The missing link in gravitational-wave astronomy: discoveries waiting in the decihertz range

Author(s)

Sedda, Manuel Arca, Berry, Christopher P.L., Jani, Karan, Amaro-Seoane, Pau, Auclair, Pierre, Baird, Jonathon, Baker, Tessa, Berti, Emanuele, Breivik, Katelyn, Burrows, Adam, Caprini, Chiara, Chen, Xian, Doneva, Daniela, Ezquiaga, Jose M., Ford, K E Saavik, Katz, Michael L., Kolkowitz, Shimon, McKernan, Barry, Mueller, Guido, Nardini, Germano, Pikovski, Igor, Rajendran, Surjeet, Sesana, Alberto, Shao, Lijing, Tamanini, Nicola, Vartanyan, David, Warburton, Niels, Witek, Helvi, Wong, Kaze, Zevin, Michael

Abstract

The gravitational-wave astronomical revolution began in 2015 with LIGO’s observation of the coalescence of two stellar-mass black holes. Over the coming decades, ground-based detectors like laser interferometer gravitational-wave observatory (LIGO), Virgo and KAGRA will extend their reach, discovering thousands of stellar-mass binaries. In the 2030s, the space-based laser interferometer space antenna (LISA) will enable gravitational-wave observations of the massive black holes in galactic centres. Between ground-based observatories and LISA lies the unexplored dHz gravitational-wave frequency band. Here, we show the potential of a decihertz observatory (DO) which could cover this band, and complement discoveries made by other gravitational-wave observatories. The dHz range is uniquely suited to observation of intermediate-mass (∼102–104 M ⊙) black holes, which may form the missing link between stellar-mass and massive black holes, offering an opportunity to measure their properties. DOs will be able to detect stellar-mass binaries days to years before they merge and are observed by ground-based detectors, providing early warning of nearby binary neutron star mergers, and enabling measurements of the eccentricity of binary black holes, providing revealing insights into their formation. Observing dHz gravitational-waves also opens the possibility of testing fundamental physics in a new laboratory, permitting unique tests of general relativity (GR) and the standard model of particle physics. Overall, a DO would answer outstanding questions about how black holes form and evolve across cosmic time, open new avenues for multimessenger astronomy, and advance our understanding of gravitation, particle physics and cosmology.

Figures

Eccentricity distributions of binary black holes formed in globular clusters when observed at different gravitational-wave frequencies. Binary binary black hole mergers in globular clusters form $3$ distinct populations: binaries that are ejected from the cluster due to a strong encounter, binaries that leave a strong encounter in a hardened state and merge before the next encounter, and binaries that merge during the strong encounter itself~\citep{Samsing:2017rat,Rodriguez:2018pss,Zevin:2018kzq}. The first $2$ populations make up the broad peak at lower eccentricity, and the third results in the distribution at $e \lesssim 10^{-2}$ seen for the gravitational-wave frequencies of $f_\mathrm{ref} = 10.0~\mathrm{Hz}$ and $f_\mathrm{ref} = 1.0~\mathrm{Hz}$. At lower frequencies it is easier to distinguish between the ejected and in-cluster merger populations~\citep{DOrazio:2018jnv,Samsing:2018nxk}; the dashed and dotted green lines differentiate the ejected and in-cluster populations, respectively, at $f_\mathrm{ref} = 0.1~\mathrm{Hz}$. The peak near $e \sim 1$ in the $f_\mathrm{ref} = 10.0~\mathrm{Hz}$ histogram is populated by systems that form in-band and merge on the timescale of days--years.

Three-dimensional map illustrating the gravitational-wave strain $h$ (multiplied by distance $D$) generated by neutrino emission anisotropies $253~\mathrm{ms}$ after the SN bounce, assuming a stellar progenitor with mass $M = 19 \Ms$~\citep{Vartanyan:2020nmt}. The signal is shown for both $h_+$ (\emph{left}) and $h_\times$ (\emph{right}) polarization, and as a function of the viewing angle. Hotter colors (yellow to red; convex surfaces), indicate positive strains, whereas cooler colors (blue to yellow; concave surfaces) indicate negative strains.

Ability to detect a stochastic gravitational-wave background, characterised by the power-law sensitivity $h^2 \Omega_\mathrm{GW}(f)$~\citep{Thrane:2013oya,Caprini:2019pxz,Mohamadnejad:2019vzg}. Sensitivities are calculated assuming a $4~\mathrm{yr}$ mission with a $70\%$ efficiency, and a required signal-to-noise ratio threshold of $10$.

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