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1. Cosmology with the Laser Interferometer Space Antenna

Author

Pierre Auclair, David Bacon, Tessa Baker, Tiago Barreiro, Nicola Bartolo, Enis Belgacem, Nicola Bellomo, Ido Ben-Dayan, Daniele Bertacca, Marc Besancon, Jose J. Blanco-Pillado, Diego Blas, Guillaume Boileau, Gianluca Calcagni, Robert Caldwell, Chiara Caprini, Carmelita Carbone, Chia-Feng Chang, Hsin-Yu Chen, Nelson Christensen, Sebastien Clesse, Denis Comelli, Giuseppe Congedo, Carlo Contaldi, Marco Crisostomi, Djuna Croon, Yanou Cui, Giulia Cusin, Daniel Cutting, Charles Dalang, Valerio De Luca, Walter Del Pozzo, Vincent Desjacques, Emanuela Dimastrogiovanni, Glauber C. Dorsch, Jose Maria Ezquiaga, Matteo Fasiello, Daniel G. Figueroa, Raphael Flauger, Gabriele Franciolini, Noemi Frusciante, Jacopo Fumagalli, Juan García-Bellido, Oliver Gould, Daniel Holz, Laura Iacconi, Rajeev Kumar Jain, Alexander C. Jenkins, Ryusuke Jinno, Cristian Joana, Nikolaos Karnesis, Thomas Konstandin, Kazuya Koyama, Jonathan Kozaczuk, Sachiko Kuroyanagi, Danny Laghi, Marek Lewicki, Lucas Lombriser, Eric Madge, Michele Maggiore, Ameek Malhotra, Michele Mancarella, Vuk Mandic, Alberto Mangiagli, Sabino Matarrese, Anupam Mazumdar, Suvodip Mukherjee, Ilia Musco, Germano Nardini, Jose Miguel No, Theodoros Papanikolaou, Marco Peloso, Mauro Pieroni, Luigi Pilo, Alvise Raccanelli, Sébastien Renaux-Petel, Arianna I. Renzini, Angelo Ricciardone, Antonio Riotto, Joseph D. Romano, Rocco Rollo, Alberto Roper Pol, Ester Ruiz Morales, Mairi Sakellariadou, Ippocratis D. Saltas, Marco Scalisi, Kai Schmitz, Pedro Schwaller, Olga Sergijenko, Geraldine Servant, Peera Simakachorn, Lorenzo Sorbo, Lara Sousa, Lorenzo Speri, Danièle A. Steer, Nicola Tamanini, Gianmassimo Tasinato, Jesús Torrado, Caner Unal, Vincent Vennin, Daniele Vernieri, Filippo Vernizzi, Marta Volonteri, Jeremy M. Wachter, David Wands, Lukas T. Witkowski, Miguel Zumalacárregui, James Annis, Fëanor Reuben Ares, Pedro P. Avelino, Anastasios Avgoustidis, Enrico Barausse, Alexander Bonilla, Camille Bonvin, Pasquale Bosso, Matteo Calabrese, Mesut Çalışkan, Jose A. R. Cembranos, Mikael Chala, David Chernoff, Katy Clough, Alexander Criswell, Saurya Das, Antonio da Silva, Pratika Dayal, Valerie Domcke, Ruth Durrer, Richard Easther, Stephanie Escoffier, Sandrine Ferrans, Chris Fryer, Jonathan Gair, Chris Gordon, Martin Hendry, Mark Hindmarsh, Deanna C. Hooper, Eric Kajfasz, Joachim Kopp, Savvas M. Koushiappas, Utkarsh Kumar, Martin Kunz, Macarena Lagos, Marc Lilley, Joanes Lizarraga, Francisco S. N. Lobo, Azadeh Maleknejad, C. J. A. P. Martins, P. Daniel Meerburg, Renate Meyer, José Pedro Mimoso, Savvas Nesseris, Nelson Nunes, Vasilis Oikonomou, Giorgio Orlando, Ogan Özsoy, Fabio Pacucci, Antonella Palmese, Antoine Petiteau, Lucas Pinol, Simon Portegies Zwart, Geraint Pratten, Tomislav Prokopec, John Quenby, Saeed Rastgoo, Diederik Roest, Kari Rummukainen, Carlo Schimd, Aurélia Secroun, Alberto Sesana, Carlos F. Sopuerta, Ismael Tereno, Andrew Tolley, Jon Urrestilla, Elias C. Vagenas, Jorinde van de Vis, Rien van de Weygaert, Barry Wardell, David J. Weir, Graham White, Bogumiła Świeżewska, Valery I. Zhdanov, and The LISA Cosmology Working Group

Subjects
Laser Interferometer Space Antenna (LISA), Cosmology, Atomic physics. Constitution and properties of matter, QC170-197
Abstract

Abstract The Laser Interferometer Space Antenna (LISA) has two scientific objectives of cosmological focus: to probe the expansion rate of the universe, and to understand stochastic gravitational-wave backgrounds and their implications for early universe and particle physics, from the MeV to the Planck scale. However, the range of potential cosmological applications of gravitational-wave observations extends well beyond these two objectives. This publication presents a summary of the state of the art in LISA cosmology, theory and methods, and identifies new opportunities to use gravitational-wave observations by LISA to probe the universe.

Published
2023
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2. The missing link in gravitational-wave astronomy

Author

Manuel Arca Sedda, Christopher P. L. Berry, Karan Jani, Pau Amaro-Seoane, Pierre Auclair, Jonathon Baird, Tessa Baker, Emanuele Berti, Katelyn Breivik, Chiara Caprini, Xian Chen, Daniela Doneva, Jose M. Ezquiaga, K. E. Saavik Ford, Michael L. Katz, Shimon Kolkowitz, Barry McKernan, Guido Mueller, Germano Nardini, Igor Pikovski, Surjeet Rajendran, Alberto Sesana, Lijing Shao, Nicola Tamanini, Niels Warburton, Helvi Witek, Kaze Wong, and Michael Zevin

Published
2021
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3. Overview and progress on the Laser Interferometer Space Antenna mission

Author

Jean-Baptiste Bayle, Béatrice Bonga, Chiara Caprini, Daniela Doneva, Martina Muratore, Antoine Petiteau, Elena Rossi, Lijing Shao, 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, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
LISA, cosmological model, Astronomy and Astrophysics, High Energy Physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Lorentz
Abstract

International audience; At a Lorentz Center workshop, Chiara Caprini, Antoine Petiteau and Elena Maria Rossi gave a series of presentations about the Laser Interferometer Space Antenna (LISA) mission, the instrument, and the associated science in cosmology and astrophysics.

Published
2022
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4. Étonnants infinis

Author

Maud Baylac, Jean-Luc Biarrotte, Julien Billard, Dominique Boutigny, Chiara Caprini, Gabriel Chardin, Patrick Chardon, Pierre Cladé, Sabine Crépé-Renaudin, Hélène Courtois, Sylvain David, Sacha Davidson, Emmanuel Dartois, Mirella Del Nero, Jean Duprat, Josquin Errard, Fanny Farget, Berrie Giebels, Vladimir Vava Gligorov, Raphaël Granier De Cassagnac, Saida Guellati, Francesca Gulminelli, Ferid Haddad, Sébastien Incerti, Marc Knecht, Antoine Lemasson, Marianne Lemoine-Goumard, Anne Le Pennec, Araceli Lopez-Martens, Benoit Lott, Pierre-Etienne Macchi, Frédérique Marion, Jacques Marteau, Silvia Niccolai, Mathieu Perrin-Terrin, Guillaume Pignol, Vincent Poireau, Daniel Pomarède, Vivian Poulin, Laurent Serin, Justine Serrano, Yves Sirois, Olivier Sorlin, David Rousseau, Vincent Tatischeff, Teixeira, Ana M., Laurent Vacavant, Véronique Van Elewyck, Marco Zito, Fabian Zomer, 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 (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), 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)-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), European Organization for Nuclear Research (CERN), 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 de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Laboratoire Kastler Brossel (LKB (Jussieu)), 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), 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), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM), Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Grand Accélérateur National d'Ions Lourds (GANIL), 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 Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique corpusculaire de Caen (LPCC), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-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 des technologies associées (SUBATECH), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Laboratoire de Physique des Deux Infinis Bordeaux (LP2I - Bordeaux), Université de Bordeaux (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Calcul de l'IN2P3 (CC-IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, APC - Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Ursula Bassler

Subjects
[PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; L’immensité de notre Univers ne cesse d’intriguer et de stimuler les imaginations.Pour mieux appréhender l’infiniment grand et l’histoire de l’Univers depuis ses tout premiers instants, il faut se tourner vers un autre infini, l’infiniment petit, et ses quarks, leptons et bosons, à la base du modèle standard de la physique des particules. En les étudiant, on cherche à percer le secret de l’organisation de la matière à la plus petite échelle. Sans l’infiniment petit, on ne peut décrire ni le Big Bang, ni le comportement des grandes structures stellaires, ni la naissance de la matière. Et sans ces deux infinis ensemble, on ne peut bâtir les modèles théoriques expliquant la matière noire, l’énergie noire ou fonder la gravitation quantique.Les physiques des infinis sont des physiques hors normes qui se racontent à grand renfort de superlatifs. Elles nécessitent des installations internationales de très grande envergure, et nous entraînent dans des voyages aux confins de la perception où l’on flirte avec la vitesse de la lumière et jongle avec les limites des propriétés de la matière.En trente courts chapitres abondamment illustrés, cet ouvrage rend compte de ce que l’on sait déjà comme de ce que l’on cherche encore.

Published
2022

5. Massive black hole binaries in LISA: multimessenger prospects and electromagnetic counterparts

Author

Alberto Mangiagli, Chiara Caprini, Marta Volonteri, Sylvain Marsat, Susanna Vergani, Nicola Tamanini, Henri Inchauspé, 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), European Organization for Nuclear Research (CERN), 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 des deux Infinis de Toulouse (L2IT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)

Subjects
astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics and Astronomy, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], General Relativity and Cosmology, [SDU]Sciences of the Universe [physics], gr-qc, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract

In the next decade, the Laser Interferometer Space Antenna (LISA) will detect the coalescence of massive black hole binaries (MBHBs) in the range $[10^4, 10^8] \, \rm M_{\odot}$, up to $z\sim10$. Their gravitational wave (GW) signal is expected to be accompanied by an electromagnetic counterpart (EMcp), generated by the gas accreting on the binary or on the remnant BH. In this work, we present the number and characteristics (such as redshift and mass distribution, apparent magnitudes or fluxes) of EMcps detectable jointly by LISA and some representative EM telescopes. We combine state-of-the-art astrophysical models for the galaxies formation and evolution to build the MBHBs catalogues, with Bayesian tools to estimate the binary sky position uncertainty from the GW signal. Exploiting additional information from the astrophysical models, such as the amount of accreted gas and the BH spins, we evaluate the expected EM emission in the soft X-ray, optical and radio bands. Overall, we predict between 7 and 21 EMcps in 4 yrs of joint observations by LISA and the considered EM facilities, depending on the astrophysical model. We also explore the impact of the hydrogen and dust obscuration of the optical and X-ray emissions, as well as of the collimation of the radio emission: these effects reduce the number to EMcps to 2 or 3, depending on the astrophysical model, again in 4 yrs of observations. Most of the EMcps are characterised by faint EM emission, challenging the observational capabilities of future telescopes. Finally, we also find that systems with multi-modal sky position posterior distributions represent only a minority of cases and do not affect significantly the number of EMcps., 28 pages, 18 figures. Accepted for publication in PRD

