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11 results on '"redshift: low"'

1. Interpretation of the neutrino emission from Tidal Disruption Events

Author

Winter, Walter and Lunardini, Cecilia

Subjects
confinement: magnetic, mass [black hole], redshift: low, neutrino: flux, neutrino: production, X-ray, production [neutrino], ultraviolet, optical, calorimeter, low [redshift], magnetic [confinement], energy: high, photon, flux [neutrino], black hole: mass, time delay [neutrino], neutrino: time delay, efficiency, infrared, ddc:520, high [energy], time dependence, statistical
Abstract

The astrophysical journal / 1 948(1), 42 (2023). doi:10.3847/1538-4357/acbe9e, Three Tidal Disruption Event candidates (AT2019dsg, AT2019fdr, and AT2019aalc) have been associated with high-energy astrophysical neutrinos in multimessenger follow-ups. In all cases, the neutrino observation occurred days after the maximum of the optical-ultraviolet (OUV) luminosity. We discuss unified fully time-dependent interpretations of the neutrino signals where the neutrino delays are not a statistical effect, but rather the consequence of a physical scale of the post-disruption system. Noting that X-ray flares and infrared (IR) dust echoes have been observed in all cases, we consider three models in which quasi-isotropic neutrino emission is due to the interactions of accelerated protons of moderate, medium, and ultra-high energies with X-rays, OUV, and IR photons, respectively. We find that the neutrino time delays can be well described in the X-ray model assuming magnetic confinement of protons in a calorimetric approach if the unobscured X-ray luminosity is roughly constant over time, and in the IR model, where the delay is directly correlated with the time evolution of the echo luminosity (for which a model is developed here). The OUV model exhibits the highest neutrino production efficiency. In all three models, the highest neutrino fluence is predicted for AT2019aalc, due to its high estimated supermassive black hole mass and low redshift. All models result in diffuse neutrino fluxes that are consistent with observations., Published by Institute of Physics Publ., London

Published
2023
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2. Probing the theory of gravity with gravitational lensing of gravitational waves and galaxy surveys

Author

Joseph Silk, 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 Université (SU), and Sorbonne Universités

Subjects
cosmological model, Physics::General Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Virgo interferometer, General Relativity and Quantum Cosmology (gr-qc), detector: network, Astrophysics::Cosmology and Extragalactic Astrophysics, redshift: low, 01 natural sciences, General Relativity and Quantum Cosmology, dark matter, Gravitation, Einstein Telescope, gravitational lensing: weak, gravitation: lens, gravitational radiation: propagation, 0103 physical sciences, structure, Weak lensing, dark energy, gravitational wave, 010303 astronomy & astrophysics, Weak gravitational lensing, Physics, LISA, 010308 nuclear & particles physics, Gravitational wave, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, LIGO, Redshift, Automatic Keywords, VIRGO, Gravitational lens, space-time, gravitational waves, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], galaxy, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The cross-correlation of gravitational wave strain with upcoming galaxy surveys probe theories of gravity in a new way. This method enables testing the theory of gravity by combining the effects from both gravitational lensing of gravitational waves and the propagation of gravitational waves in spacetime. We find that within 10 years, the combination of the Advanced-LIGO and VIRGO detector networks with planned galaxy surveys should detect weak gravitational lensing of gravitational waves in the low redshift Universe ($z, 16 pages, 7 figures. Minor changes in the text and added new references. Matches the version accepted for publication in MNRAS

Published
2020
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3. Snowmass2021 Cosmic Frontier White Paper: Prospects for obtaining Dark Matter Constraints with DESI

