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LISA (the Laser Interferometer Space Antenna) is a planned space observatory that will measure gravitational waves at far lower frequencies than ground-based detectors. That band should let it study mergers of massive black holes across cosmic time, map the extreme gravity around those black holes with small objects spiralling into them, test whether black holes match general-relativistic predictions, and search for a faint gravitational-wave background left by processes in the early Universe. LISA may also measure cosmic expansion using gravitational-wave distances. These are mission capabilities and scientific goals, not completed observations: the European Space Agency currently plans launch around 2035.
What LISA is designed to discover
LISA will listen for slow changes in spacetime that are largely inaccessible to observatories on Earth. Its planned sensitivity is approximately 0.1 millihertz to 0.1 hertz, a range suited to sources whose orbital periods are minutes to hours or whose signals evolve over months and years. ESA describes this as a complementary window to ground-based interferometers, which observe much higher-frequency events.
The observatory will consist of three spacecraft flying in a triangular formation around the Sun while trailing Earth. Each side of the triangle is planned to be 2.5 million kilometres long. Laser interferometry will compare the separations between freely falling test masses inside the spacecraft. A gravitational wave passing through the constellation will stretch one arm while compressing another by an extraordinarily small amount; the laser measurements are intended to record that changing pattern.
Because the arms are millions of kilometres long and the spacecraft operate in space, LISA can follow long-period gravitational waves before they sweep into the higher-frequency range measured by terrestrial detectors. The result is not a camera image of a black hole. It is a precisely modelled waveform from which researchers infer masses, spins, distances, orbital motion and, in some cases, the geometry of the source’s spacetime.
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ESA’s LISA mission overview and mission factsheet describe the observatory and its science objectives.
Massive black-hole mergers and the history of growth
What LISA will measure
When two massive black holes orbit one another, they lose energy through gravitational radiation and spiral together. In LISA’s band, the system can remain observable for a long time, allowing the instrument to track the gradual evolution of the orbit and the final merger. The waveform carries the masses and spins of the black holes, but the directly measured quantities are redshifted: cosmic expansion changes the signal in a way that combines source-frame mass and redshift.
Detailed waveform modelling can separate many of these effects statistically and, when an electromagnetic counterpart or another distance indicator is available, improve the redshift determination. LISA’s observations should therefore produce a population of massive-black-hole events rather than a single snapshot of one object.
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How a population becomes a formation history
The mass, spin and merger-rate distributions of many events can be compared with competing growth scenarios. For example, models in which early black-hole seeds were relatively light predict different typical masses, spins and merger histories from models that began with heavier seeds. Repeated mergers can also alter spin distributions and the timing of growth. By measuring those patterns over a range of redshifts, researchers can test which pathways are compatible with the data.
A single merger will not by itself reconstruct the entire history of black-hole growth. The inference depends on the number and quality of detections, accurate waveform models, and assumptions about how the population evolves. LISA’s value is the combination of long-duration signals and a statistically useful sample across cosmic time.
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ESA identifies massive-black-hole mergers as a core target in its science overview and explains the planned mission in its factsheet.
Extreme mass-ratio inspirals: testing gravity close to a black hole
The source
An extreme mass-ratio inspiral (EMRI) occurs when a much smaller compact object—such as a stellar-mass black hole, neutron star or white dwarf—gradually spirals into a massive black hole. The mass ratio is so large that the smaller body behaves almost like a precision probe moving through the larger object’s gravitational field.
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An EMRI can complete thousands of orbits while its signal remains in LISA’s sensitive band. Each orbit samples the central gravitational field at a slightly different radius. Small changes in the waveform encode relativistic effects such as orbital precession and the way the black hole’s spin drags spacetime around it. Long observations give the analysis many repeated measurements instead of one brief burst.
From those patterns, scientists can estimate the central object’s mass and spin and measure its quadrupole moment, a description of how its mass distribution departs from perfect spherical symmetry. General relativity predicts a specific relationship among these quantities for an astrophysical black hole. Testing that relationship is a direct probe of the black-hole spacetime, not merely a measurement of the object’s total mass.
A mismatch between the observed waveform and the general-relativistic prediction would first require checking instrumental effects, environmental influences and waveform-systematic errors. If it survived those tests, it could indicate a limitation of the theory or an object unlike the black holes described by the standard solution. ESA discusses EMRIs and the mission’s gravity tests in its 2024 LISA go-ahead announcement.
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Other compact binaries in the Milky Way
LISA will not be limited to distant massive-black-hole systems. Thousands of compact binaries in our Galaxy, especially pairs containing white dwarfs, are expected to produce persistent signals in the millihertz band. Their nearly periodic waveforms can reveal orbital periods, masses and, for suitable systems, distances.
Those measurements support questions about how stars evolve, how binary systems exchange mass, and how compact remnants form. Some binaries may be individually resolvable; a large collection of weaker systems will contribute to a combined Galactic foreground that itself is an important measurement for understanding the population.
Stellar-origin black-hole binaries can also appear in LISA’s low-frequency band while they are still widely separated. In favorable cases, a later merger could be observed at higher frequencies by a ground-based detector, creating a multiband observation. Such a joint signal would track the same system over a much larger range of orbital scales, although the number of systems suitable for this treatment is uncertain.
