From AAS NOVA : “Jumping the Gap to Probe Large Black Holes”



10 May 2021
Susanna Kohler

Theory predicts that gravitational-wave detectors should be able to observe a population of huge black holes. A new study explores what we’ll learn from these mysterious objects and when we can hope to find them.

A Preferred Size

So-called stellar-mass black holes — the black holes probed by gravitational-wave detectors like LIGO/Virgo — can theoretically span a broad range of sizes, from just a few solar masses to hundreds of times the mass of the Sun.

The LIGO/Virgo gravitational-wave detectors have discovered signals from dozens of black-hole binaries completing their final death spirals and merging. So far, these observed primary black holes have primarily fallen into a mass range below ~45 solar masses, indicating a precipitous drop in the population of binary black holes above this mass.

Avoiding an Unstable End

Why the dearth of heavier black holes? Theorists have an explanation: the pair-instability supernova mass gap. Based on our understanding of stellar evolution, black holes in a certain mass range — roughly 50–120 solar masses — shouldn’t be able to form. This mass gap arises because the progenitor stars needed to produce black holes of this size are predicted to undergo a runaway process, eventually exploding as violent supernovae that prevent remnant black holes from forming.

The formation of black holes above ~120 solar masses, however, should still be possible — so we’d expect a population of enormous far-side-of-the-mass-gap black holes to be lurking in our galaxy and beyond. In a new study, University of Chicago (US) scientists Jose María Ezquiaga and Daniel Holz dig further into this prediction.

Hunt on the Far Side

Ezquiaga and Holz use the statistics of past black-hole binary detections and predictions of the capabilities of current and future gravitational-wave detectors to estimate what’s in store for us in terms of far-side black holes.

First, the authors show that these heavyweights would be the most massive sources detectable by LIGO/Virgo, and — if they exist — we should be able to spot up to tens of them during LIGO/Virgo’s next two observing runs (O4 and O5).

The estimated maximum number of black-hole-binary mergers detected per year for various current and upcoming ground-based gravitational-wave detectors, and in 4 years for LISA. [Adapted from Ezquiaga & Holz 2021]

What’s more, far-side binaries should also lie in the observing band of LISA, the upcoming space-based gravitational-wave mission. They may dominate the population of binaries that can be observed by both LIGO/Virgo and LISA, providing valuable information about how the merger rate for black-hole binaries changes over time.

Finally, Ezquiaga and Holz show that observations of far-side binaries with LISA, LIGO/Virgo, and the Einstein Telescope (a next-generation detector) will provide an independent measure of the expansion of the universe at different redshifts: z ~ 0.4, 0.8, and 1.5, respectively. By exploiting the upper edge of the mass gap, far-side black holes can act as standard sirens and enable precision cosmology.

Soon To Be Found?

So what’s the upshot? The outlook is good for far-side black holes!

If these heavyweights exist, we should spot them within the next couple years and they’ll be able to provide us with valuable insight into a variety of science questions. If we don’t observe any within this time frame, that also provides a powerful statement about black-hole formation, demanding new theories to explain the dearth.


“Jumping the Gap: Searching for LIGO’s Biggest Black Holes,” Jose María Ezquiaga and Daniel E. Holz 2021 ApJL 909 L23.

See the full article here .


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