Searcharxiv⌕ Search
Home/Archive/arXiv

arXiv · 2307.10421

Characterizing Gravitational Wave Detector Networks: From A$^\sharp$ to Cosmic Explorer

Ish Gupta·Chaitanya Afle·K. G. Arun·Ananya Bandopadhyay·Masha Baryakhtar·Sylvia Biscoveanu·Ssohrab Borhanian·Floor Broekgaarden·Alessandra Corsi·Arnab Dhani·Matthew Evans·Evan D. Hall·Otto A. Hannuksela·Keisi Kacanja·Rahul Kashyap·Sanika Khadkikar·Kevin Kuns·Tjonnie G. F. Li·Andrew L. Miller·Alexander Harvey Nitz·Benjamin J. Owen·Cristiano Palomba·Anthony Pearce·Hemantakumar Phurailatpam·Binod Rajbhandari·Jocelyn Read·Joseph D. Romano·Bangalore S. Sathyaprakash·David H. Shoemaker·Divya Singh·Salvatore Vitale·Lisa Barsotti·Emanuele Berti·Craig Cahillane·Hsin-Yu Chen·Peter Fritschel·Carl-Johan Haster·Philippe Landry·Geoffrey Lovelace·David McClelland·Bram J J Slagmolen·Joshua Smith·Marcelle Soares-Santos·Ling Sun·David Tanner·Hiro Yamamoto·Michael Zucker
View original source ↗Read source document ↗Export metadata ↓

Abstract

Gravitational-wave observations by the Laser Interferometer Gravitational-Wave Observatory (LIGO) and Virgo have provided us a new tool to explore the Universe on all scales from nuclear physics to the cosmos and have the massive potential to further impact fundamental physics, astrophysics, and cosmology for decades to come. In this paper we have studied the science capabilities of a network of LIGO detectors when they reach their best possible sensitivity, called A#, given the infrastructure in which they exist and a new generation of observatories that are factor of 10 to 100 times more sensitive (depending on the frequency), in particular a pair of L-shaped Cosmic Explorer observatories (one 40 km and one 20 km arm length) in the US and the triangular Einstein Telescope with 10 km arms in Europe. The presence of one or two A# observatories in a network containing two or one next generation observatories, respectively, will provide good localization capabilities for facilitating multimessenger astronomy and precision measurement of the Hubble parameter. Two Cosmic Explorer observatories are indispensable for achieving precise localization of binary neutron star events, facilitating detection of electromagnetic counterparts and transforming multimessenger astronomy. Their combined operation is even more important in the detection and localization of high-redshift sources, such as binary neutron stars, beyond the star-formation peak, and primordial black hole mergers, which may occur roughly 100 million years after the Big Bang. The addition of the Einstein Telescope to a network of two Cosmic Explorer observatories is critical for accomplishing all the identified science metrics. For most metrics the triple network of next generation terrestrial observatories are a factor 100 better than what can be accomplished by a network of three A# observatories.

Explore related subjects

gr-qcastro-ph.COastro-ph.HEastro-ph.IM

Keep this discovery

BibTeXRIS

Ish Gupta, Chaitanya Afle, K. G. Arun, Ananya Bandopadhyay, Masha Baryakhtar, Sylvia Biscoveanu, Ssohrab Borhanian, Floor Broekgaarden, Alessandra Corsi, Arnab Dhani, Matthew Evans, Evan D. Hall, Otto A. Hannuksela, Keisi Kacanja, Rahul Kashyap, Sanika Khadkikar, Kevin Kuns, Tjonnie G. F. Li, Andrew L. Miller, Alexander Harvey Nitz, Benjamin J. Owen, Cristiano Palomba, Anthony Pearce, Hemantakumar Phurailatpam, Binod Rajbhandari, Jocelyn Read, Joseph D. Romano, Bangalore S. Sathyaprakash, David H. Shoemaker, Divya Singh, Salvatore Vitale, Lisa Barsotti, Emanuele Berti, Craig Cahillane, Hsin-Yu Chen, Peter Fritschel, Carl-Johan Haster, Philippe Landry, Geoffrey Lovelace, David McClelland, Bram J J Slagmolen, Joshua Smith, Marcelle Soares-Santos, Ling Sun, David Tanner, Hiro Yamamoto, Michael Zucker. 2023-07-19. Characterizing Gravitational Wave Detector Networks: From A$^\sharp$ to Cosmic Explorer. https://arxiv.org/abs/2307.10421

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

Electrovacuum Black Hole Uniqueness

We prove the black hole uniqueness conjecture in the axially symmetric, stationary, electrovacuum setting, subject to the refined asymptotic analysis of the associated singular harmonic maps, which includes an analyticity hypothesis at the axes. More precisely, it is shown that any asymptotically flat solution of the Einstein--Maxwell equations in this class, with more than one black hole horizon component is either: Majumdar--Papapetrou, up to a duality rotation, in which case all logarithmic angle defects vanish, or every finite axis rod logarithmic angle defect is strictly negative and hence every interaction force is strictly attractive. The proof extends the singular harmonic map method used for vacuum Kerr uniqueness in [18].

gr-qc↗
arXiv2026

Constraining Modified Mass-to-Horizon Cosmology Through Primordial Inflationary Observables

We investigate slow-roll inflation in a modified cosmological framework inspired by a generalized mass-to-horizon relation (MHR), $M=\gamma {c^2 L^n}/{G}$, where $n$ is a real parameter and $\gamma$ a dimensional constant. Using Padmanabhan's emergence paradigm, we derive the modified Friedmann equations for a flat FRW universe and analyze the dynamics of a canonical scalar field (inflaton) under the slow-roll approximation. We study the resulting inflationary phenomenology for power-law and Starobinsky potentials. For power-law potentials, the MHR modification fails to reconcile these models with current CMB constraints on $r$ and $n_s$. In contrast, Starobinsky inflation exhibits significant sensitivity to deviations from $n=1$. A perturbative analysis ($n=1+\Delta$) yields corrections to inflationary observables. We observe that the scalar power-spectrum normalization, under a fixed-Starobinsky prescription, imposes the stringent constraint $0.960 \lesssim n \lesssim 1.040$ for $N=60$ efolds. This is considerably tighter than spectral-index bounds. Our results establish inflation, particularly Starobinsky-like models, as a sensitive probe of generalized horizon thermodynamics and departures from standard MHR scaling.

gr-qc↗
arXiv2026

Improving the Sensitivity of Gravitational Wave Detection with Weighted Conformal Prediction

In the last decade, kilometre-scale interferometric gravitational-wave detectors have observed hundreds of compact binary mergers, the majority of which are binary black holes. However, the data are noise-dominated, and multiple independent search algorithms (pipelines) are used to enhance sensitivity and improve robustness. Rather than the standard approach of selecting the most significant pipeline output, we combine the outputs from all pipelines using a conformal prediction-based framework to provide statistically rigorous confidence estimates for candidate events. While combining pipelines improves sensitivity and ranking robustness, it requires a principled statistical framework that remains valid as data properties evolve across observing runs. A key challenge is distribution shifts between simulated datasets used for training and calibration and the real, unlabelled, observations used for testing, which can invalidate coverage guarantees and bias confidence estimates. In this work, we address this challenge by incorporating likelihood-ratio reweighting into our conformal prediction framework to account for covariate shift. Using mock datasets containing simulated signals, we demonstrate that weighted conformal prediction restores well-calibrated coverage under covariate shift and increases the confidence of events near the detection threshold, recovering true signals that would otherwise be missed.

gr-qc↗