Author

Valluri, Monica, Chabanier, Solene, Irsic, Vid, Armengaud, Eric, Walther, Michael, Rockosi, Connie, Sanchez-Conde, Miguel A., Silva, Leandro Beraldo e, Cooper, Andrew P., Darragh-Ford, Elise, Dawson, Kyle, Deason, Alis J., Ferraro, Simone, Forero-Romero, Jaime E., Garzilli, Antonella, Li, Ting, Lukic, Zarija, Manser, Christopher J., Palanque-Delabrouille, Nathalie, Ravoux, Corentin, Tan, Ting, Wang, Wenting, Wechsler, Risa, Carrillo, Andreia, Dey, Arjun, Koposov, Sergey E., Mao, Yao-Yuan, Montero-Camacho, Paulo, Patel, Ekta, Rossi, Graziano, Urena-Lopez, L. Arturo, Valenzuela, Octavio, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
velocity, Cosmology and Nongalactic Astrophysics (astro-ph.CO), WIMP, satellite, FOS: Physical sciences, redshift: low, mass: scale, DESI, High Energy Physics - Phenomenology (hep-ph), dark matter: halo, star, gas, cosmological model: parameter space, numerical methods, energy: density, structure, dark energy, cluster, redshift: high, formation, artificial intelligence, Astrophysics - Astrophysics of Galaxies, High Energy Physics - Phenomenology, kinematics, Astrophysics of Galaxies (astro-ph.GA), hydrogen, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], direct detection, dark matter: fuzzy, galaxy, self-force, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Despite efforts over several decades, direct-detection experiments have not yet led to the discovery of the dark matter (DM) particle. This has led to increasing interest in alternatives to the Lambda CDM (LCDM) paradigm and alternative DM scenarios (including fuzzy DM, warm DM, self-interacting DM, etc.). In many of these scenarios, DM particles cannot be detected directly and constraints on their properties can ONLY be arrived at using astrophysical observations. The Dark Energy Spectroscopic Instrument (DESI) is currently one of the most powerful instruments for wide-field surveys. The synergy of DESI with ESA's Gaia satellite and future observing facilities will yield datasets of unprecedented size and coverage that will enable constraints on DM over a wide range of physical and mass scales and across redshifts. DESI will obtain spectra of the Lyman-alpha forest out to z~5 by detecting about 1 million QSO spectra that will put constraints on clustering of the low-density intergalactic gas and DM halos at high redshift. DESI will obtain radial velocities of 10 million stars in the Milky Way (MW) and Local Group satellites enabling us to constrain their global DM distributions, as well as the DM distribution on smaller scales. The paradigm of cosmological structure formation has been extensively tested with simulations. However, the majority of simulations to date have focused on collisionless CDM. Simulations with alternatives to CDM have recently been gaining ground but are still in their infancy. While there are numerous publicly available large-box and zoom-in simulations in the LCDM framework, there are no comparable publicly available WDM, SIDM, FDM simulations. DOE support for a public simulation suite will enable a more cohesive community effort to compare observations from DESI (and other surveys) with numerical predictions and will greatly impact DM science., Contributed white paper to Snowmass 2021, CF03; minor revisions

Published
2022

4. Into the darkness: Ultra-high energy neutrinos from high-redshift electromagnetic cascades

Author

Esmaeili, Amirfarzan, Capanema, Antonio, Esmaili, Arman, Serpico, Pasquale Dario, and HEP, INSPIRE

Subjects
energy: high, background, energy loss, astrophysics: effect, photon, cosmic background radiation, energy: electromagnetic, muon: production, redshift: low, neutrino: UHE, muon: pair production, cascade: electromagnetic, electron: pair production, [PHYS.HPHE] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], neutrino: spectrum, muon: multiplicity, gamma ray: flux, numerical calculations, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph]
Abstract

We study the impact of the muon pair production and double pair production processes induced by ultra-high energy photons on the cosmic microwave background. Although the muon pair production cross section is smaller than the electron pair production one, the associated energy loss length is comparable or shorter than the latter (followed by inverse Compton in the deep Klein-Nishina regime) at high-redshift, where the effect of the astrophysical radio background is expected to be negligible. By performing a simulation taking into account the details of $e/\gamma$ interactions at high energies, we show that a significant fraction of the electromagnetic energy injected at $E\gtrsim 10^{19}\,$eV at redshift $z\gtrsim 5$ is channeled into neutrinos. The double pair production plays a crucial role in enhancing the multiplicity of muon production in these electromagnetic cascades. The ultra-high energy neutrino spectrum, yet to be detected, can in principle harbour information on ultra-high energy sources in the young universe, either conventional or exotic ones, with weaker constraints from the diffuse gamma ray flux compared to their low redshift counterparts.

