Cosmology with the angular cross-correlation of gravitational-wave and galaxy catalogs: Forecasts for next-generation interferometers and the Euclid survey
4 affiliations
- 1Aix-Marseille Université, Université de Toulon, CNRS, CPT
- 2CPT - Centre de Physique Théorique - UMR 7332 (Centre de Physique Théorique Campus de Luminy, Case 907 163 Avenue de Luminy 13288 Marseille cedex 9, France - France)
- 3Dipartimento di Fisica “G. Occhialini”, Universitá degli Studi di Milano-Bicocca
- 4INFN, Sezione di Milano-Bicocca
Abstract
Context. The spatial clustering of galaxies has long been a key probe of cosmology. Gravitational–wave (GW) sources, which provide direct luminosity–distance measurements, have recently emerged as a complementary tracer of large–scale structures. The cross–correlation of GW and galaxy catalogs offers a novel way to test cosmic expansion. Aims. We investigate the potential of tomographic GW–galaxy angular power spectra to constrain cosmological parameters, focusing on the Hubble constant and matter density, in the context of third–generation (3G) GW detectors combined with the Euclid survey. Methods. We constructed our forecasts using realistic GW source populations and error models calibrated on recent detector designs. We adopted a Fisher–matrix approach, marginalized over nuisance parameters including tracer biases, primordial spectrum parameters, and baryon density, and compared different survey configurations, binning schemes, and GW detector networks. Results. We find that tomographic cross–correlation can constrain H 0 at a percent or sub–percent precision, depending on the binning strategy, network configuration, and observing time. Combining galaxy autocorrelations with GW–galaxy cross–correlations improves constraints by up to a factor of ∼10 relative to either probe alone. We further show that this performance requires multiple interferometers with accurate sky localization, and we discuss the added value of spectroscopic surveys and the detectability of GW clustering bias. Conclusions. Our results demonstrate that this technique, applied to 3G GW detectors in synergy with large galaxy surveys, can deliver competitive measurements of cosmic expansion, even when marginalizing over a wide range of astrophysical and cosmological nuisance parameters.
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BibTeX
@article{pedrotti2026cosmology,
title = {{Cosmology with the angular cross-correlation of gravitational-wave and galaxy catalogs: Forecasts for next-generation interferometers and the Euclid survey}},
author = {Alessandro Pedrotti and Michele Mancarella and J. Bel and Michele Santoni and Davide Gerosa},
journal = {Astronomy and Astrophysics},
year = {2026},
month = jun,
doi = {10.1051/0004-6361/202557264},
url = {https://doi.org/10.1051/0004-6361/202557264},
note = {CC BY},
}
RIS
TY - JOUR
TI - Cosmology with the angular cross-correlation of gravitational-wave and galaxy catalogs: Forecasts for next-generation interferometers and the Euclid survey
AU - Alessandro Pedrotti
AU - Michele Mancarella
AU - J. Bel
AU - Michele Santoni
AU - Davide Gerosa
PY - 2026
DA - 2026/06/19
JO - Astronomy and Astrophysics
DO - 10.1051/0004-6361/202557264
UR - https://doi.org/10.1051/0004-6361/202557264
AB - Context. The spatial clustering of galaxies has long been a key probe of cosmology. Gravitational–wave (GW) sources, which provide direct luminosity–distance measurements, have recently emerged as a complementary tracer of large–scale structures. The cross–correlation of GW and galaxy catalogs offers a novel way to test cosmic expansion. Aims. We investigate the potential of tomographic GW–galaxy angular power spectra to constrain cosmological parameters, focusing on the Hubble constant and matter density, in the context of third–generation (3G) GW detectors combined with the Euclid survey. Methods. We constructed our forecasts using realistic GW source populations and error models calibrated on recent detector designs. We adopted a Fisher–matrix approach, marginalized over nuisance parameters including tracer biases, primordial spectrum parameters, and baryon density, and compared different survey configurations, binning schemes, and GW detector networks. Results. We find that tomographic cross–correlation can constrain H 0 at a percent or sub–percent precision, depending on the binning strategy, network configuration, and observing time. Combining galaxy autocorrelations with GW–galaxy cross–correlations improves constraints by up to a factor of ∼10 relative to either probe alone. We further show that this performance requires multiple interferometers with accurate sky localization, and we discuss the added value of spectroscopic surveys and the detectability of GW clustering bias. Conclusions. Our results demonstrate that this technique, applied to 3G GW detectors in synergy with large galaxy surveys, can deliver competitive measurements of cosmic expansion, even when marginalizing over a wide range of astrophysical and cosmological nuisance parameters.
SN - 0004-6361
SN - 1432-0746
ER -