Mauro Pieroni

European Organization for Nuclear Research

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Angelo Ricciardone

University of Padua

Germano Nardini

University of Stavanger

Gianmassimo Tasinato

Swansea University

Daniel G. Figueroa

Instituto de Física Corpuscular

Nikolaos Karnesis

Aristotle University of Thessaloniki

Marco Peloso

Istituto Nazionale di Fisica Nucleare, Sezione di Padova

Valerie Domcke

European Organization for Nuclear Research

Chiara Caprini

Istituto Nazionale di Fisica Nucleare, Galileo Galilei Institute for Theoretical Physics

Tessa Baker

University of Portsmouth

Jesús Torrado

University of Padua

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Centre National de la Recherche Scientifique

140

Université Paris Cité

Laboratoire AstroParticule et Cosmologie

Sorbonne Université

Max Planck Institute for Gravitational Physics

Institut National de Physique Nucléaire et de Physique des Particules

Istituto Nazionale di Fisica Nucleare, Laboratori Nazionali del Gran Sasso

Istituto Nazionale di Fisica Nucleare

Commissariat à l'Énergie Atomique et aux Énergies Alternatives

European Organization for Nuclear Research

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Gravitational waves from double white dwarfs as probes of the milky way

Monthly Notices of the Royal Astronomical Society (2022)

Maria Georgousi Nikolaos Karnesis Valeriya Korol Mauro Pieroni Nikolaos Stergioulas

Future gravitational wave detectors, such as the Laser Interferometer Space Antenna (\textit{LISA}), will be able to resolve a significant number of the ultra compact stellar-mass binaries in our own Galaxy and its neighborhood. These will be mostly double white dwarf (DWD) binaries, and their underlying population characteristics can be directly correlated to the different properties of the Galaxy. In particular, with \textit{LISA} we will be able to resolve $\sim\mathcal{O}(10^4)$ binaries, while the rest will generate a confusion foreground signal. Analogously to how the total electromagnetic radiation emitted by a galaxy can be related to the underlying total stellar mass, in this work we propose a framework to infer the same quantity by investigating the spectral shape and amplitude of the confusion foreground signal. For a fixed DWD evolution model, and thus a fixed binary fraction, we retrieve percentage-level relative errors on the total stellar mass, which improves for increasing values of the mass. At the same time, we find that variations in the Milky Way shape, at a fixed mass and at scale heights smaller than 500~pc, are not distinguishable based on the shape of stochastic signal alone. We perform this analysis on simulations of the LISA data, estimating the resolvable sources based on signal-to-noise criteria. Finally, we utilize the catalogue of resolvable sources to probe the characteristics of the underlying population of DWD binaries. We show that the DWD frequency, coalescence time and chirp mass (up to $<0.7\,$M$_\odot$) distributions can be reconstructed from \textit{LISA} data with no bias.

Gravitational wave background

Stellar mass

10.1093/mnras/stac3686

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Citations (30)

Quantum gravity phenomenology at the dawn of the multi-messenger era -- A review.

arXiv (Cornell University) (2021)

Andrea Addazi J. Álvarez-Muñiz Rafael Alves Batista Giovanni Amelino-Camelia V. Antonelli

The exploration of the universe has recently entered a new era thanks to the multi-messenger paradigm, characterized by a continuous increase in the quantity and quality of experimental data that is obtained by the detection of the various cosmic messengers (photons, neutrinos, cosmic rays and gravitational waves) from numerous origins. They give us information about their sources in the universe and the properties of the intergalactic medium. Moreover, multi-messenger astronomy opens up the possibility to search for phenomenological signatures of quantum gravity. On the one hand, the most energetic events allow us to test our physical theories at energy regimes which are not directly accessible in accelerators; on the other hand, tiny effects in the propagation of very high energy particles could be amplified by cosmological distances. After decades of merely theoretical investigations, the possibility of obtaining phenomenological indications of Planck-scale effects is a revolutionary step in the quest for a quantum theory of gravity, but it requires cooperation between different communities of physicists (both theoretical and experimental). This review is aimed at promoting this cooperation by giving a state-of-the art account of the interdisciplinary expertise that is needed in the effective search of quantum gravity footprints in the production, propagation and detection of cosmic messengers.