Published
2022

5. Mergers of Maximally Charged Primordial Black Holes

Author

Kritos, Konstantinos, Silk, Joseph, 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
coalescence, Cosmology and Nongalactic Astrophysics (astro-ph.CO), background: induced, Astrophysics::High Energy Astrophysical Phenomena, black hole: charge, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, redshift: low, dark matter, General Relativity and Quantum Cosmology, mass spectrum, High Energy Physics - Phenomenology (hep-ph), black hole: formation, black hole: evaporation, gamma ray: detector, cluster, photon: flux, energy: high, gravitational radiation: background, radiation: Hawking, black hole: stability, black hole: mass, observatory, High Energy Physics - Phenomenology, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], black hole: primordial, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Near-extremal primordial black holes stable over cosmological timescales may constitute a significant fraction of the dark matter. Due to their charge the coalescence rate of such black holes is enhanced inside clusters and the non-extremal merger remnants are prone to Hawking evaporation. We demonstrate that if these clusters of near-extremal holes contain a sufficient number of members to survive up to low redshift, the hard photons from continued evaporation begin to dominate the high energy diffuse background. We find that the diffuse photon flux can be observed for a monochromatic mass spectrum of holes lighter than about $10^{12}\rm g$. We place upper bounds on their abundance respecting the current bounds set by gamma ray telescopes. Furthermore, the gravitational wave background induced at the epoch of primordial black hole formation may be detectable by future planned and proposed ground-based and space-borne gravitational wave observatories operating in the mHz to kHz frequency range and can be an important tool for studying light charged primordial black holes over masses in the range $\rm 10^{12}g - 10^{19}g$., 13 pages, 3 figures

Published
2021

6. Does Hubble Tension Signal a Breakdown in FLRW Cosmology?

Author

Mohammad M. Sheikh-Jabbari, Eoin Ó Colgáin, Lu Yin, Roya Mohayaee, Chethan Krishnan, Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
High Energy Physics - Theory, cosmological model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics and Astronomy (miscellaneous), Age of the universe, constraint, media_common.quotation_subject, FOS: Physical sciences, Cosmological constant, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, redshift: low, Cosmology, General Relativity and Quantum Cosmology, symbols.namesake, High Energy Physics - Phenomenology (hep-ph), gravitation: lens, Friedmann–Lemaître–Robertson–Walker metric, 0103 physical sciences, quasar, dark energy, 010303 astronomy & astrophysics, media_common, Physics, cosmological constant, Hubble constant, 010308 nuclear & particles physics, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], resolution, tension, horizon: acoustic, Universe, Redshift, analytic properties, High Energy Physics - Phenomenology, High Energy Physics - Theory (hep-th), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Robertson-Walker, Dark energy, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hubble's law, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The tension between early and late Universe probes of the Hubble constant has motivated various new FLRW cosmologies. Here, we reanalyse the Hubble tension with a recent age of the Universe constraint. This allows us to restrict attention to matter and a dark energy sector that we treat without assuming a specific model. Assuming analyticity of the Hubble parameter $H(z)$, and a generic low redshift modification to flat $\Lambda$CDM, we find that low redshift data ($z \lesssim 2.5$) and well-motivated priors only permit a dark energy sector close to the cosmological constant $\Lambda$. This restriction rules out late Universe modifications within FLRW. We show that early Universe physics that alters the sound horizon can yield an upper limit of $H_0 \sim 71 \pm 1$ km/s/Mpc. Since various local determinations may be converging to $H_0 \sim 73$ km/s/Mpc, a breakdown of the FLRW framework is a plausible resolution. We outline how future data, in particular strongly lensed quasar data, could also provide further confirmations of such a resolution., Comment: v1 10 pages, comments welcome, especially on appendix D & Figure 4; v2, typos corrected, Figure 4 improved, observations strengthened; v3 references added, matches version published as invited contribution to CQG "Focus Issue on the Hubble Constant Tension"

Published
2021
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7. The Schrödinger-Poisson method for Large-Scale Structure

Author

Garny, Mathias, Konstandin, Thomas, and Rubira, Henrique

Subjects
baryon, phase space, background, formation, nonlinear, oscillation: acoustic, structure, power spectrum, matter: correlation function, redshift: low, dark matter
Abstract

Journal of cosmology and astroparticle physics 2020(04), 003 - 003 (2020). doi:10.1088/1475-7516/2020/04/003, We study the Schrödinger-Poisson (SP) method in the context of cosmological large-scale structure formation in an expanding background. In the limit 0ℏ &to; , the SP technique can be viewed as an effective method to sample the phase space distribution of cold dark matter that remains valid on non-linear scales. We present results for the 2D and 3D matter correlation function and power spectrum at length scales corresponding to the baryon acoustic oscillation (BAO) peak. We discuss systematic effects of the SP method applied to cold dark matter and explore how they depend on the simulation parameters. In particular, we identify a combination of simulation parameters that controls the scale-independent loss of power observed at low redshifts, and discuss the scale relevant to this effect., Published by IOP, London