Published
2022
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7. Gravitational wave signal from primordial magnetic fields in the Pulsar Timing Array frequency band

Author

Alberto Roper Pol, Chiara Caprini, Andrii Neronov, Dmitri Semikoz, 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), and ANR-19-CE31-0020,MMUniverse,Nouvelles fenêtres sur l'Univers par l'astronomie multi-messenger(2019)

Subjects
Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitational radiation: stochastic, gr-qc, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), black-hole binaries, General Relativity and Quantum Cosmology, gamma ray: detector, energy: density, radiation: energy, gravitational radiation: frequency, search, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, magnetic field: decay, General Relativity and Cosmology, quark: confinement, turbulence, gravitational radiation: background, magnetic field: primordial, radiation, hydrodynamics: magnetic, pressure: anisotropy, critical phenomena: confinement, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], astro-ph.CO, limits, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The NANOGrav, Parkes, European, and International Pulsar Timing Array (PTA) Collaborations have reported evidence for a common-spectrum process that can potentially correspond to a stochastic gravitational wave background (SGWB) in the 1--100 nHz frequency range. We consider the scenario in which this signal is produced by magnetohydrodynamic (MHD) turbulence in the early Universe, induced by a nonhelical primordial magnetic field at the energy scale corresponding to the quark confinement phase transition. We perform MHD simulations to study the dynamical evolution of the magnetic field and compute the resulting SGWB. We show that the SGWB output from the simulations can be very well approximated by assuming that the magnetic anisotropic stress is constant in time, over a time interval related to the eddy turnover time. The analytical spectrum that we derive under this assumption features a change of slope at a frequency corresponding to the GW source duration that we confirm with the numerical simulations. We compare the SGWB signal with the PTA data to constrain the temperature scale at which the SGWB is sourced, as well as the amplitude and characteristic scale of the initial magnetic field. We find that the generation temperature is constrained to be in the 1--200 MeV range, the magnetic field amplitude must be $>1$\% of the radiation energy density at that time, and the magnetic field characteristic scale is constrained to be $>10$\% of the horizon scale. We show that the turbulent decay of this magnetic field will lead to a field at recombination that can help to alleviate the Hubble tension and can be tested by measurements in the voids of the Large Scale Structure with gamma-ray telescopes like the Cherenkov Telescope Array., 28 pages, 9 figures, 1 table, accepted for publication in Phys. Rev. D, files and code available in https://github.com/AlbertoRoper/GW_turbulence

Published
2022
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8. Observing GW190521-like binary black holes and their environment with LISA

Author

Laura Sberna, Stanislav Babak, Sylvain Marsat, Andrea Caputo, Giulia Cusin, Alexandre Toubiana, Enrico Barausse, Chiara Caprini, Tito Dal Canton, Alberto Sesana, Nicola Tamanini, 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 des deux Infinis de Toulouse (L2IT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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 de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)

Subjects
Astrophysics and Astronomy, gr-qc, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), General Relativity and Quantum Cosmology, Settore FIS/05 - Astronomia e Astrofisica, gas, general relativity, AGN, gravitational radiation: frequency, Astrophysics::Galaxy Astrophysics, orbit, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, LISA, density, General Relativity and Cosmology, binary: formation, black hole: mass, time delay, Doppler effect, modulation, electromagnetic, frequency: low, black hole: binary, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], history, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Binaries of relatively massive black holes like GW190521 have been proposed to form in dense gas environments, such as the disks of Active Galactic Nuclei (AGNs), and they might be associated with transient electromagnetic counterparts. The interactions of this putative environment with the binary could leave a significant imprint at the low gravitational wave frequencies observable with the Laser Interferometer Space Antenna (LISA). We show that LISA will be able to detect up to ten GW190521-like black hole binaries, with sky position errors $\lesssim1$ deg$^2$. Moreover, it will measure directly various effects due to the orbital motion around the supermassive black hole at the center of the AGN, especially the Doppler modulation and the Shapiro time delay. Thanks to a careful treatment of their frequency domain signal, we were able to perform the full parameter estimation of Doppler and Shapiro-modulated binaries as seen by LISA. We find that the Doppler and Shapiro effects will allow for measuring the AGN parameters (radius and inclination of the orbit around the AGN, central black hole mass) with up to percent-level precision. Properly modeling these low-frequency environmental effects is crucial to determine the binary formation history, as well as to avoid biases in the reconstruction of the source parameters and in tests of general relativity with gravitational waves., 13+4 pages, 7+1 figures v3: corrected typo in Fig 5

Published
2022
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10. Unveiling the gravitational universe at μ-Hz frequencies

Author

Alberto Mangiagli, Oliver Jennrich, Lijing Shao, N. Korsakova, Simon Barke, Miguel Zumalacarregui, Alberto Sesana, Astrid Lamberts, John A. Regan, Fazeel Mahmood Khan, Kaze Wong, Peter H. Johansson, Enrico Barausse, Juan Garcia-Bellido, Matteo Bonetti, Vishal Baibhav, Surjeet Rajendran, Manuel Arca Sedda, Lucio Mayer, Marta Volonteri, Germano Nardini, Alessandro Lupi, Karan Jani, Nicola Tamanini, Zoltan Haiman, Alessandro D. A. M. Spallicci, Emanuele Berti, Niels Warburton, Chiara Caprini, Alvise Raccanelli, Fabio Pacucci, Antoine Petiteau, Valeriya Korol, Pedro R. Capelo, Observatoire de la Côte d'Azur (OCA), 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 Paris Cité (UPCité), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire des deux Infinis de Toulouse (L2IT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Sesana, A, Korsakova, N, Sedda, M, Baibhav, V, Barausse, E, Barke, S, Berti, E, Bonetti, M, Capelo, P, Caprini, C, Garcia-Bellido, J, Haiman, Z, Jani, K, Jennrich, O, Johansson, P, Khan, F, Korol, V, Lamberts, A, Lupi, A, Mangiagli, A, Mayer, L, Nardini, G, Pacucci, F, Petiteau, A, Raccanelli, A, Rajendran, S, Regan, J, Shao, L, Spallicci, A, Tamanini, N, Volonteri, M, Warburton, N, Wong, K, Zumalacarregui, M, Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Leibniz Universität Hannover [Hannover] (LUH), Department of Physics and Astronomy [U Mississippi], The University of Mississippi [Oxford], 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), Agence Spatiale Européenne (ESA), European Space Agency (ESA), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Interactions Sol Plante Atmosphère (ISPA), Institut National de la Recherche Agronomique (INRA)-Ecole Nationale Supérieure des Sciences Agronomiques de Bordeaux-Aquitaine (Bordeaux Sciences Agro), PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), 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), University of Helsinki, Department of Physics, Doctoral Programme in Particle Physics and Universe Sciences, Particle Physics and Astrophysics, Division of Geophysics and Astronomy (-2017), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Interactions Sol Plante Atmosphère (UMR ISPA), Ecole Nationale Supérieure des Sciences Agronomiques de Bordeaux-Aquitaine (Bordeaux Sciences Agro)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), Leibniz Universität Hannover=Leibniz University Hannover, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA), 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
astronomi, Cosmology and cosmography, Milky Way science, 01 natural sciences, Cosmology, General Relativity and Quantum Cosmology, Observatory, Matematikk og Naturvitenskap: 400::Fysikk: 430::Astrofysikk, astronomi: 438 [VDP], Micro-Hz band, 010303 astronomy & astrophysics, media_common, astro-ph.HE, Physics, [PHYS]Physics [physics], General relativity and beyond, General Relativity and Cosmology, Astrophysics::Instrumentation and Methods for Astrophysics, Massive black hole binaries, Interferometry, WHITE-DWARF BINARIES, GAS, GROWTH, MASSIVE BLACK-HOLE, MILKY-WAY, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Multimessenger and multiband Astronomy, Astrophysics and Astronomy, GALACTIC NUCLEI, gr-qc, media_common.quotation_subject, Astrophysics::Cosmology and Extragalactic Astrophysics, 114 Physical sciences, Settore FIS/05 - Astronomia e Astrofisica, Pulsar, 0103 physical sciences, POST-NEWTONIAN EVOLUTION, LISA, 010308 nuclear & particles physics, Gravitational wave, Astronomy, Astronomy and Astrophysics, 115 Astronomy, Space science, Space gravitational wave detector, Universe, Galaxy, Black hole, Space and Planetary Science, [SDU]Sciences of the Universe [physics], PHASE-TRANSITION, astrofysikk, Massive black hole binarie, astro-ph.IM, HUBBLE CONSTANT
Abstract

We propose a space-based interferometer surveying the gravitational wave (GW) sky in the milli-Hz to $\mu$-Hz frequency range. By the 2040s', the $\mu$-Hz frequency band, bracketed in between the Laser Interferometer Space Antenna (LISA) and pulsar timing arrays, will constitute the largest gap in the coverage of the astrophysically relevant GW spectrum. Yet many outstanding questions related to astrophysics and cosmology are best answered by GW observations in this band. We show that a $\mu$-Hz GW detector will be a truly overarching observatory for the scientific community at large, greatly extending the potential of LISA. Conceived to detect massive black hole binaries from their early inspiral with high signal-to-noise ratio, and low-frequency stellar binaries in the Galaxy, this instrument will be a cornerstone for multimessenger astronomy from the solar neighbourhood to the high-redshift Universe., Comment: 28 pages, 8 figures; White Paper submitted to ESA's Voyage 2050 call for papers on behalf of the LISA Consortium 2050 Task Force

Published
2021
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11. Generation of gravitational waves from freely decaying turbulence

Author

Pierre Auclair, Chiara Caprini, Daniel Cutting, Mark Hindmarsh, Kari Rummukainen, Danièle A. Steer, David J. Weir, UCL - SST/IRMP - Institut de recherche en mathématique et physique, 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, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
Astrophysics and Astronomy, velocity, cosmological model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitational radiation: stochastic, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), Fourier transformation, cosmological phase transitions, correlation function, numerical calculations, Monte Carlo, cosmology of theories beyond the SM, Particle Physics - Phenomenology, energy: kinetic, General Relativity and Cosmology, gravitational radiation: background, turbulence, scaling, Astronomy and Astrophysics, High Energy Physics - Phenomenology, correlation: time, pressure: anisotropy, flow, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], spectral, gravitational waves / sources, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study the stochastic gravitational wave background (SGWB) produced by freely decaying vortical turbulence in the early Universe. We thoroughly investigate the time correlation of the velocity field, and hence of the anisotropic stresses producing the gravitational waves. With hydrodynamical simulations, we show that the unequal time correlation function (UETC) of the Fourier components of the velocity field is Gaussian in the time difference, as predicted by the "sweeping" decorrelation model. We introduce a decorrelation model that can be extended to wavelengths around the integral scale of the flow. Supplemented with the evolution laws of the kinetic energy and of the integral scale, this provides a new model UETC of the turbulent velocity field consistent with the simulations. We discuss the UETC as a positive definite kernel, and propose to use the Gibbs kernel for the velocity UETC as a natural way to ensure positive definiteness of the SGWB. The SGWB is given by a 4-dimensional integration of the resulting anisotropic stress UETC with the gravitational wave Green's function. We perform this integration using a Monte Carlo algorithm based on importance sampling, and find that the result matches that of the simulations. Furthermore, the SGWB obtained from the numerical integration and from the simulations show close agreement with a model in which the source is constant in time and abruptly turns off after a few eddy turnover times. Based on this assumption, we provide an approximate analytical form for the SGWB spectrum and its scaling with the initial kinetic energy and integral scale. Finally, we use our model and numerical integration algorithm to show that including an initial growth phase for the turbulent flow heavily influences the spectral shape of the SGWB. This highlights the importance of a complete understanding of the turbulence generation mechanism., Comment: 54 pages, 30 figures

