Airline Altitudes

Author: Licia Verde, Stephen M. Feeney, Jon E. Gudmundsson, Josquin Errard, Hiranya V. Peiris, Institut Lagrange de Paris, Sorbonne Universités, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), and Sorbonne Université (SU)
Subjects: Planck, Cosmology and Nongalactic Astrophysics (astro-ph.CO), air, media_common.quotation_subject, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, 7. Clean energy, 01 natural sciences, microwaves, symbols.namesake, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics::Galaxy Astrophysics, media_common, Physics, polarization, methods: statistical, hybrid, 010308 nuclear & particles physics, Gravitational wave, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation: primordial, Astronomy, Astronomy and Astrophysics, early Universe, Polarization (waves), Space and Planetary Science, Sky, symbols, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Microwave, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Obtaining high-sensitivity measurements of degree-scale cosmic microwave background (CMB) polarization is the most direct path to detecting primordial gravitational waves. Robustly recovering any primordial signal from the dominant foreground emission will require high-fidelity observations at multiple frequencies, with excellent control of systematics. We explore the potential for a new platform for CMB observations, the Airlander 10 hybrid air vehicle, to perform this task. We show that the Airlander 10 platform, operating at commercial airline altitudes, is well-suited to mapping frequencies above 220 GHz, which are critical for cleaning CMB maps of dust emission. Optimizing the distribution of detectors across frequencies, we forecast the ability of Airlander 10 to clean foregrounds of varying complexity as a function of altitude, demonstrating its complementarity with both existing (Planck) and ongoing (C-BASS) foreground observations. This novel platform could play a key role in defining our ultimate view of the polarized microwave sky., Comment: Six pages, four figures. v2: matches version published in MNRAS Letters
Published: 2017

40. Digging deeper: Observing primordial gravitational waves below the binary black hole produced stochastic background

Author: Bangalore Suryanarayana Sathyaprakash, Salvatore Vitale, E. Katsavounidis, Nelson Christensen, Tania Regimbau, Matthew Evans, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Observatoire de la Côte d'Azur ( OCA ), Centre National de la Recherche Scientifique ( CNRS ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), and Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), background: primordial, Astrophysics::High Energy Astrophysical Phenomena, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, General Physics and Astronomy, Primordial black hole, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Gravitational wave background, Einstein Telescope, Binary black hole, 0103 physical sciences, KAGRA, LIGO, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, 010308 nuclear & particles physics, Gravitational wave, 95.85.Sz, gravitational radiation: background, gravitational radiation: primordial, Astronomy, 04.25.dg, 04.80.Nn, background: stochastic, gravitational radiation detector, Black hole, black hole: binary, 97.80.-d, efficiency, gravitational radiation: emission, Stellar black hole, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hawking radiation, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The merger rate of black hole binaries inferred from the detections in the first Advanced LIGO science run, implies that a stochastic background produced by a cosmological population of mergers will likely mask the primordial gravitational-wave background. Here we demonstrate that the next generation of ground-based detectors, such as the Einstein Telescope and Cosmic Explorer, will be able to observe binary black hole mergers throughout the universe with sufficient efficiency that the confusion background can potentially be subtracted to observe the primordial background at the level of $\Omega_{\mathrm{GW}} \simeq 10^{-13}$ after five years of observation., Comment: accepted for publication in PRL (7 pages, 4 figures)
Published: 2017