Published
2020
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8. Planck 2018 results: I. Overview and the cosmological legacy of Planck

Author

Planck Collaboration, Aghanim, N., Akrami, Y., Arroja, F., 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, CARLO, Butler, R. C., Calabrese, E., Cardoso, J. -F., Carron, J., Casaponsa, B., Challinor, A., Chiang, H. C., Colombo, L. P. L., Combet, C., Contreras, D., Crill, B. P., CUTTAIA, FRANCESCO, de Bernardis, P., de Zotti, G., Delabrouille, J., Delouis, J. -M., Désert, F. -X., Di Valentino, E., Dickinson, C., Diego, J. M., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Fantaye, Y., Fergusson, J., Fernandez-Cobos, R., FINELLI, FABIO, Forastieri, F., FRAILIS, Marco, FRANCESCHI, ENRICO, Frolov, A., GALEOTTA, Samuele, Galli, S., Ganga, K., Génova-Santos, R. T., Gerbino, M., Ghosh, T., González-Nuevo, J., Górski, K. M., Gratton, S., GRUPPUSO, ALESSANDRO, Gudmundsson, J. E., Hamann, J., Handley, W., Hansen, F. K., Helou, G., Herranz, D., Hildebrandt, S. R., Hivon, E., Huang, Z., Jaffe, A. H., Jones, W. C., Karakci, A., Keihänen, E., Keskitalo, R., Kiiveri, K., Kim, J., Kisner, T. S., Knox, L., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Langer, M., Lasenby, A., LATTANZI, Mario Gilberto, Lawrence, C. R., Le Jeune, M., Leahy, J. P., Lesgourgues, J., Levrier, F., Lewis, A., Liguori, M., Lilje, P. B., Lilley, M., Lindholm, V., López-Caniego, M., Lubin, P. M., Ma, Y. -Z., Macías-Pérez, J. F., MAGGIO, Gianmarco, Maino, D., Mandolesi, N., Mangilli, A., Marcos-Caballero, A., MARIS, Michele, Martin, P. G., Martinelli, M., Martínez-González, E., Matarrese, S., Mauri, N., McEwen, J. D., Meerburg, P. D., Meinhold, P. R., Melchiorri, A., Mennella, A., Migliaccio, M., Millea, M., Mitra, S., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Montier, L., MORGANTE, GIANLUCA, Moss, A., Mottet, S., Münchmeyer, M., Natoli, P., Nørgaard-Nielsen, H. U., Oxborrow, C. A., Pagano, L., PAOLETTI, DANIELA, Partridge, B., Patanchon, G., Pearson, T. J., Peel, M., Peiris, H. V., PERROTTA, Francesca, Pettorino, V., Piacentini, F., Polastri, L., Polenta, G., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Rocha, G., Rosset, C., Roudier, G., Rubiño-Martín, J. A., Ruiz-Granados, B., SALVATI, LAURA, SANDRI, MAURA, 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 , DANIELE, Tenti, M., TERENZI, LUCA, Toffolatti, L., Tomasi, M., Trombetti, T., Valiviita, J., Van Tent, B., Vibert, L., Vielva, P., VILLA, FABRIZIO, Vittorio, N., Wandelt, B. D., Wehus, I. K., White, M., White, S. D. M., ZACCHEI, Andrea, Zonca, A., Universidad de Cantabria, 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), 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)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de 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), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), 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)), 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, 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), 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2020-....] (Grenoble INP [2020-....]), Université Grenoble Alpes [2020-....] (UGA [2020-....]), Institut de Planétologie et d'Astrophysique de Grenoble [2020-....] (IPAG [2020-....]), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble [2020-....] (OSUG [2020-....]), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes [2020-....] (UGA [2020-....]), 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, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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), University of Parma = Università degli studi di Parma [Parme, Italie], Computing and Mathematical Sciences [Pasadena]], California Institute of Technology (CALTECH), Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Patrimoine, Littérature, Histoire (PLH), Université Toulouse - Jean Jaurès (UT2J), Laboratoire de Recherche en Informatique (LRI), CentraleSupélec-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), CentraleSupélec, Universidade Aberta [Lisboa], Centre National d'Études Spatiales [Toulouse] (CNES), Centre de Recherche en Cancérologie de Lyon (UNICANCER/CRCL), Centre Léon Bérard [Lyon]-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM), Centre Léon Bérard [Lyon], Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - 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Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Dipartimento di Fisica 'G. Galilei', Universita degli Studi di Padova, University of Cambridge [UK] (CAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), University College of London [London] (UCL), University of Manchester [Manchester], Venetian Institute Molecular Medicine (VIMM), University of British Columbia (UBC), Laboratoire de neurobiologie cellulaire et moléculaire (NBCM), Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), USDA-ARS : Agricultural Research Service, Planck Collaboration, Department of Physics, Helsinki Institute of Physics, European Commission, Ministerio de Ciencia e Innovación (España), Consejo Superior de Investigaciones Científicas (España), European Research Council, European Space Agency, Aghanim N., Akrami Y., Arroja F., 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., Casaponsa B., 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., Desert F.-X., Di Valentino E., Dickinson C., Diego J.M., Donzelli S., Dore O., Douspis M., Ducout A., Dupac X., Efstathiou G., Elsner F., Ensslin T.A., Eriksen H.K., Falgarone E., Fantaye Y., Fergusson J., Fernandez-Cobos R., Finelli F., Forastieri F., Frailis M., 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., Helou G., 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., Langer M., Lasenby A., Lattanzi M., Lawrence C.R., Le Jeune M., Leahy J.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., Meerburg P.D., Meinhold P.R., Melchiorri A., Mennella A., Migliaccio M., Millea M., Mitra S., Miville-Deschenes M.-A., Molinari D., Moneti A., Montier L., Morgante G., Moss A., Mottet S., Munchmeyer M., Natoli P., Norgaard-Nielsen H.U., Oxborrow C.A., Pagano L., Paoletti D., Partridge B., Patanchon G., Pearson T.J., Peel M., Peiris H.V., Perrotta F., Pettorino V., Piacentini F., Polastri L., Polenta G., Puget J.-L., Rachen J.P., Reinecke M., Remazeilles M., Renault C., 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., Terenzi L., Toffolatti L., Tomasi M., Trombetti T., 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., Zonca A., Van Swinderen Institute for Particle Physics and G, High-Energy Frontier, 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), 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 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), Università degli studi di Parma = University of Parma (UNIPR), Université de Toulouse (UT)-Université de Toulouse (UT), 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 Lyon-Université de Lyon-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), 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), 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 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), Challinor, Anthony [0000-0003-3479-7823], Fergusson, James [0000-0003-4820-171X], Handley, William [0000-0002-5866-0445], Lasenby, Anthony [0000-0002-8208-6332], and Apollo - University of Cambridge Repository

