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14 results on '"Alberto Sesana"'

1. 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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2. 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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3. Massive black hole binary systems and the NANOGrav 12.5 yr results

Author

Siyuan Chen, Alberto Sesana, W. Del Pozzo, Alberto Vecchio, H. Middleton, Pablo Rosado, 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)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), and Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitational radiation: stochastic, Population, black hole physics, Binary number, FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Gravitational wave background, Pulsar, Bulge, pulsars: general, 0103 physical sciences, black hole, galaxies: formation, black hole: pair, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, pulsar, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, 010308 nuclear & particles physics, Gravitational wave, scaling, gravitational radiation: background, Astronomy and Astrophysics, NANOGrav, Astrophysics - Astrophysics of Galaxies, methods: data analysis, Galaxy, Black hole, observatory, black hole: binary, gravitational waves, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], galaxy, Astrophysics - High Energy Astrophysical Phenomena, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The North American Nanohertz Observatory for Gravitational Waves (NANOGrav) has recently reported evidence for the presence of a common stochastic signal across their array of pulsars. The origin of this signal is still unclear. One of the possibilities is that it is due to a stochastic gravitational wave background (SGWB) in the $\sim 1-10\,{\rm nHz}$ frequency region. Taking the NANOGrav observational result at face value, we show that this signal would be fully consistent with a SGWB produced by an unresolved population of in-spiralling massive black hole binaries (MBHBs) predicted by current theoretical models. Considering an astrophysically agnostic model we find that the MBHB merger rate is loosely constrained to the range $10^{-11} - 2$ $\mathrm{Mpc}^{-3}\,\mathrm{Gyr}^{-1}$. Including additional constraints from galaxy pairing fractions and MBH-bulge scaling relations, we find that the MBHB merger rate is $10^{-5} - 5\times10^{-4}$ $\mathrm{Mpc}^{-3}\,\mathrm{Gyr}^{-1}$, the MBHB merger time-scale is $\le 3\,\mathrm{Gyr}$ and the norm of the $M_\mathrm{BH}-M_\mathrm{bulge}$ relation $\ge 1.2\times 10^{8}\,M_\odot$ (all intervals quoted at 90\% confidence). Regardless of the astrophysical details of MBHB assembly, this result would imply that a sufficiently large population of massive black holes pair up, form binaries and merge within a Hubble time., Comment: 6 pages, 4 figures, to be submitted

Published
2021
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4. Science with the TianQin observatory: Preliminary result on extreme-mass-ratio inspirals

Author

Yi-Ming Hu, Jianwei Mei, Huimin Fan, Alberto Sesana, Enrico Barausse, Tie-Guang Zi, Xuefeng Zhang, Jian-dong Zhang, 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), Fan, H, Hu, Y, Barausse, E, Sesana, A, Zhang, J, Zhang, X, Zi, T, and Mei, J

Subjects
FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Compact star, 01 natural sciences, General Relativity and Quantum Cosmology, localization, Gravitation, Settore FIS/05 - Astronomia e Astrofisica, Observatory, strong field, 0103 physical sciences, black hole, 010306 general physics, capture, Luminosity distance, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Mass ratio, redshift, Redshift, gravitational radiation detector, moment, Black hole, observatory, gravitation, Quadrupole, network, fractional, Kerr, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], mass ratio, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics and astroparticle physics
Abstract

Systems consisting of a massive black hole and a stellar-origin compact object (CO), known as extreme-mass-ratio inspirals (EMRIs), are of great significance for space-based gravitational-wave detectors, as they will allow for testing gravitational theories in the strong field regime, and for checking the validity of the black hole no-hair theorem. In this work, we present a calculation of the EMRI rate and parameter estimation capabilities of the TianQin observatory, for various astrophysical models for these sources. We find that TianQin can observe EMRIs involving COs with mass of 10$M_\odot$ up to redshift $\sim2$. We also find that detections could reach tens or hundreds per year in the most optimistic astrophysical scenarios. Intrinsic parameters are expected to be recovered to within fractional errors of $\sim 10^{-6}$, while typical errors on the luminosity distance and sky localization are 10% and 10 deg$^2$, respectively. TianQin observation of EMRIs can also constrain possible deviations from the Kerr quadrupole moment to within fractional errors $\lesssim10^{-4}$. We also find that a network of multiple detectors would allow for improvements in both detection rates (by a factor $\sim 1.5$ -$3$) and in parameter estimation precision (20-fold improvement for the sky localization and fivefold improvement for the other parameters)., Comment: 13 pages, 5 figures