Published
2022
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12. NANOGrav signal from magnetohydrodynamic turbulence at the QCD phase transition in the early Universe

Author

Andrii Neronov, Alberto Roper Pol, Chiara Caprini, Dmitri Semikoz, 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), ANR-19-CE31-0020,MMUniverse,Nouvelles fenêtres sur l'Univers par l'astronomie multi-messenger(2019), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
Cherenkov Telescope Array, magnetic field: high, media_common.quotation_subject, Field strength, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Magnetohydrodynamic turbulence, 01 natural sciences, Gravitational wave background, quantum chromodynamics: critical phenomena, gravitation: stochastic, 0103 physical sciences, gamma ray: detector, structure, 010306 general physics, media_common, Quantum chromodynamics, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, turbulence, tension, Universe, correlation: length, recombination, Magnetic field, Hubble volume, Magnetohydrodynamics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], gravitation: background
Abstract

International audience; The NANOGrav Collaboration has recently reported evidence for the existence of a stochastic gravitational wave background in the 1–100 nHz frequency range. We argue that such a background could have been produced by magnetohydrodynamic (MHD) turbulence at the QCD scale. From the NANOGrav measurement, one can infer the magnetic field parameters: a comoving field strength close to microGauss and a correlation length close to 10% of the Hubble radius at the QCD phase transition epoch. We point out that the turbulent decay of a nonhelical magnetic field with such parameters leads to a magnetic field at the recombination epoch, which would be sufficiently strong to provide a solution to the Hubble tension problem, as recently proposed. We also show that the MHD turbulence interpretation of the NANOGrav signal can be tested via measurements of the relic magnetic field in the voids of the large scale structure, with gamma-ray telescopes like CTA.

Published
2021
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13. Detectable Environmental Effects in GW190521-like Black-Hole Binaries with LISA

Author

Giulia Cusin, Paolo Pani, Nicola Tamanini, Andrea Caputo, Chiara Caprini, Alberto Sesana, Enrico Barausse, Alexandre Toubiana, Laura Sberna, Karan Jani, Stanislav Babak, Sylvain Marsat, 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
Active galactic nucleus, Gravitational-wave observatory, General relativity, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Physics and Astronomy, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitation and Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Astronomical interferometer, 010306 general physics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysics::Instrumentation and Methods for Astrophysics, black holes, Accretion (astrophysics), black holes, gravitational waves, Black hole, Interferometry, gravitational waves, 13. Climate action, Orbital motion, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena
Abstract

GW190521 is the compact binary with the largest masses observed to date, with at least one in the pair-instability gap. This event has also been claimed to be associated with an optical flare observed by the Zwicky Transient Facility in an Active Galactic Nucleus (AGN), possibly due to the post-merger motion of the merger remnant in the AGN gaseous disk. We show that the Laser Interferometer Space Antenna (LISA) will detect up to ten of such gas-rich black hole binaries months to years before their detection by LIGO/Virgo-like interferometers, localizing them in the sky within $\approx1$ deg$^2$. LISA will also measure directly deviations from purely vacuum and stationary waveforms, arising from gas accretion, dynamical friction, and orbital motion around the AGN's massive black hole (acceleration, strong lensing, and Doppler modulation). LISA will therefore be crucial to alert and point electromagnetic telescopes ahead of time on this novel class of gas-rich sources, to gain direct insight on their physics, and to disentangle environmental effects from corrections to General Relativity that may also appear in the waveforms at low frequencies., 6 pages, 4 figures. Matches published version

Published
2021
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14. The missing link in gravitational-wave astronomy: A summary of discoveries waiting in the decihertz range

Author

Barry McKernan, Igor Pikovski, Kaze Wong, Xian Chen, Jose María Ezquiaga, J. Baird, Alberto Sesana, Shimon Kolkowitz, Christopher P. L. Berry, Lijing Shao, Daniela D. Doneva, K. E. Saavik Ford, Guido Mueller, Germano Nardini, Katelyn Breivik, Michael L. Katz, Pau Amaro-Seoane, Tessa Baker, Emanuele Berti, Niels Warburton, Surjeet Rajendran, Michael Zevin, Pierre Auclair, Helvi Witek, Chiara Caprini, Karan Jani, Manuel Arca Sedda, Nicola Tamanini, 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
astronomi, binary: orbit, cosmological model, neutron star: binary, gravitational radiation: stochastic, standard model, 7. Clean energy, 01 natural sciences, Multimessenger astronomy, Cosmology, General Relativity and Quantum Cosmology, Tests of general relativity, Binary evolution, Voyage 2050, Observatory, Decihertz observatories, Matematikk og Naturvitenskap: 400::Fysikk: 430::Astrofysikk, astronomi: 438 [VDP], general relativity, LIGO, white dwarf, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Black holes, Astrophysics::Instrumentation and Methods for Astrophysics, Intermediate-mass black holes, 3. Good health, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Gravitational-wave astronomy, electromagnetic field: production, Neutron stars, Gravitational waves, Binary black hole, binary: coalescence, 0103 physical sciences, Stochastic backgrounds, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, gravitational radiation: frequency, Instrumentation and Methods for Astrophysics (astro-ph.IM), LISA, Space-based detectors, Gravitational wave, Multiband gravitational-wave astronomy, gravitational radiation: background, Astronomy, White dwarfs, Astronomy and Astrophysics, black hole: mass, binary: compact, gravitational radiation detector, detector: sensitivity, Neutron star, VIRGO, black hole: binary, Space and Planetary Science, gravitation, gravitational radiation: emission, star: mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Since 2015 the gravitational-wave observations of LIGO and Virgo have transformed our understanding of compact-object binaries. In the years to come, ground-based gravitational-wave observatories such as LIGO, Virgo, and their successors will increase in sensitivity, discovering thousands of stellar-mass binaries. In the 2030s, the space-based LISA will provide gravitational-wave observations of massive black holes binaries. Between the $\sim 10$-$10^3~\mathrm{Hz}$ band of ground-based observatories and the $\sim10^{-4}$-$10^{-1}~\mathrm{Hz}$ band of LISA lies the uncharted decihertz gravitational-wave band. We propose a Decihertz Observatory to study this frequency range, and to complement observations made by other detectors. Decihertz observatories are well suited to observation of intermediate-mass ($\sim10^2$-$10^4 M_\odot$) black holes; they will be able to detect stellar-mass binaries days to years before they merge, providing early warning of nearby binary neutron star mergers and measurements of the eccentricity of binary black holes, and they will enable new tests of general relativity and the Standard Model of particle physics. Here we summarise how a Decihertz Observatory could provide unique insights into how black holes form and evolve across cosmic time, improve prospects for both multimessenger astronomy and multiband gravitational-wave astronomy, and enable new probes of gravity, particle physics and cosmology., Comment: 13 pages, 1 figure. Published in Experimental Astronomy. Summarising white paper arXiv:1908.11375

Published
2021
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15. Detecting gravitational waves from cosmological phase transitions with LISA: an update

Author

Germano Nardini, Mikael Chala, David J. Weir, G. C. Dorsch, Geraldine Servant, Jonathan Kozaczuk, Pedro Schwaller, Chiara Caprini, Stephan J. Huber, Mark Hindmarsh, Anders Tranberg, Kari Rummukainen, Thomas Konstandin, Jose Miguel No, 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), 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
Phase transition, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics beyond the Standard Model, Dark matter, standard model, FOS: Physical sciences, Context (language use), gravitational radiation: direct detection, 01 natural sciences, dark matter, bubble: nucleation, Gravitational waves, Theoretical physics, High Energy Physics - Phenomenology (hep-ph), effective field theory, 0103 physical sciences, Effective field theory, energy: density, numerical calculations, Cosmological phase transitions, perturbation theory, Physics, Matematikk og Naturvitenskap: 400::Fysikk: 430 [VDP], wave: acoustic, LISA, COSMIC cancer database, 010308 nuclear & particles physics, Gravitational wave, new physics, Gravitational theory, gravitational radiation, Astronomy and Astrophysics, critical phenomena, gravitational radiation detector, High Energy Physics - Phenomenology, Gravitational sources, gravitational radiation: emission, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Higgs model, Perturbation theory (quantum mechanics), gravitational radiation: power spectrum, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], dilaton, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

MC was funded by the Royal Society under the Newton International Fellowship program. GD would like to thank CNPq (Brazil) for financial support. MH was supported by the Science and Technology Facilities Council (grant number ST/P000819/1), and the Academy of Finland (grant number 286769). SJH was supported by the Science and Technology Facilities Council (grant number ST/P000819/1). The work of JK was supported by Department of Energy (DOE) grant DE-SC0019195 and NSF grant PHY-1719642. TK and GS are funded by the Deutsche Forschungsgemeinschaft under Germany's Excellence Strategy - EXC 2121 \Quantum Universe" - 390833306. JMN is supported by Ramon y Cajal Fellowship contract RYC-2017-22986, and also acknowledges support from the Spanish MINECO's "Centro de Excelencia Severo Ochoa" Programme under grant SEV-2016-0597, from the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreements 690575 (RISE InvisiblesPlus) and 674896 (ITN ELUSIVES) and from the Spanish Proyectos de I+D de Generacion de Conocimiento via grant PGC2018-096646-A-I00. KR is funded by the Academy of Finland grants 308791, 319066 and 320123. PS is supported by the Cluster of Excellence "Precision Physics, Fundamental Interactions, and Structure of Matter"(PRISMA+ EXC 2118/1) funded by the German Research Foundation(DFG). PS would like to thank Moritz Breitbach and Eric Madge for providing the data for figures (14), (15) and (16), and Eric Madge for checking the ptplot code. DJW (ORCID ID 0000-00016986-0517) was supported by an Science and Technology Facilities Council Ernest Rutherford Fellowship, grant no. ST/R003904/1, by the Research Funds of the University of Helsinki, and by the Academy of Finland, grant nos. 286769, 324882 and 328958. The original LISA Cosmology Working Group preprint number of this paper is \LISA CosWG-19-04"., We investigate the potential for observing gravitational waves from cosmological phase transitions with LISA in light of recent theoretical and experimental developments. Our analysis is based on current state-of-the-art simulations of sound waves in the cosmic fluid after the phase transition completes. We discuss the various sources of gravitational radiation, the underlying parameters describing the phase transition and a variety of viable particle physics models in this context, clarifying common misconceptions that appear in the literature and identifying open questions requiring future study. We also present a web-based tool, PTPlot, that allows users to obtain up-to-date detection prospects for a given set of phase transition parameters at LISA., Royal Society under the Newton International Fellowship program, National Council for Scientific and Technological Development (CNPq), UK Research & Innovation (UKRI) Science & Technology Facilities Council (STFC) ST/P000819/1, Academy of Finland European Commission 286769 308791 319066 320123 324882 328958, United States Department of Energy (DOE) DE-SC0019195, National Science Foundation (NSF) PHY-1719642, German Research Foundation (DFG) EXC 2121 390833306, Spanish Government RYC-2017-22986, Spanish MINECO's "Centro de Excelencia Severo Ochoa" Programme SEV-2016-0597, European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant 690575 674896, Spanish Proyectos de I+D de Generacion de Conocimiento PGC2018-096646-A-I00, German Research Foundation (DFG) EXC 2118/1, Science and Technology Facilities Council Ernest Rutherford Fellowship 0000-00016986-0517 ST/R003904/1, Research Funds of the University of Helsinki