Subjects
Cosmic background radiation, Cosmology: observations, Cosmology: theory, Surveys, cosmological model, Cosmic background radiation, Cosmology: observations, Cosmology: theory, Surveys, Astronomy, Cosmic microwave background, cosmic background radiation: polarization, Astrophysics, 01 natural sciences, 7. Clean energy, Cosmology: observation, redshift: low, RADIAÇÃO DE FUNDO, LENSING TOMOGRAPHY, observations [Cosmology], 010303 astronomy & astrophysics, media_common, Physics, Polarization (waves), MULTIBAND IMAGING PHOTOMETER, symbols, astro-ph.CO, power spectrum: angular dependence, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and Astronomy, Structure formation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), COMPONENT SEPARATION, satellite: Planck, ANGULAR POWER SPECTRUM, PARAMETER CONSTRAINTS, media_common.quotation_subject, FOS: Physical sciences, Lambda-CDM model, MAIN GALAXY SAMPLE, Astrophysics::Cosmology and Extragalactic Astrophysics, Radio spectrum, microwaves, NO, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, theory [Cosmology], 0103 physical sciences, detector: pixel, Planck, 010308 nuclear & particles physics, Astronomy and Astrophysics, 115 Astronomy, Space science, Redshift, cosmic background radiation: temperature, Space and Planetary Science, Sky, PROBE WMAP OBSERVATIONS, DARK ENERGY, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], MICROWAVE BACKGROUND POLARIZATION, BARYON ACOUSTIC-OSCILLATIONS
Abstract

