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33 results on '"cosmic background radiation: anisotropy"'

1. Do supernovae indicate an accelerating universe?

Author

Subir Sarkar, Roya Mohayaee, Mohamed Rameez, 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
cosmological model, quasar: redshift, Cosmic microwave background, General Physics and Astronomy, Cosmological constant, Astrophysics, baryon: oscillation: acoustic, 01 natural sciences, General Relativity and Quantum Cosmology, Cosmology, High Energy Physics - Phenomenology (hep-ph), general relativity, Peculiar velocity, General Materials Science, dark energy, 010303 astronomy & astrophysics, media_common, supernova: Type I, Physics, Hubble constant, cosmological constant, redshift: high, High Energy Physics - Phenomenology, kinematics, density: perturbation, flow, Robertson-Walker, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Computer Science::Mathematical Software, symbols, Baryon acoustic oscillations, expansion: acceleration, Astrophysics - Cosmology and Nongalactic Astrophysics, velocity, density: primordial, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Computer Science::Digital Libraries, temperature: fluctuation, symbols.namesake, 0103 physical sciences, structure, Physical and Theoretical Chemistry, 010308 nuclear & particles physics, Universe, gravitation, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], anisotropy: dipole, Dark energy, Einstein, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmic background radiation: anisotropy, Hubble's law
Abstract

In the late 1990's, observations of 93 Type Ia supernovae were analysed in the framework of the FLRW cosmology assuming these to be `standard(isable) candles'. It was thus inferred that the Hubble expansion rate is accelerating as if driven by a positive Cosmological Constant $\Lambda$. This is still the only direct evidence for the `dark energy' that is the dominant component of the standard $\Lambda$CDM cosmological model. Other data such as BAO, CMB anisotropies, stellar ages, the rate of structure growth, etc are all `concordant' with this model but do not provide independent evidence for accelerated expansion. Analysis of a larger sample of 740 SNe Ia shows that these are not quite standard candles, and highlights the "corrections" applied to analyse the data in the FLRW framework. The latter holds in the reference frame in which the CMB is isotropic, whereas observations are made in our heliocentric frame in which the CMB has a large dipole anisotropy. This is assumed to be of kinematic origin i.e. due to our non-Hubble motion driven by local inhomogeneity in the matter distribution. The $\Lambda$CDM model predicts how this peculiar velocity should fall off as the averaging scale is raised and the universe becomes sensibly homogeneous. However observations of the local `bulk flow' are inconsistent with this expectation and convergence to the CMB frame is not seen. Moreover the kinematic interpretation implies a corresponding dipole in the sky distribution of high redshift quasars, which is rejected by observations at 4.9$\sigma$. The acceleration of the Hubble expansion rate is also anisotropic at 3.9$\sigma$ and aligned with the bulk flow. Thus dark energy may be an artefact of analysing data assuming that we are idealised observers in an FLRW universe, when in fact the real universe is inhomogeneous and anisotropic out to distances large enough to impact on cosmological analyses., Comment: 14 pages, 4 figures, 4 tables

Published
2021

2. A health checkup test of the standard cosmological model in view of recent Cosmic Microwave Background Anisotropies experiments

Author

Di Valentino, Eleonora, Giarè, William, Melchiorri, Alessandro, Silk, Joseph, and HEP, INSPIRE

Subjects
cosmological model, polarization, data analysis method, satellite: Planck, WMAP, power spectrum: angular dependence, pole, anomaly, tension, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], cosmic background radiation: temperature, temperature: anisotropy, cosmic background radiation: anisotropy
Abstract

We present an updated data-analysis comparison of the most recent observations of the Cosmic Microwave Background temperature anisotropies and polarization angular power spectra released by four different experiments: the Planck satellite on one side, and the Atacama Cosmology Telescope (ACTPol) and the South Pole Telescope (SPT-3G), combined with the WMAP satellite 9-years observation data in order to be "Planck-independent" on the other side. We investigate in a systematic way 8 extended cosmological models that differ from the baseline $\Lambda$CDM case by the inclusion of many different combinations of additional degrees of freedom. Our analysis provides several hints for anomalies in the CMB angular power spectra in tension with the standard cosmological model. This indicates that either significant unaccounted-for systematics in the data are producing biased results or that $\Lambda$CDM is an incorrect/incomplete description of Nature. We conclude that only future independent high-precision CMB temperature and polarization measurements could provide a definitive answer.

Published
2022

3. A Constraint on Primordial B-modes from the First Flight of the Spider Balloon-borne Telescope

Author

Collaboration, SPIDER, Ade, PAR, Amiri, M, Benton, SJ, Bergman, AS, Bihary, R, Bock, JJ, Bond, JR, Bonetti, JA, Bryan, SA, Chiang, HC, Contaldi, CR, Doré, O, Duivenvoorden, AJ, Eriksen, HK, Farhang, M, Filippini, JP, Fraisse, AA, Freese, K, Galloway, M, Gambrel, AE, Gandilo, NN, Ganga, K, Gualtieri, R, Gudmundsson, JE, Halpern, M, Hartley, J, Hasselfield, M, Hilton, G, Holmes, W, Hristov, VV, Huang, Z, Irwin, KD, Jones, WC, Karakci, A, Kuo, CL, Kermish, ZD, Leung, JS-Y, Li, S, Mak, DSY, Mason, PV, Megerian, K, Moncelsi, L, Morford, TA, Nagy, JM, Netterfield, CB, Nolta, M, O'Brient, R, Osherson, B, Padilla, IL, Racine, B, Rahlin, AS, Reintsema, C, Ruhl, JE, Runyan, MC, Ruud, TM, Shariff, JA, Shaw, EC, Shiu, C, Soler, JD, Song, X, Trangsrud, A, Tucker, C, Tucker, RS, Turner, AD, List, JFVD, Weber, AC, Wehus, IK, Wen, S, Wiebe, DV, Young, EY, 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), SPIDER, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and Science and Technology Facilities Council (STFC)

Subjects
noise, cosmological model, data analysis method, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, ANGULAR POWER SPECTRUM, CIRCULAR-POLARIZATION, FOS: Physical sciences, cosmic background radiation: polarization, detector: noise, STATISTICAL-ANALYSIS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, POLARIMETRY, Monte Carlo: Markov chain, cosmic background radiation: B-mode, DESIGN, 0201 Astronomical and Space Sciences, MICROWAVE BACKGROUND DATA, numerical calculations, Astrophysics::Galaxy Astrophysics, ANISOTROPY, 0306 Physical Chemistry (incl. Structural), polarization: linear, Science & Technology, perturbation: primordial, BOLOMETERS, synchrotron radiation, Computer Science::Information Retrieval, LIKELIHOOD ESTIMATOR, statistical analysis: Bayesian, Astronomy and Astrophysics, SPIDER, detector: sensitivity, Space and Planetary Science, density: perturbation, Physical Sciences, 0202 Atomic, Molecular, Nuclear, Particle and Plasma Physics, black body, astro-ph.CO, power spectrum: angular dependence, energy: density: primordial, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], TRANSITION, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic background radiation: anisotropy
Abstract

We present the first linear polarization measurements from the 2015 long-duration balloon flight of SPIDER, an experiment designed to map the polarization of the cosmic microwave background (CMB) on degree angular scales. Results from these measurements include maps and angular power spectra from observations of 4.8% of the sky at 95 and 150 GHz, along with the results of internal consistency tests on these data. While the polarized CMB anisotropy from primordial density perturbations is the dominant signal in this region of sky, Galactic dust emission is also detected with high significance; Galactic synchrotron emission is found to be negligible in the SPIDER bands. We employ two independent foreground-removal techniques in order to explore the sensitivity of the cosmological result to the assumptions made by each. The primary method uses a dust template derived from Planck data to subtract the Galactic dust signal. A second approach, employing a joint analysis of SPIDER and Planck data in the harmonic domain, assumes a modified-blackbody model for the spectral energy distribution of the dust with no constraint on its spatial morphology. Using a likelihood that jointly samples the template amplitude and $r$ parameter space, we derive 95% upper limits on the primordial tensor-to-scalar ratio from Feldman-Cousins and Bayesian constructions, finding $r, 29 pages, 13 figures

Published
2022

4. Early dark energy is not excluded by current large-scale structure data

Author

José Luis Bernal, Tristan L. Smith, Kimberly K. Boddy, Riccardo Murgia, Marc Kamionkowski, Vivian Poulin, Swarthmore College, Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Johns Hopkins University (JHU), University of Texas at Austin [Austin], and TLS is supported by NSF Grant No. 2009377, NASA Grant No. 80NSSC18K0728,and the Research Corporation. This work was supported at Johns Hopkins by NSF Grant No. 1818899 and the Simons Foundation. JLB is supported by the Allan C. and Dorothy H. Davis Fellowship.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, constraint, Cosmic microwave background, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Parameter space, 01 natural sciences, symbols.namesake, High Energy Physics - Phenomenology (hep-ph), effective field theory, cosmological model: parameter space, 0103 physical sciences, supernova, Effective field theory, energy: density, structure, Planck, 010306 general physics, dark energy, Physics, Hubble constant, 010308 nuclear & particles physics, redshift: high, resolution, tension, galaxy: power spectrum, Galaxy, High Energy Physics - Phenomenology, symbols, Dark energy, galaxy: cluster, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Hubble's law, cosmic background radiation: anisotropy
Abstract

We revisit the impact of early dark energy (EDE) on galaxy clustering using BOSS galaxy power spectra, analyzed using the effective field theory (EFT) of large-scale structure (LSS), and anisotropies of the cosmic microwave background (CMB) from Planck. Recent studies found that these data place stringent constraints on the maximum abundance of EDE allowed in the Universe. We argue here that their conclusions are a consequence of their choice of priors on the EDE parameter space, rather than any disagreement between the data and the model. For example, when considering EFT-LSS, CMB, and high-redshift supernovae data we find the EDE and $\Lambda$CDM models can provide statistically indistinguishable fits ($\Delta \chi^2 = 0.12$) with a relatively large value for the maximum fraction of energy density in the EDE ($f_{\rm ede} = 0.09$) and Hubble constant ($H_0 = 71$ km/s/Mpc) in the EDE model. Moreover, we demonstrate that the constraining power added from the inclusion of EFT-LSS traces to the potential tension between the power-spectrum amplitudes $A_s$ derived from BOSS and from Planck that arises even within the context of $\Lambda$CDM. Until this is better understood, caution should be used when interpreting EFT-BOSS+Planck constraints to models beyond $\Lambda$CDM. These findings suggest that EDE still provides a potential resolution to the Hubble tension and that it is worthwhile to test the predictions of EDE with future data-sets and further study its theoretical possibilities., Comment: 8 pages, 3 figures, comments welcome

Published
2021

5. First constraint on the neutrino-induced phase shift in the spectrum of baryon acoustic oscillations

Author

Anže Slosar, Mariana Vargas-Magaña, Daniel Green, Benjamin Wallisch, Daniel Baumann, Raphael Flauger, Christophe Yèche, Florian Beutler, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Beutler, Florian [0000-0003-0467-5438], Flauger, Raphael [0000-0001-9527-8678], Green, Daniel [0000-0001-5496-0347], Wallisch, Benjamin [0000-0001-5713-1720], Apollo - University of Cambridge Repository, and String Theory (ITFA, IoP, FNWI)

Subjects
Planck, Cosmic microwave background, General Physics and Astronomy, Astrophysics, oscillation: acoustic, 01 natural sciences, 010305 fluids & plasmas, energy: density, media_common, Physics, wave: acoustic, ST/J005673/1, ST/H008586/1, neutrino: effect, Cosmic neutrino background, symbols, Baryon acoustic oscillations, history, Neutrino, Big Bang, satellite: Planck, perturbation, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Physics and Astronomy(all), neutrino: density, symbols.namesake, phase shift, 0103 physical sciences, 010306 general physics, STFC, plasma, ST/K00333X/1, cosmic background radiation: fluctuation, fluctuation, High Energy Physics::Phenomenology, big bang, RCUK, neutrino: background, Universe, Baryon, baryon, Automatic Keywords, 13. Climate action, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmic background radiation: anisotropy
Abstract

The existence of the cosmic neutrino background is a robust prediction of the hot big bang model. These neutrinos were a dominant component of the energy density in the early Universe and therefore played an important role in the evolution of cosmological perturbations. The energy density of the cosmic neutrino background has been measured using the abundances of light elements and the anisotropies of the cosmic microwave background. A complementary and more robust probe is provided by a distinct shift in the temporal phase of sound waves in the primordial plasma that is produced by fluctuations in the neutrino density. Here, we report on the first constraint on this neutrino-induced phase shift in the spectrum of baryon acoustic oscillations of the BOSS DR12 data. Constraining the acoustic scale using Planck data while marginalizing over the effects of neutrinos in the cosmic microwave background, we find a non-zero phase shift at greater than 95% confidence. Besides providing a new test of the cosmic neutrino background, our work is the first application of the baryon acoustic oscillation signal to early Universe physics. In the early Universe, fluctuations in the neutrino density produced a distinct shift in the temporal phase of sound waves in the primordial plasma. The size of this phase shift has now been constrained through baryon acoustic oscillation data.