Published
2020
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5. Science with the TianQin observatory: Preliminary results on massive black hole binaries

Author

Wen-Fan Feng, Yan Wang, Jianwei Mei, Zhen Jiang, Shun-Jia Huang, Alberto Sesana, Hai-Tian Wang, Enrico Barausse, Yi-Fan Wang, Yi-Ming Hu, Jun Luo, 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), Wang, H, Jiang, Z, Sesana, A, Barausse, E, Huang, S, Wang, Y, Feng, W, Hu, Y, Mei, J, and Luo, J

Subjects
noise, coalescence, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, astro-ph.GA, interferometer, FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, General Relativity and Quantum Cosmology, localization, Settore FIS/05 - Astronomia e Astrofisica, Observatory, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, astro-ph.HE, astro-ph.CO, black hole, Astrophysics - Cosmology and Nongalactic Astrophysic, 010306 general physics, Luminosity distance, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Gravitational wave, gravitational radiation, redshift, Astrophysics - Astrophysics of Galaxies, Redshift, Black hole, messenger, observatory, Interferometry, black hole: binary, Sky, Astrophysics of Galaxies (astro-ph.GA), [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], history, Detection rate, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and astroparticle physics
Abstract

We investigate the prospects of detecting gravitational waves from coalescing massive black hole binaries in the Universe with the TianQin observatory, a space-based gravitational wave interferometer proposed to be launched in the 2030s. To frame the scientific scope of the mission, in this paper, we carry out a preliminary estimation of the signal-to-noise ratio, detection rate and parameter estimation precision of massive black hole binaries detectable by TianQin. In order to make our results as robust as possible, we consider several models of the growth history of massive black holes, exploring the effect of some key astrophysical prescriptions as well the impact of the employed computational methods. In the most optimistic model, TianQin can detect as many as approximately 60 mergers per year. If TianQin detects a merger at redshift of 15, it will be capable of estimating its luminosity distance to within an accuracy of 10%; for a nearby event at redshift approximately 2, TianQin can issue early warnings 24 hours before coalescence, with a timing accuracy of around three hours and a sky localization ability of approximately 80 deg$^2$, thus enabling multi-messenger observations., Comment: 17 pages, 6 figures

Published
2019
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6. Post-Newtonian phase accuracy requirements for stellar black hole binaries with LISA

Author

Alberto Sesana, Enrico Barausse, Alberto Mangiagli, Antoine Klein, Monica Colpi, 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), Mangiagli, A, Klein, A, Sesana, A, Barausse, E, and Colpi, M

Subjects
General relativity, General Relativity and Quantum Cosmology, astro-ph.HE, Binary number, FOS: Physical sciences, alternative theories of gravity, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Newtonian fluid, Waveform, 010306 general physics, Physics, Coalescence (physics), High Energy Astrophysical Phenomena (astro-ph.HE), 04.30.Tv, 010308 nuclear & particles physics, Gravitational wave, Statistical parameter, 04.30.-w, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Stellar black hole, Black hole binaries, Gravitational waves, LISA, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The Laser Interferometer Space Antenna (LISA) will observe black hole binaries of stellar origin during their gravitational wave inspiral, months to years before coalescence. Due to the long duration of the signal in the LISA band, a faithful waveform is necessary in order to keep track of the binary phase. This is crucial to extract the signal from the data and to perform an unbiased estimation of the source parameters. We consider Post-Newtonian (PN) waveforms, and analyze the PN order needed to keep the bias caused by the PN approximation negligible relative to the statistical parameter estimation error, as a function of the source parameters. By considering realistic population models, we conclude that for $\sim 90\%$ of the stellar black hole binaries detectable by LISA, waveforms at low Post-Newtonian (PN) order (PN $\le 2$) are sufficiently accurate for an unbiased recovery of the source parameters. Our results provide a first estimate of the trade-off between waveform accuracy and information recovery for this class of LISA sources., 11 pages, 6 figures. Submitted to Physical Review D

Published
2019
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7. Science with the TianQin observatory: Preliminary results on testing the no-hair theorem with ringdown signals