Source

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Stochastic gravitational wave background from stellar origin binary black holes in LISA

Journal of Cosmology and Astroparticle Physics (2023)

S. Babak Chiara Caprini Daniel G. Figueroa Nikolaos Karnesis Paolo Marcoccia

Abstract We use the latest constraints on the population of stellar origin binary black holes (SOBBH) from LIGO/Virgo/KAGRA (LVK) observations, to estimate the stochastic gravitational wave background (SGWB) they generate in the frequency band of LISA. In order to account for the faint and distant binaries, which contribute the most to the SGWB, we extend the merger rate at high redshift assuming that it tracks the star formation rate. We adopt different methods to compute the SGWB signal: we perform an analytical evaluation, we use Monte Carlo sums over the SOBBH population realisations, and we account for the role of the detector by simulating LISA data and iteratively removing the resolvable signals until only the confusion noise is left. The last method allows the extraction of both the expected SGWB and the number of resolvable SOBBHs. Since the latter are few for signal-to-noise ratio thresholds larger than five, we confirm that the spectral shape of the SGWB in the LISA band agrees with the analytical prediction of a single power law. We infer the probability distribution of the SGWB amplitude from the LVK GWTC-3 posterior of the binary population model: at the reference frequency of 0.003 Hz it has an interquartile range of h 2 Ω GW ( f = 3 × 10 -3 Hz) ∈ [5.65, 11.5] × 10 -13 , in agreement with most previous estimates. We then perform a MC analysis to assess LISA's capability to detect and characterise this signal. Accounting for both the instrumental noise and the galactic binaries foreground, with four years of data, LISA will be able to detect the SOBBH SGWB with percent accuracy, narrowing down the uncertainty on the amplitude by one order of magnitude with respect to the range of possible amplitudes inferred from the population model. A measurement of this signal by LISA will help to break the degeneracy among some of the population parameters, and provide interesting constraints, in particular on the redshift evolution of the SOBBH merger rate.

Gravitational wave background

10.1088/1475-7516/2023/08/034

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Measuring the net circular polarization of the stochastic gravitational wave background with interferometers

Journal of Cosmology and Astroparticle Physics (2020)

Valerie Domcke J. García-Bellido Marco Peloso Mauro Pieroni Angelo Ricciardone

Parity violating interactions in the early Universe can source a stochastic gravitational wave background (SGWB) with a net circular polarization. In this paper, we study possible ways to search for circular polarization of the SGWB with interferometers. Planar detectors are unable to measure the net circular polarization of an isotropic SGWB . We discuss the possibility of using the dipolar anisotropy kinematically induced by the motion of the solar system with respect to the cosmic reference frame to measure the net circular polarization of the SGWB with planar detectors. We apply this approach to LISA, re-assessing previous analyses by means of a more detailed computation and using the most recent instrument specifications, and to the Einstein Telescope (ET), estimating for the first time its sensitivity to circular polarization. We find that both LISA and ET, despite operating at different frequencies, could detect net circular polarization with a signal-to-noise ratio of order one in a SGWB with amplitude h2 ΩGW ≃ 10−11. We also investigate the case of a network of ground based detectors. We present fully analytical, covariant formulas for the detector overlap functions in the presence of circular polarization. Our formulas do not rely on particular choices of reference frame, and can be applied to interferometers with arbitrary angles among their arms.

Einstein Telescope

Gravitational wave background

10.1088/1475-7516/2020/05/028

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Classification of inflationary models and constraints on fundamental physics

arXiv (Cornell University) (2016)

Mauro Pieroni

This work is focused on the study of early time cosmology and in particular on the study of inflation. After an introduction on the standard Big Bang theory, we discuss the physics of CMB and we explain how its observations can be used to set constraints on cosmological models. We introduce inflation and we carry out its simplest realization by presenting the observables and the experimental constraints that can be set on inflationary models. The possibility of observing primordial gravitational waves (GWs) produced during inflation is discussed. We present the reasons to define a classification of inflationary models and introduce the β-function formalism for inflation by explaining why in this framework we can naturally define a set of universality classes for inflationary models. Theoretical motivations to support the formulation of inflation in terms of this formalism are presented. Some generalized models of inflation are introduced and the extension of the β-function formalism for inflation to these models is discussed. Finally we focus on the study of models where the (pseudo-scalar) inflaton is coupled to some Abelian gauge fields that can be present during inflation. The analysis of the problem is carried out by using a characterization of inflationary models in terms of their asymptotic behavior. A wide set of theoretical aspects and of observational consequences is discussed.

Inflationary epoch

Cosmic background radiation

10.48550/arxiv.1611.03732

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Quantum gravity phenomenology at the dawn of the multi-messenger era—A review

Progress in Particle and Nuclear Physics (2022)

Andrea Addazi J. Álvarez-Muñiz Rafael Alves Batista Giovanni Amelino-Camelia V. Antonelli