Published
2020
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16. Peculiar acceleration of stellar-origin black hole binaries: Measurement and biases with LISA

Author

Antoine Klein, Chiara Caprini, Enrico Barausse, Nicola Tamanini, Camille Bonvin, 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), 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), 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), 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
coalescence, long-lived, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, star: cluster, accretion, LIGO, [PHYS]Physics [physics], Physics, lifetime, education.field_of_study, Hubble constant, formation, Astrophysics::Instrumentation and Methods for Astrophysics, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - Instrumentation and Methods for Astrophysics, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Population, astro-ph.IM, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], AGN, 010306 general physics, education, Luminosity distance, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, LISA, 010308 nuclear & particles physics, Gravitational wave, nucleus, acceleration, black hole: mass, redshift, calibration, Galaxy, Redshift, VIRGO, frequency: low, black hole: binary, 13. Climate action, gravitational radiation: emission, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hubble's law, Astrophysics and astroparticle physics
Abstract

We investigate the ability of the Laser Interferometer Space Antenna (LISA) to measure the center of mass acceleration of stellar-origin black hole binaries emitting gravitational waves. Our analysis is based on the idea that the acceleration of the center of mass induces a time variation in the redshift of the gravitational wave, which in turn modifies its waveform. We confirm that while the cosmological acceleration is too small to leave a detectable imprint on the gravitational waveforms observable by LISA, larger peculiar accelerations may be measurable for sufficiently long lived sources. We focus on stellar mass black hole binaries, which will be detectable at low frequencies by LISA and near coalescence by ground based detectors. These sources may have large peculiar accelerations, for instance, if they form in nuclear star clusters or in AGN accretion disks. If that is the case, we find that in an astrophysical population calibrated to the LIGO-Virgo observed merger rate, LISA will be able to measure the peculiar acceleration of a small but significant fraction of the events if the mission lifetime is extended beyond the nominal duration of 4 years. In this scenario LISA will be able to assess whether black hole binaries form close to galactic centers, particularly in AGN disks, and will thus help discriminate between different formation mechanisms. Although for a nominal 4 years LISA mission the peculiar acceleration effect cannot be measured, a consistent fraction of events may be biased by strong peculiar accelerations which, if present, may imprint large systematic errors on some waveform parameters. In particular, estimates of the luminosity distance could be strongly biased and consequently induce large systematic errors on LISA measurements of the Hubble constant with stellar mass black hole binaries., Comment: 21 pages, 2 figures, 3 tables; v2 matches published version

Published
2020
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17. The missing link in gravitational-wave astronomy: discoveries waiting in the decihertz range

Author

K. E. Saavik Ford, Christopher P. L. Berry, Daniela D. Doneva, Niels Warburton, Tessa Baker, Kaze Wong, Jose María Ezquiaga, Guido Mueller, Michael L. Katz, Karan Jani, Surjeet Rajendran, Katelyn Breivik, Barry McKernan, Pau Amaro-Seoane, Nicola Tamanini, Adam Burrows, Shimon Kolkowitz, Germano Nardini, Chiara Caprini, Michael Zevin, Igor Pikovski, Pierre Auclair, Manuel Arca Sedda, Alberto Sesana, David Vartanyan, Helvi Witek, Xian Chen, Lijing Shao, J. Baird, Emanuele Berti, 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), Max Planck Institute for Gravitational Physics (Albert Einstein Institute) (AEI), Max-Planck-Gesellschaft, 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), Department of Physics and Astronomy [U Mississippi], The University of Mississippi [Oxford], Affymetrix Inc., Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), 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), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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)-Université Paris Diderot - Paris 7 (UPD7)-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), and Harvard University-Smithsonian Institution

Subjects
Physics and Astronomy (miscellaneous), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 7. Clean energy, 01 natural sciences, Gravitational-wave astronomy, General Relativity and Quantum Cosmology, Cosmology, Gravitation, Binary black hole, Observatory, Tests of general relativity, 0103 physical sciences, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics - Astrophysics of Galaxies, LIGO, Neutron star, 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The gravitational-wave astronomical revolution began in 2015 with LIGO's observation of the coalescence of two stellar-mass black holes. Over the coming decades, ground-based detectors like LIGO will extend their reach, discovering thousands of stellar-mass binaries. In the 2030s, the space-based LISA will enable gravitational-wave observations of the massive black holes in galactic centres. Between LISA and ground-based observatories lies the unexplored decihertz gravitational-wave frequency band. Here, we propose a Decihertz Observatory to cover this band, and complement observations made by other gravitational-wave observatories. The decihertz band is uniquely suited to observation of intermediate-mass ($\sim 10^2$-$10^4 M_\odot$) black holes, which may form the missing link between stellar-mass and massive black holes, offering a unique opportunity to measure their properties. Decihertz observations will be able to detect stellar-mass binaries days to years before they merge and are observed by ground-based detectors, providing early warning of nearby binary neutron star mergers, and enabling measurements of the eccentricity of binary black holes, providing revealing insights into their formation. Observing decihertz gravitational-waves also opens the possibility of testing fundamental physics in a new laboratory, permitting unique tests of general relativity and the Standard Model of particle physics. Overall, a Decihertz Observatory will answer key questions about how black holes form and evolve across cosmic time, open new avenues for multimessenger astronomy, and advance our understanding of gravitation, particle physics and cosmology., 52 pages, 5 figures, 4 tables. Submitted to Classical & Quantum Gravity. Based upon a white paper for ESA's Voyage 2050 on behalf of the LISA Consortium 2050 Task Force

Published
2020
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18. Reconstructing the spectral shape of a stochastic gravitational wave background with LISA

Author

Daniel G. Figueroa, Raphael Flauger, Mauro Pieroni, Angelo Ricciardone, Chiara Caprini, Marco Peloso, Gianmassimo Tasinato, Germano Nardini, 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), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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, data analysis method, noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Spectral shape analysis, gravitational radiation: stochastic, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, Noise (electronics), Signal, General Relativity and Quantum Cosmology, Gravitational wave background, High Energy Physics - Phenomenology (hep-ph), gravitational waves / experiments, LISA: sensitivity, 0103 physical sciences, numerical methods, Sensitivity (control systems), primordial gravitational waves (theory), astro-ph.CO, High Energy Physics - Phenomenology, 010306 general physics, Physics, 010308 nuclear & particles physics, Numerical analysis, gravitational radiation: background, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, Astronomy and Astrophysics, radiation, detector: sensitivity, Amplitude, High Energy Physics - Theory (hep-th), gravitational radiation: power spectrum, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Algorithm, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a set of tools to assess the capabilities of LISA to detect and reconstruct the spectral shape and amplitude of a stochastic gravitational wave background (SGWB). We first provide the LISA power-law sensitivity curve and binned power-law sensitivity curves, based on the latest updates on the LISA design. These curves are useful to make a qualitative assessment of the detection and reconstruction prospects of a SGWB. For a quantitative reconstruction of a SGWB with arbitrary power spectrum shape, we propose a novel data analysis technique: by means of an automatized adaptive procedure, we conveniently split the LISA sensitivity band into frequency bins, and fit the data inside each bin with a power law signal plus a model of the instrumental noise. We apply the procedure to SGWB signals with a variety of representative frequency profiles, and prove that LISA can reconstruct their spectral shape. Our procedure, implemented in the code SGWBinner, is suitable for homogeneous and isotropic SGWBs detectable at LISA, and it is also expected to work for other gravitational wave observatories., 40 pages, 22 figures

Published
2019
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19. Astrophysical Gravitational Waves in Conformal Gravity

Author

Chiara Caprini, Patric Hölscher, Dominik J. Schwarz, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie ( APC - UMR 7164 ), and Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA )

Subjects
General relativity, Dark matter, FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), graviton: mass, 01 natural sciences, General Relativity and Quantum Cosmology, dark matter, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Gravitation, nonrelativistic, gravitation: conformal, 0103 physical sciences, 010306 general physics, Galaxy rotation curve, orbit, Physics, 010308 nuclear & particles physics, Gravitational wave, Graviton, field equations, binary: compact, moment, Conformal gravity, Weyl, quantum gravity, Quantum electrodynamics, gravitational radiation: emission, tensor: energy-momentum, galaxy: rotation, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Quantum gravity, time dependence, energy-momentum: conservation law, mass: gravitation
Abstract

We investigate the gravitational radiation from binary systems in conformal gravity (CG) and massive conformal gravity (MCG). CG might explain observed galaxy rotation curves without dark matter, and both models are of interest in the context of quantum gravity. Here we show that gravitational radiation emitted by compact binaries allows us to strongly constrain both models. We work in Weyl gauge, which fixes the rescaling invariance of the models, and derive the linearized fourth-order equation of motion for the metric, which describes massless and massive modes of propagation. In the limit of a large graviton mass, MCG reduces to general relativity (GR), whereas CG does not. Coordinates are fixed by Teyssandier gauge to show that for a conserved energy-momentum tensor the gravitational radiation is due to the time-dependent quadrupole moment of a non-relativistic source and we derive the gravitational energy-momentum tensor for both models. We apply our findings to the case of close binaries on circular orbits, which have been used to indirectly infer the existence of gravitational radiation prior to the direct observation of gravitational waves. As an example, we analyze the binary system PSR J1012+5307, chosen for its small eccentricity. When fixing the graviton mass in CG such that observed galaxy rotation curves could be explained without dark matter, the gravitational radiation of a binary system is much smaller than in GR. The same holds for MCG for small masses of the graviton. Thus gravitational radiation cannot explain the orbital decay of binary systems and replace dark matter simultaneously. We also analyse MCG for large graviton masses and conclude that MCG can describe the orbital periods of compact binaries in agreement with data, as it reduces to GR in that limit., Comment: v2: 21 pages, no figures; Uses REVTeX 4.1; added a comment and references in section 1; corrected sign in eqn. (3)

Published
2018
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20. Inflationary magnetogenesis with added helicity: constraints from non-gaussianities

