Author:
Branchesi Marica,Maggiore Michele,Alonso David,Badger Charles,Banerjee Biswajit,Beirnaert Freija,Belgacem Enis,Bhagwat Swetha,Boileau Guillaume,Borhanian Ssohrab,Brown Daniel David,Leong Chan Man,Cusin Giulia,Danilishin Stefan L.,Degallaix Jerome,De Luca Valerio,Dhani Arnab,Dietrich Tim,Dupletsa Ulyana,Foffa Stefano,Franciolini Gabriele,Freise Andreas,Gemme Gianluca,Goncharov Boris,Ghosh Archisman,Gulminelli Francesca,Gupta Ish,Kumar Gupta Pawan,Harms Jan,Hazra Nandini,Hild Stefan,Hinderer Tanja,Siong Heng Ik,Iacovelli Francesco,Janquart Justin,Janssens Kamiel,Jenkins Alexander C.,Kalaghatgi Chinmay,Koroveshi Xhesika,Li Tjonnie G.F.,Li Yufeng,Loffredo Eleonora,Maggio Elisa,Mancarella Michele,Mapelli Michela,Martinovic Katarina,Maselli Andrea,Meyers Patrick,Miller Andrew L.,Mondal Chiranjib,Muttoni Niccolò,Narola Harsh,Oertel Micaela,Oganesyan Gor,Pacilio Costantino,Palomba Cristiano,Pani Paolo,Pasqualetti Antonio,Perego Albino,Périgois Carole,Pieroni Mauro,Piccinni Ornella Juliana,Puecher Anna,Puppo Paola,Ricciardone Angelo,Riotto Antonio,Ronchini Samuele,Sakellariadou Mairi,Samajdar Anuradha,Santoliquido Filippo,Sathyaprakash B.S.,Steinlechner Jessica,Steinlechner Sebastian,Utina Andrei,Van Den Broeck Chris,Zhang Teng
Abstract
AbstractThe 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 each detector has 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.
Subject
Astronomy and Astrophysics