Author

Jianwei Mei, Alberto Sesana, Jun Luo, Changfu Shi, Hai-Tian Wang, Enrico Barausse, Jian-dong Zhang, Jiahui Bao, Yi-Ming Hu, 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), Shi, C, Bao, J, Wang, H, Zhang, J, Hu, Y, Sesana, A, Barausse, E, Mei, J, and Luo, J

Subjects
noise, coalescence, Gravitational-wave observatory, General relativity, FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, gravitational radiation: direct detection, 01 natural sciences, General Relativity and Quantum Cosmology, Settore FIS/05 - Astronomia e Astrofisica, Observatory, 0103 physical sciences, Quasinormal mode, decay: time, 010306 general physics, Physics, LISA, 010308 nuclear & particles physics, Gravitational wave, quasinormal mode, gravitational radiation, black hole: mass, gravitational radiation detector, 3. Good health, Decay time, black hole: binary, No-hair theorem, gravitational radiation: emission, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc]
Abstract

We study the capability of the space-based gravitational wave observatory TianQin to test the no-hair theorem of General Relativity, using the ringdown signal from the coalescence of massive black hole binaries. We parameterize the ringdown signal by the four strongest quasinormal modes and estimate the signal to noise ratio for various source parameters. We consider constraints both from single detections and from all the events combined throughout the lifetime of the observatory, for different astrophysical models. We find that at the end of the mission, TianQin will have constrained deviations of the frequency and decay time of the dominant 22 mode from the general relativistic predictions to within 0.2% and 1.5% respectively, the frequencies of the subleading modes can be also constrained within 0.3%. We also find that TianQin and LISA are highly complementary, by virtue of their different frequency windows. Indeed, LISA can best perform ringdown tests for black hole masses in excess of $\sim 3\times 10^6 M_\odot$, while TianQin is best suited for lower masses., Comment: 10 pages, 12 figures

Published
2019
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8. Constraining astrophysical observables of Galaxy and Supermassive Black Hole Binary Mergers using Pulsar Timing Arrays

Author

Alberto Sesana, Siyuan Chen, Christopher J. Conselice, Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Technologie de Belfort-Montbeliard (UTBM), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Chen, S, Sesana, A, and Conselice, C

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Astrophysics::High Energy Astrophysical Phenomena, Population, black hole physics, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Gravitational wave background, Pulsar timing array, Black hole physic, General Relativity and Quantum Cosmology, Pulsar, pulsars: general, 0103 physical sciences, galaxies: formation, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Supermassive black hole, education.field_of_study, 010308 nuclear & particles physics, Gravitational wave, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, methods: data analysis, Galaxy, gravitational waves, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Methods: data analysi, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present an analytic model to describe the supermassive black hole binary (SMBHB) merger rate in the Universe with astrophysical observables: galaxy stellar mass function, pair fraction, merger timescale and black hole - host galaxy relations. We construct observational priors and compute the allowed range of the characteristic spectrum $h_c$ of the gravitational wave background (GWB) to be $10^{-16}, Comment: 18 + 10 appendix pages, 12 + 10 appendix figures, 3 tables

Published
2019
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9. Improving timing sensitivity in the microhertz frequency regime: limits from PSR J1713$+$0747 on gravitational waves produced by super-massive black-hole binaries

Author

John Antoniadis, Gregory Desvignes, R. N. Caballero, Benjamin Stappers, Gilles Theureau, James Mckee, G. Shaifullah, E. Graikou, Andrew Lyne, Cees Bassa, Stefan Oslowski, Sotirios A. Sanidas, L. Lentati, Lucas Guillemot, Benetge Perera, Ramesh Karuppusamy, Ismaël Cognard, Michael Kramer, Delphine Perrodin, Joris P. W. Verbiest, Stephen Taylor, Michael Keith, Kang Liu, P. Lazarus, Gemma H. Janssen, Alberto Sesana, S Babak, D. J. Champion, AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace ( LPC2E ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Unité Scientifique de la Station de Nançay ( USN ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Univers et Théories ( LUTH ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), ITA, USA, GBR, FRA, DEU, AUS, NLD, RUS, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique 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), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Laboratoire Univers et Théories (LUTH (UMR_8102)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-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), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-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), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Perera, B, Stappers, B, Babak, S, Keith, M, Antoniadis, J, Bassa, C, Caballero, R, Champion, D, Cognard, I, Desvignes, G, Graikou, E, Guillemot, L, Janssen, G, Karuppusamy, R, Kramer, M, Lazarus, P, Lentati, L, Liu, K, Lyne, A, Mckee, J, Osłowski, S, Perrodin, D, Sanidas, S, Sesana, A, Shaifullah, G, Theureau, G, Verbiest, J, Taylor, S, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics, 01 natural sciences, Bayesian, stars: neutron, neutron, Pulsar, Millisecond pulsar, 0103 physical sciences, Quasars: Supermassive black hole, black hole, 010303 astronomy & astrophysics, orbit, quasars: supermassive, pulsar, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Supermassive black hole, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Gravitational wave, stars, quasars: supermassive black holes, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation, Astronomy and Astrophysics, sensitivity, black holes, Black hole, Orbit, European Pulsar Timing Array, Amplitude, binaries: general, gravitational waves, black hole: binary, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], frequency, spectral, Stars: Black hole, pulsars: individual: PSR J1713+0747, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], stars: black holes
Abstract