Author

Lorenzo Sorbo, Chiara Caprini, Maria Chiara Guzzetti, 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut 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
scale: inflation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics and Astronomy (miscellaneous), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Scalar (mathematics), FOS: Physical sciences, magnetic field, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Theoretical physics, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), Non-Gaussianity, 0103 physical sciences, strong coupling, spectrum: scalar, 010306 general physics, Physics, Inflation (cosmology), Slow roll, 010308 nuclear & particles physics, inflation: slow-roll approximation, back reaction, helicity, inflation: model, bispectrum, High Energy Physics - Phenomenology, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], non-Gaussianity, [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Back-reaction, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Scalar field, Bispectrum, Dynamo, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In previous work, two of us have proposed a model of inflationary magnetogenesis based on a rolling auxiliary field able both to account for the magnetic fields inferred by the (non) observation of gamma-rays from blazars, and to start the galactic dynamo, without incurring in any strong coupling or strong backreaction regime. Here we evaluate the correction to the scalar spectrum and bispectrum with respect to single-field slow-roll inflation generated in that scenario. The strongest constraints on the model originate from the non-observation of a scalar bispectrum. Nevertheless, even when those constraints are taken into consideration, the scenario can successfully account for the observed magnetic fields as long as the energy scale of inflation is smaller than $10^6\div10^8$~GeV, under some conditions on the slow roll of the auxiliary scalar field., 34 pages, 4 figures; published version, references added; changes in the requirements on the duration and velocity of the rolling of the auxiliary field; main conclusions unaffected

Published
2018
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21. Multi-wavelength observations of cosmological phase transitions using LISA and Cosmic Explorer

Author

Andrew Matas, S. Banagiri, Chiara Caprini, Vuk Mandic, Margot Fitz Axen, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
Phase transition, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitational radiation: stochastic, media_common.quotation_subject, Critical phenomena, FOS: Physical sciences, Astrophysics, Parameter space, 01 natural sciences, Gravitational wave background, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), media_common, Physics, LISA, COSMIC cancer database, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: background, Detector, critical phenomena, sensitivity, Universe, Cosmology, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We reanalyze the detection possibilities for gravitational waves arising from cosmological first order phase transitions. We discuss the stochastic gravitational wave background corresponding to the three expected scenarios of phase transition dynamics. We then perform an analysis on the detection possibilities for each case using sensitivities for the next generation ground-based detector Cosmic Explorer and the current LISA proposal, using two analysis methods. We find that having both detectors allows wide detection possibilities over much of the parameter space, including that corresponding to several points relevant to different early Universe models.

Published
2018
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22. Cosmological Backgrounds of Gravitational Waves

Author

Chiara Caprini, Daniel G. Figueroa, 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), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut 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), 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
cosmological model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics and Astronomy (miscellaneous), gravitational radiation: stochastic, electroweak interaction: symmetry breaking, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, defect: topological, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, resonance: parametric, Cosmology, General Relativity and Quantum Cosmology, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], High Energy Physics - Phenomenology (hep-ph), Vacuum energy, 0103 physical sciences, KAGRA, 010306 general physics, cosmic string, Physics, energy: high, Einstein Telescope, preheating, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: background, Astrophysics::Instrumentation and Methods for Astrophysics, inflation: slow-roll approximation, gravitational radiation, Astronomy, critical phenomena, LIGO, gravitational radiation detector, background: stochastic, Cosmic string, High Energy Physics - Phenomenology, gravitational radiation: emission, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Phenomenology (particle physics), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Gravitational waves (GWs) have a great potential to probe cosmology. We review early universe sources that can lead to cosmological backgrounds of GWs. We begin by presenting definitions of GWs in flat space-time and in a cosmological setting, and discussing the reasons why GW backgrounds from the early universe are of a stochastic nature. We recap current observational constraints on stochastic backgrounds, and discuss some of the characteristics of present and future GW detectors including advanced LIGO, advanced Virgo, the Einstein Telescope, KAGRA, LISA. We then review in detail early universe GW generation mechanisms proposed in the literature, as well as the properties of the GW backgrounds they give rise to. We classify the backgrounds in five categories: GWs from quantum vacuum fluctuations during standard slow-roll inflation, GWs from processes that operate within extensions of the standard inflationary paradigm, GWs from post-inflationary preheating and related non-perturbative phenomena, GWs from first order phase transitions (related or not to the electroweak symmetry breaking), and GWs from topological defects, in particular from cosmic strings. The phenomenology of early universe processes that can generate a stochastic background of GWs is extremely rich, and some backgrounds are within the reach of near-future GW detectors. A future detection of any of these backgrounds will provide crucial information on the underlying high energy theory describing the early universe, probing energy scales well beyond the reach of particle accelerators., third version, corrected typos and the section about the transfer function, acknowledgements added

Published
2018
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23. Effect of matter structure on the gravitational waveform

Author

Chiara Caprini, Nicola Tamanini, Riccardo Sturani, Camille Bonvin, University of Geneva, Université Paris-Saclay, Université Paris-Diderot, Universidade Estadual Paulista (Unesp), 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 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), 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), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-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)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut de 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 ), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
binary: mass, Cosmology and Nongalactic Astrophysics (astro-ph.CO), General relativity, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], interferometer, FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Gravitational acceleration, 01 natural sciences, General Relativity and Quantum Cosmology, Metric expansion of space, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Gravitation, Acceleration, binary: coalescence, 0103 physical sciences, Chirp, general relativity, 010306 general physics, Physics, LISA, 010308 nuclear & particles physics, Gravitational wave, matter: effect, redshift, gravitational radiation detector, Interferometry, gravitational radiation: emission, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], expansion: acceleration, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Third generation ground-based interferometers as well as the planned space-based interferometer LISA are expected to detect a plethora of gravitational wave signals from coalescing binaries at cosmological distance. The emitted gravitational waves propagate in the expanding universe through the inhomogeneous distribution of matter. Here we show that the acceleration of the universe and the peculiar acceleration of the binary with respect to the observer distort the gravitational chirp signal from the simplest General Relativity prediction beyond a mere time independent rescaling of the chirp mass, affecting intrinsic parameter estimations for the binaries visible by LISA. We find that the effect due to the peculiar acceleration can be much larger than the one due to the universe acceleration. Moreover, peculiar accelerations can introduce a bias in the estimation of parameters such as the time of coalescence and the individual masses of the binary. An error in the estimation of the arrival time will have an impact in the case of sources visible first by LISA and later by ground based interferometers., Comment: 15 pages, 7 figures. v2: added references and one new figure; extended discussion, conclusions unchanged. v3: matching published version

Published
2017
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24. Probing stellar binary black hole formation in galactic nuclei via the imprint of their center of mass acceleration on their gravitational wave signal

Author

Chiara Caprini, Zoltan Haiman, Kohei Inayoshi, Nicola Tamanini, 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), 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), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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 ), AstroParticule et Cosmologie ( APC - UMR 7164 ), and Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA )

Subjects
04.25.-g, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, galaxy: coalescence, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), 04.80.Cc, 01 natural sciences, General Relativity and Quantum Cosmology, star: cluster, black hole: formation, accretion, Binary black hole, 0103 physical sciences, AGN, capture, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), LISA, Supermassive black hole, Gravitational wave, nucleus, gravitational radiation, Astronomy, acceleration, 04.30.-w, Galaxy, electromagnetic, black hole: binary, Intermediate-mass black hole, Stellar black hole, Spin-flip, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Multi-frequency gravitational wave (GW) observations are useful probes of the formation processes of coalescing stellar-mass binary black holes (BBHs). We discuss the phase drift in the GW inspiral waveform of the merging BBH caused by its center-of-mass acceleration. The acceleration strongly depends on the location where a BBH forms within a galaxy, allowing observations of the early inspiral phase of LIGO-like BBH mergers by the Laser Interferometer Space Antenna (LISA) to test the formation mechanism. In particular, BBHs formed in dense nuclear star clusters or via compact accretion disks around a nuclear supermassive black hole in active galactic nuclei would suffer strong acceleration, and produce large phase drifts measurable by LISA. The host galaxies of the coalescing BBHs in these scenarios can also be uniquely identified in the LISA error volume, without electromagnetic counterparts. A non-detection of phase drifts would rule out or constrain the contribution of the nuclear formation channels to the stellar-mass BBH population., Comment: 8 pages, 4 figures, 1 table, accepted for publication in Physical Review D

Published
2017
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26. Constraints on the Electrical Charge Asymmetry of the Universe

Author

Pedro G. Ferreira and Chiara Caprini

Subjects
Physics, Particle physics, Spectral index, media_common.quotation_subject, Dark matter, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Charge (physics), Electron, Astrophysics, Electric charge, Asymmetry, Baryon, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Neutrino, media_common
Abstract

We use the isotropy of the Cosmic Microwave Background to place stringent constraints on a possible electrical charge asymmetry of the universe. We find the excess charge per baryon to be $q_{e-p}, New version to appear in JCAP

Published
2016
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27. Science with the space-based interferometer eLISA. II: gravitational waves from cosmological phase transitions

Author

Germano Nardini, Thomas Konstandin, Jose Miguel No, Stephan J. Huber, Mark Hindmarsh, Antoine Petiteau, David J. Weir, Pedro Schwaller, Chiara Caprini, Jonathan Kozaczuk, Geraldine Servant, 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), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), 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 ), 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 ), 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
Phase transition, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitational radiation: stochastic, 530 Physics, media_common.quotation_subject, Physics beyond the Standard Model, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Magnetohydrodynamic turbulence, 01 natural sciences, General Relativity and Quantum Cosmology, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Gravitational wave background, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, ddc:530, 010306 general physics, detector: design, media_common, Physics, 010308 nuclear & particles physics, Gravitational wave, new physics, Detector, turbulence, gravitational radiation: background, Astronomy and Astrophysics, critical phenomena, gravitational radiation detector: satellite, sensitivity, Universe, background: stochastic, Computational physics, Interferometry, 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], gravitational radiation detector: interferometer, [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We investigate the potential for the eLISA space-based interferometer to detect the stochastic gravitational wave background produced by strong first-order cosmological phase transitions. We discuss the resulting contributions from bubble collisions, magnetohydrodynamic turbulence, and sound waves to the stochastic background, and estimate the total corresponding signal predicted in gravitational waves. The projected sensitivity of eLISA to cosmological phase transitions is computed in a model-independent way for various detector designs and configurations. By applying these results to several specific models, we demonstrate that eLISA is able to probe many well-motivated scenarios beyond the Standard Model of particle physics predicting strong first-order cosmological phase transitions in the early Universe., Comment: 45 pages, 7 figures. Accepted for publication in JCAP, added discussion on noise from galactic binaries and citations

Published
2016
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28. Science with the space-based interferometer eLISA. III: probing the expansion of the universe using gravitational wave standard sirens

Author

Antoine Klein, Antoine Petiteau, Nicola Tamanini, Enrico Barausse, Alberto Sesana, Chiara Caprini, 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), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of Birmingham [Birmingham], Mississippi State University [Mississippi], AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Pierre et Marie Curie - Paris 6 (UPMC)-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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Tamanini, N, Caprini, C, Barausse, E, Sesana, A, Klein, A, Petiteau, A, 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
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Metric expansion of space, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, massive black holes, 010303 astronomy & astrophysics, gravitational wave detector, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Gravitational wave, Astronomy and Astrophysics, Observable, Redshift, Black hole, Interferometry, 13. Climate action, dark energy experiment, gravitational waves / source, symbols, Dark energy, Astrophysics - High Energy Astrophysical Phenomena, Hubble's law, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We investigate the capability of various configurations of the space interferometer eLISA to probe the late-time background expansion of the universe using gravitational wave standard sirens. We simulate catalogues of standard sirens composed by massive black hole binaries whose gravitational radiation is detectable by eLISA, and which are likely to produce an electromagnetic counterpart observable by future surveys. The main issue for the identification of a counterpart resides in the capability of obtaining an accurate enough sky localisation with eLISA. This seriously challenges the capability of four-link (2 arm) configurations to successfully constrain the cosmological parameters. Conversely, six-link (3 arm) configurations have the potential to provide a test of the expansion of the universe up to $z\sim 8$ which is complementary to other cosmological probes based on electromagnetic observations only. In particular, in the most favourable scenarios, they can provide a significant constraint on $H_0$ at the level of 0.5%. Furthermore, $(\Omega_M, \Omega_\Lambda)$ can be constrained to a level competitive with present SNIa results. On the other hand, the lack of massive black hole binary standard sirens at low redshift allows to constrain dark energy only at the level of few percent., Comment: JCAP style, 48 pages, 16 figures, 10 tables; v2: minor addition to match published version; v3: acknowledgements added