Published
2019

6. Primordial black holes and secondary gravitational waves from ultraslow roll and punctuated inflation

Author

Pankaj Saha, H. V. Ragavendra, L. Sriramkumar, Joseph Silk, 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, and Sorbonne Université (SU)

Subjects
Cosmic microwave background, Scalar (mathematics), Primordial black hole, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, power spectrum: scalar, 0103 physical sciences, power spectrum: tensor, 010306 general physics, Inflation (cosmology), Physics, Slow roll, 010308 nuclear & particles physics, Gravitational wave, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], inflation: slow-roll approximation, gravitational radiation, inflation: model, field theory: scalar, Cosmology, bispectrum, non-Gaussianity, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Scalar field, Bispectrum, black hole: primordial, cosmic background radiation: anisotropy
Abstract

International audience; The primordial scalar power spectrum is well constrained by the cosmological data on large scales, primarily from the observations of the anisotropies in the cosmic microwave background. Over the last few years, it has been recognized that a sharp rise in power on small scales will lead to the enhanced formation of primordial black holes (PBHs) and also generate secondary gravitational waves (GWs) of higher and, possibly, detectable amplitudes. It is well understood that scalar power spectra with COBE normalized amplitude on the cosmic microwave background scales and enhanced amplitudes on smaller scales can be generated due to deviations from slow roll in single, canonical scalar field models of inflation. In fact, an epoch of so-called ultraslow roll inflation can lead to the desired amplification. We find that scenarios that lead to ultraslow roll can be broadly classified into two types, one wherein there is a brief departure from inflation (a scenario referred to as punctuated inflation) and another wherein such a departure does not arise. In this work, we consider a set of single field inflationary models involving the canonical scalar field that lead to ultraslow roll and punctuated inflation and examine the formation of PBHs as well as the generation of secondary GWs in these models. Apart from considering specific models, we reconstruct potentials from certain functional choices of the first slow roll parameter leading to ultraslow roll and punctuated inflation and investigate their observational signatures. In addition to the secondary tensor power spectrum, we calculate the secondary tensor bispectrum in the equilateral limit in these scenarios. Moreover, we calculate the inflationary scalar bispectrum that arises in all the cases and discuss the imprints of the scalar non-Gaussianities on the extent of PBHs formed and the amplitude of the secondary GWs generated. We conclude with a discussion on the wider implications of our results.

Published
2021

7. BICEP Array: 150 GHz detector module development

Author

Schillaci, A., Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Basu Thakur, R., Bischoff, C. A., Beck, D., Bock, J. J., Buza, V., Cheshire, J., Connors, J., Cornelison, J., Crumrine, M., Cukierman, A., Denison, E., Dierickx, M., Duband, L., Eiben, M., Fatigoni, S., Filippini, J. P., Giannakopoulos, C., Goeckner-Wald, N., Goldfinger, D., Grayson, J. A., Grimes, P., Hall, G., Halal, 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., Kefeli, S., Kovac, J. M., Kuo, C. L., Lau, K., Leitch, E. M., Lennox, A., Megerian, K. G., Miller, O. Y., Minutolo, L., Moncelsi, L., Nakato, Y., Namikawa, T., Nguyen, H. T., Brient, R. O., Palladino, S., Petroff, M., Precup, N., Prouve, T., Pryke, C., Benjamin Racine, Reintsema, C. D., Schmitt, B. L., Singari, B., Soliman, A., St Germaine, T., Steinbach, B., Sudiwala, R. V., Thompson, K. L., Tucker, C., Turner, A. D., Umilta, C., Verges, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wu, W. L. K., Yang, E., Yoon, K. W., Young, E., Yu, C., Zeng, L., Zhang, C., Zhang, S., 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), Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)

Subjects
density, detector: cryogenics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics::Instrumentation and Detectors, superconductivity, pole, Astrophysics::Instrumentation and Methods for Astrophysics, costs, FOS: Physical sciences, fabrication, sensitivity, BICEP, buildings, cryogenics: design, amplifier, readout, upgrade, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM), performance, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic background radiation: anisotropy
Abstract

The BICEP/Keck Collaboration is currently leading the quest to the highest sensitivity measurements of the polarized CMB anisotropies on degree scale with a series of cryogenic telescopes, of which BICEP Array is the latest Stage-3 upgrade with a total of $\sim32,000$ detectors. The instrument comprises 4 receivers spanning 30 to 270 GHz, with the low-frequency 30/40 GHz deployed to the South Pole Station in late 2019. The full complement of receivers is forecast to set the most stringent constraints on the tensor to scalar ratio $r$. Building on these advances, the overarching small-aperture telescope concept is already being used as the reference for further Stage-4 experiment design. In this paper I will present the development of the BICEP Array 150 GHz detector module and its fabrication requirements, with highlights on the high-density time division multiplexing (TDM) design of the cryogenic circuit boards. The low-impedance wiring required between the detectors and the first-stage SQUID amplifiers is crucial to maintain a stiff voltage bias on the detectors. A novel multi-layer FR4 Printed Circuit Board (PCB) with superconducting traces, capable of reading out up to 648 detectors, is presented along with its validation tests. I will also describe an ultra-high density TDM detector module we developed for a CMB-S4-like experiment that allows up to 1,920 detectors to be read out. TDM has been chosen as the detector readout technology for the Cosmic Microwave Background Stage-4 (CMB-S4) experiment based on its proven low-noise performance, predictable costs and overall maturity of the architecture. The heritage for TDM is rooted in mm- and submm-wave experiments dating back 20 years and has since evolved to support a multiplexing factor of 64x in Stage-3 experiments., Comment: 9 pages, 5 figure, Proceeding of LTD19 submitted to Journal of Low Temperature Physics

Published
2021
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8. Unlocking the synergy between CMB spectral distortions and anisotropies

Author

Hao Fu, Matteo Lucca, Silvia Galli, Elia S. Battistelli, Deanna C. Hooper, Julien Lesgourgues, Nils Schöneberg, 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
cosmological model, noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, polarization: anisotropy, redshift: dependence, nucleosynthesis: big bang, satellite, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, power spectrum: scalar, 0103 physical sciences, ionization, CMBR experiments, physics of the early universe, structure, inflation, 010303 astronomy & astrophysics, 010308 nuclear & particles physics, formation, cosmological parameters from CMBR, Astronomy and Astrophysics, dark matter: annihilation, sensitivity, CMBR theory, cosmic background radiation: temperature, 13. Climate action, spectral, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic background radiation: anisotropy
Abstract

Measurements of the cosmic microwave background (CMB) spectral distortions (SDs) will open a new window on the very early universe, providing new information complementary to that gathered from CMB temperature and polarization anisotropies. In this paper, we study their synergy as a function of the characteristics of the considered experiments. In particular, we examine a wide range of sensitivities for possible SD measurements, spanning from FIRAS up to noise levels 1000 times better than PIXIE, and study their constraining power when combined with current or future CMB anisotropy experiments such as Planck or LiteBIRD plus CMB-S4. We consider a number of different cosmological models such as the $\Lambda$CDM, as well as its extensions with the running of the scalar spectral index, the decay or the annihilation of dark matter (DM) particles. While upcoming CMB anisotropy experiments will be able to decrease the uncertainties on inflationary parameters such as $A_s$ and $n_s$ by about a factor 2 in the $\Lambda$CDM case, we find that an SD experiment 100 times more sensitive than PIXIE (comparable to the proposed Super-PIXIE satellite) could potentially further contribute to constrain these parameters. This is even more significant in the case of the running of the scalar spectral index. Furthermore, as expected, constraints on DM particles decaying at redshifts probed by SDs will improve by orders of magnitude even with an experiment 10 times worse than PIXIE as compared to CMB anisotropies or Big Bang Nucleosynthesis bounds. On the contrary, DM annihilation constraints will not significantly improve over CMB anisotropy measurements. Finally, we forecast the constraints obtainable with sensitivities achievable either from the ground or from a balloon., Comment: 25+4 pages with 8 figures and 7 tables, published version

Published
2021

9. Atacama Cosmology Telescope: Constraints on cosmic birefringence

Author

Michael D. Niemack, Mathew S. Madhavacheril, Sigurd Naess, J. Richard Bond, Adam D. Hincks, Neelima Sehgal, Kavilan Moodley, Loïc Maurin, Thibaut Louis, Joanna Dunkley, Grace E. Chesmore, Frank J. Qu, Omar Darwish, Johannes Hubmayr, Simone Aiola, Gene C. Hilton, Lyman A. Page, Toshiya Namikawa, Rolando Dünner, Maya Mallaby-Kay, C. Sifon, Mark J. Devlin, Patricio A. Gallardo, Daniel T. Becker, Amanda MacInnis, Alexander van Engelen, Renée Hložek, John P. Nibarger, Sara M. Simon, Emilie R. Storer, Matthew Hasselfield, Blake D. Sherwin, Kevin M. Huffenberger, Yilun Guan, Laura Newburgh, Vera Gluscevic, Arthur Kosowsky, Jeff Van Lanen, Edward J. Wollack, Anna E. Fox, Brian J. Koopman, Erminia Calabrese, Jeff McMahon, James A. Beall, Steve K. Choi, Alessandro Schillaci, Naomi Robertson, Nicholas Battaglia, Marius Lungu, John P. Hughes, Suzanne T. Staggs, David N. Spergel, Federico Nati, Dongwon Han, Namikawa, T, Guan, Y, Darwish, O, Sherwin, B, Aiola, S, Battaglia, N, Beall, J, Becker, D, Bond, J, Calabrese, E, Chesmore, G, Choi, S, Devlin, M, Dunkley, J, Dunner, R, Fox, A, Gallardo, P, Gluscevic, V, Han, D, Hasselfield, M, Hilton, G, Hincks, A, Hlozek, R, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Kosowsky, A, Louis, T, Lungu, M, Macinnis, A, Madhavacheril, M, Mallaby-Kay, M, Maurin, L, Mcmahon, J, Moodley, K, Naess, S, Nati, F, Newburgh, L, Nibarger, J, Niemack, M, Page, L, Qu, F, Robertson, N, Schillaci, A, Sehgal, N, Sifon, C, Simon, S, Spergel, D, Staggs, S, Storer, E, Van Engelen, A, Van Lanen, J, Wollack, E, 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 d'astrophysique spatiale (IAS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
data analysis method, cosmological model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, cosmic background radiation: polarization, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, power spectrum, 01 natural sciences, 7. Clean energy, Cosmology, High Energy Physics - Experiment, current: constraint, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), statistical analysis, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Cosmic Birefringence, CMB, Cosmology, inflation, 010303 astronomy & astrophysics, Axion, Physics, Birefringence, birefringence, 010308 nuclear & particles physics, Chern-Simons term, photon, coupling constant, Polarization (waves), Massless particle, High Energy Physics - Phenomenology, Amplitude, axion, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Atacama Cosmology Telescope, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic background radiation: anisotropy
Abstract

We present new constraints on anisotropic birefringence of the cosmic microwave background polarization using two seasons of data from the Atacama Cosmology Telescope covering $456$ square degrees of sky. The birefringence power spectrum, measured using a curved-sky quadratic estimator, is consistent with zero. Our results provide the tightest current constraint on birefringence over a range of angular scales between $5$ arcminutes and $9$ degrees. We improve previous upper limits on the amplitude of a scale-invariant birefringence power spectrum by a factor of between $2$ and $3$. Assuming a nearly-massless axion field during inflation, our result is equivalent to a $2\,\sigma$ upper limit on the Chern-Simons coupling constant between axions and photons of $g_{\alpha\gamma}, Comment: 18 pages, 3 figures, Accepted for publication in PRD

Published
2020

10. A new probe of Axion-Like Particles: CMB polarization distortions due to cluster magnetic fields

Author

Suvodip Mukherjee, Benjamin D. Wandelt, David N. Spergel, Rishi Khatri, 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, and Sorbonne Université (SU)

Subjects
High Energy Physics - Theory, galaxy cluster, noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Photon, Cosmic microwave background, kinetic, FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, electron: density, High Energy Physics - Phenomenology (hep-ph), Axion, spectral distortions, magnetic field: cluster, 0103 physical sciences, Cosmic Microwave Background, structure, 010303 astronomy & astrophysics, Galaxy cluster, Physics, 010308 nuclear & particles physics, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], galaxy: redshift, photon, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Polarization (waves), Redshift, Galaxy, Magnetic field, observatory, High Energy Physics - Phenomenology, High Energy Physics - Theory (hep-th), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], spectral, axion-like particles, galaxy: cluster, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic background radiation: anisotropy
Abstract

We propose using the upcoming Cosmic Microwave Background (CMB) ground based experiments to detect the signal of ALPs (Axion like particles) interacting with magnetic fields in galaxy clusters. The conversion between CMB photons and ALPs in the presence of the cluster magnetic field can cause a polarized spectral distortion in the CMB around a galaxy cluster. The strength of the signal depends upon the redshift of the galaxy cluster and will exhibit a distinctive spatial profile around it depending upon the structure of electron density and magnetic field. This distortion produces a different shape from the other known spectral distortions like $y$-type and $\mu$-type and hence are separable from the multi-frequency CMB observation. The spectrum is close to kinematic Sunyaev-Zeldovich (kSZ) signal but can be separated from it using the polarization information. For the future ground-based CMB experiments such as Simons Observatory and CMB-S4, we estimate the measurability of this signal in the presence of foreground contamination, instrument noise and CMB anisotropies. This new avenue can probe the photon-ALP coupling over the ALP mass range from $10^{-13}$ eV to $10^{-12}$ eV with two orders of magnitude better accuracy from CMB-S4 than the current existing bounds., Comment: 34 pages, 15 figures. Matches the version accepted for publication in JCAP. Fig. 5 and Fig. 6 are added in the revised version

Published
2020

11. The exponential tail of inflationary fluctuations: consequences for primordial black holes

Author

Juan Garcia-Bellido, Jose María Ezquiaga, Vincent Vennin, 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
High Energy Physics - Theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, FOS: Physical sciences, Primordial black hole, General Relativity and Quantum Cosmology (gr-qc), Curvature, 01 natural sciences, General Relativity and Quantum Cosmology, Non-Gaussianity, 0103 physical sciences, nonminimal, physics of the early universe, Statistical physics, structure, distribution function, inflation, numerical calculations, Physics, Slow roll, 010308 nuclear & particles physics, fluctuation, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], diffusion, inflation: slow-roll approximation, primordial black holes, Astronomy and Astrophysics, Inflaton, inflaton, Exponential function, Automatic Keywords, High Energy Physics - Theory (hep-th), Inflection point, non-Gaussianity, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], curvature: perturbation, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], black hole: primordial, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic background radiation: anisotropy
Abstract