Planck Collaboration: et al., arXiv:1807.06205v2, The European Space Agency’s Planck satellite, which was dedicated to studying the early Universe and its subsequent evolution, was launched on 14 May 2009. It scanned the microwave and submillimetre sky continuously between 12 August 2009 and 23 October 2013, producing deep, high-resolution, all-sky maps in nine frequency bands from 30 to 857 GHz. This paper presents the cosmological legacy of Planck, which currently provides our strongest constraints on the parameters of the standard cosmological model and some of the tightest limits available on deviations from that model. The 6-parameter ΛCDM model continues to provide an excellent fit to the cosmic microwave background data at high and low redshift, describing the cosmological information in over a billion map pixels with just six parameters. With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the six parameters to better than 1% (simultaneously), with the best-determined parameter (θ*) now known to 0.03%. We describe the multi-component sky as seen by Planck, the success of the ΛCDM model, and the connection to lower-redshift probes of structure formation. We also give a comprehensive summary of the major changes introduced in this 2018 release. The Planck data, alone and in combination with other probes, provide stringent constraints on our models of the early Universe and the large-scale structure within which all astrophysical objects form and evolve. We discuss some lessons learned from the Planck mission, and highlight areas ripe for further experimental advances., The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU).

Published
2020
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9. Are $H_0$ and $\sigma_8$ tensions generic to present cosmological data?

Author

Subinoy Das, Supratik Pal, Kanhaiya L. Pandey, Ujjaini Alam, Archita Bhattacharyya, 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 national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)

Subjects
satellite: Planck, interaction: model, Dark matter, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, redshift: low, dark matter: parametrization, dark matter, cosmological model: parameter space, 0103 physical sciences, cosmic background radiation: power spectrum, cosmological parameters, cluster, dark energy, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, redshift: high, parametrization, Astronomy and Astrophysics, phantom, tension, 13. Climate action, Space and Planetary Science, correlation, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], signature, Astrophysics - Cosmology and Nongalactic Astrophysics, dark energy: equation of state
Abstract

Yes, for a wide range of cosmological models ($\Lambda$CDM, non-interacting $w_z$CDM or models with possible interactions between dark energy and dark matter, in either phantom or non-phantom regimes). In the recent past there have been many attempts to solve the tension between direct measurements of $H_0$ and $\sigma_8 \sqrt{\Omega_{0 {\rm m}}}$ from the respective low redshift observables and indirect measurements of these quantities from the cosmic microwave background (CMB). In this work we reconstruct a model independent approach that boils down to different classes of cosmological models under suitable parameters choices. We test this parameterization against the latest Planck CMB data combined with recent BAO, SNeIa datasets and the R16 direct $H_0$ measurements, and compare among different cosmological models. Our analysis reveals that a strong positive correlation between $H_0$ and $\sigma_8$ is more or less generic, irrespective of the choice of cosmological models. We also find that present data slightly prefers a phantom equation of state for dark energy and a slight negative value for effective equation of state for dark matter (which is a direct signature of interacting models) with a relatively high value for $H_0$ consistent with R16 and simultaneously, a consistent value for $\Omega_{0 {\rm m}}$. Thus, even though the tensions cannot be fully resolved, interacting models with phantom equation of state get a slight edge over the others for currently available data. We also see that allowing interaction between dark energy and dark matter may resolve the tension between the high redshift CMB data and individual low redshift datasets, but the low redshift datasets have inconsistencies between them (e.g. between BAO and $H_0$, SNeIa and BAO, and cluster counts and $H_0$) that are practically independent of the cosmological model., Comment: 16 pages, 6 figures, to be appeared in The Astrophysical Journal

Published
2019
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10. Self-acceleration in scalar-bimetric theories

