Massive black hole binaries in LISA: constraining cosmological parameters at high redshifts

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Preprint
Report number	arXiv:2312.04632
Title	Massive black hole binaries in LISA: constraining cosmological parameters at high redshifts
Author(s)	Mangiagli, Alberto (APC, Paris) ; Caprini, Chiara (U. Geneva (main) ; CERN) ; Marsat, Sylvain (L2IT, Toulouse) ; Speri, Lorenzo (Potsdam, Max Planck Inst.) ; Caldwell, Robert R. (Dartmouth Coll.) ; Tamanini, Nicola (L2IT, Toulouse)
Imprint	2023-12-07
Number of pages	33
Note	33 pages, 21 figures. Submitted to PRD. Improved text quality and added clarifications
Subject category	gr-qc ; General Relativity and Cosmology ; astro-ph.CO ; Astrophysics and Astronomy
Abstract	One of the scientific objectives of the Laser Interferometer Space Antenna (LISA) is to probe the expansion of the Universe using gravitational wave observations. Indeed, as gravitational waves from the coalescence of a massive black hole binary (MBHB) carry direct information of its luminosity distance, an accompanying electromagnetic (EM) counterpart can be used to determine its redshift. This method of $bright$$sirens$, when applied to LISA, enables one to build a gravitational Hubble diagram to high redshift. In this work, we forecast the ability of LISA-detected MBHB bright sirens to constrain cosmological models. The expected EM emission from MBHBs can be detected up to redshift $z\sim 7$ with future astronomical facilities, and the distribution of MBHBs with detectable counterpart peaks at $z\sim 2-3$. Therefore, we propose several methods to leverage the ability of LISA to constrain the expansion of the Universe at $z\sim 2-3$, a poorly charted epoch in cosmography. We find that the most promising method consists in using a model-independent approach based on a spline interpolation of the luminosity distance-redshift relation: in this case, LISA can constrain the Hubble parameter at $z\sim2-3$ with a relative precision of at least $10\%$.
Other source	Inspire
Copyright/License	preprint: (License: CC BY 4.0)

$: width=1\textwidth$ $Representation of the \hyperref[itm:bins]{\color{mycolormodel}redshift bins} and \hyperref[itm:matteronly]{\color{mycolormodel}matter-only} models. The blue, solid line corresponds to the comoving distance in the standard \lcdm Universe; the yellow, dotted-dashed line represents the matter-only approximation from Eq.~\ref{eq:matter-only} with $z_p=3$; the two red, dashed lines denote the redshift bins approach in Eq.~\ref{eq:linear_fit} for two redshift bins with $z_p=1.5$ and $z_p=3$ (black stars) \textcolor{\colorref}{and the vertical dotted-dashed grey lines visualise the boundaries of the corresponding redshift bins}. The green points show the MBHBs from a random Universe realisation, \textcolor{\colorref}{based on the astrophysical model Q3d, assuming 10 yrs of data (and therefore correspondingly of LISA mission duration),} with the respective \textcolor{\colorref}{1$\sigma$} errors bars on the redshift and comoving distance, accounting also for lensing and peculiar velocities errors (as described in Sec.~\ref{sec:cat_construction}). For the low-redshift events, the errors are smaller than the size of the dot.$ $Representation of the \hyperref[itm:bins]{\color{mycolormodel}redshift bins} and \hyperref[itm:matteronly]{\color{mycolormodel}matter-only} approximation models, according to the legend. The blue line corresponds to the comoving distance in the standard \lcdm Universe; the yellow dotted-dashed line represents the matter-only approximation from Eq.~\ref{eq:matter-only} with $z_p=3$ and the two orange dashed lines the redshift bins approach in Eq.~\ref{eq:linear_fit} for two redshift bins with $z_p=1.5$ and $z_p=3$ (black stars). Green points correspond to the MBHBs from a random realisation of Q3d with the corresponding errors on redshift and comoving distance, accounting also for lensing and peculiar velocities errors as described in Sec.~\ref{sec:cat_construction}. For low-redshift events, the errors are smaller than the size of the dot.$ Show more plots

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Record created 2023-12-21, last modified 2024-07-19

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