The curvature perturbations produced during an early era of inflation are known to have quasi-Gaussian distribution functions close to their maximum, where they are well constrained by measurements of the cosmic microwave background anisotropies and of the large-scale structures. In contrast, the tails of these distributions are poorly known, although this part is the relevant one for rare, extreme objects such as primordial black holes. We show that these tails are highly non-Gaussian, and cannot be described with standard non-Gaussian expansions, that are designed to approximate the distributions close to their maximum only. Using the stochastic-$\delta N$ formalism, we develop a generic framework to compute the tails, which are found to have an exponential, rather than Gaussian, decay. These exponential tails are inevitable, and do not require any non-minimal feature as they simply result from the quantum diffusion of the inflaton field along its potential. We apply our formalism to a few relevant single-field, slow-roll inflationary potentials, where our analytical treatment is confirmed by comparison with numerical results. We discuss the implications for the expected abundance of primordial black holes in these models, and highlight that it can differ from standard results by several orders of magnitude. In particular, we find that potentials with an inflection point overproduce primordial black holes, unless slow roll is violated., Comment: 34 pages, 14 figures. Justification of the characteristic function expansion in section 2.2 amended; definition of a new scalar product in equation (2.21); figure 13 is corrected. Our results are unchanged

Published
2020

12. Planck 2018 results. VI. Cosmological parameters

Author

M. López-Caniego, Richard A. Battye, Hannu Kurki-Suonio, J. Aumont, Charles R. Lawrence, P. Vielva, E. Martínez-González, François R. Bouchet, L. Montier, K. Ganga, Francesca Perrotta, Lloyd Knox, M. Le Jeune, Jan Hamann, E. Franceschi, M. Tenti, C. Combet, Torsten A. Enßlin, Andrea Zacchei, R. A. Sunyaev, J.-M. Delouis, J. F. Macías-Pérez, Tiziana Trombetti, Zhiqi Huang, Graca Rocha, L. Polastri, Alessandro Melchiorri, A. Mennella, Nabila Aghanim, Sabino Matarrese, Jose Alberto Rubino-Martin, N. Bartolo, Theodore Kisner, Peter Meinhold, L. Salvati, Jose M. Diego, K. Benabed, J.-P. Bernard, J. González-Nuevo, M. Ashdown, H. K. Eriksen, Erminia Calabrese, Olivier Doré, Serge Gratton, G. de Zotti, L. Vibert, J. R. Bond, Marzieh Farhang, Benjamin D. Wandelt, Julian Borrill, L. Toffolatti, F. Piacentini, Yin-Zhe Ma, Will Handley, S. Galeotta, A. Karakci, A. A. Fraisse, Anthony Lasenby, M. Sandri, X. Dupac, G. Sirri, Adam Moss, B. Ruiz-Granados, D. Contreras, A.-S. Suur-Uski, Mario G. Lattanzi, Ricardo Genova-Santos, Jean-François Cardoso, Marian Douspis, G. Polenta, E. Keihänen, A. J. Banday, M. Migliaccio, R. B. Barreiro, B. P. Crill, J. Valiviita, Yabebal Fantaye, B. Van Tent, Tuhin Ghosh, D. Tavagnacco, A. Renzi, Martin White, M. Bucher, Douglas Scott, Jörg P. Rachen, Hans Ulrik Nørgaard-Nielsen, Jason D. McEwen, R. C. Butler, Locke D. Spencer, Nicola Vittorio, V. Lindholm, Fabrizio Villa, K. Kiiveri, Ingunn Kathrine Wehus, Julien Lesgourgues, Hiranya V. Peiris, Reijo Keskitalo, Krzysztof M. Gorski, S. R. Hildebrandt, E. Di Valentino, A. Marcos-Caballero, G. Patanchon, P. de Bernardis, M. Lilley, Simon D. M. White, C. Sirignano, M. Frailis, Carlo Baccigalupi, Francesco Forastieri, W. C. Jones, P. Lemos, François Levrier, E. Hivon, R. Fernandez-Cobos, Carlo Burigana, Nicoletta Krachmalnicoff, D. Herranz, Andrei V. Frolov, M. Tomasi, Marius Millea, J.-L. Puget, Paolo Natoli, James R. Fergusson, D. Paoletti, L. Pagano, M.-A. Miville-Deschênes, Julien Carron, Luca Valenziano, F. K. Hansen, S. Dusini, Andrea Zonca, Bruce Partridge, Jens Chluba, S. Basak, H. C. Chiang, Alessandro Gruppuso, Marco Bersanelli, Peter G. Martin, Martin Kunz, Valeria Pettorino, Mathieu Remazeilles, Jacques Delabrouille, Jon E. Gudmundsson, J.-M. Lamarre, P. Bielewicz, F. Cuttaia, Franz Elsner, G. Roudier, S. Galli, Michele Liguori, Gianluca Morgante, A. Ducout, Fabio Finelli, James J. Bock, M. Reinecke, C. Rosset, Yashar Akrami, Anthony Challinor, Subhabrata Mitra, J. A. Tauber, Matteo Martinelli, M. Savelainen, N. Mauri, E. P. S. Shellard, Antony Lewis, Diego Molinari, G. Maggio, P. B. Lilje, Davide Maino, A. Mangilli, L. P. L. Colombo, Mario Ballardini, N. Mandolesi, Andrew H. Jaffe, Philip Lubin, J. Kim, M. Maris, Martina Gerbino, George Efstathiou, F. Boulanger, Guilaine Lagache, Challinor, Anthony [0000-0003-3479-7823], Fergusson, James [0000-0003-4820-171X], Handley, William [0000-0002-5866-0445], Lasenby, Anthony [0000-0002-8208-6332], Apollo - University of Cambridge Repository, 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 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), 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), 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 Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut Lagrange de Paris, Sorbonne Universités, 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 de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Planck, 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), Astrophysique, 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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), Computing and Mathematical Sciences [Pasadena]], California Institute of Technology (CALTECH), Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), 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), 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), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Laboratoire d'Océanographie Physique et Spatiale (LOPS), Institut de Recherche pour le Développement (IRD)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Dipartimento di Fisica 'G. Galilei', Università degli Studi di Padova = University of Padua (Unipd), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), University College of London [London] (UCL), University of Manchester [Manchester], University of British Columbia (UBC), 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), funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 725456, CMBSPEC)., Planck Collaboration, European Project: 616170,EC:FP7:ERC,ERC-2013-CoG,COSMOPARS(2014), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Sorbonne Université (SU)-Observatoire de Paris, Université Paris-Seine-Université Paris-Seine-Institut national des sciences de l'Univers (INSU - CNRS)-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 de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2020-....] (Grenoble INP [2020-....]), Université Grenoble Alpes [2020-....] (UGA [2020-....]), Sorbonne Université, 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), 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), 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), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Institut de Recherche pour le Développement (IRD)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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, Universita degli Studi di Padova, Sorbonne Université (SU), Science and Technology Facilities Council (STFC), Science and Technology Facilities Council, Universidad de Cantabria, Ministerio de Economía y Competitividad (España), Consejo Superior de Investigaciones Científicas (España), European Commission, European Research Council, European Space Agency, Department of Physics, Helsinki Institute of Physics, 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), 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), Aghanim N., Akrami Y., Ashdown M., Aumont J., Baccigalupi C., Ballardini M., Banday A.J., Barreiro R.B., Bartolo N., Basak S., Battye R., Benabed K., Bernard J.-P., Bersanelli M., Bielewicz P., Bock J.J., Bond J.R., Borrill J., Bouchet F.R., Boulanger F., Bucher M., Burigana C., Butler R.C., Calabrese E., Cardoso J.-F., Carron J., Challinor A., Chiang H.C., Chluba J., Colombo L.P.L., Combet C., Contreras D., Crill B.P., Cuttaia F., De Bernardis P., De Zotti G., Delabrouille J., Delouis J.-M., Di Valentino E., Diego J.M., Dore O., Douspis M., Ducout A., Dupac X., Dusini S., Efstathiou G., Elsner F., Ensslin T.A., Eriksen H.K., Fantaye Y., Farhang M., Fergusson J., Fernandez-Cobos R., Finelli F., Forastieri F., Frailis M., Fraisse A.A., Franceschi E., Frolov A., Galeotta S., Galli S., Ganga K., Genova-Santos R.T., Gerbino M., Ghosh T., Gonzalez-Nuevo J., Gorski K.M., Gratton S., Gruppuso A., Gudmundsson J.E., Hamann J., Handley W., Hansen F.K., Herranz D., Hildebrandt S.R., Hivon E., Huang Z., Jaffe A.H., Jones W.C., Karakci A., Keihanen E., Keskitalo R., Kiiveri K., Kim J., Kisner T.S., Knox L., Krachmalnicoff N., Kunz M., Kurki-Suonio H., Lagache G., Lamarre J.-M., Lasenby A., Lattanzi M., Lawrence C.R., Le Jeune M., Lemos P., Lesgourgues J., Levrier F., Lewis A., Liguori M., Lilje P.B., Lilley M., Lindholm V., Lopez-Caniego M., Lubin P.M., Ma Y.-Z., Macias-Perez J.F., Maggio G., Maino D., Mandolesi N., Mangilli A., Marcos-Caballero A., Maris M., Martin P.G., Martinelli M., Martinez-Gonzalez E., Matarrese S., Mauri N., McEwen J.D., Meinhold P.R., Melchiorri A., Mennella A., Migliaccio M., Millea M., Mitra S., Miville-Deschenes M.-A., Molinari D., Montier L., Morgante G., Moss A., Natoli P., Norgaard-Nielsen H.U., Pagano L., Paoletti D., Partridge B., Patanchon G., Peiris H.V., Perrotta F., Pettorino V., Piacentini F., Polastri L., Polenta G., Puget J.-L., Rachen J.P., Reinecke M., Remazeilles M., Renzi A., Rocha G., Rosset C., Roudier G., Rubino-Martin J.A., Ruiz-Granados B., Salvati L., Sandri M., Savelainen M., Scott D., Shellard E.P.S., Sirignano C., Sirri G., Spencer L.D., Sunyaev R., Suur-Uski A.-S., Tauber J.A., Tavagnacco D., Tenti M., Toffolatti L., Tomasi M., Trombetti T., Valenziano L., Valiviita J., Van Tent B., Vibert L., Vielva P., Villa F., Vittorio N., Wandelt B.D., Wehus I.K., White M., White S.D.M., Zacchei A., and Zonca A.

Subjects
cosmological model, Astronomy, Cosmic microwave background, INFLATIONARY PARADIGM, cosmic background radiation: polarization, Astrophysics, cosmic background radiation, baryon: oscillation: acoustic, 01 natural sciences, 7. Clean energy, Omega, Cosmology, OSCILLATION SPECTROSCOPIC SURVEY, background: geometry, GALAXY REDSHIFT SURVEY, neutrino: mass, dark energy, 010303 astronomy & astrophysics, matter: density, expansion: adiabatic, Physics, Spectral index, cosmological constant, Hubble constant, Settore FIS/05, Cosmic background radiation, Cosmological parameters, ACCURATE HALO-MODEL, statistical analysis: Bayesian, POWER-SPECTRUM, matter: fluctuation, tension, perturbation: scalar, Physical Sciences, symbols, astro-ph.CO, Neutrino, Astrophysics - Cosmology and Nongalactic Astrophysics, Particle physics, data analysis method, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, Dark matter, FOS: Physical sciences, cosmic background radiation: spectrum, dark matter: density, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, NO, symbols.namesake, power spectrum: scalar, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, 0103 physical sciences, 0201 Astronomical and Space Sciences, Planck, cosmological parameters, Astrophysics::Galaxy Astrophysics, Science & Technology, 010308 nuclear & particles physics, baryon: density, Astronomy and Astrophysics, GROWTH-RATE, stability, 115 Astronomy, Space science, cosmic background radiation: temperature, MICROWAVE BACKGROUND ANISOTROPIES, 13. Climate action, Space and Planetary Science, Cosmic background radiation, Cosmological parameters, PROBE WMAP OBSERVATIONS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], BARYON ACOUSTIC-OSCILLATIONS, Hubble's law, cosmic background radiation: anisotropy
Abstract

Planck Collaboration: et al., arXiv:1807.06209v3, We present cosmological parameter results from the final full-mission Planck measurements of the cosmic microwave background (CMB) anisotropies, combining information from the temperature and polarization maps and the lensing reconstruction. Compared to the 2015 results, improved measurements of large-scale polarization allow the reionization optical depth to be measured with higher precision, leading to significant gains in the precision of other correlated parameters. Improved modelling of the small-scale polarization leads to more robust constraints on many parameters, with residual modelling uncertainties estimated to affect them only at the 0.5σ level. We find good consistency with the standard spatially-flat 6-parameter ΛCDM cosmology having a power-law spectrum of adiabatic scalar perturbations (denoted “base ΛCDM” in this paper), from polarization, temperature, and lensing, separately and in combination. A combined analysis gives dark matter density Ωch2 = 0.120 ± 0.001, baryon density Ωbh2 = 0.0224 ± 0.0001, scalar spectral index ns = 0.965 ± 0.004, and optical depth τ = 0.054 ± 0.007 (in this abstract we quote 68% confidence regions on measured parameters and 95% on upper limits). The angular acoustic scale is measured to 0.03% precision, with 100θ* = 1.0411 ± 0.0003. These results are only weakly dependent on the cosmological model and remain stable, with somewhat increased errors, in many commonly considered extensions. Assuming the base-ΛCDM cosmology, the inferred (model-dependent) late-Universe parameters are: Hubble constant H0 = (67.4 ± 0.5) km s−1 Mpc−1; matter density parameter Ωm = 0.315 ± 0.007; and matter fluctuation amplitude σ8 = 0.811 ± 0.006. We find no compelling evidence for extensions to the base-ΛCDM model. Combining with baryon acoustic oscillation (BAO) measurements (and considering single-parameter extensions) we constrain the effective extra relativistic degrees of freedom to be Neff = 2.99 ± 0.17, in agreement with the Standard Model prediction Neff = 3.046, and find that the neutrino mass is tightly constrained to ∑mν < 0.12 eV. The CMB spectra continue to prefer higher lensing amplitudes than predicted in base ΛCDM at over 2σ, which pulls some parameters that affect the lensing amplitude away from the ΛCDM model; however, this is not supported by the lensing reconstruction or (in models that also change the background geometry) BAO data. The joint constraint with BAO measurements on spatial curvature is consistent with a flat universe, ΩK = 0.001 ± 0.002. Also combining with Type Ia supernovae (SNe), the dark-energy equation of state parameter is measured to be w0 = −1.03 ± 0.03, consistent with a cosmological constant. We find no evidence for deviations from a purely power-law primordial spectrum, and combining with data from BAO, BICEP2, and Keck Array data, we place a limit on the tensor-to-scalar ratio r0.002 < 0.06. Standard big-bang nucleosynthesis predictions for the helium and deuterium abundances for the base-ΛCDM cosmology are in excellent agreement with observations. The Planck base-ΛCDM results are in good agreement with BAO, SNe, and some galaxy lensing observations, but in slight tension with the Dark Energy Survey’s combined-probe results including galaxy clustering (which prefers lower fluctuation amplitudes or matter density parameters), and in significant, 3.6σ, tension with local measurements of the Hubble constant (which prefer a higher value). Simple model extensions that can partially resolve these tensions are not favoured by the Planck data., The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU).