Published
2016
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29. Science with the space-based interferometer LISA. IV: Probing inflation with gravitational waves

Author

Valerie Domcke, Lorenzo Sorbo, Juan Garcia-Bellido, Angelo Ricciardone, Chiara Caprini, Gianmassimo Tasinato, Nicola Bartolo, Michele Liguori, Marco Peloso, Sabino Matarrese, Daniel G. Figueroa, Mairi Sakellariadou, Antoine Petiteau, Maria Chiara Guzzetti, 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), AstroParticule et Cosmologie ( APC - UMR 7164 ), and Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA )

Subjects
Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), gravitational radiation: stochastic, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], interferometer, FOS: Physical sciences, Primordial black hole, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symmetry breaking, General Relativity and Quantum Cosmology, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Gravitational wave background, Theoretical physics, High Energy Physics - Phenomenology (hep-ph), LISA: sensitivity, 0103 physical sciences, Symmetry breaking, Tensor, 010306 general physics, detector: design, Physics, Inflation (cosmology), inflation: effective field theory, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: background, Astronomy and Astrophysics, gravitational radiation detector: satellite, velocity: acoustic, gravitational radiation detector, High Energy Physics - Phenomenology, Interferometry, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Gravitational waves. Inflation. LISA, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], black hole: primordial, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We investigate the potential for the LISA space-based interferometer to detect the stochastic gravitational wave background produced from different mechanisms during inflation. Focusing on well-motivated scenarios, we study the resulting contributions from particle production during inflation, inflationary spectator fields with varying speed of sound, effective field theories of inflation with specific patterns of symmetry breaking and models leading to the formation of primordial black holes. The projected sensitivities of LISA are used in a model-independent way for various detector designs and configurations. We demonstrate that LISA is able to probe these well-motivated inflationary scenarios beyond the irreducible vacuum tensor modes expected from any inflationary background., Comment: 53 pages, 18 figures; v2: minor changes to match published version

Published
2016
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30. Gamma-ray observations of blazars and the intergalactic magnetic field spectrum

Author

Stefano Gabici, Chiara Caprini, 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), 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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 Astrophysical Phenomena (astro-ph.HE), Inflation (cosmology), Physics, [PHYS]Physics [physics], Nuclear and High Energy Physics, Spectral index, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), 010308 nuclear & particles physics, FOS: Physical sciences, Field strength, Astrophysics, 01 natural sciences, Upper and lower bounds, Spectral line, Magnetic field, 0103 physical sciences, Intergalactic travel, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Very-high energy observations of blazars can be used to constrain the strength of the intergalactic magnetic field. A simplifying assumption which is often made is that of a magnetic field of constant strength composed by randomly oriented and identical cells. In this paper, we demonstrate that a more realistic description of the structure of the intergalactic magnetic field is indeed needed. If such a description is adopted, the observational bounds on the field strength are significantly affected in the limit of short field correlation lengths: in particular, they acquire a dependence on the magnetic field power spectrum. In the case of intergalactic magnetic fields which are generated causally, for which the magnetic field large scale spectral index is $n_B\geq 2$ and even, the observational lower bound becomes more constraining by about a factor 3. If instead $-3, Comment: 9 pages, 5 figures

Published
2015
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31. Stochastic background of gravitational waves from cosmological sources

Author

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

Subjects
Physics, History, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Gravitational wave, media_common.quotation_subject, FOS: Physical sciences, Observable, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Universe, Computer Science Applications, Education, 0103 physical sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], 010306 general physics, Astrophysics - Cosmology and Nongalactic Astrophysics, media_common
Abstract

Gravitational waves (GW) can constitute a unique probe of the primordial universe. In many cases, the characteristic frequency of the emitted GW is directly related to the energy scale at which the GW source is operating in the early universe. Consequently, different GW detectors can probe different energy scales in the evolution of the universe. After a general introduction on the properties of a GW stochastic background of primordial origin, some examples of cosmological sources are presented, which may lead to observable GW signals., Comment: Proceedings of LISA Symposium X, accepted for publication in Journal of Physics: Conference Series. Typos corrected, two references added

Published
2015
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32. Adding helicity to inflationary magnetogenesis

Author

Lorenzo Sorbo, Chiara Caprini, Institut de Physique Théorique - UMR CNRS 3681 (IPHT), 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, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Kinetic term, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Gravitation, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Gauge theory, Tensor, 010306 general physics, Inflation (cosmology), Physics, 010308 nuclear & particles physics, Gravitational wave, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], Astronomy and Astrophysics, Helicity, Pseudoscalar, High Energy Physics - Phenomenology, High Energy Physics - Theory (hep-th), Quantum electrodynamics, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The most studied mechanism of inflationary magnetogenesis relies on the time-dependence of the coefficient of the gauge kinetic term $F_{\mu\nu}\,{F}^{\mu\nu}$. Unfortunately, only extremely finely tuned versions of the model can consistently generate the cosmological magnetic fields required by observations. We propose a generalization of this model, where also the pseudoscalar invariant $F_{\mu\nu}\,\tilde{F}^{\mu\nu}$ is multiplied by a time dependent function. The new parity violating term allows more freedom in tuning the amplitude of the field at the end of inflation. Moreover, it leads to a helical magnetic field that is amplified at large scales by magnetohydrodynamical processes during the radiation dominated epoch. As a consequence, our model can satisfy the observational lower bounds on fields in the intergalactic medium, while providing a seed for the galactic dynamo, if inflation occurs at an energy scale ranging from $10^5$ to $10^{10}$ GeV. Such energy scale is well below that suggested by the recent BICEP2 result, if the latter is due to primordial tensor modes. However, the gauge field is a source of tensors during inflation and generates a spectrum of gravitational waves that can give a sizable tensor to scalar ratio $r={\cal O}(0.2)$ even if inflation occurs at low energies. This system therefore evades the Lyth bound. For smaller values of $r$, lower values of the inflationary energy scale are required. The model predicts fully helical cosmological magnetic fields and a chiral spectrum of primordial gravitational waves., Comment: 17 pages, 4 figures. Minor changes to match the version accepted for publication in JCAP

Published
2014
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33. Gravitational waves from first order phase transitions

Author

Chiara Caprini

Subjects
Physics, Atom interferometer, Gravitational-wave observatory, Classical mechanics, Gravitational field, Gravitational wave, Quantum electrodynamics, Gravitational acceleration, Magnetohydrodynamic turbulence, Gravitational redshift, Gravitational energy
Abstract

Gravitational waves can constitute a unique probe of the very early universe. We discuss here the gravitational wave signal from a primordial first order phase transition occurring at high energy scales. The gravitational waves are produced by the collision of broken phase bubbles and by the magnetohydrodynamic turbulence in the primordial plasma stirred by the bubble collision. We show how the shape and amplitude of the gravitational wave power spectrum can be predicted by general arguments based on the source properties, such as its time evolution and space structure. The parametersdescribing the characteristics of the phasetransition (for instance, its duration and strength), which enter in the determination of the gravitational wave spectrum, can be evaluated in the context of specific models of the first order phase transition. We present here two examples of first order phase transitions which lead to a gravitational wave signal falling in the frequency range of detection of the future space-based interferometer eLISA.

Published
2014
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34. Magnetic fields from inflation: The CMB temperature anisotropies

Author

Ruth Durrer, Chiara Caprini, Camille Bonvin, 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), Kavli Institute for Cosmology [Cambridge] (KICC), University of Cambridge [UK] (CAM), Department of Applied Mathematics and Theoretical Physics [Cambridge] (DAMTP), Faculty of mathematics Centre for Mathematical Sciences [Cambridge] (CMS), University of Cambridge [UK] (CAM)-University of Cambridge [UK] (CAM), Departement de Physique Théorique [Genève], Université de Genève = University of Geneva (UNIGE), and the Swiss National Science Foundation and the (U.S.) National Science Foundation under Grant No. NSF PHY11-25915

Subjects
Physics, Inflation (cosmology), Nuclear and High Energy Physics, Spectral index, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Cosmic microwave background, FOS: Physical sciences, Spectral density, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Scale invariance, 01 natural sciences, General Relativity and Quantum Cosmology, Magnetic field, PACS numbers: 98.80.k, 07.55.Db, 98.80.Cq, 98.80.Es, Amplitude, Quantum mechanics, 0103 physical sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], 010306 general physics, Anisotropy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The cosmic microwave background (CMB) temperature anisotropies from primordial magnetic fields are studied. In addition to the known passive and the compensated mode we discuss an inflationary magnetic mode in the curvature perturbation, present when magnetic fields are generated during inflation. This mode is absent if the generation mechanism is causal, e.g. a phase transition. We compute and discuss the effect of this mode on the observed CMB anisotropy spectrum, in comparison with the passive and compensated ones. We find that it dominates the CMB anisotropy, and consequently leads to stronger constraints on the amplitude $B_{1\,{\rm Mpc}}$ and spectral index $n_B$ of the magnetic field than what usually found in CMB analyses from the compensated mode. This happens in particular for spectral indexes $n_B>-3$: the inflationary magnetic mode is always scale invariant, therefore through this mode even a magnetic field with a spectrum which is not scale invariant can leave a detectable signal in the CMB at large scales., 15 pages, 4 figures; v2 minor changes, matches published version

Published
2013
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35. Constraining early and interacting dark energy with gravitational wave standard sirens: the potential of the eLISA mission

Author

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

Subjects
noise, cosmological model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], interferometer, Dark matter, Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), cosmic background radiation, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, dark matter, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], 0103 physical sciences, energy: density, 010306 general physics, Physics, LISA, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation, Astronomy and Astrophysics, redshift, gravitational radiation detector: satellite, dark energy: interaction, Redshift, Black hole, frequency: low, electromagnetic, black hole: binary, dark energy: density, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Dark energy, energy: exchange, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Noise (radio), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We perform a forecast analysis of the capability of the eLISA space-based interferometer to constrain models of early and interacting dark energy using gravitational wave standard sirens. We employ simulated catalogues of standard sirens given by merging massive black hole binaries visible by eLISA, with an electromagnetic counterpart detectable by future telescopes. We consider three-arms mission designs with arm length of 1, 2 and 5 million km, 5 years of mission duration and the best-level low frequency noise as recently tested by the LISA Pathfinder. Standard sirens with eLISA give access to an intermediate range of redshift $1\lesssim z \lesssim 8$, and can therefore provide competitive constraints on models where the onset of the deviation from $\Lambda$CDM (i.e. the epoch when early dark energy starts to be non-negligible, or when the interaction with dark matter begins) occurs relatively late, at $z\lesssim 6$. If instead early or interacting dark energy is relevant already in the pre-recombination era, current cosmological probes (especially the cosmic microwave background) are more efficient than eLISA in constraining these models, except possibly in the interacting dark energy model if the energy exchange is proportional to the energy density of dark energy., Comment: JCAP style, 26 pages, 11 figures, 3 tables; v2: acknowledgements added