41. Statistical simulations of the dust foreground to cosmic microwave background polarization

Author: L. Montier, Tuhin Ghosh, Jonathan Aumont, Benjamin D. Wandelt, F. Vansyngel, François Levrier, Francois Boulanger, Andrea Bracco, Peter G. Martin, Université Paris-Sud - Paris 11 (UP11), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Université Pierre et Marie Curie - Paris 6 ( UPMC ), Institut Lagrange de Paris, Sorbonne Universités, Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, CEA/DSM, Laboratoire de Physique Théorique de l'ENS ( LPTENS ), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris ( FRDPENS ), Centre National de la Recherche Scientifique ( CNRS ) -École normale supérieure - Paris ( ENS Paris ) -Centre National de la Recherche Scientifique ( CNRS ) -École normale supérieure - Paris ( ENS Paris ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Sorbonne Université (SU), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and École normale supérieure - Paris (ENS Paris)
Subjects: polarization: spectrum, satellite: Planck, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, Cosmic background radiation, cosmic background radiation: polarization, Astrophysics, magnetic field: galaxy, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, power spectrum, 01 natural sciences, cosmic background radiation: B-mode, symbols.namesake, statistical analysis, 0103 physical sciences, Planck, numerical calculations, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ISM: general, Physics, polarization, 010308 nuclear & particles physics, Gravitational wave, Computer Science::Information Retrieval, turbulence, gravitational radiation: primordial, Spectral density, Astronomy and Astrophysics, Galactic plane, Galaxy: ISM, Polarization (waves), Interstellar medium, cosmology: comic background radiation, Space and Planetary Science, covariance, symbols, submillimeter: ISM, dispersion, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmic background radiation: anisotropy
Abstract: The characterization of the dust polarization foreground to the cosmic microwave background (CMB) is a necessary step toward the detection of the B-mode signal associated with primordial gravitational waves. We present a method to simulate maps of polarized dust emission on the sphere that is similar to the approach used for CMB anisotropies. This method builds on the understanding of Galactic polarization stemming from the analysis of Planck data. It relates the dust polarization sky to the structure of the Galactic magnetic field and its coupling with interstellar matter and turbulence. The Galactic magnetic field is modeled as a superposition of a mean uniform field and a Gaussian random (turbulent) component with a power-law power spectrum of exponent αM. The integration along the line of sight carried out to compute Stokes maps is approximated by a sum over a small number of emitting layers with different realizations of the random component of the magnetic field. The model parameters are constrained to fit the power spectra of dust polarization EE, BB, and TE measured using Planck data. We find that the slopes of the E and B power spectra of dust polarization are matched for αM = −2.5, an exponent close to that measured for total dust intensity but larger than the Kolmogorov exponent − 11/3. The model allows us to compute multiple realizations of the Stokes Q and U maps for different realizations of the random component of the magnetic field, and to quantify the variance of dust polarization spectra for any given sky area outside of the Galactic plane. The simulations reproduce the scaling relation between the dust polarization power and the mean total dust intensity including the observed dispersion around the mean relation. We also propose a method to carry out multifrequency simulations, including the decorrelation measured recently by Planck, using a given covariance matrix of the polarization maps. These simulations are well suited to optimize component separation methods and to quantify the confidence with which the dust and CMB B-modes can be separated in present and future experiments. We also provide an astrophysical perspective on our phenomenological modeling of the dust polarization spectra.
Published: 2017