We search for continuous gravitational waves (CGWs) produced by individual super-massive black-hole binaries (SMBHBs) in circular orbits using high-cadence timing observations of PSR J1713$+$0747. We observe this millisecond pulsar using the telescopes in the European Pulsar Timing Array (EPTA) with an average cadence of approximately 1.6 days over the period between April 2011 and July 2015, including an approximately daily average between February 2013 and April 2014. The high-cadence observations are used to improve the pulsar timing sensitivity across the GW frequency range of $0.008-5$ $\mu$Hz. We use two algorithms in the analysis, including a spectral fitting method and a Bayesian approach. For an independent comparison, we also use a previously published Bayesian algorithm. We find that the Bayesian approaches provide optimal results and the timing observations of the pulsar place a 95 per cent upper limit on the sky-averaged strain amplitude of CGWs to be $\lesssim3.5\times10^{-13}$ at a reference frequency of 1 $\mu$Hz. We also find a 95 per cent upper limit on the sky-averaged strain amplitude of low-frequency CGWs to be $\lesssim1.4\times10^{-14}$ at a reference frequency of 20~nHz., Comment: 12 pages, 4 figures. Accepted for publication in MNRAS

Published
2018
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10. Stellar binary black holes in the LISA band: a new class of standard sirens

Author

Antoine Klein, Alberto Sesana, Walter Del Pozzo, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Pozzo, W, Sesana, A, and Klein, A

Subjects
cosmological model, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], black hole physics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, localization, Black hole physic, LIGO, 010303 astronomy & astrophysics, Physics, education.field_of_study, Hubble constant, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational waves, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], cosmology: cosmological parameters, black hole physics, gravitational waves, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, black hole: binary: coalescence, Population, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, gravitational radiation: direct detection, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], symbols.namesake, Binary black hole, 0103 physical sciences, 010306 general physics, education, Luminosity distance, Astrophysics::Galaxy Astrophysics, LISA, Gravitational wave, gravitational radiation, Astronomy, Astronomy and Astrophysics, redshift, Redshift, gravitational radiation detector, Black hole, Space and Planetary Science, gravitational radiation: emission, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hubble's law
Abstract

The recent Advanced LIGO detections of coalescing black hole binaries (BHBs) imply a large population of such systems emitting at milli-Hz frequencies, accessible to the Laser Interferometer Space Antenna (LISA). We show that these systems provide a new class of cosmological standard sirens. Direct LISA luminosity distance -$D_l$- measurements, combined with the inhomogeneous redshift -$z$- distribution of possible host galaxies provide an effective way to populate the $D_l-z$ diagram at $z, 9 pages 4 figures, to be submitted to MNRAS

Published
2018
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11. Post-Newtonian evolution of massive black hole triplets in galactic nuclei – III. A robust lower limit to the nHz stochastic background of gravitational waves

Author

Matteo Bonetti, Enrico Barausse, Francesco Haardt, Alberto Sesana, 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), Bonetti, M, Sesana, A, Barausse, E, and Haardt, F

