5 research outputs found
Dark siren cosmology with binary black holes in the era of third-generation gravitational wave detectors
Third-generation (3G) gravitational wave detectors, in particular Einstein
Telescope (ET) and Cosmic Explorer (CE), will explore unprecedented cosmic
volumes in search for compact binary mergers, providing us with tens of
thousands of detections per year. In this study, we simulate and employ binary
black holes detected by 3G interferometers as dark sirens, to extract and infer
cosmological parameters by cross-matching gravitational wave data with
electromagnetic information retrieved from a simulated galaxy catalog.
Considering a standard CDM model, we apply a suitable Bayesian
framework to obtain joint posterior distributions for the Hubble constant
and the matter energy density parameter in different scenarios.
Assuming a galaxy catalog complete up to and dark sirens detected with a
network signal-to-noise ratio greater than 300, we show that a network made of
ET and two CEs can constrain () to a promising
() at confidence interval within one year of continuous
observations. Additionally, we find that most of the information on is
contained in local, single-host dark sirens, and that dark sirens at do
not substantially improve these estimates. Our results imply that a sub-percent
measure of can confidently be attained by a network of 3G detectors,
highlighting the need for characterising all systematic effects to a higher
accuracy.Comment: 23 pages, 8 figures. Major update on results, updated figures, v2
accepted for publication in PR
Science with the Einstein Telescope: a comparison of different designs
The Einstein Telescope (ET), the European project for a third-generation
gravitational-wave detector, has a reference configuration based on a
triangular shape consisting of three nested detectors with 10 km arms, where in
each arm there is a `xylophone' configuration made of an interferometer tuned
toward high frequencies, and an interferometer tuned toward low frequencies and
working at cryogenic temperature. Here, we examine the scientific perspectives
under possible variations of this reference design. We perform a detailed
evaluation of the science case for a single triangular geometry observatory,
and we compare it with the results obtained for a network of two L-shaped
detectors (either parallel or misaligned) located in Europe, considering
different choices of arm-length for both the triangle and the 2L geometries. We
also study how the science output changes in the absence of the low-frequency
instrument, both for the triangle and the 2L configurations. We examine a broad
class of simple `metrics' that quantify the science output, related to compact
binary coalescences, multi-messenger astronomy and stochastic backgrounds, and
we then examine the impact of different detector designs on a more specific set
of scientific objectives.Comment: 197 pages, 72 figure
Dark siren cosmology with binary black holes in the era of third-generation gravitational wave detectors
International audienceThird-generation (3G) gravitational wave detectors, in particular Einstein Telescope (ET) and Cosmic Explorer (CE), will explore unprecedented cosmic volumes in search for compact binary mergers, providing us with tens of thousands of detections per year. In this study, we simulate and employ binary black holes detected by 3G interferometers as dark sirens, to extract and infer cosmological parameters by cross-matching gravitational wave data with electromagnetic information retrieved from a simulated galaxy catalog. Considering a standard CDM model, we apply a suitable Bayesian framework to obtain joint posterior distributions for the Hubble constant and the matter energy density parameter in different scenarios. Assuming a galaxy catalog complete up to and dark sirens detected with a network signal-to-noise ratio greater than 300, we show that a network made of ET and two CEs can constrain () to a promising () at confidence interval within one year of continuous observations. Additionally, we find that most of the information on is contained in local, single-host dark sirens, and that dark sirens at do not substantially improve these estimates. Our results imply that a sub-percent measure of can confidently be attained by a network of 3G detectors, highlighting the need for characterising all systematic effects to a higher accuracy
Multiband gravitational wave cosmology with stellar origin black hole binaries
International audienceMassive stellar origin black hole binaries (SBHBs), originating from stars above the pair-instability mass gap, are primary candidates for multiband gravitational wave (GW) observations. Here we study the possibility to use them as effective dark standard sirens to constrain cosmological parameters. The long lasting inspiral signal emitted by these systems is accessible by the future Laser Interferometer Space Antenna (LISA), while the late inspiral and merger are eventually detected by third generation ground-based telescopes such as the Einstein Telescope (ET). The direct measurement of the luminosity distance and the sky position to the source, together with the inhomogeneous redshift distribution of possible host galaxies, allow us to infer cosmological parameters by probabilistic means. The efficiency of this statistical method relies in high parameter estimation performances. We show that this multiband approach allows a precise determination of the Hubble constant H0 with just O(10) detected sources. For selected SBHB population models, assuming 4 (10) years of LISA observations, we find that H0 is typically determined at âŒ2% (âŒ1.5%), whereas Ωm is only mildly constrained with a typical precision of 30% (20%). We discuss the origin of some outliers in our final estimates and we comment on ways to reduce their presence
The Lunar Gravitational-wave Antenna: Mission Studies and Science Case
International audienceThe Lunar Gravitational-wave Antenna (LGWA) is a proposed array of next-generation inertial sensors to monitor the response of the Moon to gravitational waves (GWs). Given the size of the Moon and the expected noise produced by the lunar seismic background, the LGWA would be able to observe GWs from about 1 mHz to 1 Hz. This would make the LGWA the missing link between space-borne detectors like LISA with peak sensitivities around a few millihertz and proposed future terrestrial detectors like Einstein Telescope or Cosmic Explorer. In this article, we provide a first comprehensive analysis of the LGWA science case including its multi-messenger aspects and lunar science with LGWA data. We also describe the scientific analyses of the Moon required to plan the LGWA mission