Searching for gravitational waves from the early Universe
What the signal would look like
Some early-Universe processes would not produce isolated, easily identifiable events. Instead, they could leave a stochastic gravitational-wave background: a persistent, statistically described superposition of waves arriving from many directions and times. LISA will search for the characteristic frequency dependence and correlation pattern of such a background.
Possible sources
ESA lists relic gravitational waves from the early evolution of the Universe among LISA’s objectives. One possible source is a first-order phase transition, in which a field changes state through expanding bubbles. Collisions and fluid motions associated with that transition could generate gravitational waves. Other theoretical mechanisms can also produce a background in the millihertz range.
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Whether LISA detects such a signal depends on the early-Universe model, the transition’s energy scale and duration, the strength of the resulting waves, and how well astrophysical foregrounds can be separated. ESA therefore presents these sources as possibilities to search for, not as guaranteed detections. A non-detection would still constrain models by ruling out portions of their predicted parameter space.
The range of candidate relic signals and the analysis issues are described in ESA’s LISA science survey.
Independent reader supportYour contribution helps us test, update, and keep practical guides available for everyone.Using gravitational waves to measure cosmic expansion
Gravitational-wave signals provide an intrinsic distance estimate because the waveform’s amplitude and evolution are set by the source’s masses and orbital dynamics. These measurements are often called standard-siren distances. They do not automatically provide a redshift, so identifying a host galaxy or using a statistical catalogue of galaxies can be important for turning distance into an expansion measurement.
LISA may use massive-black-hole mergers and other suitable sources to study how the expansion rate changes with cosmic time. The result would be a complementary distance ladder: it relies on gravity and waveform physics rather than the calibration steps used by electromagnetic standard candles. Combining LISA’s distances with redshift information from electromagnetic observations could test cosmological models and help compare independent measurements of the expansion history.
ESA explains this potential in its overview of how LISA can measure gravitational waves.
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What each source can tell us
| Source | Physical question | Primary inference |
|---|---|---|
| Massive black-hole mergers | How did massive black holes form and grow over cosmic time? | Redshifted masses, spins and population patterns that distinguish growth scenarios |
| Extreme mass-ratio inspirals | Does the strong gravitational field match general relativity? | Central mass, spin, quadrupole moment and detailed orbital waveform |
| Galactic compact binaries | How do stars and compact remnants evolve in binary systems? | Orbital periods, masses and distances for individual systems, plus a Galactic population signal |
| Early-Universe stochastic background | Did relic processes such as phase transitions generate gravitational waves? | A statistical background spectrum and constraints on early-Universe models |
| Standard-siren sources | How fast has the Universe expanded? | Gravitational-wave distances combined with host-galaxy or statistical redshifts |
Why LISA’s frequency band matters
Frequency determines which physical scale and orbital stage an observatory can see. Ground-based detectors are tuned to signals that sweep through tens to thousands of hertz during the final seconds of stellar-mass black-hole and neutron-star mergers. LISA’s approximate 0.1 millihertz-to-0.1 hertz range captures much slower systems: massive black holes with orbital periods of many minutes or longer, compact Galactic binaries, and long inspirals that may eventually become ground-based sources.
The lower band also changes how an observation is analysed. A source can be followed for months or years, allowing parameters to accumulate gradually. The spacecraft’s motion around the Sun helps encode source direction in the changing signal, while the three-arm geometry supplies multiple interferometric measurements. These features should improve sky localisation for some events, although the actual accuracy will vary with signal strength, source position and the final instrument performance.
Mission status: planned, not yet observing
LISA is a future observatory. ESA currently lists launch around 2035, a schedule that can change as design, testing and launch planning progress. On 17 June 2025, ESA announced that it and OHB System AG had signed the agreement to build the mission and that industrial development was beginning. The mission is led by ESA with NASA and an international consortium of scientists.
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Consequently, no LISA detection or LISA-measured black-hole population exists yet. Statements about event counts, early-Universe backgrounds or precision tests describe forecasts and expected capabilities. The mission’s final sensitivity, observing duration, data-analysis methods and source population will determine which forecasts are achieved.
For the latest schedule and programme milestones, consult ESA’s 17 June 2025 construction announcement and its factsheet. ESA’s science director Carole Mundell described the goal as opening “a brand-new window on the dark Universe” and testing known laws of physics under extreme conditions.
What LISA could change in astrophysics
The mission’s impact would come from combining several kinds of inference. Massive-black-hole mergers could connect black-hole demographics to galaxy evolution. EMRIs could turn individual inspirals into precision tests of strong gravity. Galactic binaries would provide a census of compact remnants in the Milky Way. A stochastic background, if detected, could reveal physics at energies and epochs inaccessible to particle accelerators. Standard-siren measurements could add an independent way to study cosmic expansion.
Those outcomes are complementary rather than interchangeable. A merger population addresses formation history; an EMRI tests the geometry around one central object; a background search tests statistical relic radiation; and a standard siren measures distance. LISA’s planned low-frequency coverage is what allows all of these questions to be pursued by one observatory.
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