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Exploration of features in the black hole mass spectrum inspired by non-parametric analyses of gravitational wave observations

Context: Current gravitational-wave data reveal structures in the mass function of binary compact objects. Properly modelling and deciphering such structures is the ultimate goal of gravitational-wave population analysis; in this context, non-parametric models are a powerful tool to infer the distri...

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Autori principali: Rinaldi, Stefano (Autore) , Liang, Yajie (Autore) , Demasi, Gabriele (Autore) , Mapelli, Michela (Autore) , Pozzo, Walter Del (Autore)
Natura: Article (Journal)
Lingua:inglese
Pubblicazione: October 2025
In: Astronomy and astrophysics
Year: 2025, Volume: 702, Pages: 1-8
ISSN:1432-0746
DOI:10.1051/0004-6361/202555870
Accesso online:Verlag, kostenfrei, Volltext: https://doi.org/10.1051/0004-6361/202555870
Verlag, kostenfrei, Volltext: https://www.aanda.org/articles/aa/abs/2025/10/aa55870-25/aa55870-25.html
Testo
Note sull'autore:Stefano Rinaldi, Yajie Liang, Gabriele Demasi, Michela Mapelli, and Walter Del Pozzo
Descrizione
Riassunto:Context: Current gravitational-wave data reveal structures in the mass function of binary compact objects. Properly modelling and deciphering such structures is the ultimate goal of gravitational-wave population analysis; in this context, non-parametric models are a powerful tool to infer the distribution of black holes from gravitational waves without committing to any specific functional form. - Aims: Here we aim to quantitatively corroborate the findings of non-parametric methods with parametrised models incorporating the features found in such analyses. - Methods: We propose two modifications of the currently favoured POWERLAW+PEAK model, inspired by non-parametric studies, and use them to analyse the third Gravitational Wave Transient Catalogue. - Results: Our analysis marginally supports the existence of two distinct, differently redshift-evolving subpopulations in the black hole primary mass function, and suggests that, to date, we are still unable to robustly assess the shape of the mass ratio distribution for symmetric (q > 0.7) binaries.
Descrizione del documento:Online veröffentlicht: 6. Oktober 2025
Gesehen am 20.04.2026
Descrizione fisica:Online Resource
ISSN:1432-0746
DOI:10.1051/0004-6361/202555870

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