Author

Patrick Valageas, Philippe Brax, Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), action: Einstein-Hilbert, Dark matter, Scalar (mathematics), FOS: Physical sciences, Cosmological constant, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, coupling: scalar, 01 natural sciences, redshift: low, General Relativity and Quantum Cosmology, Metric expansion of space, Gravitation, dark matter: perturbation, Theoretical physics, PACS numbers: 98.80.-k, 98.80.-k, 0103 physical sciences, 010306 general physics, dark energy, Physics, [PHYS]Physics [physics], cosmological constant, energy: kinetic, 010308 nuclear & particles physics, Fifth force, chameleon: field theory, fifth force, field theory: scalar, baryon, screening: Vainshtein, density: perturbation, force: gravitation, Dark energy, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], gravitation: fundamental constant, expansion: acceleration, Scalar field, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We describe scalar-bimetric theories where the dynamics of the Universe are governed by two separate metrics, each with an Einstein-Hilbert term. In this setting, the baryonic and dark matter components of the Universe couple to metrics which are constructed as functions of these two gravitational metrics. The scalar field, contrary to dark energy models, does not have a potential whose role is to mimic a late-time cosmological constant. The late-time acceleration of the expansion of the Universe can be easily obtained at the background level in these models by appropriately choosing the coupling functions appearing in the decomposition of the vierbeins for the baryonic and dark matter metrics. We explicitly show how the concordance model can be retrieved with negligible scalar kinetic energy. This requires the scalar coupling functions to show variations of order unity during the accelerated expansion era. This leads in turn to deviations of order unity for the effective Newton constants and a fifth force that is of the same order as Newtonian gravity, with peculiar features. The baryonic and dark matter self-gravities are amplified although the gravitational force between baryons and dark matter is reduced and even becomes repulsive at low redshift. This slows down the growth of baryonic density perturbations on cosmological scales, while dark matter perturbations are enhanced. In our local environment, the upper bound on the time evolution of Newton's constant requires an efficient screening mechanism that both damps the fifth force on small scales and decouples the local value of Newton constant from its cosmological value. This cannot be achieved by a quasi-static chameleon mechanism, and requires going beyond the quasi-static regime and probably using derivative screenings, such as Kmouflage or Vainshtein screening, on small scales., 35 pages

Published
2018
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11. Dark Energy After GW170817: Dead Ends and the Road Ahead

Author

Miguel Zumalacárregui, Jose María Ezquiaga, Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut de Physique Théorique - UMR CNRS 3681 ( IPHT ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Centre National de la Recherche Scientifique ( CNRS ), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)

Subjects
High Energy Physics - Theory, cosmological model, neutron star: binary, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], scalar tensor, General Physics and Astronomy, Binary number, 01 natural sciences, redshift: low, General Relativity and Quantum Cosmology, Mathematical Sciences, localization, [ PHYS.HTHE ] Physics [physics]/High Energy Physics - Theory [hep-th], Gravitation, High Energy Physics - Phenomenology (hep-ph), Engineering, dark energy, 010303 astronomy & astrophysics, Physics, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], hep-th, hep-ph, gravitation: Proca, High Energy Physics - Phenomenology, interaction: derivative, curvature, Physical Sciences, astro-ph.CO, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Galileon, Astrophysics - Cosmology and Nongalactic Astrophysics, Gravity (chemistry), General Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gr-qc, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), gamma ray: burst, gravitational radiation: direct detection, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Theoretical physics, 0103 physical sciences, Covariant transformation, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation, Redshift, Neutron star, electromagnetic, High Energy Physics - Theory (hep-th), gravitation, gravitational radiation: emission, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Dark energy, [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Multi-messenger gravitational wave (GW) astronomy has commenced with the detection of the binary neutron star merger GW170817 and its associated electromagnetic counterparts. The almost coincident observation of both signals places an exquisite bound on the GW speed $|c_g/c-1|\leq5\cdot10^{-16}$. We use this result to probe the nature of dark energy (DE), showing that a large class of scalar-tensor theories and DE models are highly disfavored. As an example we consider the covariant Galileon, a cosmologically viable, well motivated gravity theory which predicts a variable GW speed at low redshift. Our results eliminate any late-universe application of these models, as well as their Horndeski and most of their beyond Horndeski generalizations. Three alternatives (and their combinations) emerge as the only possible scalar-tensor DE models: 1) restricting Horndeski's action to its simplest terms, 2) applying a conformal transformation which preserves the causal structure and 3) compensating the different terms that modify the GW speed (to be robust, the compensation has to be independent on the background on which GWs propagate). Our conclusions extend to any other gravity theory predicting varying $c_g$ such as Einstein-Aether, Ho\v{r}ava gravity, Generalized Proca, TeVeS and other MOND-like gravities., Comment: 6 pages, 2 figures. Matches PRL version

Published
2017
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