42. POLARBEAR-2: an instrument for CMB polarization measurements

Author: Y. Inoue, P. Ade, Y. Akiba, C. Aleman, K. Arnold, C. Baccigalupi, B. Barch, D. Barron, A. Bender, D. Boettger, J. Borrill, S. Chapman, Y. Chinone, A. Cukierman, T. de Haan, M. A. Dobbs, A. Ducout, R. Dünner, T. Elleflot, J. Errard, G. Fabbian, S. Feeney, C. Feng, G. Fuller, A. J. Gilbert, N. Goeckner-Wald, J. Groh, G. Hall, N. Halverson, T. Hamada, M. Hasegawa, K. Hattori, M. Hazumi, C. Hill, W. L. Holzapfel, Y. Hori, L. Howe, F. Irie, G. Jaehnig, A. Jaffe, O. Jeong, N. Katayama, J. P. Kaufman, K. Kazemzadeh, B. G. Keating, Z. Kermish, R. Keskitalo, T. S. Kisner, A. Kusaka, M. Le Jeune, A. T. Lee, D. Leon, E. V. Linder, L. Lowry, F. Matsuda, T. Matsumura, N. Miller, K. Mizukami, J. Montgomery, M. Navaroli, H. Nishino, H. Paar, J. Peloton, D. Poletti, G. Puglisi, C. R. Raum, G. M. Rebeiz, C. L. Reichardt, P. L. Richards, C. Ross, K. M. Rotermund, Y. Segawa, B. D. Sherwin, I. Shirley, P. Siritanasak, N. Stebor, R. Stompor, J. Suzuki, A. Suzuki, O. Tajima, S. Takada, S. Takatori, G. P. Teply, A. Tikhomirov, T. Tomaru, N. Whitehorn, A. Zahn, O. Zahn, Holland, Wayne S, Zmuidzinas, Jonas, Institut Lagrange de Paris, Sorbonne Université (SU), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), POLARBEAR, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Sorbonne Universités, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Inoue, Y, Ade, P, Akiba, Y, Aleman, C, Arnold, K, Baccigalupi, C, Barch, B, Barron, D, Bender, A, Boettger, D, Borrill, J, Chapman, S, Chinone, Y, Cukierman, A, De Haan, T, Dobbs, M, Ducout, A, Dunner, R, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fuller, G, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hattori, K, Hazumi, M, Hill, C, Holzapfel, W, Hori, Y, Howe, L, Irie, F, Jaehnig, G, Jaffe, A, Jeong, O, Katayama, N, Kaufman, J, Kazemzadeh, K, Keating, B, Kermish, Z, Keskitalo, R, Kisner, T, Kusaka, A, Le Jeune, M, Lee, A, Leon, D, Linder, E, Lowry, L, Matsuda, F, Matsumura, T, Miller, N, Mizukami, K, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Poletti, D, Puglisi, G, Raum, C, Rebeiz, G, Reichardt, C, Richards, P, Ross, C, Rotermund, K, Segawa, Y, Sherwin, B, Shirley, I, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takada, S, Takatori, S, Teply, G, Tikhomirov, A, Tomaru, T, Whitehorn, N, Zahn, A, Zahn, O, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie ( APC - UMR 7164 ), and Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA )
Subjects: [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, cosmic background radiation: polarization, Gravitational Wave, Astrophysics, 01 natural sciences, law.invention, law, Polarization, Cosmic Microwave Background, neutrino: mass, mirror, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Weak gravitational lensing, Physics, Equipment and services, Settore FIS/05, superconductivity, Astrophysics::Instrumentation and Methods for Astrophysics, Bolometers, Polarization (waves), vacuum system, astro-ph.CO, readout, Neutrino, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, IR filter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), lens, Bolometer, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 010309 optics, POLARBEAR-2, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Sensors, Gravitational wave, gravitational radiation: primordial, temperature, millimeter wave, optics, Gravitational lens, Extremely high frequency, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM
Abstract: POLARBEAR-2 (PB-2) is a cosmic microwave background (CMB) polarization experiment that will be located in the Atacama highland in Chile at an altitude of 5200 m. Its science goals are to measure the CMB polarization signals originating from both primordial gravitational waves and weak lensing. PB-2 is designed to measure the tensor to scalar ratio, r, with precision {\sigma}(r) < 0.01, and the sum of neutrino masses, {\Sigma}m{\nu}, with {\sigma}({\Sigma}m{\nu}) < 90 meV. To achieve these goals, PB-2 will employ 7588 transition-edge sensor bolometers at 95 GHz and 150 GHz, which will be operated at the base temperature of 250 mK. Science observations will begin in 2017., Comment: 9pages,8figures
Published: 2016

43. Probing inflation models with gravitational waves

Author: Valerie Domcke, AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: gauge field theory: abelian, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], gravitational radiation: primordial, inflation: slow-roll approximation, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, tachyon: stability, cosmic background radiation, Astrophysics::Cosmology and Extragalactic Astrophysics, gravitational radiation: direct detection, inflation: model, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), VIRGO, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], gravitational radiation detector: interferometer, gravitational radiation: spectrum, [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], LIGO, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: A direct detection of primordial gravitational waves is the ultimate probe for any inflation model. While current CMB bounds predict the generic scale-invariant gravitational wave spectrum from slow-roll inflation to be below the reach of upcoming gravitational wave interferometers, this prospect may dramatically change if the inflaton is a pseudoscalar. In this case, a coupling to any abelian gauge field leads to a tachyonic instability for the latter and hence to a new source of gravitational waves, directly related to the dynamics of inflation. In this contribution we discuss how this setup enables the upcoming gravitational wave interferometers advanced LIGO/VIRGO and eLISA to probe the microphysics of inflation, distinguishing between different universality classes of single-field slow-roll inflation models. We find that the prime candidate for an early detection is a Starobinsky-like model., 4 pages, 3 figures. To appear in the conference proceedings of the 51st Rencontres de Moriond, Cosmology Session, 19-26 March 2016 in La Thuile, Italy. Based on arXiv:1603.01287
Published: 2016