The exploration of the universe has recently entered a new era thanks to the multi-messenger paradigm, characterized by a continuous increase in the quantity and quality of experimental data that is obtained by the detection of the various cosmic messengers (photons, neutrinos, cosmic rays and gravitational waves) from numerous origins. They give us information about their sources in the universe and the properties of the intergalactic medium. Moreover, multi-messenger astronomy opens up the possibility to search for phenomenological signatures of quantum gravity. On the one hand, the most energetic events allow us to test our physical theories at energy regimes which are not directly accessible in accelerators; on the other hand, tiny effects in the propagation of very high energy particles could be amplified by cosmological distances. After decades of merely theoretical investigations, the possibility of obtaining phenomenological indications of Planck-scale effects is a revolutionary step in the quest for a quantum theory of gravity, but it requires cooperation between different communities of physicists (both theoretical and experimental). This review, prepared within the COST Action CA18108 "Quantum gravity phenomenology in the multi-messenger approach", is aimed at promoting this cooperation by giving a state-of-the art account of the interdisciplinary expertise that is needed in the effective search of quantum gravity footprints in the production, propagation and detection of cosmic messengers.

10.1016/j.ppnp.2022.103948

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Citations (308)

Detectability and parameter estimation of stellar origin black hole binaries with next generation gravitational wave detectors

Scientific Reports (2022)

Mauro Pieroni Angelo Ricciardone Enrico Barausse

We consider stellar-origin black hole binaries, which are among the main astrophysical sources for next generation gravitational wave (GW) detectors such as the Einstein Telescope (ET) and Cosmic Explorer (CE). Using population models calibrated with the most recent LIGO/Virgo results from O3b run, we show that ET and CE will be capable of detecting tens of thousands of such sources (and virtually all of those present in our past light cone up to [Formula: see text] for ET and [Formula: see text] for CE) with a signal-to-noise ratio up to several hundreds, irrespective of the detector design. When it comes to parameter estimation, we use a Fisher-matrix analysis to assess the impact of the design on the estimation of the intrinsic and extrinsic parameters. We find that the CE detector, consisting of two distinct [Formula: see text]shape interferometers, has better sky localization performance compared to ET in its triangular configuration. We also find that the network is typically capable of measuring the chirp mass, symmetric mass ratio and spins of the binary at order of [Formula: see text], [Formula: see text] and [Formula: see text] fractional error respectively. While the fractional errors for the extrinsic parameters are of order [Formula: see text] for the sky localization, luminosity distance and inclination.

Einstein Telescope

Luminosity distance

Black hole (networking)

10.1038/s41598-022-19540-7

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Citations (26)

Quest for CMB spectral distortions to probe the scalar-induced gravitational wave background interpretation of pulsar timing array data

Physical review. D/Physical review. D. (2025)

Matteo Tagliazucchi Matteo Braglia F. Finelli⋆Mauro Pieroni

Gravitational wave background

10.1103/physrevd.111.l021305

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Citations (1)

The effect of mission duration on LISA science objectives

General Relativity and Gravitation (2021)

Pau Amaro‐Seoane Manuel Arca Sedda S. Babak C. P. L. Berry Emanuele Berti

Abstract The science objectives of the LISA mission have been defined under the implicit assumption of a 4-years continuous data stream. Based on the performance of LISA Pathfinder, it is now expected that LISA will have a duty cycle of $$\approx 0.75$$ ≈ 0.75 , which would reduce the effective span of usable data to 3 years. This paper reports the results of a study by the LISA Science Group, which was charged with assessing the additional science return of increasing the mission lifetime. We explore various observational scenarios to assess the impact of mission duration on the main science objectives of the mission. We find that the science investigations most affected by mission duration concern the search for seed black holes at cosmic dawn, as well as the study of stellar-origin black holes and of their formation channels via multi-band and multi-messenger observations. We conclude that an extension to 6 years of mission operations is recommended.

10.1007/s10714-021-02889-x

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Citations (44)

Testing gravitational wave propagation with multiband detections

arXiv (Cornell University) (2022)

Tessa Baker Enrico Barausse Anson Chen Claudia de Rham Mauro Pieroni

Effective field theories (EFT) of dark energy (DE) -- built to parameterise the properties of DE in an agnostic manner -- are severely constrained by measurements of the propagation speed of gravitational waves (GW). However, GW frequencies probed by ground-based interferometers lie around the typical strong coupling scale of the EFT, and it is likely that the effective description breaks down before even reaching that scale. We discuss how this leaves the possibility that an appropriate ultraviolet completion of DE scenarios, valid at scales beyond an EFT description, can avoid present constraints on the GW speed. Instead, additional constraints in the lower frequency LISA band would be harder to escape, since the energies involved are orders of magnitude lower. By implementing a method based on GW multiband detections, we show indeed that a single joint observation of a GW150914-like event by LISA and a terrestrial interferometer would allow one to constrain the speed of light and gravitons to match to within $10^{-15}$. Multiband GW observations can therefore firmly constrain scenarios based on the EFT of DE, in a robust and unambiguous way.

10.48550/arxiv.2209.14398

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Citations (2)