PoS - Proceedings of Science
Volume 414 - 41st International Conference on High Energy physics (ICHEP2022) - Astroparticle Physics and Cosmology
Cosmology with massive black hole binary mergers in the LISA era.
A. Mangiagli*, C. Caprini, M. Volonteri, S. Marsat, S. Vergani, N. Tamanini and L. Speri
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Pre-published on: October 28, 2022
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Abstract
In $\sim2034$ the Laser Interferometer Space Antenna (LISA) will detect the coalescence of massive black hole binaries (MBHBs) from $10^5$ to $10^7 {\, \rm M}_\odot$ up to $z\sim10$. The gravitational wave (GW) signal is expected to be accompanied by a powerful electromagnetic (EM) counterpart, from radio to X-ray, generated by the gas accreting on the binary.
If LISA locates the MBHB merger within an error box $<10 \, \rm deg^2$, EM telescopes can be pointed in the same portion of the sky to detect the emission from the last stages of the MBHB orbits or the very onset of the nuclear activity, paving the way to test the nature of gas in a rapidly changing space-time. Moreover, an EM counterpart will allow independent measurements of the source redshift which, combined with the luminosity distance estimate from the GW signal, will lead to exquisite tests on the expansion of the Universe as well as on the velocity propagation of GWs.
Here, I present some recent results on the standard sirens rates detectable jointly by LISA and EM facilities. We combine state-of-the-art models for the galaxy formation and evolution, realistic modeling of the EM counterpart and Bayesian tools to perform the parameter estimation of the GW event as well as of the cosmological parameters.
We explore three different astrophysical scenarios employing different seed formation (light or heavy seeds) and delay-time models, in order to have realistic predictions on the expected number of events. We estimate the detectability of the source in terms of its signal-to-noise ratio in LISA and perform parameter estimation, focusing especially on the sky localization of the source. Exploiting the additional information from the astrophysical models, such as the amount of accreted gas and BH spins, we model the expected EM counterpart to the GW signal in soft X-ray, optical and radio.
In our standard scenario, we predict $\sim14$ EM counterparts over 4 yr of LISA time mission and $\sim6$ ($\sim20$) in the pessimistic (optimistic) one.
We also explore the impact of absorption from the surrounding gas both for optical and X-ray emission: assuming typical hydrogen and metal column density distribution, we estimate only $\sim3$ EM counterparts in 4 yr in the standard scenario.
DOI: https://doi.org/10.22323/1.414.0125
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