Published
2020

13. Electromagnetic probes of primordial black holes as dark matter

Author

Kashlinsky, A., Ali-Haimoud, Y., Clesse, S., Garcia-Bellido, J., Wyrzykowski, L., Achucarro, A., Amendola, L., Annis, J., Arbey, A., Arendt, R. G., Atriobarandela, F., Bellomo, N., Belotsky, K., Bernal, J-L, Bird, S., Bozza, V., Byrnes, C., Calchi Novati, S., Calore, F., Carr, B. J., Chluba, J., Cholis, I., Cieplak, A., Cole, P., Dalianis, I., Davis, A-C, Davis, T., Luca, V., Dvorkin, I., Emparan, R., Ezquiaga, J-M, Fleury, P., Franciolini, G., Gaggero, D., Georg, J., Germani, C., Giudice, G-F, Goobar, A., Hasinger, G., Hector, A., Hundertmark, M., Hutsi, G., Jansen, R., Kamionkowski, M., Kawasaki, M., Kazanas, D., Kehagias, A., Khlopov, M., Knebe, A., Kohri, K., Koushiappas, S., Kovetz, E., Kuhnel, F., Macgibbon, J., Marzola, L., Mediavilla, E., Meszaros, P., Mroz, P., Munoz, J., Musco, I., Nesseris, S., Ozsoy, O., Pani, P., Poulin, V., Raccanelli, A., Racco, D., Raidal, M., Ranc, C., Rattenbury, N., Rhodes, J., Ricotti, M., Riotto, A., Rubin, S., Rubio, J., Ruiz-Morales, E., Sasaki, M., Schnittman, J., Shvartzvald, Y., Street, R., Takada, M., Takhistov, V., Tashiro, H., Tasinato, G., Tringas, G., Caner Unal, Tada, Y., Tsapras, Y., Vaskonen, V., Veermae, H., Vidotto, F., Watson, S., Windhorst, R., Yokoyama, S., Young, S., Université Claude Bernard Lyon 1 (UCBL), Université de Lyon, Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), and Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), lens, Astrophysics::High Energy Astrophysical Phenomena, spin: 0, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter: density, galaxy: halo, star, accretion, supernova, quasar, LIGO, Astrophysics::Galaxy Astrophysics, pulsar, fluctuation, Astrophysics::Instrumentation and Methods for Astrophysics, stability, coherence, electromagnetic, X-ray: background, infrared, astro-ph.CO, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], black hole: primordial, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic background radiation: anisotropy
Abstract

The LIGO discoveries have rekindled suggestions that primordial black holes (BHs) may constitute part to all of the dark matter (DM) in the Universe. Such suggestions came from 1) the observed merger rate of the BHs, 2) their unusual masses, 3) their low/zero spins, and 4) also from the independently uncovered cosmic infrared background (CIB) fluctuations signal of high amplitude and coherence with unresolved cosmic X-ray background (CXB). Here we summarize the prospects to resolve this important issue with electromagnetic observations using the instruments and tools expected in the 2020's. These prospects appear promising to make significant, and potentially critical, advances. We demonstrate that in the next decade, new space- and ground-borne electromagnetic instruments, combined with concurrent theoretical efforts, should shed critical light on the long-considered link between primordial BHs and DM. Specifically the new data and methodologies under this program will involve: I) Probing with high precision the spatial spectrum of source-subtracted CIB with Euclid and WFIRST, and its coherence with unresolved cosmic X-ray background using eROSITA and Athena, II) Advanced searches for microlensing of Galactic stars by the intervening Galactic Halo BHs with OGLE, Gaia, LSST and WFIRST, III) Supernovae (SNe) lensing in the upcoming surveys with WFIRST, LSST and also potentially with Euclid and JWST, IV) Advanced theoretical work to understand the details of PBH accretion and evolution and their influence on cosmic microwave background (CMB) anisotropies in light of the next generation CMB experiments, V) Better new samples and theoretical understanding involving stability and properties of ultra faint dwarf galaxies, pulsar timing, and cosmological quasar lensing., Comment: Science whitepaper submitted to the Astro2020 Decadal Survey

Published
2019

14. Cosmological Probes of Dark Matter Interactions: The Next Decade

Author

Yacine Ali-Haïmoud, Keith Bechtol, Kimberly Boddy, Céline Bœhm, Jens Chluba, Francis-Yan Cyr-Racine, Cora Dvorkin, Vera Gluscevic, Daniel Grin, Julien Lesgourgues, Madhavacheril, Mathew S., Mcdermott, Samuel D., Muñoz, Julian B., Nadler, Ethan O., Vivian Poulin, Sarah Shandera, Katelin Schutz, Slatyer, Tracy R., Benjamin Wallisch, 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 Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), and HEP, INSPIRE

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), dark matter: interaction, FOS: Physical sciences, spectral, galaxy, structure, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmic background radiation: anisotropy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Cosmological observations offer unique and robust avenues for probing the fundamental nature of dark matter particles-they broadly test a range of compelling theoretical scenarios, often surpassing or complementing the reach of terrestrial and other experiments. We discuss observational and theoretical advancements that will play a pivotal role in realizing a strong program of cosmological searches for the identity of dark matter in the coming decade. Specifically, we focus on measurements of the cosmic-microwave-background anisotropy and spectral distortions, and tracers of structure (such as the Lyman-$\alpha$ forest, galaxies, and the cosmological 21-cm signal)., Comment: Astro2020 Decadal Survey science white paper; list of endorsers available at https://github.com/veragluscevic/Astro2020-DM-Cosmology-Endorsers

Published
2019

15. 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

16. The LiteBIRD Satellite Mission: Sub-Kelvin Instrument

Author

A. Suzuki, P. A. R. Ade, Y. Akiba, D. Alonso, K. Arnold, J. Aumont, C. Baccigalupi, D. Barron, S. Basak, S. Beckman, J. Borrill, F. Boulanger, M. Bucher, E. Calabrese, Y. Chinone, S. Cho, B. Crill, A. Cukierman, D. W. Curtis, T. de Haan, M. Dobbs, A. Dominjon, T. Dotani, L. Duband, A. Ducout, J. Dunkley, J. M. Duval, T. Elleflot, H. K. Eriksen, J. Errard, J. Fischer, T. Fujino, T. Funaki, U. Fuskeland, K. Ganga, N. Goeckner-Wald, J. Grain, N. W. Halverson, T. Hamada, T. Hasebe, M. Hasegawa, K. Hattori, M. Hattori, L. Hayes, M. Hazumi, N. Hidehira, C. A. Hill, G. Hilton, J. Hubmayr, K. Ichiki, T. Iida, H. Imada, M. Inoue, Y. Inoue, K. D. Irwin, H. Ishino, O. Jeong, H. Kanai, D. Kaneko, S. Kashima, N. Katayama, T. Kawasaki, S. A. Kernasovskiy, R. Keskitalo, A. Kibayashi, Y. Kida, K. Kimura, T. Kisner, K. Kohri, E. Komatsu, K. Komatsu, C. L. Kuo, N. A. Kurinsky, A. Kusaka, A. Lazarian, A. T. Lee, D. Li, E. Linder, B. Maffei, A. Mangilli, M. Maki, T. Matsumura, S. Matsuura, D. Meilhan, S. Mima, Y. Minami, K. Mitsuda, L. Montier, M. Nagai, T. Nagasaki, R. Nagata, M. Nakajima, S. Nakamura, T. Namikawa, M. Naruse, H. Nishino, T. Nitta, T. Noguchi, H. Ogawa, S. Oguri, N. Okada, A. Okamoto, T. Okamura, C. Otani, G. Patanchon, G. Pisano, G. Rebeiz, M. Remazeilles, P. L. Richards, S. Sakai, Y. Sakurai, Y. Sato, N. Sato, M. Sawada, Y. Segawa, Y. Sekimoto, U. Seljak, B. D. Sherwin, T. Shimizu, K. Shinozaki, R. Stompor, H. Sugai, H. Sugita, J. Suzuki, O. Tajima, S. Takada, R. Takaku, S. Takakura, S. Takatori, D. Tanabe, E. Taylor, K. L. Thompson, B. Thorne, T. Tomaru, T. Tomida, N. Tomita, M. Tristram, C. Tucker, P. Turin, M. Tsujimoto, S. Uozumi, S. Utsunomiya, Y. Uzawa, F. Vansyngel, I. K. Wehus, B. Westbrook, M. Willer, N. Whitehorn, Y. Yamada, R. Yamamoto, N. Yamasaki, T. Yamashita, M. Yoshida, 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), 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), 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)), 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 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 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 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 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)-Université de Cergy Pontoise (UCP), 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), 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 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), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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
Cosmic microwave background, FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Radio spectrum, law.invention, Antenna array, Telescope, Optics, bolometer, Settore FIS/05 - Astronomia e Astrofisica, law, Polarization, 0103 physical sciences, B-mode, Inflation, Satellite, General Materials Science, [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, activity report, detector: design, Physics, 010308 nuclear & particles physics, business.industry, Gravitational wave, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Condensed Matter Physics, Astrophysics - Astrophysics of Galaxies, Atomic and Molecular Physics, and Optics, cryogenics, Astrophysics of Galaxies (astro-ph.GA), electronics: readout, interference: quantum, Transition edge sensor, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], business, cosmic background radiation: anisotropy
Abstract

著者人数: 153名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 羽澄, 昌史; 今田, 大皓; 満田, 和久; 坂井, 真一郎; Tomida, T.; 辻本, 匡弘; Yamamoto, R.; 山崎, 典子）, Accepted: 2018-04-30, 資料番号: SA1180210000