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Black hole physics, Galaxies: kinematics and dynamics, Gravitation, Gravitational waves, Methods: numerical, Astronomy and Astrophysics, Space and Planetary Science, Population, black hole physics, FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, 01 natural sciences, General Relativity and Quantum Cosmology, methods: numerical, gravitation, gravitational waves, galaxies: kinematics and dynamics, Black hole physic, Galaxies: kinematics and dynamic, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Galaxy formation and evolution, education, 010303 astronomy & astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Gravitational wave, Astronomy, Astrophysics - Astrophysics of Galaxies, Galaxy, Black hole, Amplitude, Astrophysics of Galaxies (astro-ph.GA), [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Inspiraling massive black-hole binaries (MBHBs) forming in the aftermath of galaxy mergers are expected to be the loudest gravitational-wave (GW) sources relevant for pulsar-timing arrays (PTAs) at nHz frequencies. The incoherent overlap of signals from a cosmic population of MBHBs gives rise to a stochastic GW background (GWB) with characteristic strain around $h_c\sim10^{-15}$ at a reference frequency of 1 yr$^{-1}$, although uncertainties around this value are large. Current PTAs are piercing into the GW amplitude range predicted by MBHB-population models, but no detection has been reported so far. To assess the future success prospects of PTA experiments, it is therefore important to estimate the minimum GWB level consistent with our current understanding of the formation and evolution of galaxies and massive black holes (MBHs). To this purpose, we couple a semianalytic model of galaxy evolution and an extensive study of the statistical outcome of triple MBH interactions. We show that even in the most pessimistic scenario where all MBHBs stall before entering the GW-dominated regime, triple interactions resulting from subsequent galaxy mergers inevitably drive a considerable fraction of the MBHB population to coalescence. At frequencies relevant for PTA, the resulting GWB is only a factor of 2-to-3 suppressed compared to a fiducial model where binaries are allowed to merge over Gyr timescales. Coupled with current estimates of the expected GWB amplitude range, our findings suggest that the minimum GWB from cosmic MBHBs is unlikely to be lower than $h_c\sim 10^{-16}$ (at $f = 1$ yr$^{-1}$), well within the expected sensitivity of projected PTAs based on future observations with FAST, MeerKAT and SKA., 16 pages, 9 figures, accepted for publication in MNRAS

Published
2018
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12. Post-Newtonian evolution of massive black hole triplets in galactic nuclei -- II. Survey of the parameter space

Author

Francesco Haardt, Matteo Bonetti, Alberto Sesana, Enrico Barausse, Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Bonetti, M, Haardt, F, Sesana, A, and Barausse, E

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], black hole physics, FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, Parameter space, 01 natural sciences, General Relativity and Quantum Cosmology, methods: numerical, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Gravitation, gravitation, gravitational waves, galaxies: kinematics and dynamics, Black hole physic, Pulsar timing array, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Gravitational wave, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Stars, Space and Planetary Science, Intermediate-mass black hole, Astrophysics of Galaxies (astro-ph.GA), [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Galaxies: Kinematics and dynamic, Stellar black hole, Black hole physics, Galaxies: Kinematics and dynamics, Gravitational waves, Methods: Numerical, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Massive black hole binaries (MBHBs) are expected to form at the centre of merging galaxies during the hierarchical assembly of the cosmic structure, and are expected to be the loudest sources of gravitational waves (GWs) in the low frequency domain. However, because of the dearth of energy exchanges with background stars and gas, many of these MBHBs may stall at separations too large for GW emission to drive them to coalescence in less than a Hubble time. Triple MBH systems are then bound to form after a further galaxy merger, triggering a complex and rich dynamics that can eventually lead to MBH coalescence. Here we report on the results of a large set of numerical simulations, where MBH triplets are set in spherical stellar potentials and MBH dynamics is followed through 2.5 post-Newtonian order in the equations of motion. From our full suite of simulated systems we find that a fraction $\simeq 20-30$% of the MBH binaries that would otherwise stall are led to coalesce within a Hubble time. The corresponding coalescence timescale peaks around 300 Myr, while the eccentricity close to the plunge, albeit small, is non-negligible ($\lesssim 0.1$). We construct and discuss marginalised probability distributions of the main parameters involved and, in a companion paper of the series, we will use the results presented here to forecast the contribution of MBH triplets to the GW signal in the nHz regime probed by Pulsar Timing Array experiments., 19 pages, 14 figures, accepted for publication in MNRAS

Published
2018
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13. Science with the space-based interferometer LISA. V: Extreme mass-ratio inspirals