44. Primordial gravitational waves for universality classes of pseudoscalar inflation

Author: Valerie Domcke, Pierre Binétruy, Mauro Pieroni, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Paris Centre for Cosmological Physics (PCCP), Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Paris Centre for Cosmological Physics ( PCCP ), Université Paris Diderot - Paris 7 ( UPD7 ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Particle physics, gauge field theory: abelian, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], interferometer, Cosmic microwave background, FOS: Physical sciences, cosmic background radiation: polarization, Scalar potential, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Gauge theory, universality, 010306 general physics, pseudoscalar, Physics, Inflation (cosmology), 010308 nuclear & particles physics, Gravitational wave, background, potential: scalar, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation: primordial, Astronomy and Astrophysics, Inflaton, inflaton, inflation: model, Universality (dynamical systems), Pseudoscalar, High Energy Physics - Phenomenology, Automatic Keywords, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], signature, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: International audience; Current bounds from the polarization of the CMB predict the scale-invariant gravitational wave (GW) background of inflation to be out of reach for upcoming GW interferometers. This prospect dramatically changes if the inflaton is a pseudoscalar, in which case its generic coupling to any abelian gauge field provides a new source of GWs, directly related to the dynamics of inflation. This opens up new ways of probing the scalar potential responsible for cosmic inflation. Dividing inflation models into universality classes, we analyze the possible observational signatures. One of the most promising scenarios is Starobinsky inflation, which may lead to observational signatures both in direct GW detection as well as in upcoming CMB detectors. In this case, the complementarity between the CMB and direct GW detection, as well as the possibility of a multi-frequency analysis with upcoming ground and space based GW interferometers, may provide a first clue to the microphysics of inflation.
Published: 2016

45. Measurements of Degree-Scale B-mode Polarization with the BICEP/$Keck$ Experiments at South Pole

Author: Racine, Benjamin, Ahmed, Z., Aikin, R. W., Alexander, K. D., Barkats, D., Benton, S. J., Bischoff, C. A., Bock, J. J., Boenish, H., Bowens-Rubin, R., Brevik, J. A., Buder, I., Bullock, E., Buza, V., Connors, J., Cornelison, J., Crill, B. P., Crumrine, M., Dierickx, M., Duband, L., Dvorkin, C., Filippini, J. P., Fliescher, S., Grayson, J., Hall, G., Halpern, M., Harrison, S., Hildebrandt, S. R., Hilton, G. C., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Karpel, E., Kaufman, J. P., Keating, B. G., Kefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kuo, C. L., Lau, K., Larsen, N. A., Leitch, E. M., Lueker, M., Megerian, K. G., Moncelsi, L., Toshiya Namikawa, Netterfield, B., Nguyen, H. T., O Brient, R., Ogburn, R. W., Palladino, S., Pryke, C., Racine, B., Richter, S., Schwarz, R., Schillaci, A., Sheehy, C. D., Soliman, A., Germaine, T. St, Staniszewski, Z. K., Steinbach, B., Sudiwala, R. V., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C., Turner, A. D., Umiltà, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wong, C. L., Wu, W. L. K., Yang, H., Yoon, K. W., Zhang, C., Institut Nanosciences et Cryogénie (INAC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), BICEP, Keck, Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation: primordial, FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, BICEP, frequency: high, detector: sensitivity, gravitation: lens, B-mode, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The BICEP and Keck Array experiments are a suite of small-aperture refracting telescopes observing the microwave sky from the South Pole. They target the degree-scale B-mode polarization signal imprinted in the Cosmic Microwave Background (CMB) by primordial gravitational waves. Such a measurement would shed light on the physics of the very early universe. While BICEP2 observed for the first time a B-mode signal at 150 GHz, higher frequencies from the Planck satellite showed that it could be entirely due to the polarized emission from Galactic dust, though uncertainty remained high. Keck Array has been observing the same region of the sky for several years, with an increased detector count, producing the deepest polarized CMB maps to date. New detectors at 95 GHz were installed in 2014, and at 220 GHz in 2015. These observations enable a better constraint of galactic foreground emissions, as presented here. In 2015, BICEP2 was replaced by BICEP3, a 10 times higher throughput telescope observing at 95 GHz, while Keck Array is now focusing on higher frequencies. In the near future, BICEP Array will replace Keck Array, and will allow unprecedented sensitivity to the gravitational wave signal. High resolution observations from the South Pole Telescope (SPT) will also be used to remove the lensing contribution to B-modes., Comment: 9 pages, 8 figures: conference proceedings, 53rd Rencontres de Moriond, Cosmology 2018