Published
2018

17. Exploring cosmic origins with CORE: Inflation

Author

F. Finelli, M. Bucher, A. Achúcarro, M. Ballardini, N. Bartolo, D. Baumann, S. Clesse, J. Errard, W. Handley, M. Hindmarsh, K. Kiiveri, M. Kunz, A. Lasenby, M. Liguori, D. Paoletti, C. Ringeval, J. Väliviita, B. van Tent, V. Vennin, P. Ade, R. Allison, F. Arroja, M. Ashdown, A.J. Banday, R. Banerji, J.G. Bartlett, S. Basak, P. de Bernardis, M. Bersanelli, A. Bonaldi, J. Borril, F.R. Bouchet, F. Boulanger, T. Brinckmann, C. Burigana, A. Buzzelli, Z.-Y. Cai, M. Calvo, C.S. Carvalho, G. Castellano, A. Challinor, J. Chluba, I. Colantoni, A. Coppolecchia, M. Crook, G. D'Alessandro, G. D'Amico, J. Delabrouille, V. Desjacques, G. De Zotti, J.M. Diego, E. Di Valentino, S. Feeney, J.R. Fergusson, R. Fernandez-Cobos, S. Ferraro, F. Forastieri, S. Galli, J. García-Bellido, G. de Gasperis, R.T. Génova-Santos, M. Gerbino, J. González-Nuevo, S. Grandis, J. Greenslade, S. Hagstotz, S. Hanany, D.K. Hazra, C. Hernández-Monteagudo, C. Hervias-Caimapo, M. Hills, E. Hivon, B. Hu, T. Kisner, T. Kitching, E.D. Kovetz, H. Kurki-Suonio, L. Lamagna, M. Lattanzi, J. Lesgourgues, A. Lewis, V. Lindholm, J. Lizarraga, M. López-Caniego, G. Luzzi, B. Maffei, N. Mandolesi, E. Martínez-González, C.J.A.P. Martins, S. Masi, D. McCarthy, S. Matarrese, A. Melchiorri, J.-B. Melin, D. Molinari, A. Monfardini, P. Natoli, M. Negrello, A. Notari, F. Oppizzi, A. Paiella, E. Pajer, G. Patanchon, S.P. Patil, M. Piat, G. Pisano, L. Polastri, G. Polenta, A. Pollo, V. Poulin, M. Quartin, A. Ravenni, M. Remazeilles, A. Renzi, D. Roest, M. Roman, J.A. Rubiño-Martin, L. Salvati, A.A. Starobinsky, A. Tartari, G. Tasinato, M. Tomasi, J. Torrado, N. Trappe, T. Trombetti, M. Tucci, C. Tucker, J. Urrestilla, R. van de Weygaert, P. Vielva, N. Vittorio, K. Young, M. Zannoni, ITA, 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 Lagrange de Paris, Sorbonne Université (SU), 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 Théorique d'Orsay [Orsay] (LPT), 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 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 Nanosciences et Cryogénie (INAC), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), 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, Institut Néel (NEEL), 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]), Université Pierre et Marie Curie - Paris 6 (UPMC), 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), CORE, Department of Physics, Helsinki Institute of Physics, 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), Sorbonne Universités, Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Grenoble Alpes (UGA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), 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 Grenoble Alpes (UGA), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Finelli, F, Bucher, M, Achúcarro, A, Ballardini, M, Bartolo, N, Baumann, D, Clesse, S, Errard, J, Handley, W, Hindmarsh, M, Kiiveri, K, Kunz, M, Lasenby, A, Liguori, M, Paoletti, D, Ringeval, C, Väliviita, J, Tent, B, Vennin, V, Ade, P, Allison, R, Arroja, F, Ashdown, M, Banday, A, Banerji, R, Bartlett, J, Basak, S, de Bernardis, P, Bersanelli, M, Bonaldi, A, Borril, J, Bouchet, F, Boulanger, F, Brinckmann, T, Burigana, C, Buzzelli, A, Cai, Z, Calvo, M, Carvalho, C, Castellano, G, Challinor, A, Chluba, J, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, D'Amico, G, Delabrouille, J, Desjacques, V, Zotti, G, Diego, J, Valentino, E, Feeney, S, Fergusson, J, Fernandez-Cobos, R, Ferraro, S, Forastieri, F, Galli, S, García-Bellido, J, de Gasperis, G, Génova-Santos, R, Gerbino, M, González-Nuevo, J, Grandis, S, Greenslade, J, Hagstotz, S, Hanany, S, Hazra, D, Hernández-Monteagudo, C, Hervias-Caimapo, C, Hills, M, Hivon, E, Hu, B, Kisner, T, Kitching, T, Kovetz, E, Kurki-Suonio, H, Lamagna, L, Lattanzi, M, Lesgourgues, J, Lewis, A, Lindholm, V, Lizarraga, J, López-Caniego, M, Luzzi, G, Maffei, B, Mandolesi, N, Martínez-González, E, Martins, C, Masi, S, Mccarthy, D, Matarrese, S, Melchiorri, A, Melin, J, Molinari, D, Monfardini, A, Natoli, P, Negrello, M, Notari, A, Oppizzi, F, Paiella, A, Pajer, E, Patanchon, G, Patil, S, Piat, M, Pisano, G, Polastri, L, Polenta, G, Pollo, A, Poulin, V, Quartin, M, Ravenni, A, Remazeilles, M, Renzi, A, Roest, D, Roman, M, Rubiño-Martin, J, Salvati, L, Starobinsky, A, Tartari, A, Tasinato, G, Tomasi, M, Torrado, J, Trappe, N, Trombetti, T, Tucci, M, Tucker, C, Urrestilla, J, de Weygaert, R, Vielva, P, Vittorio, N, Young, K, Zannoni, M, Finelli F., Bucher M., Achucarro A., Ballardini M., Bartolo N., Baumann D., Clesse S., Errard J., Handley W., Hindmarsh M., Kiiveri K., Kunz M., Lasenby A., Liguori M., Paoletti D., Ringeval C., Valiviita J., Tent B.V., Vennin V., Ade P., Allison R., Arroja F., Ashdown M., Banday A.J., Banerji R., Bartlett J.G., Basak S., De Bernardis P., Bersanelli M., Bonaldi A., Borril J., Bouchet F.R., Boulanger F., Brinckmann T., Burigana C., Buzzelli A., Cai Z.-Y., Calvo M., Carvalho C.S., Castellano G., Challinor A., Chluba J., Colantoni I., Coppolecchia A., Crook M., D'Alessandro G., D'Amico G., Delabrouille J., Desjacques V., Zotti G.D., Diego J.M., Valentino E.D., Feeney S., Fergusson J.R., Fernandez-Cobos R., Ferraro S., Forastieri F., Galli S., Garcia-Bellido J., De Gasperis G., Genova-Santos R.T., Gerbino M., Gonzalez-Nuevo J., Grandis S., Greenslade J., Hagstotz S., Hanany S., Hazra D.K., Hernandez-Monteagudo C., Hervias-Caimapo C., Hills M., Hivon E., Hu B., Kisner T., Kitching T., Kovetz E.D., Kurki-Suonio H., Lamagna L., Lattanzi M., Lesgourgues J., Lewis A., Lindholm V., Lizarraga J., Lopez-Caniego M., Luzzi G., Maffei B., Mandolesi N., Martinez-Gonzalez E., Martins C.J.A.P., Masi S., McCarthy D., Matarrese S., Melchiorri A., Melin J.-B., Molinari D., Monfardini A., Natoli P., Negrello M., Notari A., Oppizzi F., Paiella A., Pajer E., Patanchon G., Patil S.P., Piat M., Pisano G., Polastri L., Polenta G., Pollo A., Poulin V., Quartin M., Ravenni A., Remazeilles M., Renzi A., Roest D., Roman M., Rubino-Martin J.A., Salvati L., Starobinsky A.A., Tartari A., Tasinato G., Tomasi M., Torrado J., Trappe N., Trombetti T., Tucci M., Tucker C., Urrestilla J., De Weygaert R.V., Vielva P., Vittorio N., Young K., Zannoni M., String Theory (ITFA, IoP, FNWI), High-Energy Frontier, Astronomy, 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]), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-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
cosmological model, reheating, Cosmic microwave background, cosmic background radiation: polarization, SPECTRAL DISTORTIONS, astro-ph.CO, Astrophysics, cosmic background radiation, 7. Clean energy, 01 natural sciences, GRAVITATIONAL-WAVES, law.invention, law, 010303 astronomy & astrophysics, CMBR theory, ination, Astronomy and Astrophysics, CMBR theory, inflation, QC, QB, Physics, COSMIC cancer database, ST/J005673/1, ST/H008586/1, inflation: model, MICROWAVE BACKGROUND ANISOTROPY, Core inflation, Astrophysics - Cosmology and Nongalactic Astrophysics, Big Bang, scale: grand unified theory, Astrophysics and Astronomy, noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), STANDARD MODEL, satellite, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, isocurvature: perturbation, frequency: high, PRIMORDIAL NON-GAUSSIANITY, NO, Telescope, power spectrum: primordial, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, LARGE-SCALE STRUCTURE, 0103 physical sciences, inflation, cosmic string, STFC, MODEL SELECTION, Inflation (cosmology), non-Gaussianity: primordial, ST/K00333X/1, ISOCURVATURE PERTURBATIONS, 010308 nuclear & particles physics, string tension, big bang, inflation: slow-roll approximation, RCUK, Spectral density, 115 Astronomy, Space science, cosmic background radiation: temperature, Cosmic string, detector: sensitivity, angular resolution, 13. Climate action, PRE-BIG-BANG, BAYESIAN-INFERENCE, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmic background radiation: anisotropy
Abstract

We forecast the scientific capabilities to improve our understanding of cosmic inflation of CORE, a proposed CMB space satellite submitted in response to the ESA fifth call for a medium-size mission opportunity. The CORE satellite will map the CMB anisotropies in temperature and polarization in 19 frequency channels spanning the range 60-600 GHz. CORE will have an aggregate noise sensitivity of $1.7 ��$K$\cdot \,$arcmin and an angular resolution of 5' at 200 GHz. We explore the impact of telescope size and noise sensitivity on the inflation science return by making forecasts for several instrumental configurations. This study assumes that the lower and higher frequency channels suffice to remove foreground contaminations and complements other related studies of component separation and systematic effects, which will be reported in other papers of the series "Exploring Cosmic Origins with CORE." We forecast the capability to determine key inflationary parameters, to lower the detection limit for the tensor-to-scalar ratio down to the $10^{-3}$ level, to chart the landscape of single field slow-roll inflationary models, to constrain the epoch of reheating, thus connecting inflation to the standard radiation-matter dominated Big Bang era, to reconstruct the primordial power spectrum, to constrain the contribution from isocurvature perturbations to the $10^{-3}$ level, to improve constraints on the cosmic string tension to a level below the presumptive GUT scale, and to improve the current measurements of primordial non-Gaussianities down to the $f_{NL}^{\rm local} < 1$ level. For all the models explored, CORE alone will improve significantly on the present constraints on the physics of inflation. Its capabilities will be further enhanced by combining with complementary future cosmological observations., Latex 107 pages, revised with updated author list and minor modifications

Published
2018

18. A Multiscale pipeline for the search of string-induced CMB anisotropies

Author

Marzieh Farhang, A. Vafaei Sadr, Christophe Ringeval, François R. Bouchet, S. M. S. Movahed, 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 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 UCL - SST/IRMP - Institut de recherche en mathématique et physique

Subjects
FOS: Computer and information sciences, Gaussian, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, techniques: image processing, Astrophysics, cosmic background radiation, 01 natural sciences, Cosmology, correlation function, 010303 astronomy & astrophysics, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Physics, [PHYS]Physics [physics], density, [ PHYS ] Physics [physics], Astrophysics::Instrumentation and Methods for Astrophysics, early Universe, symbols, large-scale structure of Universe, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.PHYS.PHYS-DATA-AN]Physics [physics]/Physics [physics]/Data Analysis, Statistics and Probability [physics.data-an], Astrophysics - Cosmology and Nongalactic Astrophysics, noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic background radiation, FOS: Physical sciences, inflation: anisotropy, Probability density function, Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (quantum field theory), Statistics - Applications, [ PHYS.PHYS.PHYS-DATA-AN ] Physics [physics]/Physics [physics]/Data Analysis, Statistics and Probability [physics.data-an], symbols.namesake, 0103 physical sciences, C++ string handling, Applications (stat.AP), [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], numerical calculations, cosmic string, theory, Instrumentation and Methods for Astrophysics (astro-ph.IM), methods: statistical, 010308 nuclear & particles physics, string tension, resolution, Astronomy and Astrophysics, methods: data analysis, Cosmic string, angular resolution, Space and Planetary Science, Physics - Data Analysis, Statistics and Probability, string, network, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical, cosmology, Data Analysis, Statistics and Probability (physics.data-an), cosmic background radiation: anisotropy
Abstract

We propose a multi-scale edge-detection algorithm to search for the Gott-Kaiser-Stebbins imprints of a cosmic string (CS) network on the Cosmic Microwave Background (CMB) anisotropies. Curvelet decomposition and extended Canny algorithm are used to enhance the string detectability. Various statistical tools are then applied to quantify the deviation of CMB maps having a cosmic string contribution with respect to pure Gaussian anisotropies of inflationary origin. These statistical measures include the one-point probability density function, the weighted two-point correlation function (TPCF) of the anisotropies, the unweighted TPCF of the peaks and of the up-crossing map, as well as their cross-correlation. We use this algorithm on a hundred of simulated Nambu-Goto CMB flat sky maps, covering approximately $10\%$ of the sky, and for different string tensions $G\mu$. On noiseless sky maps with an angular resolution of $0.9'$, we show that our pipeline detects CSs with $G\mu$ as low as $G\mu\gtrsim 4.3\times 10^{-10}$. At the same resolution, but with a noise level typical to a CMB-S4 phase II experiment, the detection threshold would be to $G\mu\gtrsim 1.2 \times 10^{-7}$., Comment: 13 pages, 5 figures, 1 table, Comments are welcome

Published
2018

19. Polarized anisotropic spectral distortions of the CMB: Galactic and extragalactic constraints on photon-axion conversion

Author

Rishi Khatri, Benjamin D. Wandelt, Suvodip Mukherjee, 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, Sorbonne Université (SU), Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
High Energy Physics - Theory, electron, Photon, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, magnetic field: galaxy, 01 natural sciences, symbols.namesake, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Planck, Anisotropy, 010303 astronomy & astrophysics, Axion, pseudoscalar, Physics, magnetic field: turbulence, 010308 nuclear & particles physics, pseudoscalar particle, photon, magnetic field: primordial, Astronomy and Astrophysics, calibration, Galaxy, Magnetic field, coherence, photon axion: coupling, Pseudoscalar, High Energy Physics - Phenomenology, transverse, scalar particle, High Energy Physics - Theory (hep-th), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], symbols, spectral, axion-like particles, [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], axion: mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], signature, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic background radiation: anisotropy
Abstract

We revisit the cosmological constraints on resonant and non-resonant conversion of photons to axions in the cosmological magnetic fields. We find that the constraints on photon-axion coupling and primordial magnetic fields are much weaker than previously claimed for low mass axion like particles with masses $m_{\rm a} \lesssim 5\times 10^{-13}\,\text{eV}$. In particular we find that the axion mass range $10^{-14}\,\text{eV} \le m_{\rm a} \le 5\times 10^{-13}\,\text{eV}$ is not excluded by the CMB data contrary to the previous claims. We also examine the photon-axion conversion in the Galactic magnetic fields. Resonant conversion in the large scale coherent Galactic magnetic field results in $100\%$ polarized anisotropic spectral distortions of the CMB for the mass range $10^{-13}\,\text{eV} \lesssim m_{\rm a} \lesssim 10^{-11}\,\text{eV}$. The polarization pattern traces the transverse to line of sight component of the Galactic magnetic field while both the anisotropy in the Galactic magnetic field and electron distribution imprint a characteristic anisotropy pattern in the spectral distortion. Our results apply to scalar as well as pseudoscalar particles. For conversion to scalar particles, the polarization is rotated by $90^{\circ}$ allowing us to distinguish them from the pseudoscalars. For $m_{\rm a} \lesssim 10^{-14} \,\text{eV}$ we have non-resonant conversion in the small scale turbulent magnetic field of the Galaxy resulting in anisotropic but unpolarized spectral distortion in the CMB. These unique signatures are potential discriminants against the isotropic and non-polarized signals such as primary CMB, and $\mu$ and $y$ distortions with the anisotropic nature making it accessible to experiments with only relative calibration like Planck, LiteBIRD, and CORE. We forecast for PIXIE as well as for these experiments using Fisher matrix formalism., Comment: 36 pages, 11 figures, 2 tables. Matches the published version