Author

Emanuele Berti, Alberto Sesana, Antoine Petiteau, Carlos F. Sopuerta, Jonathan R. Gair, Enrico Barausse, Stanislav Babak, Christopher P. L. Berry, Antoine Klein, Pau Amaro-Seoane, 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)), 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 Paris Cité (UPCité), ANR-16-CE31-0001,APACHE,Astroparticules et pulsars : connexions de basse à ultra-haute énergies(2016), Babak, S, Gair, J, Sesana, A, Barausse, E, Sopuerta, C, Berry, C, Berti, E, Amaro-Seoane, P, Petiteau, A, Klein, A, 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 ), 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 de Paris (UP)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics and Astronomy (miscellaneous), gr-qc, astro-ph.GA, interferometer, Kerr metric, FOS: Physical sciences, Orbital eccentricity, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Compact star, 01 natural sciences, General Relativity and Quantum Cosmology, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Settore FIS/05 - Astronomia e Astrofisica, statistical analysis, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, black hole, Astrophysics - Cosmology and Nongalactic Astrophysic, 010303 astronomy & astrophysics, Luminosity distance, Physics, binary: mass ratio, LISA, black hole: spin, 010308 nuclear & particles physics, Gravitational wave, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation, Astronomy, Mass ratio, metric: Kerr, Astrophysics - Astrophysics of Galaxies, Redshift, gravitational radiation detector, Black hole, error: statistical, gravitational waves, Astrophysics of Galaxies (astro-ph.GA), gravitational radiation: emission, fractional, astro-ph.CO, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The space-based Laser Interferometer Space Antenna (LISA) will be able to observe the gravitational-wave signals from systems comprised of a massive black hole and a stellar-mass compact object. These systems are known as extreme-mass-ratio inspirals (EMRIs) and are expected to complete $\sim 10^4$-$10^5$ cycles in band, thus allowing exquisite measurements of their parameters. In this work, we attempt to quantify the astrophysical uncertainties affecting the predictions for the number of EMRIs detectable by LISA, and find that competing astrophysical assumptions produce a variance of about three orders of magnitude in the expected intrinsic EMRI rate. However, we find that irrespective of the astrophysical model, at least a few EMRIs per year should be detectable by the LISA mission, with up to a few thousands per year under the most optimistic astrophysical assumptions. We also investigate the precision with which LISA will be able to extract the parameters of these sources. We find that typical fractional statistical errors with which the intrinsic parameters (redshifted masses, massive black hole spin and orbital eccentricity) can be recovered are $\sim 10^{-6}$-$10^{-4}$. Luminosity distance (which is required to infer true masses) is inferred to about $10\%$ precision and sky position is localized to a few square degrees, while tests of the multipolar structure of the Kerr metric can be performed to percent-level precision or better., Comment: 13 figures, 22 pages; updated to match published version

Published
2017
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14. Resolving multiple supermassive black hole binaries with pulsar timing arrays. II. Genetic algorithm implementation

Author

Antoine Petiteau, Alberto Sesana, Stanislav Babak, Mariana Araujo, 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), Max Planck Institute for Gravitational Physics (Albert Einstein Institute) (AEI), Max-Planck-Gesellschaft, Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, [PHYS]Physics [physics], Nuclear and High Energy Physics, Supermassive black hole, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Gravitational wave, FOS: Physical sciences, Astronomy, Astrophysics, 01 natural sciences, Black hole, Pulsar timing array, symbols.namesake, Additive white Gaussian noise, Pulsar, Search algorithm, 0103 physical sciences, symbols, Monochromatic color, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Pulsar timing arrays (PTAs) might detect gravitational waves (GWs) from massive black hole (MBH) binaries within this decade. The signal is expected to be an incoherent superposition of several nearly-monochromatic waves of different strength. The brightest sources might be individually resolved, and the overall deconvolved, at least partially, in its individual components. In this paper we extend the maximum-likelihood based method developed in Babak & Sesana 2012, to search for individual MBH binaries in PTA data. We model the signal as a collection of circular monochromatic binaries, each characterized by three free parameters: two angles defining the sky location, and the frequency. We marginalize over all other source parameters and we apply an efficient multi-search genetic algorithm to maximize the likelihood function and look for sources in synthetic datasets. On datasets characterized by white Gaussian noise plus few injected sources with signal-to-noise ratio (SNR) in the range 10-60, our search algorithm performs well, recovering all the injections with no false positives. Individual source SNRs are estimated within few % of the injected values, sky locations are recovered within few degrees, and frequencies are determined with sub-Fourier bin precision., 12 pages, 4 figures, 1 table; submitted to Physical Review D

Published
2013
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