Gravitational waves × HI intensity mapping: cosmological and astrophysical applications

Spinelli, M.; Raccanelli, Alvise; Boco, Lumen; Lapi, A.; Viel, Matteo

doi:10.1088/1475-7516/2022/01/004

Cited by 24 publications

(26 citation statements)

References 199 publications

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“…The cross-correlation technique and the statistical host identification will also be useful for the dark standard sirens detectable from LISA in combination with the Vera Rubin Observatory, which can observe EM counterparts at high redshift. In the future, cross-correlation of 3G detector measurements with the CMB, 21 cm and other line intensity signals will be useful to map the expansion history up to high redshift [99,375,376]. Spectral standard sirens: An alternative to bright or dark sirens is to use information about the intrinsic spectrum of GW source properties to provide a scale, and thereby calibrate the signal and allow for the inference of redshift.…”

Section: Hubble Constant Measurementmentioning

confidence: 99%

Snowmass2021 Cosmic Frontier White Paper: Fundamental Physics and Beyond the Standard Model

Berti¹,

Cardoso²,

Haiman³

et al. 2022

Preprint

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Gravitational wave detectors are formidable tools to explore strong-field gravity, especially black holes and neutron stars. These compact objects are extraordinarily efficient at producing electromagnetic and gravitational radiation. As such, they are ideal laboratories for fundamental physics and have an immense discovery potential. The detection of black hole binaries by third-generation Earth-based detectors, space-based detectors and pulsar timing arrays will provide exquisite tests of general relativity. Loud "golden" events and extreme mass-ratio inspirals can strengthen the observational evidence for horizons by mapping the exterior spacetime geometry, inform us on possible near-horizon modifications, and perhaps reveal a breakdown of Einstein's gravity. Measurements of the black-hole spin distribution and continuous gravitational-wave searches can turn black holes into efficient detectors of ultralight bosons across ten or more orders of magnitude in mass. A precise monitoring of the phase of inspiralling binaries can constrain the existence of additional propagating fields and characterize the environment in which the binaries live, bounding the local dark matter density and properties. Gravitational waves from compact binaries will probe general relativity and fundamental physics in previously inaccessible regimes, and allow us to address fundamental issues in our current understanding of the cosmos.

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Section: Hubble Constant Measurementmentioning

confidence: 99%

Snowmass2021 Cosmic Frontier White Paper: Fundamental Physics and Beyond the Standard Model

Berti¹,

Cardoso²,

Haiman³

et al. 2022

Preprint

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“…As the masses of the GW sources are redshifted (m det = (1 + z)m), one can expect to infer the redshift from the mass distribution of the GW sources, if the mass distribution of the BBHs can exhibit a universal property or at least a standardized behavior. We can break the mass-redshift degeneracy and infer the cosmic expansion history from dark standard sirens without applying the cross-correlation technique (Oguri 2016;Mukherjee & Wandelt 2018;Mukherjee et al 2020Mukherjee et al , 2021aBera et al 2020;Scelfo et al 2020;Mukherjee et al 2021b;Cañas-Herrera et al 2021;Scelfo et al 2022;Cigarrán Díaz & Mukherjee 2022;Mukherjee et al 2022) or statistical host identification technique (Schutz 1986;MacLeod & Hogan 2008;Del Pozzo 2012;Arabsalmani et al 2013;Gray et al 2020;Fishbach et al 2019;Abbott et al 2021e;Soares-Santos et al 2019;Finke et al 2021;Abbott et al 2020b;Palmese et al 2021). However, if BBHs mass distribution exhibits redshift dependence due to its intrinsic dependence on the delay time distribution, then cosmic redshifts cannot be accurately inferred (Mukherjee 2021;Ezquiaga & Holz 2022), and it can bias the results if the redshift dependence of the mass distribution is not considered.…”

Section: Introductionmentioning

confidence: 99%

Binary black holes population and cosmology in new lights: Signature of PISN mass and formation channel in GWTC-3

Karathanasis¹,

Mukherjee²,

Mastrogiovanni³

2022

Preprint

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The mass, spin, and merger rate distribution of the binary black holes (BBHs) across cosmic redshifts provide a unique way to shed light on their formation channel. Along with the redshift dependence of the BBH merger rate, the mass distribution of BBHs can also exhibit redshift dependence due to different formation channels and due to its dependence on the metallicity of the parent stars. In this work, we explore the redshift dependence of the BBH mass distribution jointly with the merger rate evolution from the third gravitational wave (GW) catalog GWTC-3 of the LIGO-Virgo-KAGRA collaboration. This analysis sheds light on multiple new aspects of the BBH formation channel and mass distribution. We obtain interesting constraints on the minimum delay time between the formation of stars and mergers of BBHs t min d = 1.95 +0.97 −0.93 Gyrs, along with a hint towards a steeper power-law form of the delay time distribution ((t d ) d ) with an index d < −1.55 at 68% C.L. The mass distribution of the BBHs agrees with a power-law form with a Gaussian peak at µ g = 40.26 +1.04 −2.32 M which agrees with the theoretical prediction of the lower edge of the PISN mass scale and differs from the previous analysis. This analysis sheds light on the lower edge of the PISN mass scale of black holes and provides hints toward the formation channel of the BBH systems that are different from the usual fiducial scenario with a power-law index d = −1. Our results are consistent with the scenarios of varying (or fixed) Hubble constant and also for events with lower matched filtering network signal to noise ratio.

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“…Since the proposed method does not rely on the cross-correlation of GW sources with EM probes, the results are not susceptible to the poor sky localization errors of GW sources. For GW sources with very good sky localizations, spatial cross-correlation with EM probes to explore the delay time would provide additional constraining power (Diaz & Mukherjee 2022;Scelfo et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Toward a Precision Measurement of Binary Black Holes Formation Channels Using Gravitational Waves and Emission Lines

Mukherjee

Dizgah

2022

ApJL

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The formation of compact objects—neutron stars, black holes, and supermassive black holes—and their connection to the chemical composition of galaxies is one of the central questions in astrophysics. We propose a novel data-driven, multi-messenger technique to address this question by exploiting the inevitable correlation between gravitational waves and atomic/molecular emission-line signals. For a fiducial probability distribution function p ( t d ) ∝ t d − κ of time delays, this method can provide a measurement of the minimum delay time of 0.5 Gyr and a power-law index of κ = 1 with a standard deviation of 0.12 (and 0.45) and 0.06 (and 0.34), respectively, from five years of LIGO–Virgo–KAGRA observations in synergy with SPHEREx line intensity mapping (and DESI emission-line galaxies). Such measurements will provide data-driven, multi-messenger constraints on the delay time distribution which is currently not well known.

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Gravitational waves × HI intensity mapping: cosmological and astrophysical applications

Cited by 24 publications

References 199 publications

Snowmass2021 Cosmic Frontier White Paper: Fundamental Physics and Beyond the Standard Model

Snowmass2021 Cosmic Frontier White Paper: Fundamental Physics and Beyond the Standard Model

Binary black holes population and cosmology in new lights: Signature of PISN mass and formation channel in GWTC-3

Toward a Precision Measurement of Binary Black Holes Formation Channels Using Gravitational Waves and Emission Lines

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