Published
2018

20. Planck 2018 results. X. Constraints on inflation

Author

Planck Collaboration, Akrami, Y., Arroja, F., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A. J., Barreiro, R. B., Bartolo, N., Basak, S., Benabed, K., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bock, J. J., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bucher, M., Burigana, C., Butler, R. C., Calabrese, E., Cardoso, J. -F., Carron, J., Challinor, A., Chiang, H. C., Colombo, L. P. L., Combet, C., Contreras, D., Crill, B. P., Cuttaia, F., de Bernardis, P., de Zotti, G., Delabrouille, J., Delouis, J. -M., Di Valentino, E., Diego, J. M., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Dusini, S., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Fantaye, Y., Fergusson, J., Fernandez-Cobos, R., Finelli, F., Forastieri, F., Frailis, M., Franceschi, E., Frolov, A., Galeotta, S., Galli, S., Ganga, K., Gauthier, C., Génova-Santos, R. T., Gerbino, M., Ghosh, T., González-Nuevo, J., Górski, K. M., Gratton, S., Gruppuso, A., Gudmundsson, J. E., Hamann, J., Handley, W., Hansen, F. K., Herranz, D., Hivon, E., Hooper, D. C., Huang, Z., Jaffe, A. H., Jones, W. C., Keihänen, E., Keskitalo, R., Kiiveri, K., Kim, J., Kisner, T. S., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Jeune, M. Le, Lesgourgues, J., Levrier, F., Lewis, A., Liguori, M., Lilje, P. B., Lindholm, V., Lpez-Caniego, M., Lubin, P. M., Ma, Y. -Z., Macías-Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Marcos-Caballero, A., Maris, M., Martin, P. G., Martínez-González, E., Matarrese, S., Mauri, N., McEwen, J. D., Meerburg, P. D., Meinhold, P. R., Melchiorri, A., Mennella, A., Migliaccio, M., Mitra, S., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Moss, A., Münchmeyer, M., Natoli, P., Nørgaard-Nielsen, H. U., Pagano, L., Paoletti, D., Partridge, B., Patanchon, G., Peiris, H. V., Perrotta, F., Pettorino, V., Piacentini, F., Polastri, L., Polenta, G., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rosset, C., Roudier, G., Rubiño-Martín, J. A., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Shellard, E. P. S., Shiraishi, M., Sirignano, C., Sirri, G., Spencer, L. D., Sunyaev, R., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Trombetti, T., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., White, S. D. M., Zacchei, A., Zibin, J. P., Zonca, A., Universidad de Cantabria, Institut de recherche en astrophysique et planétologie (IRAP), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - 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)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-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), 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), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2020-....] (Grenoble INP [2020-....]), Université Grenoble Alpes [2020-....] (UGA [2020-....]), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), 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), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Planck, 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), Computing and Mathematical Sciences [Pasadena]], California Institute of Technology (CALTECH), Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), 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), 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), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), 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 national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Fisica 'G. Galilei', Università degli Studi di Padova = University of Padua (Unipd), University of Cambridge [UK] (CAM), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), 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), University College of London [London] (UCL), University of Manchester [Manchester], University of British Columbia (UBC), Planck Collaboration, Department of Physics, Helsinki Institute of Physics, Astronomy, 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), PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), 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 Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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 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), École normale supérieure - Paris (ENS Paris), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), Universita degli Studi di Padova, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Ministerio de Economía y Competitividad (España), Consejo Superior de Investigaciones Científicas (España), European Commission, European Research Council, European Space Agency, Department of Applied Physics, Aalto-yliopisto, Aalto University, Akrami Y., Arroja F., Ashdown M., Aumont J., Baccigalupi C., Ballardini M., Banday A.J., Barreiro R.B., Bartolo N., Basak S., Benabed K., Bernard J.-P., Bersanelli M., Bielewicz P., Bock J.J., Bond J.R., Borrill J., Bouchet F.R., Boulanger F., Bucher M., Burigana C., Butler R.C., Calabrese E., Cardoso J.-F., Carron J., Challinor A., Chiang H.C., Colombo L.P.L., Combet C., Contreras D., Crill B.P., Cuttaia F., De Bernardis P., De Zotti G., Delabrouille J., Delouis J.-M., Di Valentino E., Diego J.M., Donzelli S., Dore O., Douspis M., Ducout A., Dupac X., Dusini S., Efstathiou G., Elsner F., Ensslin T.A., Eriksen H.K., Fantaye Y., Fergusson J., Fernandez-Cobos R., Finelli F., Forastieri F., Frailis M., Franceschi E., Frolov A., Galeotta S., Galli S., Ganga K., Gauthier C., Genova-Santos R.T., Gerbino M., Ghosh T., Gonzalez-Nuevo J., Gorski K.M., Gratton S., Gruppuso A., Gudmundsson J.E., Hamann J., Handley W., Hansen F.K., Herranz D., Hivon E., Hooper D.C., Huang Z., Jaffe A.H., Jones W.C., Keihanen E., Keskitalo R., Kiiveri K., Kim J., Kisner T.S., Krachmalnicoff N., Kunz M., Kurki-Suonio H., Lagache G., Lamarre J.-M., Lasenby A., Lattanzi M., Lawrence C.R., Le Jeune M., Lesgourgues J., Levrier F., Lewis A., Liguori M., Lilje P.B., Lindholm V., Lopez-Caniego M., Lubin P.M., Ma Y.-Z., Macias-Perez J.F., Maggio G., Maino D., Mandolesi N., Mangilli A., Marcos-Caballero A., Maris M., Martin P.G., Martinez-Gonzalez E., Matarrese S., Mauri N., McEwen J.D., Meerburg P.D., Meinhold P.R., Melchiorri A., Mennella A., Migliaccio M., Mitra S., Miville-Deschenes M.-A., Molinari D., Moneti A., Montier L., Morgante G., Moss A., Munchmeyer M., Natoli P., Norgaard-Nielsen H.U., Pagano L., Paoletti D., Partridge B., Patanchon G., Peiris H.V., Perrotta F., Pettorino V., Piacentini F., Polastri L., Polenta G., Puget J.-L., Rachen J.P., Reinecke M., Remazeilles M., Renzi A., Rocha G., Rosset C., Roudier G., Rubino-Martin J.A., Ruiz-Granados B., Salvati L., Sandri M., Savelainen M., Scott D., Shellard E.P.S., Shiraishi M., Sirignano C., Sirri G., Spencer L.D., Sunyaev R., Suur-Uski A.-S., Tauber J.A., Tavagnacco D., Tenti M., Toffolatti L., Tomasi M., Trombetti T., Valiviita J., Van Tent B., Vielva P., Villa F., Vittorio N., Wandelt B.D., Wehus I.K., White S.D.M., Zacchei A., Zibin J.P., Zonca A., and ITA

Subjects
cosmological model, inflaton: potential, Astronomy, cosmic background radiation: polarization, cosmic background radiation, Cosmic background radiation, 01 natural sciences, 7. Clean energy, expansion: multipole, Cosmic background radiation - Inflation, 010303 astronomy & astrophysics, Settore FIS/05, slow-roll approximation, Cosmic background radiation, Inflation, BICEP, inflation: model, perturbation: scalar, DENSITY PERTURBATIONS, scale dependence, astro-ph.CO, Astrophysics - Cosmology and Nongalactic Astrophysics, temperature: anisotropy, satellite: Planck, Cosmology and Nongalactic Astrophysics (astro-ph.CO), NATURAL INFLATION, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, NO, power spectrum: primordial, power spectrum: scalar, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, 0103 physical sciences, LARGE-SCALE STRUCTURE, inflation, UNIVERSE SCENARIO, 010308 nuclear & particles physics, ISOCURVATURE PERTURBATIONS, Computer Science::Information Retrieval, fluctuation: primordial, Astronomy and Astrophysics, 115 Astronomy, Space science, Inflation, boundary condition, bispectrum, MICROWAVE BACKGROUND ANISOTROPIES, 13. Climate action, Space and Planetary Science, gravitation, PHASE-TRANSITION, PRE-BIG-BANG, BAYESIAN-INFERENCE, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], BARYON ACOUSTIC-OSCILLATIONS, cosmic background radiation: anisotropy
Abstract

Planck Collaboration: et al., We report on the implications for cosmic inflation of the 2018 release of the Planck cosmic microwave background (CMB) anisotropy measurements. The results are fully consistent with those reported using the data from the two previous Planck cosmological releases, but have smaller uncertainties thanks to improvements in the characterization of polarization at low and high multipoles. Planck temperature, polarization, and lensing data determine the spectral index of scalar perturbations to be ns = 0.9649 ± 0.0042 at 68% CL. We find no evidence for a scale dependence of ns, either as a running or as a running of the running. The Universe is found to be consistent with spatial flatness with a precision of 0.4% at 95% CL by combining Planck with a compilation of baryon acoustic oscillation data. The Planck 95% CL upper limit on the tensor-to-scalar ratio, r0.002 < 0.10, is further tightened by combining with the BICEP2/Keck Array BK15 data to obtain r0.002 < 0.056. In the framework of standard single-field inflationary models with Einstein gravity, these results imply that: (a) the predictions of slow-roll models with a concave potential, V″(ϕ) < 0, are increasingly favoured by the data; and (b) based on two different methods for reconstructing the inflaton potential, we find no evidence for dynamics beyond slow roll. Three different methods for the non-parametric reconstruction of the primordial power spectrum consistently confirm a pure power law in the range of comoving scales 0.005 Mpc−1 ≲ k ≲ 0.2 Mpc−1. A complementary analysis also finds no evidence for theoretically motivated parameterized features in the Planck power spectra. For the case of oscillatory features that are logarithmic or linear in k, this result is further strengthened by a new combined analysis including the Planck bispectrum data. The new Planck polarization data provide a stringent test of the adiabaticity of the initial conditions for the cosmological fluctuations. In correlated, mixed adiabatic and isocurvature models, the non-adiabatic contribution to the observed CMB temperature variance is constrained to 1.3%, 1.7%, and 1.7% at 95% CL for cold dark matter, neutrino density, and neutrino velocity, respectively. Planck power spectra plus lensing set constraints on the amplitude of compensated cold dark matter-baryon isocurvature perturbations that are consistent with current complementary measurements. The polarization data also provide improved constraints on inflationary models that predict a small statistically anisotropic quadupolar modulation of the primordial fluctuations. However, the polarization data do not support physical models for a scale-dependent dipolar modulation. All these findings support the key predictions of the standard single-field inflationary models, which will be further tested by future cosmological observations., The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU).

Published
2018
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21. CMB bounds on disk-accreting massive primordial black holes

Author

Vivian Poulin, Pasquale D. Serpico, Kazunori Kohri, Sebastien Clesse, Francesca Calore, 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 d'Annecy-le-Vieux de Physique Théorique ( LAPTH ), and Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
matter: accretion, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Photon, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Cosmic microwave background, binary, FOS: Physical sciences, Primordial black hole, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, dark matter: parametrization, thermal, Binary black hole, Ionization, ionization, 0103 physical sciences, conservation law, numerical calculations, 010306 general physics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy, Accretion (astrophysics), Dark Ages, nonlinear, Astrophysics::Earth and Planetary Astrophysics, history, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical, black hole: primordial, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic background radiation: anisotropy
Abstract

Stellar-mass Primordial Black Holes (PBH) have been recently reconsidered as a Dark Matter (DM) candidate, after the aLIGO discovery of several binary BH mergers with masses of tens of $M_\odot$. Matter accretion on such massive objects leads to the emission of high-energy photons, capable of altering the ionization and thermal history of the universe. This in turn affects the statistical properties of the cosmic microwave background (CMB) anisotropies. Previous analyses have assumed spherical accretion. We argue that this approximation likely breaks down and that an accretion disk should form in the dark ages. Using the most up-to-date tools to compute the energy deposition in the medium, we derive constraints on the fraction of DM in PBH. Provided that disks form early on, even under conservative assumptions for accretion, these constraints exclude a monochromatic distribution of PBH with masses above $\sim 2\, M_\odot$ as the dominant form of DM. The bound on the median PBH mass gets more stringent if a broad, log-normal mass function is considered. A deepened understanding of non-linear clustering properties and BH accretion disk physics would permit an improved treatment and possibly lead to more stringent constraints., Comment: 13 pages, 5 figures

Published
2017

22. What do Galactic electrons and positrons tell us about dark matter?

Author

Sylvie Rosier, Antje Putze, Sami Caroff, Vivian Poulin, Manuela Vecchi, E. F. Bueno, Yoann Génolini, Julien Lavalle, Mathieu Boudaud, V. Poireau, Pierre Salati, Laboratoire de Physique Théorique et Hautes Energies (LPTHE), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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-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 Univers et Particules de Montpellier (LUPM), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), 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), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2)

Subjects
electron, energy loss, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, Dark matter, halo, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Electron, Astrophysics, 7. Clean energy, magnetic field: solar, Positron, synchrotron, gamma ray: flux, AMS, Physics, cosmic radiation: propagation, Annihilation, shielding, diffusion, Gamma ray, dark matter: annihilation, anti-p, Compton scattering: inverse, Antiproton, positron, Physics::Accelerator Physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmic background radiation: anisotropy
Abstract

International audience; We devise a new semi-analytical method dedicated to the propagation of Galactic electrons and positrons from MeV to TeV energies: the pinching method. It is essentially based on the pinching of inverse Compton and synchrotron energy losses from the magnetic halo, where they take place, inside the Galactic disc. This new tool is fast and allows to carry out extensive scans over parameters. We strongly constrain the cosmic ray propagation parameters by requiring that the secondary component of positrons does not overshoot the AMS-02 measurements. We find that only models with a large diffusion coefficient and a large magnetic halo size are selected by this test. Therefore, we find that the positron excess appears from 1 GeV. We then explore the possibility to explain the positron excess with a component coming from the annihilation of dark matter particles. We show that the pure dark matter interpretation of the AMS-02 positron data is strongly disfavoured. This conclusion is based solely on the positron data, and no other observation, such as the antiproton and gamma ray fluxes or the CMB anisotropies, needs to be invoked. MeV dark matter particles annihilating or decaying to electron-positron pairs cannot, in principle, be observed via local cosmic ray measurements because of the shielding solar magnetic field. We take advantage of spacecraft Voyager-I's capacity for detecting interstellar cosmic rays since it crossed the heliopause in 2012. This opens up a new avenue to probe dark matter particles in the sub-GeV energy/mass range that we exploit here for the first time.

