Black hole merger rates for LISA and LGWA from semi-analytical modelling of light seeds
Artikel i vetenskaplig tidskrift, 2026
Context. With the upcoming space- and Moon-based gravitational-wave detectors, LISA and LGWA, a new era of gravitational-wave (GW) astronomy begins, with the possibility of detecting mergers of intermediate-mass black holes (IMBHs) and supermassive black holes (SMBHs). Aims. We generated populations of synthetic black hole (BH) binaries with masses ranging from the intermediate (10(3) - 10(5) M-circle dot) to the supermassive regime (> 10(5) M-circle dot), formed through the dynamical processes of merging haloes and their host galaxies, assuming that each galaxy is initially seeded with a single black hole at its centre. We aimed to estimate the rate of these BH mergers that could be detected by LISA and LGWA. Methods. Using the PINOCCHIO cosmological simulation and a semi-analytical model based on the GAlaxy Evolution and Assembly (GAEA) framework, we constructed a population of merging BHs by implementing a 'light' seeding scheme and calculated the merging timescales using the Chandrasekhar prescription. We calculated upper and lower limits of the dynamical friction timescale by varying the mass of the infalling object to create 'pessimistic' and 'optimistic' merger rates. Results. For our synthetic population of BHs, both LGWA and LISA detect more than 15 binary IMBH mergers per year in the optimistic case, while in the pessimistic case fewer than approximately five detections would be expected over the entire lifetime of the detectors. For SMBHs, the rates are slightly lower in both cases. Most mergers below z approximate to 4 are detected in the optimistic case, although mergers beyond z = 8 are also detectable at a lower rate. Conclusions. We find that LGWA is better suited for detections of IMBH with a high signal-to-noise ratio at higher redshift, while LISA is more sensitive to massive SMBHs. Joint observations will probe the full BH mass spectrum and constrain BH formation and seeding models.
quasars: supermassive black holes
gravitational waves
galaxies: kinematics and dynamics
galaxies: halos
galaxies: interactions
stars: Population III
Författare
Jasbir Singh
Istituto nazionale di astrofisica (INAF)
Paola Severgnini
Istituto nazionale di astrofisica (INAF)
Vieri Cammelli
Universita Degli Studi Di Modena E Reggio Emilia
Alessandra De Rosa
Istituto nazionale di astrofisica (INAF)
Cristian Vignali
Universita di Bologna
Istituto nazionale di astrofisica (INAF)
Fabio Rigamonti
Istituto Nazionale di Fisica Nucleare
Universita degli Studi dell'Insubria
Istituto nazionale di astrofisica (INAF)
Rosa Valiante
Ist Nazl Astrofis
Pierluigi Monaco
Universita degli Studi di Trieste
Istituto Nazionale di Fisica Nucleare
IFPU—Institute for Fundamental Physics of the Universe
Istituto nazionale di astrofisica (INAF)
Jonathan Tan
Chalmers, Rymd-, geo- och miljövetenskap
Lorenzo Battistini
Universita degli studi - Roma Tre
Istituto nazionale di astrofisica (INAF)
Roberto Della Ceca
Istituto nazionale di astrofisica (INAF)
Jan Harms
Istituto Nazionale di Fisica Nucleare
Gran Sasso Science Institute (GSSI)
Manali Parvatikar
Universita degli Studi di Roma Tor Vergata
Istituto nazionale di astrofisica (INAF)
Astronomy and Astrophysics
0004-6361 (ISSN) 1432-0746 (eISSN)
Vol. 706 A196Massive Star Formation through the Universe (MSTAR)
Europeiska kommissionen (EU) (EC/H2020/788829), 2018-09-01 -- 2023-08-31.
Ämneskategorier (SSIF 2025)
Astronomi, astrofysik och kosmologi
DOI
10.1051/0004-6361/202556833