Published
2016
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36. Magnetic fields from inflation: The transition to the radiation era

Author

Chiara Caprini, Camille Bonvin, and Ruth Durrer

Subjects
Inflation (cosmology), Physics, Nuclear and High Energy Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Cosmic microwave background, Scalar (physics), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Cosmology, Magnetic field, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Classical mechanics, Quantum electrodynamics, Observational cosmology, Magnet, 0103 physical sciences, Constant (mathematics), 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We compute the contribution to the scalar metric perturbations from large-scale magnetic fields which are generated during inflation. We show that apart from the usual passive and compensated modes, the magnetic fields also contribute to the constant mode from inflation. This is different from the causal (post inflationary) generation of magnetic fields where such a mode is absent and it might lead to significant, non-Gaussian CMB anisotropies., Comment: 19 pages, no figures. v2: Substantially revised version with different conclusions. v3: one reference added, matches version accepted for publication in PRD

Published
2012
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37. Low-frequency gravitational-wave science with eLISA/NGO

Author

Edward K. Porter, Alberto Sesana, T. J. Sumner, Pierre Binétruy, Alberto Lobo, Jonathan R. Gair, Monica Colpi, Tyson Littenberg, Ryan N. Lang, Chiara Caprini, Emanuele Berti, Sean T. McWilliams, H. Ward, Bernard F. Schutz, Gijs Nelemans, Robin Stebbins, Marta Volonteri, Pau Amaro-Seoane, Karsten Danzmann, Antoine Petiteau, Antoine Klein, Stefano Vitale, Jean-François Dufaux, Sofiane Aoudia, Michele Vallisneri, Alejandro Bohé, Neil J. Cornish, Philippe Jetzer, Stanislav Babak, Oliver Jennrich, Max Planck Institute for Gravitational Physics (Albert Einstein Institute) (AEI), Max-Planck-Gesellschaft, Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), APC - THEORIE, 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut für theoretische Physik, Universität Hamburg (UHH)-Universität Hamburg (UHH), Department of Physics and Astronomy [U Mississippi], The University of Mississippi [Oxford], California Institute of Technology (CALTECH), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut 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), Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), Department of Physics, Montana State University (MSU), Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Agence Spatiale Européenne = European Space Agency (ESA), Institute of Theoretical Physics, Universität Zürich [Zürich] = University of Zurich (UZH), Washington University in Saint Louis (WUSTL), Maryland Center for Fundamental Physics, Department of Physics [College Park] (UMD), University of Maryland [College Park], University of Maryland System-University of Maryland System-University of Maryland [College Park], University of Maryland System-University of Maryland System, Gravitational Astrophysics Laboratory, NASA Goddard Space Flight Center (GSFC), Princeton University, Department of Astrophysics [Nijmegen], Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University [Nijmegen]-Radboud University [Nijmegen], Institute of Astronomy [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), National Institute for Subatomic Physics [Amsterdam] (NIKHEF), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Quantum Optics and Laser Science, Blackett Laboratory, Blackett Laboratory, Imperial College London-Imperial College London, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Physics and INFN, University of Trento [Trento], Department of Astronomy [Ann Arbor], University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, SUPA School of Physics and Astronomy [Glasgow], University of Glasgow, eLISA/NGO, Max Planck Institute for Gravitational Physics, Albert Einstein Institute, Institut de Ciencies de l'Espai [Barcelona] ( ICE-CSIC ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), 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 ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut für theoretische Physik, Universität Hamburg ( UHH ) -Universität Hamburg ( UHH ), California Institute of Technology ( CALTECH ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut 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 ), University of Milano Bicocca, Montana State University ( MSU ), Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ), Laboratoire de Physique Théorique d'Orsay [Orsay] ( LPT ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), Institute of Astronomy, University of Cambridge [UK] ( CAM ), Agence Spatiale Européenne ( ESA ), European Space Agency ( ESA ), University of Zürich [Zürich] ( UZH ), Washington University in St Louis, NASA Goddard Space Flight Center ( GSFC ), Institute for Mathematics, Astrophysics and Particle Physics ( IMAPP ), Radboud university [Nijmegen]-Radboud university [Nijmegen], Katholieke Universiteit Leuven ( KU Leuven ), Nikhef, APC - Gravitation ( APC-Gravitation ), 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 ) -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 ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, Jet Propulsion Laboratory ( JPL ), NASA-California Institute of Technology ( CALTECH ), Department of Astronomy, Department of Physics and Astronomy [Glasgow], Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut für theoretische Physik, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Agence Spatiale Européenne (ESA), European Space Agency (ESA), University of Zürich [Zürich] (UZH), National Institute for Subatomic Physics Nikhef [Amsterdam] (NIKHEF), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 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 Pierre et Marie Curie - Paris 6 (UPMC), Amaro Seoane, P, Aoudia, S, Babak, S, Binétruy, P, Berti, E, Bohé, A, Caprini, C, Colpi, M, Cornish, N, Danzmann, K, Dufaux, J, Gair, J, Jennrich, O, Jetzer, P, Klein, A, Lang, R, Lobo, A, Littenberg, T, Mcwilliams, S, Nelemans, G, Petiteau, A, Porter, E, Schutz, B, Sesana, A, Stebbins, R, Sumner, T, Vallisneri, M, Vitale, S, Volonteri, M, Ward, H, University of Zurich, Amaro-Seoane, Pau, Science and Technology Facilities Council (STFC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 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)-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 de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut für theoretische Physik, Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI)

Subjects
Double white-dwarfs, Massive black-hole, Minute orbital period, Physics and Astronomy (miscellaneous), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy, Astrophysics, AM CVN Stars, 01 natural sciences, 7. Clean energy, Mathematical Sciences, General Relativity and Quantum Cosmology, Physics, Particles & Fields, Observatory, LISA data stream, 010303 astronomy & astrophysics, media_common, Physics, [PHYS]Physics [physics], Galaxy formation, Dynamical friction, Nuclear & Particles Physics, gravitational waves, [ SDU.ASTR.CO ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Physical Sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Astrophysics - Cosmology and Nongalactic Astrophysics, double white dwraf, Common envelope evolution, Cosmology and Nongalactic Astrophysics (astro-ph.CO), General relativity, 530 Physics, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Physics, Multidisciplinary, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Galaxy merger, [ PHYS.ASTR.CO ] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FIS/05 - ASTRONOMIA E ASTROFISICA, 0103 physical sciences, 3101 Physics and Astronomy (miscellaneous), Astrophysics::Galaxy Astrophysics, Active galactic nuclei, Science & Technology, 010308 nuclear & particles physics, Gravitational wave, Cosmology and Extragalactic Astrophysics, Spin evolution, Astrophysics - Astrophysics of Galaxies, Galaxy, Universe, massive black hole binarie, Stars, 13. Climate action, Sky, Astrophysics of Galaxies (astro-ph.GA), 10231 Institute for Computational Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxy Astrophysics
Abstract

We review the expected science performance of the New Gravitational-Wave Observatory (NGO, a.k.a. eLISA), a mission under study by the European Space Agency for launch in the early 2020s. eLISA will survey the low-frequency gravitational-wave sky (from 0.1 mHz to 1 Hz), detecting and characterizing a broad variety of systems and events throughout the Universe, including the coalescences of massive black holes brought together by galaxy mergers; the inspirals of stellar-mass black holes and compact stars into central galactic black holes; several millions of ultracompact binaries, both detached and mass transferring, in the Galaxy; and possibly unforeseen sources such as the relic gravitational-wave radiation from the early Universe. eLISA's high signal-to-noise measurements will provide new insight into the structure and history of the Universe, and they will test general relativity in its strong-field dynamical regime., Comment: 20 pages, 8 figures, proceedings of the 9th Amaldi Conference on Gravitational Waves. Final journal version. For a longer exposition of the eLISA science case, see http://arxiv.org/abs/1201.3621

Published
2012
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38. Cosmological Backgrounds of Gravitational Waves and eLISA/NGO: Phase Transitions, Cosmic Strings and Other Sources

Author

Pierre Binétruy, Chiara Caprini, Alejandro Bohé, Jean-François Dufaux, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), APC - THEORIE, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut für theoretische Physik, Universität Hamburg (UHH)-Universität Hamburg (UHH), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
High Energy Physics - Theory, Phase transition, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Computation, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Gravitational wave background, Theoretical physics, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, Physics, [PHYS]Physics [physics], COSMIC cancer database, 010308 nuclear & particles physics, Gravitational wave, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astronomy and Astrophysics, Cosmic string, High Energy Physics - Phenomenology, High Energy Physics - Theory (hep-th), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We review several cosmological backgrounds of gravitational waves accessible to direct-detection experiments, with a special emphasis on those backgrounds due to first-order phase transitions and networks of cosmic (super-)strings. For these two particular sources, we revisit in detail the computation of the gravitational wave background and improve the results of previous works in the literature. We apply our results to identify the scientific potential of the NGO/eLISA mission of ESA regarding the detectability of cosmological backgrounds., Comment: V3: 49pp, 13 Figs, minor modifications to match published version

Published
2012
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40. CMB temperature anisotropy at large scales induced by a causal primordial magnetic field

Author

Chiara Caprini and Camille Bonvin

Subjects
Physics, Phase transition, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Sachs–Wolfe effect, Magnetic field, Topological defect, symbols.namesake, symbols, Einstein, Neutrino, Anisotropy, Mathematical physics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present an analytical derivation of the Sachs Wolfe effect sourced by a primordial magnetic field. In order to consistently specify the initial conditions, we assume that the magnetic field is generated by a causal process, namely a first order phase transition in the early universe. As for the topological defects case, we apply the general relativistic junction conditions to match the perturbation variables before and after the phase transition which generates the magnetic field, in such a way that the total energy momentum tensor is conserved across the transition and Einstein's equations are satisfied. We further solve the evolution equations for the metric and fluid perturbations at large scales analytically including neutrinos, and derive the magnetic Sachs Wolfe effect. We find that the relevant contribution to the magnetic Sachs Wolfe effect comes from the metric perturbations at next-to-leading order in the large scale limit. The leading order term is in fact strongly suppressed due to the presence of free-streaming neutrinos. We derive the neutrino compensation effect dynamically and confirm that the magnetic Sachs Wolfe spectrum from a causal magnetic field behaves as l(l+1)C_l^B \propto l^2 as found in the latest numerical analyses., 31 pages, 2 figures, minor changes, matches published version

Published
2010

41. Detection of gravitational waves from the QCD phase transition with pulsar timing arrays

Author

Chiara Caprini, Ruth Durrer, and Xavier Siemens

Subjects
Quantum chromodynamics, Physics, Nuclear and High Energy Physics, Phase transition, Gravitational-wave observatory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Gravitational wave, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Cosmology, Binary pulsar, General Relativity and Quantum Cosmology, Amplitude, Pulsar, Quantum electrodynamics, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, 010306 general physics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

If the cosmological QCD phase transition is strongly first order and lasts sufficiently long, it generates a background of gravitational waves which may be detected via pulsar timing experiments. We estimate the amplitude and the spectral shape of such a background and we discuss its detectability prospects., Comment: 7 pages, 5 figs. Version accepted by PRD

Published
2010
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42. Gravitational waves from cosmological phase transitions

Author

Chiara Caprini

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

First order phase transitions in the early universe can give rise to a stochastic background of gravitational waves. A hypothetical first order electroweak phase transition is particularly interesting in this respect, since the signal is in the good frequency range to be detectable by the space interferometer LISA. Three main processes lead to the production of the gravitational wave signal: the collision of the broken phase bubbles, the magnetohydrodynamical turbulence in the plasma stirred by the bubble collisions, and the magnetic fields amplified by the magnetohydrodynamical turbulence. The main features of the gravitational wave spectrum, such as the peak frequency, the amplitude, and the slopes both at low and high wave-number can be predicted by general arguments based on the characteristics of the source: in particular, the structure of its space and time correlation. We find that the gravitational wave signal from a first order phase transition occurring at electroweak symmetry breaking falls into the LISA sensitivity range if the phase transition lasts for about one hundredth of the Hubble time and the energy density of the turbulent motions is about twenty percent of the total energy density in the universe at the phase transition time., Comment: Proceedings for the Moriond 2010 Cosmology session, 9 pages, 6 figures. Citations added

Published
2010
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43. Can the observed large scale magnetic fields be seeded by helical primordial fields?