Published
2017

23. Anisotropy of the astrophysical gravitational wave background: Analytic expression of the angular power spectrum and correlation with cosmological observations

Author

Cyril Pitrou, Jean-Philippe Uzan, Giulia Cusin, Institut Lagrange de Paris, Sorbonne Universités, 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), Sorbonne Université (SU), Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
High Energy Physics - Theory, cosmological model, gravitational radiation: stochastic, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics, cosmic background radiation, Correlation function (astronomy), 01 natural sciences, General Relativity and Quantum Cosmology, Cosmology, [ PHYS.HTHE ] Physics [physics]/High Energy Physics - Theory [hep-th], Gravitational wave background, energy: density, correlation function, gravitational radiation: energy, Weak gravitational lensing, media_common, Physics, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], mathematical methods, space-time, power spectrum: angular dependence, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - Cosmology and Nongalactic Astrophysics, Physics::General Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Cosmic background radiation, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, space-time: Robertson-Walker, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], gravitation: lens, 0103 physical sciences, cosmic background radiation: power spectrum, 010306 general physics, numerical calculations, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: background, gravitational radiation, Spectral density, Astrophysics - Astrophysics of Galaxies, Universe, background: stochastic, High Energy Physics - Theory (hep-th), Astrophysics of Galaxies (astro-ph.GA), galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmic background radiation: anisotropy
Abstract

Unresolved and resolved sources of gravitational waves are at the origin of a stochastic gravitational wave background. While the computation of its mean density as a function of frequency in a homogeneous and isotropic universe is standard lore, the computation of its anisotropies requires to understand the coarse graining from local systems, to galactic scales and then to cosmology. An expression of the gravitational wave energy density valid in any general spacetime is derived. It is then specialized to a perturbed Friedmann-Lema\^itre spacetime in order to determine the angular power spectrum of this stochastic background as well as its correlation with other cosmological probes, such as the galaxy number counts and weak lensing. Our result for the angular power spectrum also provides an expression for the variance of the gravitational wave background., Comment: 22 pages, 2 figures

Published
2017

24. Wavelet-Bayesian inference of cosmic strings embedded in the cosmic microwave background

Author

Yves Wiaux, Jason D. McEwen, Stephen M. Feeney, Christophe Ringeval, F. R. Bouchet, Hiranya V. Peiris, 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), UCL - SST/IRMP - Institut de recherche en mathématique et physique, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
data analysis method, cosmological model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, Posterior probability, Cosmic background radiation, FOS: Physical sciences, Lambda-CDM model, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, Bayesian inference, 01 natural sciences, String (physics), statistics: Bayesian, Theoretical physics, High Energy Physics::Theory, Wavelet, wavelet, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], cosmic string, 010303 astronomy & astrophysics, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, methods: statistical, 010308 nuclear & particles physics, string tension, mathematical methods, Astronomy and Astrophysics, methods: data analysis, Cosmic string, Space and Planetary Science, cosmology: cosmic background radiation, cosmology: observations, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], performance, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic background radiation: anisotropy
Abstract

Cosmic strings are a well-motivated extension to the standard cosmological model and could induce a subdominant component in the anisotropies of the cosmic microwave background (CMB), in addition to the standard inflationary component. The detection of strings, while observationally challenging, would provide a direct probe of physics at very high energy scales. We develop a new framework for cosmic string inference, constructing a Bayesian analysis in wavelet space where the string-induced CMB component has distinct statistical properties to the standard inflationary component. Our wavelet-Bayesian framework provides a principled approach to compute the posterior distribution of the string tension $G\mu$ and the Bayesian evidence ratio comparing the string model to the standard inflationary model. Furthermore, we present a technique to recover an estimate of any string-induced CMB map embedded in observational data. Using Planck-like simulations we demonstrate the application of our framework and evaluate its performance. The method is sensitive to $G\mu \sim 5 \times 10^{-7}$ for Nambu-Goto string simulations that include an integrated Sachs-Wolfe (ISW) contribution only and do not include any recombination effects, before any parameters of the analysis are optimised. The sensitivity of the method compares favourably with other techniques applied to the same simulations., Comment: 18 pages, 14 figures, minor changes to match version accepted by MNRAS

Published
2017

25. BICEP2 / Keck Array IX: New bounds on anisotropies of CMB polarization rotation and implications for axionlike particles and primordial magnetic fields

Author

Array, Keck, Bicep, Collaborations, 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., Crill, B. P., Duband, L., Dvorkin, C., Filippini, J. P., Fliescher, S., St Germaine, T., Ghosh, T., Grayson, J., 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., Leitch, E. M., Megerian, K. G., Moncelsi, L., Namikawa, T., Netterfield, C. B., Nguyen, H. T., O Brient, R., Ogburn, R. W., Pryke, C., Richter, S., Schillaci, A., Schwarz, R., Sheehy, C. D., Staniszewski, Z. K., Steinbach, B., Sudiwala, R. V., Teply, G. P., Thompson, K. L., Tolan, J. E., Carole Tucker, Turner, A. D., Vieregg, A. G., Weber, A. C., Wiebe, D. V., Willmert, J., Wong, C. L., Wu, W. L. K., Yoon, K. W., Institut Nanosciences et Cryogénie (INAC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), BICEP2, Keck Arrary, Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-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 Nanosciences et Cryogénie ( INAC ), and Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Grenoble Alpes ( UGA )

Subjects
cosmological model, Photon, Cosmology and Nongalactic Astrophysics (astro-ph.CO), polarization: anisotropy, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics, 01 natural sciences, Electromagnetic radiation, High Energy Physics - Experiment, polarization: rotation, symbols.namesake, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), statistical analysis, [ PHYS.HEXP ] Physics [physics]/High Energy Physics - Experiment [hep-ex], 0103 physical sciences, Faraday effect, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], inflation, 010306 general physics, QC, QB, Physics, Brewster's angle, 010308 nuclear & particles physics, Chern-Simons term, coupling constant, magnetic field: primordial, Fine-structure constant, photon: interaction, Polarization (waves), BICEP, detector: sensitivity, High Energy Physics - Phenomenology, Amplitude, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], symbols, power spectrum: angular dependence, axion-like particles, [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], S029IAG, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic background radiation: anisotropy
Abstract

We present the strongest constraints to date on anisotropies of cosmic microwave background (CMB) polarization rotation derived from 150 GHz data taken by the BICEP2/Keck Array CMB experiments up to and including the 2014 observing season (BK14). The definition of the polarization angle in BK14 maps has gone through self-calibration in which the overall angle is adjusted to minimize the observed TB and EB power spectra. After this procedure, the QU maps lose sensitivity to a uniform polarization rotation but are still sensitive to anisotropies of polarization rotation. This analysis places constraints on the anisotropies of polarization rotation, which could be generated by CMB photons interacting with axionlike pseudoscalar fields or Faraday rotation induced by primordial magnetic fields. The sensitivity of BK14 maps ($\sim 3\mu$K-arcmin) makes it possible to reconstruct anisotropies of the polarization rotation angle and measure their angular power spectrum much more precisely than previous attempts. Our data are found to be consistent with no polarization rotation anisotropies, improving the upper bound on the amplitude of the rotation angle spectrum by roughly an order of magnitude compared to the previous best constraints. Our results lead to an order of magnitude better constraint on the coupling constant of the Chern-Simons electromagnetic term $g_{a\gamma}\leq 7.2\times 10^{-2}/H_I$ (95% confidence) than the constraint derived from the B-mode spectrum, where $H_I$ is the inflationary Hubble scale. This constraint leads to a limit on the decay constant of $10^{-6}\lesssim f_a/M_{\rm pl}$ at mass range of $10^{-33}< m_a< 10^{-28}$ eV for $r=0.01$, assuming $g_{a\gamma}\sim\alpha/(2\pi f_a)$ with $\alpha$ denoting the fine structure constant. The upper bound on the amplitude of the primordial magnetic fields is 30nG (95% confidence) from the polarization rotation anisotropies., Comment: 6 pages, 2 figures

Published
2017

26. 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

27. The perturbed universe in the deformed algebra approach of Loop Quantum Cosmology

Author

J. Grain, 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 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 ), and Université Paris-Sud - Paris 11 ( UP11 )

Subjects
algebra: deformation, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, 98.80.Jk, 01 natural sciences, General Relativity and Quantum Cosmology, correction: quantum, 04.60.Pp, Mathematical Physics, media_common, Physics, Quantum cosmology, power spectrum: anisotropy, B-mode, space-time, bounce: quantum, power spectrum: angular dependence, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], 98.80.Qc, history, 04.60.Ds, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, Canonical quantization, perturbation, media_common.quotation_subject, FOS: Physical sciences, 04.60.Bc, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Loop quantum gravity, quantum cosmology: loop space, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], power spectrum: primordial, power spectrum: scalar, 0103 physical sciences, 010306 general physics, Loop quantum cosmology, Spacetime, 010308 nuclear & particles physics, background, Astronomy and Astrophysics, Universe, boundary condition, Algebra, Space and Planetary Science, quantum gravity, Quantum gravity, quantization, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], quantum gravity: loop space, cosmic background radiation: anisotropy
Abstract

Loop quantum cosmology is a tentative approach to model the universe down to the Planck era where quantum gravity settings are needed. The quantization of the universe as a dynamical space-time is inspired by Loop Quantum Gravity ideas. In addition, loop quantum cosmology could bridge contact with astronomical observations, and thus potentially investigate quantum cosmology modellings in the light of observations. To do so however, modelling both the background evolution and its perturbations is needed. The latter describe cosmic inhomogeneities that are the main cosmological observables. In this context, we present the so-called deformed algebra approach implementing the quantum corrections to the perturbed universe at an effective level by taking great care of gauge issues. We particularly highlight that in this framework, the algebra of hypersurface deformation receives quantum corrections, and we discuss their meaning. The primordial power spectra of scalar and tensor inhomogeneities are then presented, assuming initial conditions are set in the contracting phase preceding the quantum bounce and the well-known expanding phase of the cosmic history. These spectra are subsequently propagated to angular power spectra of the anisotropies of the cosmic microwave background. It is then shown that regardless of the choice for the initial conditions inside the effective approach for the background evolution (except that they are set in the contracting phase), the predicted angular power spectra of the polarized B-modes exceed the upper bound currently set by observations. The exclusion of this specific version of loop quantum cosmology establishes the falsifiability of the approach, though one shall not conclude here that either loop quantum cosmology or loop quantum gravity is excluded., Comment: Invited paper for a special issue of IJMPD on Loop Quantum Cosmology

Published
2016

28. Recent results and perspectives on cosmology and fundamental physics from microwave surveys

Author

Carlo, Burigana, Battistelli, Elia Stefano, Micol, Benetti, Cabass, Giovanni, DE BERNARDIS, Paolo, Sperello Di Serego Alighieri, Eleonora Di Valentino, Gerbino, Martina, Elena, Giusarma, Alessandro, Gruppuso, Michele, Liguori, Masi, Silvia, Hans Ulrik Norgaard Nielsen, Piero, Rosati, Laura, Salvati, Tiziana, Trombetti, Patricio, Vielva, Benetti, Micol, DI VALENTINO, Eleonora, Giusarma, Elena, Salvati, Laura, 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), Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, 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 ), Bianchi, Massimo, Jantzen, Robert T., and Ruffini, Remo

Subjects
Observational cosmology, Background radiations, cosmological model, background radiations, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], 98.80.Bp, Cosmic microwave background, Particle-theory and field-theory models of the early universe, Astrophysics, 01 natural sciences, 7. Clean energy, Cosmology, observational cosmology, particle-theory and field-theory models of the early universe, Dark energy, general relativity, Elementary particle processes, neutrino: mass, Large scale structure of the universe, dark energy, 010303 astronomy & astrophysics, Mathematical Physics, media_common, Physics, COSMIC cancer database, perturbation: primordial, dark matter, elementary particle processes, large scale structure of the universe, microwave, origin and formation of the universe, radio, Astronomy and Astrophysics, Space and Planetary Science, 98.80.Es, Origin and formation of the universe, 95.36.+x, inflation: model, 98.70.Vc, Sachs-Wolfe effect, equivalence principle, non-Gaussianity, axion: thermal, 95.35.+d, axion: mass, Neutrino, signature, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, 95.85.Bh, multipole, FOS: Physical sciences, Lambda-CDM model, Astrophysics::Cosmology and Extragalactic Astrophysics, NO, polarization: rotation, power spectrum: primordial, 95.30.Cq, 0103 physical sciences, 98.80.−k, Dark matter, n: lifetime, Axion, 010308 nuclear & particles physics, 98.80.Cq, Radio, Universe, Galaxy, galaxy, 98.65.Dx, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Microwave, cosmic background radiation: anisotropy
Abstract

Based on presentations at the Fourteenth Marcel Grossmann Meeting on General Relativity, Rome, July 2015.-- et al., arXiv:1604.03819v1, Recent cosmic microwave background (CMB) data in temperature and polarization have reached high precision in estimating all the parameters that describe the current so-called standard cosmological model. Recent results about the integrated Sachs-Wolfe (ISW) effect from CMB anisotropies, galaxy surveys, and their cross-correlations are presented. Looking at fine signatures in the CMB, such as the lack of power at low multipoles, the primordial power spectrum (PPS) and the bounds on non-Gaussianities, complemented by galaxy surveys, we discuss inflationary physics and the generation of primordial perturbations in the early universe. Three important topics in particle physics, the bounds on neutrinos masses and parameters, on thermal axion mass and on the neutron lifetime derived from cosmological data are reviewed, with attention to the comparison with laboratory experiment results. Recent results from cosmic polarization rotation (CPR) analyses aimed at testing the Einstein equivalence principle (EEP) are presented. Finally, we discuss the perspectives of next radio facilities for the improvement of the analysis of future CMB spectral distortion experiments., CB, AG, ML and TT acknowledge partial support by ASI/INAF Agreement 2014-024-R.0 for the Planck LFI Activity of Phase E2.