46. SPIDER: CMB polarimetry from the edge of space

Author: Carlo R. Contaldi, A. C. Weber, A. E. Gambrel, S. Li, W. Holmes, Carl D. Reintsema, Katherine Freese, W. C. Jones, T. M. Ruud, Alexandra S. Rahlin, Juan D. Soler, Steven J. Benton, Johanna Nagy, John Bond, Mark Halpern, J. F. van der List, Jon E. Gudmundsson, A. S. Bergman, X. Song, Chao-Lin Kuo, James J. Bock, P. V. Mason, Ingunn Kathrine Wehus, Zhiqi Huang, H. C. Chiang, O. Doré, Ivan L. Padilla, B. Osherson, Adri Duivenvoorden, Matthew Hasselfield, Marcus Runyan, M. Galloway, Calvin B. Netterfield, J. E. Ruhl, Carole Tucker, Gene C. Hilton, R. V. Gramillano, Sean Bryan, Jamil A. Shariff, Peter A. R. Ade, R. S. Tucker, Mandana Amiri, Lorenzo Moncelsi, J. Hartley, Kent D. Irwin, Natalie N. Gandilo, R. Gualtieri, Ken Ganga, Viktor Hristov, Amy Trangsrud, Michael R. Nolta, Laura M. Fissel, E. Y. Young, Jeffrey P. Filippini, Zigmund Kermish, Anthony D. Turner, Marzieh Farhang, B. Racine, K. G. Megerian, R. Bihary, Donald V. Wiebe, A. A. Fraisse, H. K. Eriksen, T. A. Morford, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), SPIDER, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Science and Technology Facilities Council (STFC), and Science and Technology Facilities Council
Subjects: Cosmic microwave background, cosmic background radiation, 01 natural sciences, General Materials Science, 010303 astronomy & astrophysics, media_common, Physics, 0105 Mathematical Physics, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, BICEP, Condensed Matter Physics, Polarization (waves), Bolometers, SPIDER, detector: upgrade, Atomic and Molecular Physics, and Optics, Physics, Condensed Matter, B-mode, Physical Sciences, astro-ph.CO, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, General Physics, Transition-edge sensors, Cosmology and Nongalactic Astrophysics (astro-ph.CO), detector: performance, media_common.quotation_subject, 0204 Condensed Matter Physics, Cosmic background radiation, Polarimetry, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Physics, Applied, 0203 Classical Physics, 0103 physical sciences, transition edge sensors, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Remote sensing, Spider, Science & Technology, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: primordial, Inflation, polarization: monitoring, Sky, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM
Abstract: SPIDER is a balloon-borne instrument designed to map the polarization of the millimeter-wave sky at large angular scales. SPIDER targets the B-mode signature of primordial gravitational waves in the cosmic microwave background (CMB), with a focus on mapping a large sky area with high fidelity at multiple frequencies. SPIDER's first longduration balloon (LDB) flight in January 2015 deployed a total of 2400 antenna-coupled Transition Edge Sensors (TESs) at 90 GHz and 150 GHz. In this work we review the design and in-flight performance of the SPIDER instrument, with a particular focus on the measured performance of the detectors and instrument in a space-like loading and radiation environment. SPIDER's second flight in December 2018 will incorporate payload upgrades and new receivers to map the sky at 285 GHz, providing valuable information for cleaning polarized dust emission from CMB maps., Comment: 10 pages, 7 figures, LTD17 Conference

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