Author

Chiara Caprini, Elisa Fenu, and Ruth Durrer

Subjects
Physics, Inflation (cosmology), Phase transition, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Gravitational wave, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Helicity, Magnetic field, Gravitational wave background, Amplitude, Quantum electrodynamics, Dynamo, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Gravitational wave production induces a strong constraint on the amplitude of a primordial magnetic field. It has been shown that the nucleosynthesis bound for a stochastic gravitational wave background implies that causally generated fields cannot have enough power on large scales to provide the seeds necessary for the observed magnetic fields in galaxies and clusters, even by the most optimistic dynamo amplification. Magnetic fields generated at inflation can have high enough amplitude only if their spectrum is very red. Here we show that helicity, which leads to an inverse cascade, can mitigate these limits. In particular, we find that helical fields generated at the QCD phase transition or at inflation with red spectrum are possible seeds for the dynamo. Helical fields generated at the electroweak phase transition are instead excluded as seeds at large scales. We also calculate the spectrum of gravitational waves generated by helical magnetic fields., 41 pages, 12 figures

Published
2009

44. Dirac Born Infeld (DBI) cosmic strings

Author

Philippe Brax, Chiara Caprini, Jérôme Martin, Daniele A. Steer, Eugeny Babichev, Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), 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), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), APC - THEORIE, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 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)-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 de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut für theoretische Physik, Universität Hamburg (UHH)-Universität Hamburg (UHH), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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 Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut für theoretische Physik, 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut für theoretische Physik, Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire d'Electronique et des Technologies de l'Information (CEA-LETI), and Université Grenoble Alpes (UGA)-Direction de Recherche Technologique (CEA) (DRT (CEA))

Subjects
High Energy Physics - Theory, Nuclear and High Energy Physics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Parameter space, Astrophysics, 01 natural sciences, String (physics), General Relativity and Quantum Cosmology, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], High Energy Physics::Theory, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, Mathematical physics, Coupling constant, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], Astrophysics (astro-ph), Charge (physics), Cosmic string, High Energy Physics - Phenomenology, High Energy Physics - Theory (hep-th), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Brane, Scalar field, Particle Physics - Theory, Vacuum expectation value
Abstract

Motivated by brane physics, we consider the non-linear Dirac-Born-Infeld (DBI) extension of the Abelian-Higgs model and study the corresponding cosmic string configurations. The model is defined by a potential term, assumed to be of the mexican hat form, and a DBI action for the kinetic terms. We show that it is a continuous deformation of the Abelian-Higgs model, with a single deformation parameter depending on a dimensionless combination of the scalar coupling constant, the vacuum expectation value of the scalar field at infinity, and the brane tension. By means of numerical calculations, we investigate the profiles of the corresponding DBI-cosmic strings and prove that they have a core which is narrower than that of Abelian-Higgs strings. We also show that the corresponding action is smaller than in the standard case suggesting that their formation could be favoured in brane models. Moreover we show that the DBI-cosmic string solutions are non-pathological everywhere in parameter space. Finally, in the limit in which the DBI model reduces to the Bogomolnyi-Prasad-Sommerfield (BPS) Abelian-Higgs model, we find that DBI cosmic strings are no longer BPS: rather they have positive binding energy. We thus argue that, when they meet, two DBI strings will not bind with the corresponding formation of a junction, and hence that a network of DBI strings is likely to behave as a network of standard cosmic strings., Comment: 25 pages, 12 figures

Published
2009
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45. General Properties of the Gravitational Wave Spectrum from Phase Transitions

Author

Thomas Konstandin, Ruth Durrer, Geraldine Servant, and Chiara Caprini

Subjects
Physics, Nuclear and High Energy Physics, Phase transition, Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Gravitational wave, Critical phenomena, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), ddc:500.2, Spectral line, General Relativity and Quantum Cosmology, Gravitational wave background, Correlation function (statistical mechanics), High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Quantum mechanics, Anisotropy, Gravitational redshift, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In this paper we discuss some general aspects of the gravitational wave background arising from post-inflationary short-lasting cosmological events such as phase transitions. We concentrate on the physics which determines the shape and the peak frequency of the gravitational wave spectrum. We then apply our general findings to the case of bubble collisions during a first order phase transition and compare different results in the recent literature., Comment: 11 pages, 8 figures; v2: minor clarifications, published version

Published
2009

46. The cosmic microwave background temperature bispectrum from scalar perturbations induced by primordial magnetic fields

Author

Antonio Riotto, Chiara Caprini, Daniela Paoletti, and Fabio Finelli

Subjects
Physics, Spectral index, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, Scalar (physics), Spectral density, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Computational physics, Magnetic field, Amplitude, Anisotropy, Bispectrum, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We evaluate the angular bispectrum of the CMB temperature anisotropy at large angular scale due to a stochastic background of primordial magnetic fields. The shape of non-Gaussianity depends on the spectral index of the magnetic field power spectrum and is peaked in the squeezed configuration for a scale-invariant magnetic spectrum. By using the large angular part of the bispectrum generated by magnetic fields, the present bounds on non-Gaussianity set a limit on the amplitude of the primordial magnetic field of the order of 10 nGauss for the scale-invariant case and 20 nGauss for the other spectral indexes., Comment: Replaced with revised version accepted for publication in JCAP

Published
2009
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47. Optimising large galaxy surveys for ISW detection

Author

Marian Douspis, Nabila Aghanim, Chiara Caprini, and P. G. Castro

Subjects
Physics, Equation of state (cosmology), media_common.quotation_subject, Cosmic microwave background, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Sachs–Wolfe effect, Galaxy, Redshift, Gravitation, Space and Planetary Science, Sky, Dark energy, media_common
Abstract

We report on investigations of the power of next generation cosmic microwave background and large scale structure surveys in constraining the nature of dark energy through the cross-correlation of the Integrated Sachs Wolfe effect and the galaxy distribution. First we employ a signal to noise analysis to find the most appropriate properties of a survey in order to detect the correlated signal at a level of more than 4 sigma: such a survey should cover more than 35% of the sky, the galaxy distribution should be probed with a median redshift higher than 0.8, and the number of galaxies detected should be higher than a few per squared arcmin. We consider the forthcoming surveys DUNE, LSST, SNAP, PanSTARRS. We then compute the constraints that the DUNE survey can put on the nature of dark energy (through different parametrizations of its equation of state) with a standard Fisher matrix analysis. We confirm that, with respect to pure CMB constraints, cross-correlation constraints help in breaking degeneracies among the dark energy and the cosmological parameters. Naturally, the constraining capability is not independent of the choice of the dark energy model. Despite being weaker than some other probes (like Gravitational Weak-Lensing), these constraints are complementary to them, being sensitive to the high-redshift behaviour of the dark energy., 7 pages, 9 figures, 2 tables

Published
2008

48. Gravitational wave generation from bubble collisions in first-order phase transitions: an analytic approach

Author

Ruth Durrer, Geraldine Servant, and Chiara Caprini

Subjects
Physics, Astrophysics and Astronomy, Nuclear and High Energy Physics, Phase transition, Gravitational wave, Critical phenomena, Bubble, Astrophysics (astro-ph), Electroweak interaction, FOS: Physical sciences, Spectral density, General Relativity and Quantum Cosmology (gr-qc), ddc:500.2, Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Classical mechanics, Quantum electrodynamics, Envelope (waves), Gravitational redshift
Abstract

Gravitational wave production from bubble collisions was calculated in the early nineties using numerical simulations. In this paper, we present an alternative analytic estimate, relying on a different treatment of stochasticity. In our approach, we provide a model for the bubble velocity power spectrum, suitable for both detonations and deflagrations. From this, we derive the anisotropic stress and analytically solve the gravitational wave equation. We provide analytical formulae for the peak frequency and the shape of the spectrum which we compare with numerical estimates. In contrast to the previous analysis, we do not work in the envelope approximation. This paper focuses on a particular source of gravitational waves from phase transitions. In a companion article, we will add together the different sources of gravitational wave signals from phase transitions: bubble collisions, turbulence and magnetic fields and discuss the prospects for probing the electroweak phase transition at LISA., 48 pages, 14 figures. v2 (PRD version): calculation refined; plots redone starting from Fig. 4. Factor 2 in GW energy spectrum corrected. Main conclusions unchanged. v3: Note added at the end of paper to comment on the new results of 0901.1661

Published
2008

49. Challenges for creating magnetic fields by cosmic defects

Author

Robert Crittenden, Lukas Hollenstein, Chiara Caprini, and Roy Maartens

Subjects
Physics, Nuclear and High Energy Physics, Cosmology and Gravitation, Dark matter, Astrophysics (astro-ph), Order (ring theory), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Vorticity, Astrophysics, General Relativity and Quantum Cosmology, Magnetic field, Topological defect, Gravitation, Theoretical physics, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Quantum mechanics, Production (computer science), Neutrino
Abstract

We analyse the possibility that topological defects can act as a source of magnetic fields through the Harrison mechanism in the radiation era. We give a detailed relativistic derivation of the Harrison mechanism at first order in cosmological perturbations, and show that it is only efficient for temperatures above T ~ 0.2 keV. Our main result is that the vector metric perturbations generated by the defects cannot induce vorticity in the matter fluids at linear order, thereby excluding the production of currents and magnetic fields. We show that anisotropic stress in the matter fluids is required to source vorticity and magnetic fields. Our analysis is relevant for any mechanism whereby vorticity is meant to be transferred purely by gravitational interactions, and thus would also apply to dark matter or neutrinos., Comment: 9 pages, 1 figure; minor corrections and additions; accepted for publication in Physical Review D

Published
2007
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50. Frequency of gravitational waves

Author

Riccardo Sturani, Ruth Durrer, and Chiara Caprini

Subjects
Physics, Nuclear and High Energy Physics, Wavelength, Classical mechanics, Gravitational-wave observatory, Gravitational field, Gravitational wave, Quantum electrodynamics, Gravity Probe A, ddc:500.2, Gravitational acceleration, Gravitational energy, Gravitational redshift
Abstract

We show that there are physically relevant situations where gravitational waves do not inherit the frequency spectrum of their source but its wavenumber spectrum.

Published
2006

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