Published
2016

29. The binned bispectrum estimator: template-based and non-parametric CMB non-Gaussianity searches

Author

Martin Bucher, Bartjan van Tent, B. Racine, 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 ), Laboratoire de Physique Théorique d'Orsay [Orsay] ( LPT ), Université Paris-Sud - Paris 11 ( UP11 ) -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 Paris Cité (UPCité), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-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), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), 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
noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, FOS: Physical sciences, cosmic background radiation: polarization, parametric, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, estimator, symbols.namesake, Non-Gaussianity, 0103 physical sciences, CMBR experiments, correlation function, Planck, 010303 astronomy & astrophysics, Parametric statistics, Physics, 010308 nuclear & particles physics, Nonparametric statistics, Estimator, Astronomy and Astrophysics, CMBR theory, coherence, cosmic background radiation: temperature, bispectrum, symbols, non-gaussianity, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Algorithm, Bispectrum, Smoothing, cosmic background radiation: anisotropy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We describe the details of the binned bispectrum estimator as used for the official 2013 and 2015 analyses of the temperature and polarization CMB maps from the ESA Planck satellite. The defining aspect of this estimator is the determination of a map bispectrum (3-point correlator) that has been binned in harmonic space. For a parametric determination of the non-Gaussianity in the map (the so-called fNL parameters), one takes the inner product of this binned bispectrum with theoretically motivated templates. However, as a complementary approach one can also smooth the binned bispectrum using a variable smoothing scale in order to suppress noise and make coherent features stand out above the noise. This allows one to look in a model-independent way for any statistically significant bispectral signal. This approach is useful for characterizing the bispectral shape of the galactic foreground emission, for which a theoretical prediction of the bispectral anisotropy is lacking, and for detecting a serendipitous primordial signal, for which a theoretical template has not yet been put forth. Both the template-based and the non-parametric approaches are described in this paper., Latex 42 pages with 10 figures and JCAP macros. v2: corrected small mistake in section 5.3, changed colour scale of slice figures, other minor changes and additions, matches published version

Published
2015

30. CMB observations in 2015: A status report

Author

Martin Bucher, 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), Planck, 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, 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
Nuclear and High Energy Physics, Age of the universe, Physics beyond the Standard Model, Cosmic microwave background, Cosmic background radiation, cosmic background radiation: polarization, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, power spectrum, 01 natural sciences, Early Universe, symbols.namesake, Cosmic Inflation, 0103 physical sciences, Planck, inflation, 010306 general physics, activity report, Inflation (cosmology), Physics, 010308 nuclear & particles physics, new physics, scale: Planck, Spectral density, Astronomy, boundary condition, cosmic background radiation: temperature, Cosmic neutrino background, B-mode, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmic background radiation: anisotropy
Abstract

International audience; Observations of the cosmic microwave background (CMB) anisotropies in temperature and polarization allow us to characterize the initial conditions of the universe, thus constraining new physics many orders of magnitude beyond the particle physics Standard Model and possibly just a few orders of magnitude below the Planck scale. We briefly review the physics of the CMB and present some recent highlights of the current observations of the T and E modes. The status of B mode searches is also briefly reviewed. Finally, the future of CMB observations is discussed, indicating several areas where qualitative advances may be expected.

Published
2014

31. Global fits for the spectral index of the cosmological curvature perturbation

Author

Covi, Laura and Lyth, David H.

Subjects
numerical calculations: interpretation of experiments, cosmological constant, correlation function: galaxy, space-time: perturbation, ionization, baryon: density, inflation, matter: density, dark matter, spectrum, cosmic background radiation: anisotropy
Abstract

Monthly notices of the Royal Astronomical Society 326(3), 885 - 893 (2001). doi:10.1046/j.1365-8711.2001.04466.x, Best-fit values of the spectral index of the curvature perturbation are presented, assuming the $\Lambda$CDM cosmology. Apart from the spectral index, the parameters are the Hubble parameter, the total matter density and the baryon density. The data points are intended to represent all measurements which are likely to significantly affect the result. The cosmic microwave anisotropy is represented by the COBE normalization, and heights of the first and second peaks given by the latest Boomerang and Maxima data. Quantities $\widetilde \Gamma$ and $\widetilde\sigma_8$ represent galaxy and cluster observations, and expected values of the Hubble parameter $h$ and matter density $\Omega_0$ summarize several other observations (not related to large-scale structure). The `low-deuterium' nucleosynthesis value of the baryon density is taken as data, the fit giving a value about one standard deviation higher. The results are insensitive to the reionization epoch, because this epoch is calculated from the model by assuming that it corresponds to the collapse of a fraction $f\sigma 10^{-4}$ of matter. We consider the case of a scale-independent spectral index, and also the scale-dependent spectral index predicted by running mass models of inflation. In the former case, the result is compared with the prediction of models of inflation based on effective field theory, in which the field value is small on the Planck scale, and it is argued that only these models have at present good theoretical motivation., Published by Oxford Univ. Press, Oxford

Published
2001
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32. Dark Energy Survey Year 1 Results: A Precise H0 Measurement from DES Y1, BAO, and D/H Data

Author

G. Gutierrez, A. Roodman, Tommaso Giannantonio, Elisabeth Krause, Alistair R. Walker, Flavia Sobreira, B. Flaugher, Marcelle Soares-Santos, Bhuvnesh Jain, Daniel Scolnic, Joseph J. Mohr, Tesla E. Jeltema, C. Davis, M. D. Johnson, David J. James, M. March, Enrique J. Fernández, J. Gschwend, Bradford Benson, Enrique Gaztanaga, Erin Sheldon, Gary Bernstein, Marvin Johnson, Jennifer L. Marshall, Ofer Lahav, Pablo Fosalba, J. Annis, Youngsoo Park, Ramon Miquel, R. A. Bernstein, V. Scarpine, T. Natoli, Joe Zuntz, David J. Brooks, A. Manzotti, Huan Lin, Keith Bechtol, Eli S. Rykoff, Peter Nugent, W. C. Wester, I. Sevilla-Noarbe, E. Bertin, R. C. Smith, C. B. D'Andrea, N. Kuropatkin, A. A. Plazas, Daniel Thomas, Risa H. Wechsler, Michael Schubnell, Peter Doel, S. E. Kuhlmann, Alex Drlica-Wagner, Dragan Huterer, L. N. da Costa, Andrew R. Liddle, Ashley J. Ross, Jonathan Blazek, A. Carnero Rosell, J. Carretero, Daniel Gruen, Marcos Lima, D. L. Burke, T. M. Crawford, Shantanu Desai, Michael Troxel, Jason W. Henning, M. Carrasco Kind, Matt J. Jarvis, G. Tarle, H. T. Diehl, Christian L. Reichardt, W. L. K. Wu, F. B. Abdalla, Niall MacCrann, Chihway Chang, M. A. G. Maia, E. Suchyta, D. W. Gerdes, August E. Evrard, Mathew Smith, J. P. Dietrich, Juan Garcia-Bellido, Carlos E. Cunha, Eduardo Rozo, Robert A. Gruendl, W. G. Hartley, K. Honscheid, Jochen Weller, F. J. Castander, Joshua A. Frieman, Kevin Reil, T. M. C. Abbott, Ricardo L. C. Ogando, J. DeRose, Ben Hoyle, E. J. Sanchez, Kyler Kuehn, 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), DES, UAM. Departamento de Física Teórica, and Instituto de Física Teórica (IFT)

Subjects
cosmological model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), nucleosynthesis: big bang, Cosmic microwave background, FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, baryon: oscillation: acoustic, distance scale, 01 natural sciences, 7. Clean energy, symbols.namesake, Big Bang nucleosynthesis, statistical analysis, gravitation: lens, 0103 physical sciences, neutrino: mass, cosmological parameters, dark energy, 010303 astronomy & astrophysics, STFC, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Physics, Hubble constant, 010308 nuclear & particles physics, Cosmic distance ladder, RCUK, Física, Astronomy and Astrophysics, observations [cosmology], cosmic background radiation: temperature, 13. Climate action, Space and Planetary Science, cosmology: observations, Dark energy, symbols, Baryon acoustic oscillations, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hubble's law, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic background radiation: anisotropy
Abstract

We combine Dark Energy Survey Year 1 clustering and weak lensing data with Baryon Acoustic Oscillations (BAO) and Big Bang Nucleosynthesis (BBN) experiments to constrain the Hubble constant. Assuming a flat $\Lambda$CDM model with minimal neutrino mass ($\sum m_\nu = 0.06$ eV) we find $H_0=67.2^{+1.2}_{-1.0}$ km/s/Mpc (68% CL). This result is completely independent of Hubble constant measurements based on the distance ladder, Cosmic Microwave Background (CMB) anisotropies (both temperature and polarization), and strong lensing constraints. There are now five data sets that: a) have no shared observational systematics; and b) each constrain the Hubble constant with a few percent level precision. We compare these five independent measurements, and find that, as a set, the differences between them are significant at the $2.1\sigma$ level ($\chi^2/dof=20.1/11$, probability to exceed=4%). This difference is low enough that we consider the data sets statistically consistent with each other. The best fit Hubble constant obtained by combining all five data sets is $H_0 = 69.1^{+0.4}_{-0.6}$ km/s/Mpc., Comment: 11 pages, 2 figures

33. Planck 2018 results, X. Constraints on inflation

Author

Akrami, Y., Arroja, F., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A. J., Barreiro, R. B., Bartolo, N., Basak, S., Benabed, K., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bock, J. J., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bucher, M., Burigana, C., Butler, R. C., Calabrese, E., Cardoso, J.-F., Carron, J., Challinor, A., Chiang, H. C., Colombo, L. P. L., Combet, C., Contreras, D., Crill, B. P., Cuttaia, F., De Bernardis, Paolo, De Zotti, Gianfranco, Delabrouille, J., Delouis, J.-M., Di Valentino, Eleonora, Diego, J. M., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Dusini, S., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Fantaye, Y., Fergusson, J., Fernandez-Cobos, R., Finelli, F., Forastieri, F., Frailis, M., Franceschi, E., Frolov, A., Galeotta, S., Galli, S., Ganga, K., Gauthier, C., Génova-Santos, R. T., Gerbino, M., Ghosh, T., González-Nuevo, Joaquin, Górski, K. M., Gratton, S., Gruppuso, A., Gudmundsson, J. E., Hamann, J., Handley, W., Hansen, F. K., Herranz, D., Hivon, E., Hooper, Deanna Charlotte, Huang, Z., Jaffe, A. H., Jones, W. C., Keihänen, E., Keskitalo, R., Kiiveri, K., Kim, J., Kisner, T. S., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J.-M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Le Jeune, M., Lesgourgues, Julien, Levrier, F., Lewis, A., Liguori, M., Lilje, P. B., Lindholm, V., López-Caniego, Marcos, Lubin, P. M., Ma, Y.-Z., Macías-Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Marcos-Caballero, A., Maris, M., Martin, P. G., Martínez-González, E., Matarrese, S., Mauri, N., McEwen, J. D., Meerburg, P. D., Meinhold, P. R., Melchiorri, A., Mennella, A., Migliaccio, M., Mitra, S., Miville-Deschênes, M. A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Moss, A., Münchmeyer, M., Natoli, P., Nørgaard-Nielsen, H. U., Pagano, L., Paoletti, D., Partridge, B., Patanchon, G., Peiris, H. V., Perrotta, F., Pettorino, V., Piacentini, F., Polastri, L., Polenta, G., Puget, J.-L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rosset, C., Roudier, G., Rubiño-Martín, Jose Alberto, Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Shellard, E. P. S., Shiraishi, M., Sirignano, C., Sirri, G., Spencer, L. D., Sunyaev, R., Suur-Uski, A. S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Trombetti, T., Valiviita, J., Van Tent, Bartjan, Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., White, S. D. M., Zacchei, A., Zibin, J. P., and Zonca, A.

Subjects
cosmological model, inflaton: potential, satellite: Planck, fluctuation: primordial, cosmic background radiation: polarization, slow-roll approximation, BICEP, 7. Clean energy, expansion: multipole, boundary condition, inflation: model, bispectrum, power spectrum: primordial, perturbation: scalar, power spectrum: scalar, gravitation: lens, gravitation, scale dependence, cosmic background radiation: anisotropy, temperature: anisotropy
Abstract

Astronomy and astrophysics 641(A&A), A10 (2020). doi:10.1051/0004-6361/201833887 special issue: "Planck 2018 results", Published by EDP Sciences, Les Ulis

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